Astronomy:Future of an expanding universe

From HandWiki
Short description: Future scenario assuming that the expansion of the universe may continue forever, or reach a point at which it begins to contract.
Part of a series on
Physical cosmology
Full-sky image derived from nine years' WMAP data
Early universe
Backgrounds
Expansion · Future
Components · Structure
Components
Structure
Experiments
  • Aaronson
  • Alfvén
  • Alpher
  • Bharadwaj
  • Copernicus
  • de Sitter
  • Dicke
  • Eddington
  • Ehlers
  • Einstein
  • Ellis
  • Friedman
  • Galileo
  • Gamow
  • Guth
  • Hubble
  • Lemaître
  • Linde
  • Mather
  • Newton
  • Penzias
  • Rubin
  • Schmidt
  • Schwarzschild
  • Smoot
  • Starobinsky
  • Steinhardt
  • Suntzeff
  • Sunyaev
  • Tolman
  • Wilson
  • Zeldovich
    		•
    Subject history

    Most observations suggest that the expansion of the universe will continue forever. If so, then a popular theory is that the universe will cool as it expands, eventually becoming too cold to sustain life. For this reason, this future scenario once popularly called "Heat Death" is now known as the "Big Chill" or "Big Freeze".[1][2]

    If dark energy—represented by the cosmological constant, a constant energy density filling space homogeneously,[3] or scalar fields, such as quintessence or moduli, dynamic quantities whose energy density can vary in time and space—accelerates the expansion of the universe, then the space between clusters of galaxies will grow at an increasing rate. Redshift will stretch ancient, incoming photons (even gamma rays) to undetectably long wavelengths and low energies.[4] Stars are expected to form normally for 1012 to 1014 (1–100 trillion) years, but eventually the supply of gas needed for star formation will be exhausted. As existing stars run out of fuel and cease to shine, the universe will slowly and inexorably grow darker.[5][6] According to theories that predict proton decay, the stellar remnants left behind will disappear, leaving behind only black holes, which themselves eventually disappear as they emit Hawking radiation.[7] Ultimately, if the universe reaches thermodynamic equilibrium, a state in which the temperature approaches a uniform value, no further work will be possible, resulting in a final heat death of the universe.[8]

    Cosmology

    Infinite expansion does not determine the overall spatial curvature of the universe. It can be open (with negative spatial curvature), flat, or closed (positive spatial curvature), although if it is closed, sufficient dark energy must be present to counteract the gravitational forces or else the universe will end in a Big Crunch.[9]

    Observations of the cosmic background radiation by the Wilkinson Microwave Anisotropy Probe and the Planck mission suggest that the universe is spatially flat and has a significant amount of dark energy.[10][11] In this case, the universe should continue to expand at an accelerating rate. The acceleration of the universe's expansion has also been confirmed by observations of distant supernovae.[9] If, as in the concordance model of physical cosmology (Lambda-cold dark matter or ΛCDM), dark energy is in the form of a cosmological constant, the expansion will eventually become exponential, with the size of the universe doubling at a constant rate.

    If the theory of inflation is true, the universe went through an episode dominated by a different form of dark energy in the first moments of the Big Bang; but inflation ended, indicating an equation of state much more complicated than those assumed so far for present-day dark energy. It is possible that the dark energy equation of state could change again resulting in an event that would have consequences which are extremely difficult to parametrize or predict.[citation needed]

    Future history

    In the 1970s, the future of an expanding universe was studied by the astrophysicist Jamal Islam[12] and the physicist Freeman Dyson.[13] Then, in their 1999 book The Five Ages of the Universe, the astrophysicists Fred Adams and Gregory Laughlin divided the past and future history of an expanding universe into five eras. The first, the Primordial Era, is the time in the past just after the Big Bang when stars had not yet formed. The second, the Stelliferous Era, includes the present day and all of the stars and galaxies now seen. It is the time during which stars form from collapsing clouds of gas. In the subsequent Degenerate Era, the stars will have burnt out, leaving all stellar-mass objects as stellar remnants—white dwarfs, neutron stars, and black holes. In the Black Hole Era, white dwarfs, neutron stars, and other smaller astronomical objects have been destroyed by proton decay, leaving only black holes. Finally, in the Dark Era, even black holes have disappeared, leaving only a dilute gas of photons and leptons.[14]

    This future history and the timeline below assume the continued expansion of the universe. If space in the universe begins to contract, subsequent events in the timeline may not occur because the Big Crunch, the collapse of the universe into a hot, dense state similar to that after the Big Bang, will supervene.[14][15]

    Timeline

    The Stelliferous Era

    From the present to about 1014 (100 trillion) years after the Big Bang

    The observable universe is currently 1.38×1010 (13.8 billion) years old.[16] This time is in the Stelliferous Era. About 155 million years after the Big Bang, the first star formed. Since then, stars have formed by the collapse of small, dense core regions in large, cold molecular clouds of hydrogen gas. At first, this produces a protostar, which is hot and bright because of energy generated by gravitational contraction. After the protostar contracts for a while, its core could become hot enough to fuse hydrogen, if it exceeds critical mass, a process called 'stellar ignition', and its lifetime as a star will properly begin.[14]

    Stars of very low mass will eventually exhaust all their fusible hydrogen and then become helium white dwarfs.[17] Stars of low to medium mass, such as our own sun, will expel some of their mass as a planetary nebula and eventually become white dwarfs; more massive stars will explode in a core-collapse supernova, leaving behind neutron stars or black holes.[18] In any case, although some of the star's matter may be returned to the interstellar medium, a degenerate remnant will be left behind whose mass is not returned to the interstellar medium. Therefore, the supply of gas available for star formation is steadily being exhausted.

    Milky Way Galaxy and the Andromeda Galaxy merge into one

    Main page: Astronomy:Andromeda–Milky Way collision
    4–8 billion years from now (17.8 – 21.8 billion years after the Big Bang)

    The Andromeda Galaxy is currently approximately 2.5 million light years away from our galaxy, the Milky Way Galaxy, and they are moving towards each other at approximately 300 kilometers (186 miles) per second. Approximately five billion years from now, or 19 billion years after the Big Bang, the Milky Way and the Andromeda Galaxy will collide with one another and merge into one large galaxy based on current evidence. Up until 2012, there was no way to confirm whether the possible collision was going to happen or not.[19] In 2012, researchers came to the conclusion that the collision is definite after using the Hubble Space Telescope between 2002 and 2010 to track the motion of Andromeda.[20] This results in the formation of Milkdromeda (also known as Milkomeda).

    22 billion years in the future is the earliest possible end of the Universe in the Big Rip scenario, assuming a model of dark energy with w = −1.5.[21][22]

    False vacuum decay may occur in 20 to 30 billion years if Higgs boson field is metastable.[23][24][25]

    Coalescence of Local Group and galaxies outside the Local Supercluster are no longer accessible

    1011 (100 billion) to 1012 (1 trillion) years

    The galaxies in the Local Group, the cluster of galaxies which includes the Milky Way and the Andromeda Galaxy, are gravitationally bound to each other. It is expected that between 1011 (100 billion) and 1012 (1 trillion) years from now, their orbits will decay and the entire Local Group will merge into one large galaxy.[5]

    Assuming that dark energy continues to make the universe expand at an accelerating rate, in about 150 billion years all galaxies outside the Local Supercluster will pass behind the cosmological horizon. It will then be impossible for events in the Local Supercluster to affect other galaxies. Similarly, it will be impossible for events after 150 billion years, as seen by observers in distant galaxies, to affect events in the Local Supercluster.[4] However, an observer in the Local Supercluster will continue to see distant galaxies, but events they observe will become exponentially more redshifted as the galaxy approaches the horizon until time in the distant galaxy seems to stop. The observer in the Local Supercluster never observes events after 150 billion years in their local time, and eventually all light and background radiation lying outside the Local Supercluster will appear to blink out as light becomes so redshifted that its wavelength has become longer than the physical diameter of the horizon.

    Technically, it will take an infinitely long time for all causal interaction between the Local Supercluster and this light to cease. However, due to the redshifting explained above, the light will not necessarily be observed for an infinite amount of time, and after 150 billion years, no new causal interaction will be observed.

    Therefore, after 150 billion years, intergalactic transportation and communication beyond the Local Supercluster becomes causally impossible.

    Luminosities of galaxies begin to diminish

    8×1011 (800 billion) years

    8×1011 (800 billion) years from now, the luminosities of the different galaxies, approximately similar until then to the current ones thanks to the increasing luminosity of the remaining stars as they age, will start to decrease, as the less massive red dwarf stars begin to die as white dwarfs.[26]

    Galaxies outside the Local Supercluster are no longer detectable

    2×1012 (2 trillion) years

    2×1012 (2 trillion) years from now, all galaxies outside the Local Supercluster will be redshifted to such an extent that even gamma rays they emit will have wavelengths longer than the size of the observable universe of the time. Therefore, these galaxies will no longer be detectable in any way.[4]

    Degenerate Era

    From 1014 (100 trillion) to 1040 (10 duodecillion) years

    By 1014 (100 trillion) years from now, star formation will end,[5] leaving all stellar objects in the form of degenerate remnants. If protons do not decay, stellar-mass objects will disappear more slowly, making this era last longer.

    Star formation ceases

    1012–14 (1–100 trillion) years

    By 1014 (100 trillion) years from now, star formation will end. This period, known as the "Degenerate Era", will last until the degenerate remnants finally decay.[27] The least massive stars take the longest to exhaust their hydrogen fuel (see stellar evolution). Thus, the longest living stars in the universe are low-mass red dwarfs, with a mass of about 0.08 solar masses (M☉), which have a lifetime of over 1013 (10 trillion) years.[28] Coincidentally, this is comparable to the length of time over which star formation takes place.[5] Once star formation ends and the least massive red dwarfs exhaust their fuel, nuclear fusion will cease. The low-mass red dwarfs will cool and become black dwarfs.[17] The only objects remaining with more than planetary mass will be brown dwarfs, with mass less than 0.08 M☉, and degenerate remnants; white dwarfs, produced by stars with initial masses between about 0.08 and 8 solar masses; and neutron stars and black holes, produced by stars with initial masses over 8 M☉. Most of the mass of this collection, approximately 90%, will be in the form of white dwarfs.[6] In the absence of any energy source, all of these formerly luminous bodies will cool and become faint.

    The universe will become extremely dark after the last stars burn out. Even so, there can still be occasional light in the universe. One of the ways the universe can be illuminated is if two carbon–oxygen white dwarfs with a combined mass of more than the Chandrasekhar limit of about 1.4 solar masses happen to merge. The resulting object will then undergo runaway thermonuclear fusion, producing a Type Ia supernova and dispelling the darkness of the Degenerate Era for a few weeks. Neutron stars could also collide, forming even brighter supernovae and dispelling up to 6 solar masses of degenerate gas into the interstellar medium. The resulting matter from these supernovae could potentially create new stars.[29][30] If the combined mass is not above the Chandrasekhar limit but is larger than the minimum mass to fuse carbon (about 0.9 M☉), a carbon star could be produced, with a lifetime of around 106 (1 million) years.[14] Also, if two helium white dwarfs with a combined mass of at least 0.3 M☉ collide, a helium star may be produced, with a lifetime of a few hundred million years.[14] Finally brown dwarfs can form new stars colliding with each other to form a red dwarf star, that can survive for 1013 (10 trillion) years,[28][29] or accreting gas at very slow rates from the remaining interstellar medium until they have enough mass to start hydrogen burning as red dwarfs too. This process, at least on white dwarfs, could induce Type Ia supernovae too.[31]

    Planets fall or are flung from orbits by a close encounter with another star

    1015 (1 quadrillion) years

    Over time, the orbits of planets will decay due to gravitational radiation, or planets will be ejected from their local systems by gravitational perturbations caused by encounters with another stellar remnant.[32]

    Stellar remnants escape galaxies or fall into black holes

    1019 to 1020 (10 to 100 quintillion) years

    Over time, objects in a galaxy exchange kinetic energy in a process called dynamical relaxation, making their velocity distribution approach the Maxwell–Boltzmann distribution.[33] Dynamical relaxation can proceed either by close encounters of two stars or by less violent but more frequent distant encounters.[34] In the case of a close encounter, two brown dwarfs or stellar remnants will pass close to each other. When this happens, the trajectories of the objects involved in the close encounter change slightly, in such a way that their kinetic energies are more nearly equal than before. After a large number of encounters, then, lighter objects tend to gain speed while the heavier objects lose it.[14]

    Because of dynamical relaxation, some objects will gain just enough energy to reach galactic escape velocity and depart the galaxy, leaving behind a smaller, denser galaxy. Since encounters are more frequent in this denser galaxy, the process then accelerates. The end result is that most objects (90% to 99%) are ejected from the galaxy, leaving a small fraction (maybe 1% to 10%) which fall into the central supermassive black hole.[5][14] It has been suggested that the matter of the fallen remnants will form an accretion disk around it that will create a quasar, as long as enough matter is present there.[35]

    Possible ionization of matter

    >1023 years from now

    In an expanding universe with decreasing density and non-zero cosmological constant, matter density would reach zero, resulting in most matter except black dwarfs, neutron stars, black holes, and planets ionizing and dissipating at thermal equilibrium.[36]

    Future with proton decay

    The following timeline assumes that protons do decay.

    Chance: 1034 (10 decillion) – 1039 years (1 duodecillion)

    The subsequent evolution of the universe depends on the possibility and rate of proton decay. Experimental evidence shows that if the proton is unstable, it has a half-life of at least 1034 years.[37] Some of the Grand Unified theories (GUTs) predict long-term proton instability between 1031 and 1036 years, with the upper bound on standard (non-supersymmetry) proton decay at 1.4×1036 years and an overall upper limit maximum for any proton decay (including supersymmetry models) at 6×1039 years.[38][39] Recent research showing proton lifetime (if unstable) at or exceeding 1034–1035 year range rules out simpler GUTs and most non-supersymmetry models.

    Nucleons start to decay

    Neutrons bound into nuclei are also suspected to decay with a half-life comparable to that of protons. Planets (substellar objects) would decay in a simple cascade process from heavier elements to pure hydrogen while radiating energy.[40]

    If the proton does not decay at all, then stellar objects would still disappear, but more slowly. See Future without proton decay below.

    Shorter or longer proton half-lives will accelerate or decelerate the process. This means that after 1037 years (the maximum proton half-life used by Adams & Laughlin (1997)), one-half of all baryonic matter will have been converted into gamma ray photons and leptons through proton decay.

    All nucleons decay

    1040 (10 duodecillion) years

    Given our assumed half-life of the proton, nucleons (protons and bound neutrons) will have undergone roughly 1,000 half-lives by the time the universe is 1040 years old. This means that there will be roughly 0.51,000 (approximately 10−301) as many nucleons; as there are an estimated 1080 protons currently in the universe,[41] none will remain at the end of the Degenerate Age. Effectively, all baryonic matter will have been changed into photons and leptons. Some models predict the formation of stable positronium atoms with diameters greater than the observable universe's current diameter (roughly 6 · 1034 metres)[42] in 1085 years, and that these will in turn decay to gamma radiation in 10141 years.[5][6]

    The supermassive black holes are all that remain of galaxies once all protons decay, but even these giants are not immortal.

    If protons decay on higher-order nuclear processes

    Chance: 1065 to 10200 years

    If the proton does not decay according to the theories described above, then the Degenerate Era will last longer, and will overlap or surpass the Black Hole Era. On a time scale of 1065 years solid matter is theorized to potentially rearrange its atoms and molecules via quantum tunneling, and may behave as liquid and become smooth spheres due to diffusion and gravity.[13] Degenerate stellar objects can potentially still experience proton decay, for example via processes involving the Adler–Bell–Jackiw anomaly, virtual black holes, or higher-dimension supersymmetry possibly with a half-life of under 10200 years.[5]

    >10139 years from now

    2018 estimate of Standard Model lifetime before collapse of a false vacuum; 95% confidence interval is 1058 to 10241 years due in part to uncertainty about the top quark mass.[43]

    >10150 years from now

    Although protons are stable in standard model physics, a quantum anomaly may exist on the electroweak level, which can cause groups of baryons (protons and neutrons) to annihilate into antileptons via the sphaleron transition.[44] Such baryon/lepton violations have a number of 3 and can only occur in multiples or groups of three baryons, which can restrict or prohibit such events. No experimental evidence of sphalerons has yet been observed at low energy levels, though they are believed to occur regularly at high energies and temperatures.

    The photon, electron, positron, and neutrino are now the final remnants of the universe as the last of the supermassive black holes evaporate.

    Black Hole Era

    1040 (10 duodecillion) years to approximately 10100 (1 googol) years, up to 10108 years for the largest supermassive black holes

    After 1040 years, black holes will dominate the universe. They will slowly evaporate via Hawking radiation.[5] A black hole with a mass of around 1 M☉ will vanish in around 2×1066 years. As the lifetime of a black hole is proportional to the cube of its mass, more massive black holes take longer to decay. A supermassive black hole with a mass of 1011 (100 billion) M☉ will evaporate in around 2×1099 years.[45]

    The largest black holes in the universe are predicted to continue to grow. Larger black holes of up to 1014 (100 trillion) M☉ may form during the collapse of superclusters of galaxies. Even these would evaporate over a timescale of 10106[46] to 10108 years.

    Hawking radiation has a thermal spectrum. During most of a black hole's lifetime, the radiation has a low temperature and is mainly in the form of massless particles such as photons and hypothetical gravitons. As the black hole's mass decreases, its temperature increases, becoming comparable to the Sun's by the time the black hole mass has decreased to 1019 kilograms. The hole then provides a temporary source of light during the general darkness of the Black Hole Era. During the last stages of its evaporation, a black hole will emit not only massless particles, but also heavier particles, such as electrons, positrons, protons, and antiprotons.[14]

    Dark Era and Photon Age

    From 10100 years (10 duotrigintillion years or 1 googol years)

    After all the black holes have evaporated (and after all the ordinary matter made of protons has disintegrated, if protons are unstable), the universe will be nearly empty. Photons, neutrinos, electrons, and positrons will fly from place to place, hardly ever encountering each other. Gravitationally, the universe will be dominated by dark matter, electrons, and positrons (not protons).[47]

    By this era, with only very diffuse matter remaining, activity in the universe will have tailed off dramatically (compared with previous eras), with very low energy levels and very large time scales. Electrons and positrons drifting through space will encounter one another and occasionally form positronium atoms. These structures are unstable, however, and their constituent particles must eventually annihilate. However, most electrons and positrons will remain unbound.[48] Other low-level annihilation events will also take place, albeit very slowly. The universe now reaches an extremely low-energy state.

    Future without proton decay

    If the protons do not decay, stellar-mass objects will still become black holes, but more slowly. The following timeline assumes that proton decay does not take place.

    >10139 years from now

    2018 estimate of Standard Model lifetime before collapse of a false vacuum; 95% confidence interval is 1058 to 10241 years due in part to uncertainty about the top quark mass.[43]

    Degenerate Era

    Matter decays into iron

    101100 to 1032000 years from now

    In 101500 years, cold fusion occurring via quantum tunneling should make the light nuclei in stellar-mass objects fuse into iron-56 nuclei (see isotopes of iron). Fission and alpha particle emission should make heavy nuclei also decay to iron, leaving stellar-mass objects as cold spheres of iron, called iron stars.[13] Before this happens, in some black dwarfs the process is expected to lower their Chandrasekhar limit resulting in a supernova in 101100 years. Non-degenerate silicon has been calculated to tunnel to iron in approximately 1032000 years.[49]

    Black Hole Era

    Collapse of iron stars to black holes

    101026 to 101076 years from now

    Quantum tunneling should also turn large objects into black holes, which (on these timescales) will instantaneously evaporate into subatomic particles. Depending on the assumptions made, the time this takes to happen can be calculated as from 101026 years to 101076 years. Quantum tunneling may also make iron stars collapse into neutron stars in around 101076 years.[13]

    Dark Era (without proton decay)

    101076 years from now

    With black holes evaporated, virtually no matter still exists, the universe having become an almost pure vacuum (possibly accompanied with a false vacuum). The expansion of the universe slowly cools it down to absolute zero.[citation needed]

    Beyond

    Beyond 102500 years if proton decay occurs, or 101076 years without proton decay

    It is possible that a Big Rip event may occur far off into the future.[50][51] This singularity would take place at a finite scale factor.

    If the current vacuum state is a false vacuum, the vacuum may decay into a lower-energy state.[52]

    Presumably, extreme low-energy states imply that localized quantum events become major macroscopic phenomena rather than negligible microscopic events because the smallest perturbations make the biggest difference in this era, so there is no telling what may happen to space or time. It is perceived that the laws of "macro-physics" will break down, and the laws of quantum physics will prevail.[8]

    The universe could possibly avoid eternal heat death through random quantum tunneling and quantum fluctuations, given the non-zero probability of producing a new Big Bang in roughly 10101056 years.[53]

    Over an infinite amount of time, there could be a spontaneous entropy decrease, by a Poincaré recurrence or through thermal fluctuations (see also fluctuation theorem).[54][55][56]

    Massive black dwarfs could also potentially explode into supernovae after up to 1032000 years, assuming protons do not decay.[57]

    The possibilities above are based on a simple form of dark energy. However, the physics of dark energy are still a very active area of research, and the actual form of dark energy could be much more complex. For example, during inflation dark energy affected the universe very differently than it does today, so it is possible that dark energy could trigger another inflationary period in the future. Until dark energy is better understood, its possible effects are extremely difficult to predict or parametrize.

    Graphical timeline

    <timeline>

    1. ImageSize = width:1100 height:370 # too wide

    ImageSize = width:1000 height:370 PlotArea = left:40 right:235 bottom:50 top:50

    Colors = 

     id:period1  value:rgb(1,1,0.7) # light yellow
 id:period2  value:rgb(0.7,0.7,1) # light blue
 id:events  value:rgb(1,0.7,1) # light purple
 id:era2  value:lightorange
 id:era1  Value:yellowgreen

    DateFormat = yyyy Period = from:-51 till:1000 TimeAxis = format:yyyy orientation:horizontal ScaleMajor = unit:year increment:100 start:0 ScaleMinor = unit:year increment:10 start:-50

    AlignBars = justify

    BarData = 

     bar:Era
 bar:Events

    TextData = 

     fontsize:M
 pos:(0,260)
 text:"Big"
 text:"Bang"
    1. pos:(880,260)
     pos:(780,260)
 text:"Heat"
 text:"Death"
    1. pos:(880,90)
     pos:(780,90)
 text:"log"
 text:"year"

    PlotData= 

     textcolor:black  fontsize:M

     width:110
 bar:Era  mark:(line,white)  align:left  shift:(0,0)
 from:-51  till:6  shift:(0,35)  color:era1  text:"The Primordial Era"
 from:6  till:14  shift:(0,15)  color:era2  text:"The Stelliferous Era"
 from:14  till:40  shift:(0,-5)  color:era1  text:"The Degenerate Era"
 from:40  till:100  shift:(0,-25)  color:era2  text:"The Black Hole Era"
 from:100  till:1000  shift:(0,-45)  color:era1  text:"The Dark Era"

     width:110
 bar:Events
 color:events  align:left  shift:(43,3)  mark:(line,teal)
 at:-8  shift:(0,35)  text:"One second"
 at:8  shift:(-2,15)  text:"First star began to shine"
 at:10  shift:(-2,-5)  text:"13.8 billion years, the present day"
 at:14  shift:(0,-25)  text:"The last star has died"
 at:100  shift:(0,-45)  text:"The last supermassive black holes have evaporated"

    </timeline>

    See also


    References

    1. ↑ "cds.cern.ch". https://cds.cern.ch/record/318436/files/9701131.pdf. 
    2. ↑ WMAP – Fate of the Universe, WMAP's Universe, NASA. Accessed online July 17, 2008.
    3. ↑ Sean Carroll (2001). "The cosmological constant". Living Reviews in Relativity 4 (1): 1. doi:10.12942/lrr-2001-1. PMID 28179856. PMC 5256042. Bibcode: 2001LRR.....4....1C. http://relativity.livingreviews.org/Articles/lrr-2001-1/index.html. Retrieved 2006-09-28. 
    4. ↑ 4.0 4.1 4.2 Krauss, Lawrence M.; Starkman, Glenn D. (2000). "Life, the Universe, and Nothing: Life and Death in an Ever-expanding Universe". Astrophysical Journal 531 (1): 22–30. doi:10.1086/308434. Bibcode: 2000ApJ...531...22K. 
    5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 5.7 Adams, Fred C.; Laughlin, Gregory (1997). "A dying universe: the long-term fate and evolution of astrophysical objects". Reviews of Modern Physics 69 (2): 337–372. doi:10.1103/RevModPhys.69.337. Bibcode: 1997RvMP...69..337A. 
    6. ↑ 6.0 6.1 6.2 Adams & Laughlin (1997), §IIE.
    7. ↑ Adams & Laughlin (1997), §IV.
    8. ↑ 8.0 8.1 Adams & Laughlin (1997), §VID
    9. ↑ 9.0 9.1 Chapter 7, Calibrating the Cosmos, Frank Levin, New York: Springer, 2006, ISBN:0-387-30778-8.
    10. ↑ Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Data Processing, Sky Maps, and Basic Results, G. Hinshaw et al., The Astrophysical Journal Supplement Series (2008), submitted, arXiv:0803.0732, Bibcode: 2008arXiv0803.0732H.
    11. ↑ Planck Collaboration et al. (September 1, 2016). "Planck 2015 results. XIII. Cosmological parameters". Astronomy and Astrophysics 594: A13. doi:10.1051/0004-6361/201525830. Bibcode: 2016A&A...594A..13P. 
    12. ↑ Possible Ultimate Fate of the Universe, Jamal N. Islam, Quarterly Journal of the Royal Astronomical Society 18 (March 1977), pp. 3–8, Bibcode: 1977QJRAS..18....3I
    13. ↑ 13.0 13.1 13.2 13.3 Dyson, Freeman J. (1979). "Time without end: Physics and biology in an open universe". Reviews of Modern Physics 51 (3): 447–460. doi:10.1103/RevModPhys.51.447. Bibcode: 1979RvMP...51..447D. 
    14. ↑ 14.0 14.1 14.2 14.3 14.4 14.5 14.6 14.7 The Five Ages of the Universe, Fred Adams and Greg Laughlin, New York: The Free Press, 1999, ISBN:0-684-85422-8.
    15. ↑ Adams & Laughlin (1997), §VA
    16. ↑ Planck collaboration (2013). "Planck 2013 results. XVI. Cosmological parameters". Astronomy & Astrophysics 571: A16. doi:10.1051/0004-6361/201321591. Bibcode: 2014A&A...571A..16P. 
    17. ↑ 17.0 17.1 Laughlin, Gregory; Bodenheimer, Peter; Adams, Fred C. (1997). "The End of the Main Sequence". The Astrophysical Journal 482 (1): 420–432. doi:10.1086/304125. Bibcode: 1997ApJ...482..420L. 
    18. ↑ Heger, A.; Fryer, C. L.; Woosley, S. E.; Langer, N.; Hartmann, D. H. (2003). "How Massive Single Stars End Their Life". Astrophysical Journal 591 (1): 288–300. doi:10.1086/375341. Bibcode: 2003ApJ...591..288H. 
    19. ↑ van der Marel, G. (2012). "The M31 Velocity Vector. III. Future Milky Way M31-M33 Orbital Evolution, Merging, and Fate of the Sun". The Astrophysical Journal 753 (1): 9. doi:10.1088/0004-637X/753/1/9. Bibcode: 2012ApJ...753....9V. 
    20. ↑ Cowen, R. (31 May 2012). "Andromeda on collision course with the Milky Way". Nature. doi:10.1038/nature.2012.10765. 
    21. ↑ "Universe may end in a Big Rip". April 30, 2003. https://cerncourier.com/a/universe-may-end-in-a-big-rip/. 
    22. ↑ Siegel, Ethan. "Ask Ethan: Could The Universe Be Torn Apart In A Big Rip?". https://www.forbes.com/sites/startswithabang/2018/06/30/ask-ethan-could-the-universe-be-torn-apart-in-a-big-rip/. 
    23. ↑ "Physicists have a massive problem as Higgs boson refuses to misbehave". New Scientist. https://www.newscientist.com/article/2251285-physicists-have-a-massive-problem-as-higgs-boson-refuses-to-misbehave/. 
    24. ↑ "The Higgs boson makes the universe stable – just. Coincidence?". New Scientist. https://www.newscientist.com/article/mg23230971-000-cosmic-coincidences-the-universe-is-on-the-brink-of-catastrophe/. 
    25. ↑ "Death by Higgs rids cosmos of space brain threat". New Scientist. https://www.newscientist.com/article/mg21929333-200-death-by-higgs-rids-cosmos-of-space-brain-threat/. 
    26. ↑ Adams, F. C.; Graves, G. J. M.; Laughlin, G. (December 2004). García-Segura, G.; Tenorio-Tagle, G.; Franco, J. et al.. eds. "Gravitational Collapse: From Massive Stars to Planets. / First Astrophysics meeting of the Observatorio Astronomico Nacional. / A meeting to celebrate Peter Bodenheimer for his outstanding contributions to Astrophysics: Red Dwarfs and the End of the Main Sequence". Revista Mexicana de Astronomía y Astrofísica, Serie de Conferencias 22: 46–149. Bibcode: 2004RMxAC..22...46A.  See Fig. 3.
    27. ↑ Adams & Laughlin (1997), § III–IV.
    28. ↑ 28.0 28.1 Adams & Laughlin (1997), §IIA and Figure 1.
    29. ↑ 29.0 29.1 Adams & Laughlin (1997), §IIIC.
    30. ↑ The Future of the Universe, M. Richmond, lecture notes, "Physics 240", Rochester Institute of Technology. Accessed on line July 8, 2008.
    31. ↑ Brown Dwarf Accretion: Nonconventional Star Formation over Very Long Timescales, Cirkovic, M. M., Serbian Astronomical Journal 171, (December 2005), pp. 11–17. Bibcode: 2005SerAJ.171...11C
    32. ↑ Adams & Laughlin (1997), §IIIF, Table I.
    33. ↑ p. 428, A deep focus on NGC 1883, A. L. Tadross, Bulletin of the Astronomical Society of India 33, #4 (December 2005), pp. 421–431, Bibcode: 2005BASI...33..421T.
    34. ↑ Reading notes, Liliya L. R. Williams, Astrophysics II: Galactic and Extragalactic Astronomy, University of Minnesota, accessed July 20, 2008.
    35. ↑ Deep Time, David J. Darling, New York: Delacorte Press, 1989, ISBN:978-0-38529-757-8.
    36. ↑ John Baez, University of California-Riverside (Department of Mathematics), "The End of the Universe" 7 February 2016 http://math.ucr.edu/home/baez/end.html
    37. ↑ G Senjanovic Proton decay and grand unification, Dec 2009
    38. ↑ Pavel (2007). "Upper Bound on the Proton Lifetime and the Minimal Non-SUSY Grand Unified Theory". AIP Conference Proceedings 903: 385–388. doi:10.1063/1.2735205. Bibcode: 2007AIPC..903..385P. 
    39. ↑ Pran Nath and Pavel Fileviez Perez, "Proton Stability in Grand Unified Theories, in Strings and in Branes", Appendix H; 23 April 2007. arXiv:hep-ph/0601023 https://arxiv.org/abs/hep-ph/0601023
    40. ↑ Adams & Laughlin (1997), §IV-H.
    41. ↑ Solution, exercise 17, One Universe: At Home in the Cosmos, Neil de Grasse Tyson, Charles Tsun-Chu Liu, and Robert Irion, Washington, D.C.: Joseph Henry Press, 2000. ISBN:0-309-06488-0.
    42. ↑ Page, Don N.; McKee, M. Randall (1981). "Matter annihilation in the late universe". Physical Review D 24 (6): 1458–1469. doi:10.1103/PhysRevD.24.1458. Bibcode: 1981PhRvD..24.1458P. 
    43. ↑ 43.0 43.1 Andreassen, Anders; Frost, William; Schwartz, Matthew D. (12 March 2018). "Scale-invariant instantons and the complete lifetime of the standard model". Physical Review D 97 (5): 056006. doi:10.1103/PhysRevD.97.056006. Bibcode: 2018PhRvD..97e6006A. 
    44. ↑ 't Hooft, T (1976). "Symmetry breaking through Bell-Jackiw anomalies". Phys. Rev. Lett. 37 (1): 8. doi:10.1103/physrevlett.37.8. Bibcode: 1976PhRvL..37....8T. 
    45. ↑ Page, Don N. (1976). "Particle emission rates from a black hole: Massless particles from an uncharged, nonrotating hole". Physical Review D 13 (2): 198–206. doi:10.1103/PhysRevD.13.198. Bibcode: 1976PhRvD..13..198P. . See in particular equation (27).
    46. ↑ Frautschi, S (1982). "Entropy in an expanding universe". Science 217 (4560): 593–599. doi:10.1126/science.217.4560.593. PMID 17817517. Bibcode: 1982Sci...217..593F.  See page 596: table 1 and section "black hole decay" and previous sentence on that page
      Since we have assumed a maximum scale of gravitational binding – for instance, superclusters of galaxies – black hole formation eventually comes to an end in our model, with masses of up to 1014M☉ ... the timescale for black holes to radiate away all their energy ranges ... to 10106 years for black holes of up to 1014M☉.
    47. ↑ Adams & Laughlin (1997), §VD.
    48. ↑ Adams & Laughlin (1997), §VF3.
    49. ↑ M. E. Caplan (7 August 2020). "Black Dwarf Supernova in the Far Future". MNRAS 497 (1–6): 4357–4362. doi:10.1093/mnras/staa2262. Bibcode: 2020MNRAS.497.4357C. https://arxiv.org/pdf/2008.02296.pdf. 
    50. ↑ Caldwell, Robert R.; Kamionkowski, Marc; Weinberg, Nevin N. (2003). "Phantom energy and cosmic doomsday". Phys. Rev. Lett. 91 (7): 071301. doi:10.1103/PhysRevLett.91.071301. PMID 12935004. Bibcode: 2003PhRvL..91g1301C. 
    51. ↑ Bouhmadi-López, Mariam; González-Díaz, Pedro F.; Martín-Moruno, Prado (2008). "Worse than a big rip?". Physics Letters B 659 (1–2): 1–5. doi:10.1016/j.physletb.2007.10.079. Bibcode: 2008PhLB..659....1B. 
    52. ↑ Adams & Laughlin (1997), §VE.
    53. ↑ Carroll, Sean M.; Chen, Jennifer (2004). "Spontaneous Inflation and Origin of the Arrow of Time". arXiv:hep-th/0410270.
    54. ↑ Tegmark, Max (2003). "Parallel Universes". Scientific American 288 (5): 40–51. doi:10.1038/scientificamerican0503-40. Bibcode: 2003SciAm.288e..40T. 
    55. ↑ Werlang, T.; Ribeiro, G. A. P.; Rigolin, Gustavo (2013). "Interplay between quantum phase transitions and the behavior of quantum correlations at finite temperatures". International Journal of Modern Physics B 27. doi:10.1142/S021797921345032X. Bibcode: 2013IJMPB..2745032W. 
    56. ↑ Xing, Xiu-San (2007). "Spontaneous entropy decrease and its statistical formula". arXiv:0710.4624 [cond-mat.stat-mech].
    57. ↑ Caplan, M. E. (2020). "Black dwarf supernova in the far future". Monthly Notices of the Royal Astronomical Society 497 (4): 4357–4362. doi:10.1093/mnras/staa2262. Bibcode: 2020MNRAS.497.4357C. 



    Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:Future_of_an_expanding_universe&oldid=2218625"