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    <title>topic Re: The beginning? in The Round Table</title>
    <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/166726#M282</link>
    <description>&lt;P class="mce-p"&gt;Chronology of the universeFrom Wikipedia&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&amp;nbsp;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/File:CMB_Timeline300_no_WMAP.jpg" title="Enlarge"&gt;This &lt;STRONG&gt;chronology of the universe&lt;/STRONG&gt; describes &lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&amp;nbsp;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/File:CMB_Timeline300_no_WMAP.jpg" title="Enlarge"&gt;the history and future of the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Universe" title="Universe"&gt;universe according to Big Bang cosmology, the prevailing &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Scientific_model" title="Scientific model"&gt;scientific model of how the universe came into being and developed over time, using the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Cosmology" title="Cosmology"&gt;cosmological time parameter of &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Comoving_coordinates" title="Comoving coordinates"&gt;comoving coordinates. The instant in which the universe is thought to have begun rapidly expanding from a &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Gravitational_singularity" title="Gravitational singularity"&gt;singularity is known as the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Big_Bang" title="Big Bang"&gt;Big Bang. As of 2013, this expansion is estimated to have begun &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Planck_(spacecraft)#2013_data_release" title="Planck (spacecraft)"&gt;13.798 ± 0.037 &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/1,000,000,000_(number)" title="1,000,000,000 (number)"&gt;billion years ago.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-planck_cosmological_parameters-1"&gt;[1] It is convenient to divide the evolution of the universe so far into three phases.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-planck_cosmological_parameters-1"&gt;The very earliest universe was so hot, or energetic, that initially no particles existed or could exist (except perhaps in the most fleeting sense), and the forces we see around us today were &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Grand_unified_theories" title="Grand unified theories"&gt;believed to be merged into one &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Grand_unification_epoch" title="Grand unification epoch"&gt;unified force. &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Metric_expansion_of_space" title="Metric expansion of space"&gt;Space itself expanded during an &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Inflationary_epoch" title="Inflationary epoch"&gt;inflationary epoch due to the immensity of the energies involved. Gradually the immense energies cooled - still to a temperature inconceivably hot compared to any we see around us now, but sufficiently to allow forces to gradually undergo &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Symmetry_breaking" title="Symmetry breaking"&gt;symmetry breaking, a kind of repeated condensation from one status quo to another, leading finally to the separation of the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Strong_force" title="Strong force"&gt;strong force from the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Electroweak_force" title="Electroweak force"&gt;electroweak force and &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Baryogenesis" title="Baryogenesis"&gt;the first particles.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Baryogenesis" title="Baryogenesis"&gt;In the second phase, this &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Quark-gluon_plasma" title="Quark-gluon plasma"&gt;quark-gluon plasma universe then cooled further, the current fundamental forces we know take their present forms through further symmetry breaking - notably the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Electroweak_symmetry_breaking" title="Electroweak symmetry breaking"&gt;breaking of electroweak symmetry - and the full range of complex and composite particles we see around us today became possible, leading to a matter dominated universe, the first neutral atoms (almost all of them &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Hydrogen" title="Hydrogen"&gt;hydrogen), and the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Cosmic_microwave_background_radiation" title="Cosmic microwave background radiation"&gt;cosmic microwave background radiation we can detect today. Modern &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/High-energy_physics" title="High-energy physics"&gt;high energy &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Particle_physics" title="Particle physics"&gt;particle physics theories are satisfactory at these energy levels, and so physicists believe they have a good understanding of this and subsequent development of the fundamental universe around us. Because of these changes, space had also become largely transparent to light and other &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Electromagnetic_energy" title="Electromagnetic energy"&gt;electromagnetic energy, rather than "foggy", by the end of this phase.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Electromagnetic_energy" title="Electromagnetic energy"&gt;The third phase started with a universe whose fundamental particles and forces were as we know them, and witnessed &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Structure_formation" title="Structure formation"&gt;the emergence of large scale stable structures, such as the earliest &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Star" title="Star"&gt;stars, &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Quasar" title="Quasar"&gt;quasars, &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Galaxy" title="Galaxy"&gt;galaxies, &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Clusters_of_galaxies" title="Clusters of galaxies"&gt;clusters of galaxies and &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Supercluster" title="Supercluster"&gt;superclusters, and the development of these to create the kind of universe we see today. Some researchers call the development of all this physical structure over billions of years "cosmic evolution." Other, more interdisciplinary, researchers refer to "cosmic evolution" as the entire scenario of growing complexity from big bang to humankind, thereby incorporating biology and culture into a grand unified view of all complex systems in the universe to date.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-2"&gt;[2]&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-2"&gt;Beyond the present day, scientists anticipate that the Earth will cease to support life in about a billion years, and will be drawn into the Sun in about 5 billion years. On a far longer timescale, the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Graphical_timeline_of_the_Stelliferous_Era" title="Graphical timeline of the Stelliferous Era"&gt;Stelliferous Era will end as stars eventually die and fewer are born to replace them, leading to a darkening universe. Various theories suggest a number of subsequent possibilities. If particles such as &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Proton" title="Proton"&gt;protons are unstable then eventually matter may evaporate into low level energy in a kind of &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Entropy" title="Entropy"&gt;entropy related &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Heat_death_of_the_Universe" title="Heat death of the Universe"&gt;heat death. Alternatively the universe may collapse in a &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Big_crunch" title="Big crunch"&gt;big crunch, although current data shows the rate of expansion is still increasing. If this is correct then it may end in a "big freeze" as matter and energy become very thinly spread and cool down. Alternative suggestions include a &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/False_vacuum" title="False vacuum"&gt;false vacuum catastrophe or a &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Big_Rip" title="Big Rip"&gt;Big Rip as possible ends to the universe.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Big_Rip" title="Big Rip"&gt;Contents &amp;nbsp;[&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#"&gt;hide]&amp;nbsp;&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Very_early_universe"&gt;1 Very early universe &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Planck_epoch"&gt;1.1 Planck epoch&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Grand_unification_epoch"&gt;1.2 Grand unification epoch&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Electroweak_epoch"&gt;1.3 Electroweak epoch &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Inflationary_epoch"&gt;1.3.1 Inflationary epoch&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Baryogenesis"&gt;1.3.2 Baryogenesis&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Early_universe"&gt;2 Early universe &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Supersymmetry_breaking_.28speculative.29"&gt;2.1 Supersymmetry breaking (speculative)&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Electroweak_symmetry_breaking_and_the_quark_epoch"&gt;2.2 Electroweak symmetry breaking and the quark epoch&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Hadron_epoch"&gt;2.3 Hadron epoch&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Lepton_epoch"&gt;2.4 Lepton epoch&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Photon_epoch"&gt;2.5 Photon epoch &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Nucleosynthesis"&gt;2.5.1 Nucleosynthesis&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Matter_domination"&gt;2.5.2 Matter domination&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Recombination"&gt;2.5.3 Recombination&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Dark_Ages"&gt;2.5.4 Dark Ages&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Structure_formation"&gt;3 Structure formation &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Reionization"&gt;3.1 Reionization&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Formation_of_stars"&gt;3.2 Formation of stars&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Formation_of_galaxies"&gt;3.3 Formation of galaxies&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Formation_of_groups.2C_clusters_and_superclusters"&gt;3.4 Formation of groups, clusters and superclusters&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Formation_of_the_Solar_System"&gt;3.5 Formation of the Solar System&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Today"&gt;3.6 Today&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Ultimate_fate_of_the_universe"&gt;4 Ultimate fate of the universe &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Fate_of_the_Solar_system:_1_to_5_billion_years"&gt;4.1 Fate of the Solar system: 1 to 5 billion years&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Big_freeze:_1014_years_and_beyond"&gt;4.2 Big freeze: 1014 years and beyond&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Big_Crunch:_100.2B_billion_years_from_now"&gt;4.3 Big Crunch: 100+ billion years from now&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Big_Rip:_20.2B_billion_years_from_now"&gt;4.4 Big Rip: 20+ billion years from now&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Vacuum_metastability_event"&gt;4.5 Vacuum metastability event&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#Heat_death:_10150.2B_years_from_now"&gt;4.6 Heat death: 10150+ years from now&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#See_also"&gt;5 See also&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#References"&gt;6 References&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#External_links"&gt;7 External linksVery early universe [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=1" title="Edit section: Very early universe"&gt;edit]&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=1" title="Edit section: Very early universe"&gt;All ideas concerning the very early universe (&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Cosmogony" title="Cosmogony"&gt;cosmogony) are speculative. No accelerator experiments have yet probed energies of sufficient magnitude to provide any experimental insight into the behavior of matter at the energy levels that prevailed during this period. Proposed scenarios differ radically. Some examples are the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Hartle%E2%80%93Hawking_initial_state" title="Hartle–Hawking initial state"&gt;Hartle–Hawking initial state, &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/String_landscape" title="String landscape"&gt;string landscape, &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Cosmic_inflation" title="Cosmic inflation"&gt;brane inflation, &lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=String_gas_cosmology&amp;amp;action=edit&amp;amp;redlink=1" title="String gas cosmology (page does not exist)"&gt;string gas cosmology, and the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Ekpyrotic_universe" title="Ekpyrotic universe"&gt;ekpyrotic universe. Some of these are mutually compatible, while others are not.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Ekpyrotic_universe" title="Ekpyrotic universe"&gt;Planck epoch [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=2" title="Edit section: Planck epoch"&gt;edit]&lt;I&gt;Up to 10–43 seconds after the Big Bang&lt;/I&gt;Main article: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Planck_epoch" title="Planck epoch"&gt;Planck epoch&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Planck_epoch" title="Planck epoch"&gt;The Planck epoch is an era in traditional (non-inflationary) big bang cosmology in which the temperature is high enough that the four fundamental forces—&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Electromagnetism" title="Electromagnetism"&gt;electromagnetism, &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Gravitation" title="Gravitation"&gt;gravitation, &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Weak_interaction" title="Weak interaction"&gt;weak nuclear interaction, and &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Strong_interaction" title="Strong interaction"&gt;strong nuclear interaction—are all unified in one fundamental force. Little is understood about physics at this temperature, and different theories propose different scenarios. Traditional big bang cosmology predicts a &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Gravitational_singularity" title="Gravitational singularity"&gt;gravitational singularity before this time, but this theory is based on &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/General_relativity" title="General relativity"&gt;general relativity and is expected to break down due to &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Quantum_mechanics" title="Quantum mechanics"&gt;quantum effects. Physicists hope that proposed theories of &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Quantum_gravity" title="Quantum gravity"&gt;quantum gravitation, such as &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/String_theory" title="String theory"&gt;string theory, &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Loop_quantum_gravity" title="Loop quantum gravity"&gt;loop quantum gravity, and &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Causal_sets" title="Causal sets"&gt;causal sets, will eventually lead to a better understanding of this epoch.[&lt;I&gt;&lt;/I&gt;&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Loop_quantum_gravity" title="Loop quantum gravity"&gt;&lt;I&gt;&lt;/I&gt;&lt;/A&gt;&lt;I&gt;&lt;A href="https://en.wikipedia.org/wiki/Wikipedia:Citation_needed" title="Wikipedia:Citation needed"&gt;citation needed&lt;/A&gt;&lt;/I&gt;&lt;A href="https://en.wikipedia.org/wiki/Wikipedia:Citation_needed" title="Wikipedia:Citation needed"&gt;] In inflationary cosmology, times prior to the end of inflation (roughly 10−32 seconds after the Big Bang) do not follow the traditional big bang timeline. The universe before the end of inflation is a near-vacuum with a very low temperature, and persists for much longer than 10−32 second. Times from the end of inflation are based on the big bang time of the non-inflationary big bang model, not on the actual age of the universe at that time, which cannot be determined in inflationary cosmology. Thus, in inflationary cosmology there is no Planck epoch in the traditional sense, though similar conditions may have prevailed in a pre-inflationary era of the universe.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Wikipedia:Citation_needed" title="Wikipedia:Citation needed"&gt;Grand unification epoch [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=3" title="Edit section: Grand unification epoch"&gt;edit]&lt;I&gt;Between 10–43 seconds and 10–36 seconds after the Big Bang&lt;/I&gt;&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-autogenerated1-3"&gt;[3]Main article: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Grand_unification_epoch" title="Grand unification epoch"&gt;Grand unification epoch&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Grand_unification_epoch" title="Grand unification epoch"&gt;As the universe &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Metric_expansion_of_space" title="Metric expansion of space"&gt;expands and cools, it crosses transition temperatures at which forces separate from each other. These are &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Phase_transition" title="Phase transition"&gt;phase transitions much like &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Condensation" title="Condensation"&gt;condensation and &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Freezing" title="Freezing"&gt;freezing. The grand unification epoch begins when gravitation separates from the other forces of nature, which are collectively known as &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Gauge_theory" title="Gauge theory"&gt;gauge forces. The non-gravitational physics in this epoch would be described by a so-called &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Grand_unified_theory" title="Grand unified theory"&gt;grand unified theory (GUT). The grand unification epoch ends when the GUT forces further separate into the strong and electroweak forces. This transition should produce &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Magnetic_monopoles" title="Magnetic monopoles"&gt;magnetic monopoles in large quantities, which are not observed. The lack of magnetic monopoles was one problem solved by the introduction of inflation.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Magnetic_monopoles" title="Magnetic monopoles"&gt;In modern inflationary cosmology, the traditional grand unification epoch, like the Planck epoch, does not exist, though similar conditions likely would have existed in the universe prior to inflation.[&lt;I&gt;&lt;/I&gt;&lt;/A&gt;&lt;I&gt;&lt;A href="https://en.wikipedia.org/wiki/Wikipedia:Citation_needed" title="Wikipedia:Citation needed"&gt;citation needed&lt;/A&gt;&lt;/I&gt;&lt;A href="https://en.wikipedia.org/wiki/Wikipedia:Citation_needed" title="Wikipedia:Citation needed"&gt;][&lt;I&gt;&lt;/I&gt;&lt;/A&gt;&lt;I&gt;&lt;A href="https://en.wikipedia.org/wiki/Wikipedia:Please_clarify" title="Wikipedia:Please clarify"&gt;further explanation needed&lt;/A&gt;&lt;/I&gt;&lt;A href="https://en.wikipedia.org/wiki/Wikipedia:Please_clarify" title="Wikipedia:Please clarify"&gt;]&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Wikipedia:Please_clarify" title="Wikipedia:Please clarify"&gt;Electroweak epoch [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=4" title="Edit section: Electroweak epoch"&gt;edit]&lt;I&gt;Between 10–36 seconds (or the end of inflation) and 10–12 seconds after the Big Bang&lt;/I&gt;&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-autogenerated1-3"&gt;[3]Main article: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Electroweak_epoch" title="Electroweak epoch"&gt;Electroweak epoch&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Electroweak_epoch" title="Electroweak epoch"&gt;In traditional big bang cosmology, the Electroweak epoch begins 10−36 seconds after the Big Bang, when the temperature of the universe is low enough (1028 K) to separate the strong force from the electroweak force (the name for the unified forces of &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Electromagnetism" title="Electromagnetism"&gt;electromagnetism and the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Weak_interaction" title="Weak interaction"&gt;weak interaction). In inflationary cosmology, the electroweak epoch begins when the inflationary epoch ends, at roughly 10−32 seconds.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Weak_interaction" title="Weak interaction"&gt;Inflationary epoch [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=5" title="Edit section: Inflationary epoch"&gt;edit]&lt;I&gt;Unknown duration, ending 10–32(?) seconds after the Big Bang&lt;/I&gt;Main article: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Inflationary_epoch" title="Inflationary epoch"&gt;Inflationary epoch&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Inflationary_epoch" title="Inflationary epoch"&gt;Cosmic inflation is an era of accelerating expansion produced by a hypothesized field called the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Inflaton" title="Inflaton"&gt;inflaton, which would have properties similar to the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Higgs_field" title="Higgs field"&gt;Higgs field and &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Dark_energy" title="Dark energy"&gt;dark energy. While decelerating expansion magnifies deviations from homogeneity, making the universe more chaotic, accelerating expansion makes the universe more homogeneous. A sufficiently long period of inflationary expansion in our past could explain the high degree of homogeneity that is observed in the universe today at large scales, even if the state of the universe before inflation was highly disordered.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Dark_energy" title="Dark energy"&gt;Inflation ends when the inflaton field decays into ordinary particles in a process called "reheating", at which point ordinary Big Bang expansion begins. The time of reheating is usually quoted as a time "after the Big Bang". This refers to the time that would have passed in traditional (non-inflationary) cosmology between the Big Bang singularity and the universe dropping to the same temperature that was produced by reheating, even though, in inflationary cosmology, the traditional Big Bang did not occur.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Dark_energy" title="Dark energy"&gt;According to the simplest inflationary models, inflation ended at a temperature corresponding to roughly 10−32 seconds after the Big Bang. As explained above, this does not imply that the inflationary era lasted less than 10−32 seconds. In fact, in order to explain the observed homogeneity of the universe, the duration must be longer than 10−32 seconds. In inflationary cosmology, the earliest meaningful time "after the Big Bang" is the time of the end of inflation.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Dark_energy" title="Dark energy"&gt;Baryogenesis [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=6" title="Edit section: Baryogenesis"&gt;edit]Main article: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Baryogenesis" title="Baryogenesis"&gt;Baryogenesis&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Baryogenesis" title="Baryogenesis"&gt;There is currently insufficient observational evidence to explain why the universe contains far more &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Baryon" title="Baryon"&gt;baryons than &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Antimatter" title="Antimatter"&gt;antibaryons. A candidate explanation for this phenomenon must allow the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Sakharov_conditions" title="Sakharov conditions"&gt;Sakharov conditions to be satisfied at some time after the end of &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Cosmological_inflation" title="Cosmological inflation"&gt;cosmological inflation. While &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Particle_physics" title="Particle physics"&gt;particle physics suggests asymmetries under which these conditions are met, these asymmetries are too small empirically to account for the observed baryon-antibaryon asymmetry of the universe.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Particle_physics" title="Particle physics"&gt;Early universe [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=7" title="Edit section: Early universe"&gt;edit]&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/File:Cosmic_History_020622_b.jpg" title="Enlarge"&gt; Cosmic History&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/File:Cosmic_History_020622_b.jpg" title="Enlarge"&gt;After cosmic inflation ends, the universe is filled with a &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Quark%E2%80%93gluon_plasma" title="Quark–gluon plasma"&gt;quark–gluon plasma. From this point onwards the physics of the early universe is better understood, and less speculative.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Quark%E2%80%93gluon_plasma" title="Quark–gluon plasma"&gt;Supersymmetry breaking (speculative) [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=8" title="Edit section: Supersymmetry breaking (speculative)"&gt;edit]Main article: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Supersymmetry_breaking" title="Supersymmetry breaking"&gt;Supersymmetry breaking&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Supersymmetry_breaking" title="Supersymmetry breaking"&gt;If &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Supersymmetry" title="Supersymmetry"&gt;supersymmetry is a property of our universe, then it must be broken at an energy that is no lower than 1 &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/TeV" title="TeV"&gt;TeV, the electroweak symmetry scale. The masses of particles and their &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Superpartner" title="Superpartner"&gt;superpartners would then no longer be equal, which could explain why no superpartners of known particles have ever been observed.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Superpartner" title="Superpartner"&gt;Electroweak symmetry breaking and the quark epoch [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=9" title="Edit section: Electroweak symmetry breaking and the quark epoch"&gt;edit]&lt;I&gt;Between 10–12 seconds and 10–6 seconds after the Big Bang&lt;/I&gt;Main articles: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Electroweak_symmetry_breaking" title="Electroweak symmetry breaking"&gt;Electroweak symmetry breaking and &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Quark_epoch" title="Quark epoch"&gt;Quark epoch&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Quark_epoch" title="Quark epoch"&gt;As the universe's temperature falls below a certain very high energy level, it is believed that the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Higgs_field" title="Higgs field"&gt;Higgs field spontaneously acquires a &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Vacuum_expectation_value" title="Vacuum expectation value"&gt;vacuum expectation value, which &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Electroweak_symmetry_breaking" title="Electroweak symmetry breaking"&gt;breaks electroweak gauge symmetry. (If the Higgs field does not exist then a similar effect must occur, but with &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Higgsless_model" title="Higgsless model"&gt;some other cause). This has two related effects:&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Higgsless_model" title="Higgsless model"&gt;The weak force and electromagnetic force, and their respective &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Boson" title="Boson"&gt;bosons (the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/W_and_Z_bosons" title="W and Z bosons"&gt;W and Z bosons and &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Photon" title="Photon"&gt;photon) manifest differently in the present universe, with different ranges;Via the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Higgs_mechanism" title="Higgs mechanism"&gt;Higgs mechanism, all &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Elementary_particle" title="Elementary particle"&gt;elementary particles interacting with the Higgs field become massive, having been massless at higher energy levels.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Elementary_particle" title="Elementary particle"&gt;At the end of this epoch, the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Fundamental_interactions" title="Fundamental interactions"&gt;fundamental interactions of &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Gravitation" title="Gravitation"&gt;gravitation, &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Electromagnetism" title="Electromagnetism"&gt;electromagnetism, the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Strong_interaction" title="Strong interaction"&gt;strong interaction and the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Weak_interaction" title="Weak interaction"&gt;weak interaction have now taken their present forms, and fundamental particles have mass, but the temperature of the universe is still too high to allow quarks to bind together to form hadrons.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Weak_interaction" title="Weak interaction"&gt;Hadron epoch [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=10" title="Edit section: Hadron epoch"&gt;edit]&lt;I&gt;Between 10–6 seconds and 1 second after the Big Bang&lt;/I&gt;Main article: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Hadron_epoch" title="Hadron epoch"&gt;Hadron epoch&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Hadron_epoch" title="Hadron epoch"&gt;The quark-gluon plasma that composes the universe cools until &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Hadron" title="Hadron"&gt;hadrons, including baryons such as &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Proton" title="Proton"&gt;protons and &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Neutron" title="Neutron"&gt;neutrons, can form. At approximately 1 second after the Big Bang &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Neutrino" title="Neutrino"&gt;neutrinos &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Neutrino_decoupling" title="Neutrino decoupling"&gt;decouple and begin traveling freely through space. This &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Cosmic_neutrino_background" title="Cosmic neutrino background"&gt;cosmic neutrino background, while unlikely to ever be observed in detail since the neutrino energies are very low, is analogous to the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Cosmic_microwave_background" title="Cosmic microwave background"&gt;cosmic microwave background that was emitted much later. (See above regarding the quark-gluon plasma, under the String Theory epoch). However there is strong indirect evidence that the cosmic neutrino background exists, both from &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Big_Bang_nucleosynthesis" title="Big Bang nucleosynthesis"&gt;Big Bang nucleosynthesis predictions of the Helium abundance, and from anisotropies in the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Cosmic_microwave_background" title="Cosmic microwave background"&gt;cosmic microwave background&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Cosmic_microwave_background" title="Cosmic microwave background"&gt;Lepton epoch [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=11" title="Edit section: Lepton epoch"&gt;edit]&lt;I&gt;Between 1 second and 10 seconds after the Big Bang&lt;/I&gt;Main article: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Lepton_epoch" title="Lepton epoch"&gt;Lepton epoch&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Lepton_epoch" title="Lepton epoch"&gt;The majority of hadrons and anti-hadrons annihilate each other at the end of the hadron epoch, leaving &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Lepton" title="Lepton"&gt;leptons and anti-leptons dominating the mass of the universe. Approximately 10 seconds after the Big Bang the temperature of the universe falls to the point at which new lepton/anti-lepton pairs are no longer created and most leptons and anti-leptons are eliminated in &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Annihilation" title="Annihilation"&gt;annihilation reactions, leaving a small residue of leptons.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-4"&gt;[4]&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-4"&gt;Photon epoch [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=12" title="Edit section: Photon epoch"&gt;edit]&lt;I&gt;Between 10 seconds and 380,000 years after the Big Bang&lt;/I&gt;Main article: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Photon_epoch" title="Photon epoch"&gt;Photon epoch&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Photon_epoch" title="Photon epoch"&gt;After most leptons and anti-leptons are annihilated at the end of the lepton epoch the energy of the universe is dominated by &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Photon" title="Photon"&gt;photons. These photons are still interacting frequently with charged protons, electrons and (eventually) &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Atomic_nucleus" title="Atomic nucleus"&gt;nuclei, and continue to do so for the next 380,000 years.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Atomic_nucleus" title="Atomic nucleus"&gt;Nucleosynthesis [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=13" title="Edit section: Nucleosynthesis"&gt;edit]&lt;I&gt;Between 3 minutes and 20 minutes after the Big Bang&lt;/I&gt;&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-5"&gt;[5]Main article: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Big_Bang_nucleosynthesis" title="Big Bang nucleosynthesis"&gt;Big Bang nucleosynthesis&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Big_Bang_nucleosynthesis" title="Big Bang nucleosynthesis"&gt;During the photon epoch the temperature of the universe falls to the point where atomic nuclei can begin to form. Protons (hydrogen ions) and neutrons begin to combine into atomic nuclei in the process of &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Nuclear_fusion" title="Nuclear fusion"&gt;nuclear fusion. Free neutrons combine with protons to form deuterium. Deuterium rapidly fuses into helium-4. Nucleosynthesis only lasts for about seventeen minutes, since the temperature and density of the universe has fallen to the point where nuclear fusion cannot continue. By this time, all neutrons have been incorporated into helium nuclei. This leaves about three times more hydrogen than helium-4 (by mass) and only trace quantities of other nuclei.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Nuclear_fusion" title="Nuclear fusion"&gt;Matter domination [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=14" title="Edit section: Matter domination"&gt;edit]&lt;I&gt;70,000 years after the Big Bang&lt;/I&gt;&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=14" title="Edit section: Matter domination"&gt;At this time, the densities of non-relativistic matter (atomic nuclei) and relativistic radiation (photons) are equal. The &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Jeans_length" title="Jeans length"&gt;Jeans length, which determines the smallest structures that can form (due to competition between gravitational attraction and pressure effects), begins to fall and perturbations, instead of being wiped out by &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Free-streaming" title="Free-streaming"&gt;free-streaming &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Radiation" title="Radiation"&gt;radiation, can begin to grow in amplitude.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Radiation" title="Radiation"&gt;According to &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/%CE%9BCDM" title="ΛCDM"&gt;ΛCDM, at this stage, &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Cold_dark_matter" title="Cold dark matter"&gt;cold dark matter dominates, paving the way for gravitational collapse to amplify the tiny inhomogeneities left by cosmic inflation, making dense regions denser and rarefied regions more rarefied. However, because present theories as to the nature of dark matter are inconclusive, there is as yet no consensus as to its origin at earlier times, as currently exist for baryonic matter.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Cold_dark_matter" title="Cold dark matter"&gt;Recombination [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=15" title="Edit section: Recombination"&gt;edit]&lt;I&gt;ca. 377,000 years after the Big Bang&lt;/I&gt;Main article: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Recombination_(cosmology)" title="Recombination (cosmology)"&gt;Recombination (cosmology)&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/File:Ilc_9yr_moll4096.png" title="Enlarge"&gt; 9 year &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/WMAP" title="WMAP"&gt;WMAP data (2012) shows the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Cosmic_microwave_background_radiation" title="Cosmic microwave background radiation"&gt;cosmic microwave background radiation variations throughout the Universe from our perspective, though the actual variations are much smoother than the diagram suggests.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-Space-20121221-6"&gt;[6]&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-arXiv-20121220-7"&gt;[7]&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-arXiv-20121220-7"&gt;Hydrogen and helium &lt;I&gt;&lt;/I&gt;&lt;/A&gt;&lt;I&gt;&lt;A href="https://en.wikipedia.org/wiki/Atom" title="Atom"&gt;atoms&lt;/A&gt;&lt;/I&gt;&lt;A href="https://en.wikipedia.org/wiki/Atom" title="Atom"&gt; begin to form as the density of the universe falls. This is thought to have occurred about 377,000 years after the Big Bang.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-8"&gt;[8] Hydrogen and helium are at the beginning ionized, i.e., no electrons are bound to the nuclei, which (containing positively charged protons) are therefore electrically charged (+1 and +2 respectively). As the universe cools down, the electrons get captured by the ions, forming electrically neutral atoms. This process is relatively fast (actually faster for the helium than for the hydrogen) and is known as recombination.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-9"&gt;[9] At the end of recombination, most of the protons in the universe are bound up in neutral atoms. Therefore, the photons' &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Mean_free_path" title="Mean free path"&gt;mean free path becomes effectively infinite and the photons can now travel freely (see &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Thomson_scattering" title="Thomson scattering"&gt;Thomson scattering): the universe has become transparent. This cosmic event is usually referred to as &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Decoupling#Physical_cosmology" title="Decoupling"&gt;decoupling.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Decoupling#Physical_cosmology" title="Decoupling"&gt;The photons present at the time of decoupling are the same photons that we see in the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Cosmic_microwave_background" title="Cosmic microwave background"&gt;cosmic microwave background (CMB) radiation, after being greatly cooled by the expansion of the Universe. Around the same time, existing &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Pressure_wave" title="Pressure wave"&gt;pressure waves within the electron-baryon &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Plasma_(physics)" title="Plasma (physics)"&gt;plasma-known as &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Baryon_acoustic_oscillations" title="Baryon acoustic oscillations"&gt;baryon acoustic oscillations- became embedded in the distribution of matter as it condensed, giving rise to a very slight preference in distribution of large scale objects. Therefore the cosmic microwave background is a picture of the universe at the end of this epoch including the tiny fluctuations generated during &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Inflation_(cosmology)" title="Inflation (cosmology)"&gt;inflation (see diagram), and the spread of objects such as galaxies in the universe is an indication of the scale and size of the universe as it developed over time.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-10"&gt;[10]&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-10"&gt;Dark Ages [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=16" title="Edit section: Dark Ages"&gt;edit]See also: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Hydrogen_line" title="Hydrogen line"&gt;Hydrogen line&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Hydrogen_line" title="Hydrogen line"&gt;Before &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Decoupling#Physical_cosmology" title="Decoupling"&gt;decoupling occurs, most of the photons in the universe are interacting with electrons and protons in the photon–baryon fluid. The universe is opaque or "foggy" as a result. There is light but not light we could observe through telescopes. The baryonic matter in the universe consisted of ionized plasma, and it only became neutral when it gained free electrons during "recombination," thereby releasing the photons creating the CMB. When the photons were released (or decoupled) the universe became transparent. At this point the only radiation emitted is the 21&amp;nbsp;cm spin &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Hydrogen_line" title="Hydrogen line"&gt;line of neutral hydrogen. There is currently an &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/LOFAR" title="LOFAR"&gt;observational effort underway to detect this faint radiation, as it is in principle an even more powerful tool than the cosmic microwave background for studying the early universe. The Dark Ages are currently thought to have lasted between 150 million to 800 million years after the Big Bang. The October 2010 discovery of &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/UDFy-38135539" title="UDFy-38135539"&gt;UDFy-38135539, the first observed galaxy to have existed during the following &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Reionization" title="Reionization"&gt;reionization epoch, gives us a window into these times. The galaxy earliest in this period observed and thus also the most distant galaxy ever observed is currently on the record of Leiden University's Richard J. Bouwens and Garth D. Illingsworth from UC Observatories/Lick Observatory. They found the galaxy &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/UDFj-39546284" title="UDFj-39546284"&gt;UDFj-39546284 to be at a time some 480 million years after the Big Bang or about halfway through the Cosmic Dark Ages at a distance of about 13.2 billion &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Light-years" title="Light-years"&gt;light-years. More recently, the UDFj-39546284 galaxy was found to be around "380 million years" after the Big Bang and at a distance of 13.37 billion light-years.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-Space-20121212-11"&gt;[11]&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-Space-20121212-11"&gt;Structure formation [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=17" title="Edit section: Structure formation"&gt;edit]See also: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Large-scale_structure_of_the_cosmos" title="Large-scale structure of the cosmos"&gt;Large-scale structure of the cosmos&amp;nbsp;and &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Structure_formation" title="Structure formation"&gt;Structure formation&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/File:Hubble_ultra_deep_field.jpg" title="Enlarge"&gt; The &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Hubble_Ultra_Deep_Field" title="Hubble Ultra Deep Field"&gt;Hubble Ultra Deep Fields often showcase galaxies from an ancient era that tell us what the early Stelliferous Age was like.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/File:Hubble_-_infant_galaxy.jpg" title="Enlarge"&gt; Another Hubble image shows an infant galaxy forming nearby, which means this happened very recently on the cosmological timescale. This shows that new galaxy formation in the Universe is still occurring.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/File:Hubble_-_infant_galaxy.jpg" title="Enlarge"&gt;Structure formation in the big bang model proceeds hierarchically, with smaller structures forming before larger ones. The first structures to form are &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Quasar" title="Quasar"&gt;quasars, which are thought to be bright, early &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Active_galaxies" title="Active galaxies"&gt;active galaxies, and &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Population_III_stars" title="Population III stars"&gt;population III stars. Before this epoch, the evolution of the universe could be understood through linear cosmological &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Perturbation_theory" title="Perturbation theory"&gt;perturbation theory: that is, all structures could be understood as small deviations from a perfect homogeneous universe. This is computationally relatively easy to study. At this point non-linear structures begin to form, and the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Computational_problem" title="Computational problem"&gt;computational problem becomes much more difficult, involving, for example, &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/N-body_simulation" title="N-body simulation"&gt;&lt;I&gt;N&lt;/I&gt;-body simulations with billions of particles.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/N-body_simulation" title="N-body simulation"&gt;Reionization [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=18" title="Edit section: Reionization"&gt;edit]&lt;I&gt;150 million to 1 billion years after the Big Bang&lt;/I&gt;See also: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Reionization" title="Reionization"&gt;Reionization&amp;nbsp;and &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/21_centimeter_radiation" title="21 centimeter radiation"&gt;21 centimeter radiation&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/21_centimeter_radiation" title="21 centimeter radiation"&gt;The first stars and quasars form from gravitational collapse. The intense radiation they emit reionizes the surrounding universe. From this point on, most of the universe is composed of &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Plasma_(physics)" title="Plasma (physics)"&gt;plasma.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Plasma_(physics)" title="Plasma (physics)"&gt;Formation of stars [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=19" title="Edit section: Formation of stars"&gt;edit]See also: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Star_formation" title="Star formation"&gt;Star formation&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Star_formation" title="Star formation"&gt;The first stars, most likely &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Population_III" title="Population III"&gt;Population III stars, form and start the process of turning the light elements that were formed in the Big Bang (hydrogen, helium and lithium) into heavier elements. However, as yet there have been no observed Population III stars, and understanding of them is currently based on computational models of their formation and evolution.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-12"&gt;[12]&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-12"&gt;Formation of galaxies [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=20" title="Edit section: Formation of galaxies"&gt;edit]See also: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Galaxy_formation_and_evolution" title="Galaxy formation and evolution"&gt;Galaxy formation and evolution&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Galaxy_formation_and_evolution" title="Galaxy formation and evolution"&gt;Large volumes of matter collapse to form a galaxy. &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Population_II" title="Population II"&gt;Population II stars are formed early on in this process, with &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Population_I" title="Population I"&gt;Population I stars formed later.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Population_I" title="Population I"&gt;Johannes Schedler's project has identified a quasar CFHQS 1641+3755 at 12.7 billion light-years away,&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-13"&gt;[13] when the Universe was just 7% of its present age.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-13"&gt;On July 11, 2007, using the 10-metre Keck II telescope on Mauna Kea, Richard Ellis of the California Institute of Technology at Pasadena and his team found six star forming galaxies about 13.2 billion light years away and therefore created when the universe was only 500 million years old.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-14"&gt;[14] Only about 10 of these extremely early objects are currently known.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-15"&gt;[15]&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-15"&gt;The &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Hubble_Ultra_Deep_Field" title="Hubble Ultra Deep Field"&gt;Hubble Ultra Deep Field shows a number of small galaxies merging to form larger ones, at 13 billion light years, when the Universe was only 5% its current age.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-16"&gt;[16]&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-16"&gt;Based upon the emerging science of &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Nucleocosmochronology" title="Nucleocosmochronology"&gt;nucleocosmochronology, the Galactic thin disk of the Milky Way is estimated to have been formed 8.8 ± 1.7 billion years ago.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-17"&gt;[17]&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-17"&gt;Formation of groups, clusters and superclusters [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=21" title="Edit section: Formation of groups, clusters and superclusters"&gt;edit]See also: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Large-scale_structure_of_the_cosmos" title="Large-scale structure of the cosmos"&gt;Large-scale structure of the cosmos&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;Gravitational attraction pulls galaxies towards each other to form groups, clusters and superclusters.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Large-scale_structure_of_the_cosmos" title="Large-scale structure of the cosmos"&gt;Formation of the Solar System [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=22" title="Edit section: Formation of the Solar System"&gt;edit]&lt;I&gt;9 billion years after the Big Bang&lt;/I&gt;Main article: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Formation_and_evolution_of_the_Solar_System" title="Formation and evolution of the Solar System"&gt;Formation and evolution of the Solar System&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Formation_and_evolution_of_the_Solar_System" title="Formation and evolution of the Solar System"&gt;The &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Solar_System" title="Solar System"&gt;Solar System began forming about 4.6 billion years ago, or about 9 billion years after the Big Bang. A molecular cloud made mostly of hydrogen and traces of other elements began to collapse, forming a large sphere in the center which would become the Sun, as well as a surrounding disk. The surrounding accretion disk would coalesce into a multitude of smaller objects that would become planets, asteroids, and comets. The Sun is a late-generation star, and the Solar System incorporates matter created by previous generations of stars.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Solar_System" title="Solar System"&gt;Today [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=23" title="Edit section: Today"&gt;edit]&lt;I&gt;13.8 billion years after the Big Bang&lt;/I&gt;&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=23" title="Edit section: Today"&gt;The Big Bang is estimated to have occurred about 13.8 billion years ago.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-18"&gt;[18] Since the expansion of the universe appears to be accelerating, the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Observable_universe#Large-scale_structure" title="Observable universe"&gt;cosmic web is likely to be the largest structure that will ever form in the universe. The present accelerated expansion prevents any more inflationary structures entering the horizon and prevents new gravitationally bound structures from forming.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Observable_universe#Large-scale_structure" title="Observable universe"&gt;Ultimate fate of the universe [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=24" title="Edit section: Ultimate fate of the universe"&gt;edit]Main article: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Ultimate_fate_of_the_universe" title="Ultimate fate of the universe"&gt;Ultimate fate of the universe&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;As with interpretations of what happened in the very early universe, advances in fundamental physics are required before it will be possible to know the ultimate fate of the universe with any certainty. Below are some of the main possibilities.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Ultimate_fate_of_the_universe" title="Ultimate fate of the universe"&gt;Fate of the Solar system: 1 to 5 billion years [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=25" title="Edit section: Fate of the Solar system: 1 to 5 billion years"&gt;edit]Main articles: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Formation_and_evolution_of_the_Solar_System#Future" title="Formation and evolution of the Solar System"&gt;Formation and evolution of the Solar System#Future, &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Stability_of_the_Solar_System" title="Stability of the Solar System"&gt;Stability of the Solar System, &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Future_of_the_Earth#Solar_evolution" title="Future of the Earth"&gt;Future of the Earth#Solar evolution, and &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Red_giant#The_Sun_as_a_red_giant" title="Red giant"&gt;Red giant#The Sun as a red giant&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/File:Sun_red_giant.svg" title="Enlarge"&gt; Relative size of our Sun as it is now (inset) compared to its estimated future size as a red giant&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/File:Sun_red_giant.svg" title="Enlarge"&gt;Over a timescale of a billion years or more, the Earth and Solar System are unstable. Earth's existing &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Biosphere" title="Biosphere"&gt;biosphere is expected to vanish in about a billion years, as the Sun's heat production gradually increases to the point that liquid water and life are unlikely;&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-Schroder2008-19"&gt;[19] the Earth's magnetic fields, axial tilt and atmosphere are subject to long term change; and the Solar System itself is &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chaos_theory" title="Chaos theory"&gt;chaotic over million- and billion-year timescales;&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-laskar94-20"&gt;[20] Eventually in around 5.4&amp;nbsp;billion years from now, the core of the Sun will become hot enough to trigger hydrogen fusion in its surrounding shell.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-Schroder2008-19"&gt;[19] This will cause the outer layers of the star to expand greatly, and the star will enter a phase of its life in which it is called a &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Red_giant" title="Red giant"&gt;red giant.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-FOOTNOTEZeilikGregory1998320.E2.80.93321-21"&gt;[21]&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-22"&gt;[22] Within 7.5&amp;nbsp;billion years, the Sun will have expanded to a radius of 1.2&amp;nbsp;AU—256 times its current size, and studies announced in 2008 show that due to &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Roche_limit" title="Roche limit"&gt;tidal interaction between Sun and Earth, Earth would actually fall back into a lower orbit, and get engulfed and incorporated inside the Sun before the Sun reaches its largest size, despite the Sun losing about 38% of its mass.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-23"&gt;[23] The Sun itself will continue to exist for many billions of years, passing through &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Formation_and_evolution_of_the_Solar_System" title="Formation and evolution of the Solar System"&gt;a number of phases, and eventually (if nothing else changes) ending up as a long-lived &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/White_dwarf" title="White dwarf"&gt;white dwarf. Eventually, after billions more years, the Sun will finally cease to shine altogether, becoming a &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Black_dwarf" title="Black dwarf"&gt;black dwarf.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-Fontaine2001-24"&gt;[24]&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-Fontaine2001-24"&gt;Big freeze: 1014 years and beyond [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=26" title="Edit section: Big freeze: 1014 years and beyond"&gt;edit]Main articles: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Future_of_an_expanding_universe" title="Future of an expanding universe"&gt;Future of an expanding universe and &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Heat_death_of_the_universe" title="Heat death of the universe"&gt;Heat death of the universe&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Heat_death_of_the_universe" title="Heat death of the universe"&gt;This scenario is generally considered to be the most likely,[&lt;I&gt;&lt;/I&gt;&lt;/A&gt;&lt;I&gt;&lt;A href="https://en.wikipedia.org/wiki/Wikipedia:Citation_needed" title="Wikipedia:Citation needed"&gt;citation needed&lt;/A&gt;&lt;/I&gt;&lt;A href="https://en.wikipedia.org/wiki/Wikipedia:Citation_needed" title="Wikipedia:Citation needed"&gt;] as it occurs if the universe continues expanding as it has been. Over a time scale on the order of 1014 years or less, existing &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Star" title="Star"&gt;stars burn out, stars cease to be created, and the universe goes dark.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-dying-25"&gt;[25],&amp;nbsp;§IID. Over a much longer time scale in the eras following this, the galaxy evaporates as the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Stellar_remnants" title="Stellar remnants"&gt;stellar remnants comprising it escape into space, and black holes evaporate via &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Hawking_radiation" title="Hawking radiation"&gt;Hawking radiation.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-dying-25"&gt;[25],&amp;nbsp;§III,&amp;nbsp;§IVG. In some &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Grand_unified_theories" title="Grand unified theories"&gt;grand unified theories, &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Proton_decay" title="Proton decay"&gt;proton decay after at least 1034 years will convert the remaining interstellar gas and stellar remnants into leptons (such as positrons and electrons) and photons. Some positrons and electrons will then recombine into photons.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-dying-25"&gt;[25],&amp;nbsp;§IV,&amp;nbsp;§VF. In this case, the universe has reached a high-&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Entropy" title="Entropy"&gt;entropy state consisting of a bath of particles and low-energy radiation. It is not known however whether it eventually achieves &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Thermodynamic_equilibrium" title="Thermodynamic equilibrium"&gt;thermodynamic equilibrium.&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-dying-25"&gt;[25],&amp;nbsp;§VIB,&amp;nbsp;VID.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Chronology_of_the_universe#cite_note-dying-25"&gt;Big Crunch: 100+ billion years from now [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=27" title="Edit section: Big Crunch: 100+ billion years from now"&gt;edit]See also: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Big_Crunch" title="Big Crunch"&gt;Big Crunch&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Big_Crunch" title="Big Crunch"&gt;If the energy density of &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Dark_energy" title="Dark energy"&gt;dark energy were negative or the universe were &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Shape_of_the_Universe" title="Shape of the Universe"&gt;closed, then it would be possible that the expansion of the universe would reverse and the universe would contract towards a hot, dense state. This is a required element of &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Oscillatory_universe" title="Oscillatory universe"&gt;oscillatory universe scenarios, such as the &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Cyclic_model" title="Cyclic model"&gt;cyclic model, although a Big Crunch does not necessarily imply an oscillatory Universe. Current observations suggest that this model of the universe is unlikely to be correct, and the expansion will continue or even accelerate.&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Cyclic_model" title="Cyclic model"&gt;Big Rip: 20+ billion years from now [&lt;/A&gt;&lt;A href="https://en.wikipedia.org/w/index.php?title=Chronology_of_the_universe&amp;amp;action=edit&amp;amp;section=28" title="Edit section: Big Rip: 20+ billion years from now"&gt;edit]See also: &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Big_Rip" title="Big Rip"&gt;Big Rip&lt;/A&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="https://en.wikipedia.org/wiki/Big_Rip" title="Big Rip"&gt;This scenario is possible only if the energy density of &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Dark_energy" title="Dark energy"&gt;dark energy actually increases without limit over time.[&lt;I&gt;&lt;/I&gt;&lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Big_Rip" title="Big Rip"&gt;&lt;I&gt;&lt;/I&gt;&lt;/A&gt;&lt;I&gt;&lt;A href="https://en.wikipedia.org/wiki/Wikipedia:Citation_needed" title="Wikipedia:Citation needed"&gt;citation needed&lt;/A&gt;&lt;/I&gt;&lt;A href="https://en.wikipedia.org/wiki/Wikipedia:Citation_needed" title="Wikipedia:Citation needed"&gt;] Such dark energy is called &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Phantom_energy" title="Phantom energy"&gt;phantom energy and is unlike any known kind of energy. In this case, the expansion rate of the universe will increase without limit. Gravitationally bound systems, such as clusters of galaxies, galaxies, and ultimately the Solar System will be torn apart. Eventually the expansion will be so rapid as to overcome the electromagnetic forces holding molecules and atoms together. Finally even atomic nuclei will be torn apart and the universe as we know it will end in an unusual kind of &lt;/A&gt;&lt;A href="https://en.wikipedia.org/wiki/Gravitational_singularity" title="Gravitational singularity"&gt;gravitational singularity. At the time of this singul&lt;/A&gt;&lt;/P&gt;</description>
    <pubDate>Thu, 30 May 2013 06:08:55 GMT</pubDate>
    <dc:creator>Anonymous</dc:creator>
    <dc:date>2013-05-30T06:08:55Z</dc:date>
    <item>
      <title>The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161153#M4</link>
      <description>&lt;P class="mce-p"&gt;OK, so "They" say "everything" began with the Big Bang.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;Fair enough, it was quite something and happened faster than the blink of an eye?&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;"They" also say nothing can travel faster than light?&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;If that's so, how can "They" view light which "began" shortly after the Big Bang?&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;http://www.bbc.co.uk/news/science-environment-19728375&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;We are "here", they're viewing light from a heck of a long way away, such light will have taken billions of years to get here even at approximately 186,000 miles per second.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;So how did we get out "here", so far from that light when it was Starlight so long ago?&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;OK, were we able to get to the source of that light in an instant, we'd find it was probably no longer there but we are billions of miles from where that light was so how come the matter from which our Solar System was formed got sooooo far away from the Stars they're no "seeing"?&lt;/P&gt;</description>
      <pubDate>Wed, 26 Sep 2012 13:14:48 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161153#M4</guid>
      <dc:creator>cee-dee</dc:creator>
      <dc:date>2012-09-26T13:14:48Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161192#M5</link>
      <description>&lt;P class="mce-p"&gt;This is one of my all time favourite topics unfortunately, my little brain cannot and never will be able to comprehend or even visualise the sheer vastness of time and space.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;All we can ever learn about our universe is what we have here on our habitable rock to make sense of it all and until our scientists find a fuelling method to propel space craft to the outer limits of the universe and beyond or, in this case, develop further our telescopes, I will never know unless, an extra terrestrial being visits us and tells us otherwise that we have got our sums wrong and it’s all an optical illusion. :^O&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;This is an age old question and I will be enthralled to read other’s responses.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;</description>
      <pubDate>Wed, 26 Sep 2012 15:53:10 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161192#M5</guid>
      <dc:creator>mitzigirl_123</dc:creator>
      <dc:date>2012-09-26T15:53:10Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161223#M6</link>
      <description>&lt;P class="mce-p"&gt;http://en.wikipedia.org/wiki/Redshift&lt;/P&gt;</description>
      <pubDate>Wed, 26 Sep 2012 15:56:33 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161223#M6</guid>
      <dc:creator>sir_arthur_strebe-grebling</dc:creator>
      <dc:date>2012-09-26T15:56:33Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161236#M7</link>
      <description>&lt;P class="mce-p"&gt;Sir-A&amp;nbsp; &lt;IMG src="http://www.freesmileys.org/smileys/smiley-shocked017.gif" border="0" alt="Smiley" /&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;</description>
      <pubDate>Wed, 26 Sep 2012 16:45:30 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161236#M7</guid>
      <dc:creator>mitzigirl_123</dc:creator>
      <dc:date>2012-09-26T16:45:30Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161259#M8</link>
      <description>&lt;P class="mce-p"&gt;mitzi, I think that's one of the problems, it is an age old question. It also requires a massive amount of thought - which change as new info comes to light - and knowledge, neither of which I can manage these days...&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;This is pretty cool though...&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;http://www.bbc.co.uk/news/science-environment-19728375#&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;</description>
      <pubDate>Wed, 26 Sep 2012 17:16:54 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161259#M8</guid>
      <dc:creator>lhasa.two</dc:creator>
      <dc:date>2012-09-26T17:16:54Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161273#M9</link>
      <description>&lt;P class="mce-p"&gt;Errrrrrrmmmmmmmmmmm, I'm puzzled.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;There's a link in my OP, has it disappeared in to Scotch mist or has that rascally Mitzi pinched it?&lt;/P&gt;</description>
      <pubDate>Wed, 26 Sep 2012 17:43:47 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161273#M9</guid>
      <dc:creator>cee-dee</dc:creator>
      <dc:date>2012-09-26T17:43:47Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161300#M10</link>
      <description>&lt;P class="mce-p"&gt;It's all relative CD&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;Imagine a light source travelling away from you at half the speed of light.&amp;nbsp; As far as you are concerned light being emitted from that object is travelling at the speed of light whether or not it is the light from the object coming towards you or travelling away from you.&amp;nbsp; What would be different though if you could observe the light being emitted from you by the object would be time.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;So although the photons are travelling at the speed of light the time they woul take to reach you is much longer.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;Have a read of this&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;http://www.costellospaceart.com/html/time_and_the_speed_of_light.html&lt;/P&gt;</description>
      <pubDate>Wed, 26 Sep 2012 20:03:03 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161300#M10</guid>
      <dc:creator>upthecreekyetagain</dc:creator>
      <dc:date>2012-09-26T20:03:03Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161305#M11</link>
      <description>&lt;P class="mce-p"&gt;Right, I read it all but the question isn't answered.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;The Big Bang happened OK? "Stuff" went in all directions?&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;If Einstein is right (?) things with mass cannot travel as fast as the speed of light never mind faster.....&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;Soooo, how come the "stuff" we and all that we know are made of got so far away from the point of the Big Bang (and just where WAS it?) so quickly? So fast that we've got so far away from "other stuff" that the light from that other stuff took 13.2 billion years to reach us?&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;Those Stars made from that "other stuff" are probably not there now anyway. When they "look back" further and see light from even further away and from so long ago, surely that reinforces my question as to how we came to be made of "stuff" so far away from that "other stuff" (from which they'll then be seeing light) if the Big Bang didn't propel stuff &lt;SPAN style="text-decoration: underline;"&gt;with mass&lt;/SPAN&gt; &lt;STRONG&gt;faster&lt;/STRONG&gt; than the speed of light?&lt;/P&gt;</description>
      <pubDate>Wed, 26 Sep 2012 20:46:06 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161305#M11</guid>
      <dc:creator>cee-dee</dc:creator>
      <dc:date>2012-09-26T20:46:06Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161319#M12</link>
      <description>&lt;P class="mce-p"&gt;Sorry, I'm not understanding your problem.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;The universe is about 14 billion years old, so it is not surprising that light from the most distant objects is taking 13.2 billion years to get here.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;These objects now have mass, but they didn't at the instant of the BIg Bang.&lt;/P&gt;</description>
      <pubDate>Wed, 26 Sep 2012 21:03:42 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161319#M12</guid>
      <dc:creator>sir_arthur_strebe-grebling</dc:creator>
      <dc:date>2012-09-26T21:03:42Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161335#M13</link>
      <description>&lt;P class="mce-p"&gt;&lt;STRONG&gt;If Einstein is right (?) things with mass cannot travel as fast as the speed of light never mind faster.....&lt;/STRONG&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;That's not actually what he proposed.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;SPAN style="text-decoration: underline;"&gt;Relative to your position&lt;/SPAN&gt; an object cannot travel faster than the speed of light.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;Remember speed is a combination of distance and time.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;You could have an object travelling away from your left at 3/4 the speed of light and one away from your right at 3/4 speed of light.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;However if you were on the object to your left the one travelling away to the right wouldn't be travelling away from you at one and half times the speed of light but at the speed of light.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;Time on the object moving to the left is not the same as on the "stationary" object nor on the one moving to the right.&lt;/P&gt;</description>
      <pubDate>Wed, 26 Sep 2012 21:21:45 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161335#M13</guid>
      <dc:creator>upthecreekyetagain</dc:creator>
      <dc:date>2012-09-26T21:21:45Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161348#M14</link>
      <description>&lt;P class="mce-p"&gt;The "objects" are made of "stuff" with mass, it must therefore have had mass "in the beginning".&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;I don't think anyone has "explained" yet how something without mass can, after travelling through "space" somehow gain mass?&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;If it IS possible for something without mass to gain mass, how come all the "stuff" &lt;STRONG&gt;&lt;EM&gt;without&lt;/EM&gt;&lt;/STRONG&gt; mass hasn't yet gained mass?&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;You see, when people can't explain something, they fall back on "it happened". Failing that, it's on with some other "invention" to explain away the fact that "they" don't know.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;The Singularity was supposed to exist at the beginning of the Universe but later it was stated that there was no Singularity at the beginning of the Universe.Hmmmmmm?&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;The Big Bang was supposed to have infinate density. To have density you have to have mass? Therefore whatever was propelled "out" at the time of the Big Bang had mass and "stuff" with mass can't travel as fast as the speed of light?&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;It seems an unfortunate "scientific term" because the Singularity was something coined by a science fiction writer.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;Perhaps science fiction isn't so far from fact after all and one day it &lt;STRONG&gt;will&lt;/STRONG&gt; be possible to travel at Warp Speed?&lt;/P&gt;</description>
      <pubDate>Wed, 26 Sep 2012 21:26:00 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161348#M14</guid>
      <dc:creator>cee-dee</dc:creator>
      <dc:date>2012-09-26T21:26:00Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161378#M15</link>
      <description>&lt;P class="mce-p"&gt;&lt;/P&gt;&lt;BLOCKQUOTE&gt;&lt;TABLE border="1"&gt;&lt;TBODY&gt;&lt;TR&gt;&lt;TD&gt;&lt;P&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;The "objects" are made of "stuff" with mass, it must therefore have had mass "in the beginning".&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&amp;nbsp;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;I don't think anyone has "explained" yet how something without mass can, after travelling through "space" somehow gain mass?&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&amp;nbsp;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;If it IS possible for something without mass to gain mass, how come all the "stuff" &lt;STRONG&gt;&lt;EM&gt;without&lt;/EM&gt;&lt;/STRONG&gt; mass hasn't yet gained mass?&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&amp;nbsp;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;You see, when people can't explain something, they fall back on "it happened". Failing that, it's on with some other "invention" to explain away the fact that "they" don't know.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&amp;nbsp;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;The Singularity was supposed to exist at the beginning of the Universe but later it was stated that there was no Singularity at the beginning of the Universe.Hmmmmmm?&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&amp;nbsp;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;The Big Bang was supposed to have infinate density. To have density you have to have mass? Therefore whatever was propelled "out" at the time of the Big Bang had mass and "stuff" with mass can't travel as fast as the speed of light?&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&amp;nbsp;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;It seems an unfortunate "scientific term" because the Singularity was something coined by a science fiction writer.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&amp;nbsp;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;Perhaps science fiction isn't so far from fact after all and one day it &lt;STRONG&gt;will&lt;/STRONG&gt; be possible to travel at Warp Speed?&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;/P&gt;&lt;/TD&gt;&lt;/TR&gt;&lt;/TBODY&gt;&lt;/TABLE&gt;&lt;/BLOCKQUOTE&gt;&lt;P&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&amp;nbsp;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&amp;nbsp;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;A href="http://www.youtube.com/watch?v=XBvR9CCLo1o"&gt;http://www.youtube.com/watch?v=XBvR9CCLo1o&lt;/A&gt;&lt;/P&gt;</description>
      <pubDate>Wed, 26 Sep 2012 21:30:43 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161378#M15</guid>
      <dc:creator>*forum*decorum*</dc:creator>
      <dc:date>2012-09-26T21:30:43Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161392#M16</link>
      <description>&lt;P class="mce-p"&gt;UTCYA. Now in your link, we had Bill and Mary and a game of table tennis. The stationary observer was supposed to view the ball at 100MPH.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;I think if you put that to a practical test Bill would observe the ball travelling at 10MPH, the same speed that Mary saw it.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;It seems to me that the writer has fallen for the same assumption as when two cars, both travelling at 50MPH collide, the effect is the same as one car hitting a brick wall at 100MPH which is not so.&lt;/P&gt;</description>
      <pubDate>Wed, 26 Sep 2012 21:33:30 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161392#M16</guid>
      <dc:creator>cee-dee</dc:creator>
      <dc:date>2012-09-26T21:33:30Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161408#M17</link>
      <description>&lt;P class="mce-p"&gt;CD - Bill on the platform would see the ball travelling at 100MPH.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;The train is moving to his left at 90MPH and the ball is going 10MPH faster than the train.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;Your analogy of the car is not appropriate although it is worth mentioning that the effect of one car travelling at 100MPH hitting a stationary car would be the same as two cars both travelling at 50MPH hitting each other or indeed one travelling at 80MPH and the other at 20MPH.&lt;/P&gt;</description>
      <pubDate>Wed, 26 Sep 2012 21:49:58 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161408#M17</guid>
      <dc:creator>upthecreekyetagain</dc:creator>
      <dc:date>2012-09-26T21:49:58Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161429#M18</link>
      <description>&lt;P class="mce-p"&gt;So if the ball was hit the other way, Bill would "see" the ball travelling at 80MPH?&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;It's been proven by practical test with decelerometers that that two cars colliding head on at 50MPH did NOT have the same effect as crashing one car in to a brick wall at 100MPH.&lt;/P&gt;</description>
      <pubDate>Wed, 26 Sep 2012 22:26:09 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161429#M18</guid>
      <dc:creator>cee-dee</dc:creator>
      <dc:date>2012-09-26T22:26:09Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161448#M19</link>
      <description>&lt;P class="mce-p"&gt;&lt;/P&gt;&lt;BLOCKQUOTE&gt;&lt;TABLE border="1"&gt;&lt;TBODY&gt;&lt;TR&gt;&lt;TD&gt;&lt;P&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;So if the ball was hit the other way, Bill would "see" the ball travelling at 80MPH?&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;It's been proven by practical test with decelerometers that that two cars colliding head on at 50MPH did NOT have the same effect as crashing one car in to a brick wall at 100MPH.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;/P&gt;&lt;/TD&gt;&lt;/TR&gt;&lt;/TBODY&gt;&lt;/TABLE&gt;&lt;/BLOCKQUOTE&gt;&lt;P&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;Yes&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;Comparing two cars colliding with each other and one car colliding with a brickwall is not comparing like with like.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;A car travelling at 50MPH colliding with a brick wall travelling towards it at 50MPH would have the same consequences as a car hitting a stationary wall at 100MPH &lt;span class="lia-unicode-emoji" title=":winking_face:"&gt;😉&lt;/span&gt;&lt;/P&gt;</description>
      <pubDate>Wed, 26 Sep 2012 23:49:58 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161448#M19</guid>
      <dc:creator>upthecreekyetagain</dc:creator>
      <dc:date>2012-09-26T23:49:58Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161467#M20</link>
      <description>&lt;P class="mce-p"&gt;Heck creeky, you keep late hours.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;I'm sorry but you're completely wrong.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;It's been tried practically by crashing (scrap) cars of the same make and model in to each other both at 50MPH, then one in to a brick wall at 50MPH.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;The damage and deceleration was &lt;STRONG&gt;exactly&lt;/STRONG&gt; the same.&lt;/P&gt;</description>
      <pubDate>Thu, 27 Sep 2012 09:09:23 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161467#M20</guid>
      <dc:creator>cee-dee</dc:creator>
      <dc:date>2012-09-27T09:09:23Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161485#M21</link>
      <description>&lt;P class="mce-p"&gt;&lt;/P&gt;&lt;BLOCKQUOTE&gt;&lt;TABLE border="1"&gt;&lt;TBODY&gt;&lt;TR&gt;&lt;TD&gt;&lt;P&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;Heck creeky, you keep late hours.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;I'm sorry but you're completely wrong.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;It's been tried practically by crashing (scrap) cars of the same make and model in to each other both at 50MPH, then one in to a brick wall at 50MPH.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;The damage and deceleration was &lt;STRONG&gt;exactly&lt;/STRONG&gt; the same.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;&lt;/P&gt;&lt;/TD&gt;&lt;/TR&gt;&lt;/TBODY&gt;&lt;/TABLE&gt;&lt;/BLOCKQUOTE&gt;&lt;P&gt;&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;Of course it is - or very similar - simple Newtonian physics.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;But as I said, you are not comparing like with like.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;To make a true comparison you would have to compare a car travelling at 50MPH &lt;SPAN style="text-decoration: underline;"&gt;hitting a wall also travelling at 50MPH &lt;/SPAN&gt;- the consequences of such a collision would be the same as a car hitting a stationary brick wall at 100MPH&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;OR&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt;Two cars, both travelling at 50MPH in a head on collision compared to a car travelling at 100MPH &lt;SPAN style="text-decoration: underline;"&gt;hitting a stationary car&lt;/SPAN&gt;.&amp;nbsp; The consequences again would be the same.&lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;&lt;BR /&gt;
&lt;P class="mce-p"&gt; &lt;/P&gt;</description>
      <pubDate>Thu, 27 Sep 2012 10:48:56 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161485#M21</guid>
      <dc:creator>upthecreekyetagain</dc:creator>
      <dc:date>2012-09-27T10:48:56Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161506#M22</link>
      <description>&lt;P class="mce-p"&gt;Does your question not depend on where the big bang took place? I see what you mean about how did 'we' get here before the light, but if we are close to the centre then is the light on the other side traveling away from us?&lt;/P&gt;</description>
      <pubDate>Thu, 27 Sep 2012 11:22:49 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161506#M22</guid>
      <dc:creator>logbox</dc:creator>
      <dc:date>2012-09-27T11:22:49Z</dc:date>
    </item>
    <item>
      <title>Re: The beginning?</title>
      <link>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161518#M23</link>
      <description>&lt;P class="mce-p"&gt;Good Lord&amp;nbsp;Logs, nobody expects the Spanish Inquisition. :_|&lt;/P&gt;</description>
      <pubDate>Thu, 27 Sep 2012 12:03:19 GMT</pubDate>
      <guid>https://community.ebay.co.uk/t5/The-Round-Table/The-beginning/m-p/161518#M23</guid>
      <dc:creator>electric*mayhem*band</dc:creator>
      <dc:date>2012-09-27T12:03:19Z</dc:date>
    </item>
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