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Journal articles on the topic 'Hot Big Bang cosmology'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 February 2022

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1

Kragh, Helge. "Naming the Big Bang." Historical Studies in the Natural Sciences 44, no. 1 (November 2012): 3–36. http://dx.doi.org/10.1525/hsns.2014.44.1.3.

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The standard model of modern cosmology is known as the hot big bang, a name that refers to the initial state of the universe some fourteen billion years ago. The name Big Bang introduced by Fred Hoyle in 1949 is one of the most successful scientific neologisms ever. How did the name originate and how was it received by physicists and astronomers in the period leading up to the hot big bang consensus model in the late 1960s? How did it reflect the meanings of the origin of the universe, a concept that predates the name by nearly two decades? Contrary to what is often assumed, the name was not an instant success—it took more than twenty years before Big Bang became a household word in the scientific community. When it happened, it was used with different connotations, as is still the case. Moreover, it was used earlier and more frequently in popular than in scientific contexts, and not always relating to cosmology. It turns out that Hoyle’s celebrated name has a richer and more surprising history than commonly assumed and also that the literature on modern cosmology and its history includes many common mistakes and errors. An etymological approach centering on the name Big Bang provides supplementary insight to the historical understanding of the emergence of modern cosmology.

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2

Turner, Michael S. "The Hot Big Bang and Beyond." Symposium - International Astronomical Union 168 (1996): 301–20. http://dx.doi.org/10.1017/s0074180900110186.

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The hot big-bang cosmology provides a reliable accounting of the Universe from about 10−2sec after the bang until the present, as well as a robust framework for speculating back to times as early as 10−43sec. Cosmology faces a number of important challenges; foremost among them are determining the quantity and composition of matter in the Universe and developing a detailed and coherent picture of how structure (galaxies, clusters of galaxies, superclusters, voids, great walls, and so on) developed. At present there is a working hypothesis—cold dark matter—which is based upon inflation and which, if correct, would extend the big bang model back to 10−32sec and cast important light on the unification of the forces. Many experiments and observations, from CBR anisotropy experiments to Hubble Space Telescope observations to experiments at Fermilab and CERN, are now putting the cold dark matter theory to the test. At present it appears that the theory is viable only if the Hubble constant is smaller than current measurements indicate (around 30 km s−1Mpc−1), or if the theory is modified slightly, e.g., by the addition of a cosmological constant, a small admixture of hot dark matter (5 eV “worth of neutrinos”), more relativistic particles, or a tilted spectrum of density perturbations.

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3

Rees, Martin J. "Cosmology: evidence for a ‘big bang’." European Review 2, no. 2 (April 1994): 155–64. http://dx.doi.org/10.1017/s1062798700001022.

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During the last 25 years, evidence has accumulated that our universe has evolved, over a period of 10–15 billion years, from a hot dense fireball to its present state. Telescopes can detect objects so far away that the universe had only a tenth its present age when the light we now receive set out towards us. The cosmic background radiation, and the abundances of elements such as helium and lithium, permit quantitative inferences about what the universe was like when it had been expanding for only a few seconds. The laws of physics established in the laboratory apparently suffice for interpreting all astronomical phenomena back to that time. In the initial instants of cosmic expansion, however, the particle energies and densities were so extreme that terrestrial experiments offer no firm guidance. We will not understand why the universe contains the observed ‘mix’ of matter and radiation, nor why it is expanding in the observed fashion, without further progress in fundamental physics.

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4

Peebles, P. J. E., D. N. Schramm, E. L. Turner, and R. G. Kron. "The case for the relativistic hot Big Bang cosmology." Nature 352, no. 6338 (August 1991): 769–76. http://dx.doi.org/10.1038/352769a0.

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5

KANDRUP, HENRY E., and PAWEL O. MAZUR. "GENERATING A HOT BIG BANG VIA A CHANGE IN TOPOLOGY." Modern Physics Letters A 05, no. 19 (August 10, 1990): 1471–76. http://dx.doi.org/10.1142/s0217732390001670.

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This letter uses ideas developed recently in semiclassical quantum gravity to argue that many qualitative features of the Hot Big Bang generally assumed in cosmology may be explained by the hypothesis that, interpreted semiclassically, the Universe “tunnelled into being” via a quantum fluctuation from a small (Planck-sized), topologically complex entity to a topolo-gically trivial entity (like a Friedmann Universe) that rapidly grew to a more macroscopic size.

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6

Shaposhnikov, Mikhail. "The Higgs boson and cosmology." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 373, no. 2032 (January 13, 2015): 20140038. http://dx.doi.org/10.1098/rsta.2014.0038.

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I will discuss how the Higgs field of the Standard Model may have played an important role in cosmology, leading to the homogeneity, isotropy and flatness of the Universe; producing the quantum fluctuations that seed structure formation; triggering the radiation-dominated era of the hot Big Bang; and contributing to the processes of baryogenesis and dark matter production.

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7

Narlikar, Jayant V. "Alternative Cosmologies." Symposium - International Astronomical Union 124 (1987): 447–59. http://dx.doi.org/10.1017/s0074180900159418.

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This review highlights some of the cosmological theories proposed as alternatives to the standard hot big bang model. Specific ideas discussed here are the matter - antimatter symmetric cosmologies, the empirical two-component model, the G-varying cosmologies, the chronometric cosmology and a simplified quantum cosmology. It is argued that many alternative cosmologies have contributed useful concepts and offered observational tests that have enriched the field of cosmology as a science.

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8

Traunmüller, Hartmut. "Does standard cosmology really predict the cosmic microwave background?" F1000Research 9 (September 28, 2020): 261. http://dx.doi.org/10.12688/f1000research.22432.4.

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In standard Big Bang cosmology, the universe expanded from a very dense, hot and opaque initial state. The light that was last scattered about 380,000 years later, when the universe had become transparent, has been redshifted and is now seen as thermal radiation with a temperature of 2.7 K, the cosmic microwave background (CMB). However, since light escapes faster than matter can move, it is prudent to ask how we, made of matter from this very source, can still see the light. In order for this to be possible, the light must take a return path of the right length. A curved return path is possible in spatially closed, balloon-like models, but in standard cosmology, the universe is “flat” rather than balloon-like, and it lacks a boundary surface that might function as a reflector. Under these premises, radiation that once filled the universe homogeneously cannot do so permanently after expansion, and we cannot see the last scattering event. It is shown that the traditional calculation of the CMB temperature is inappropriate and that light emitted by any source inside the Big Bang universe earlier than half its “conformal age” can only become visible to us via a return path. Although often advanced as the best evidence for a hot Big Bang, the CMB actually tells against a formerly smaller universe and so do also distant galaxies.

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9

Traunmüller, Hartmut. "Does standard cosmology really predict the cosmic microwave background?" F1000Research 9 (February 19, 2021): 261. http://dx.doi.org/10.12688/f1000research.22432.5.

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In standard Big Bang cosmology, the universe expanded from a very dense, hot and opaque initial state. The light that was last scattered about 380,000 years later, when the universe had become transparent, has been redshifted and is now seen as thermal radiation with a temperature of 2.7 K, the cosmic microwave background (CMB). However, since light escapes faster than matter can move, it is prudent to ask how we, made of matter from this very source, can still see the light. In order for this to be possible, the light must take a return path of the right length. A curved return path is possible in spatially closed, balloon-like models, but in standard cosmology, the universe is “flat” rather than balloon-like, and it lacks a boundary surface that might function as a reflector. Under these premises, radiation that once filled the universe homogeneously cannot do so permanently after expansion, and we cannot see the last scattering event. It is shown that the traditional calculation of the CMB temperature is inappropriate and that light emitted by any source inside the Big Bang universe earlier than half its “conformal age” can only become visible to us via a return path. Although often advanced as the best evidence for a hot Big Bang, the CMB actually tells against a formerly smaller universe and so do also distant galaxies.

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10

Traunmüller, Hartmut. "Does standard cosmology really predict the cosmic microwave background?" F1000Research 9 (September 23, 2021): 261. http://dx.doi.org/10.12688/f1000research.22432.6.

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In standard Big Bang cosmology, the universe expanded from a very dense, hot and opaque initial state. The light that was last scattered about 380,000 years later, when the universe had become transparent, has been redshifted and is now seen as thermal radiation with a temperature of 2.7 K, the cosmic microwave background (CMB). However, since light escapes faster than matter can move, it is prudent to ask how we, made of matter from this very source, can still see the light. In order for this to be possible, the light must take a return path of the right length. A curved return path is possible in spatially closed, balloon-like models, but in standard cosmology, the universe is “flat” rather than balloon-like, and it lacks a boundary surface that might function as a reflector. Under these premises, radiation that once filled the universe homogeneously cannot do so permanently after expansion, and we cannot see the last scattering event. It is shown that the traditional calculation of the CMB temperature is inappropriate and that light emitted by any source inside the Big Bang universe earlier than half its “conformal age” can only become visible to us via a return path. Although often advanced as the best evidence for a hot Big Bang, the CMB actually tells against a formerly smaller universe and so do also distant galaxies.

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11

Traunmüller, Hartmut. "Does standard cosmology really predict the cosmic microwave background?" F1000Research 9 (April 16, 2020): 261. http://dx.doi.org/10.12688/f1000research.22432.1.

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In standard Big Bang cosmology, the universe expanded from a very dense, hot and opaque initial state. The light that was last scattered about 380,000 years later, when the universe had become transparent, has been redshifted and is now seen as thermal radiation with a temperature of 2.7 K, the cosmic microwave background (CMB). However, since light escapes faster than matter can move, it is prudent to ask how we, made of matter from this very source, can still see the light. In order for this to be possible, the light must take a return path of the right length. A curved return path is possible in spatially closed, balloon-like models, but in standard cosmology, the universe is “flat” rather than balloon-like, and it lacks a boundary surface that might function as a reflector. Under these premises, radiation that once filled the universe homogeneously cannot do so permanently after expansion, and we cannot see the last scattering event. It is shown that the traditional calculation of the CMB temperature is flawed and that light emitted by any source inside the Big Bang universe earlier than half its “conformal age”, also by distant galaxies, can only become visible to us via a return path. Although often advanced as the best evidence for a hot Big Bang, the CMB actually tells against a formerly smaller universe and so do the most distant galaxies. While standard cosmology has additional deficiencies, those disclosed here defy rationality and therefore make a more well-founded cosmology indispensable.

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12

Gibson, Carl H., and R. Norris Keeler. "The cosmic web and microwave background fossilize the first turbulent combustion." Proceedings of the International Astronomical Union 11, S308 (June 2014): 636–37. http://dx.doi.org/10.1017/s1743921316010747.

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AbstractCollisional fluid mechanics theory predicts a turbulent hot big bang at Planck conditions from large, negative, turbulence stresses below the Fortov-Kerr limit (< −10113Pa). Big bang turbulence fossilized when quarks formed, extracting the mass energy of the universe by extreme negative viscous stresses of inflation, expanding to length scales larger than the horizon scale ct. Viscous-gravitational structure formation by fragmentation was triggered at big bang fossil vorticity turbulence vortex lines during the plasma epoch, as observed by the Planck space telescope. A cosmic web of protogalaxies, protogalaxyclusters, and protogalaxysuperclusters that formed in turbulent boundary layers of the spinning voids are hereby identified as expanding turbulence fossils that falsify CDMHC cosmology.

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13

Traunmüller, Hartmut. "Does standard cosmology really predict the cosmic microwave background?" F1000Research 9 (June 3, 2020): 261. http://dx.doi.org/10.12688/f1000research.22432.2.

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In standard Big Bang cosmology, the universe expanded from a very dense, hot and opaque initial state. The light that was last scattered about 380,000 years later, when the universe had become transparent, has been redshifted and is now seen as thermal radiation with a temperature of 2.7 K, the cosmic microwave background (CMB). However, since light escapes faster than matter can move, it is prudent to ask how we, made of matter from this very source, can still see the light. In order for this to be possible, the light must take a return path of the right length. A curved return path is possible in spatially closed, balloon-like models, but in standard cosmology, the universe is “flat” rather than balloon-like, and it lacks a boundary surface that might function as a reflector. Under these premises, radiation that once filled the universe homogeneously cannot do so permanently after expansion, and we cannot see the last scattering event. It is shown that the traditional calculation of the CMB temperature is flawed and that light emitted by any source inside the Big Bang universe earlier than half its “conformal age”, also by distant galaxies, can only become visible to us via a return path. Although often advanced as the best evidence for a hot Big Bang, the CMB actually tells against a formerly smaller universe and so do the most distant galaxies. An attempt to invoke a model in which only time had a beginning, rather than spacetime, has also failed.

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14

Traunmüller, Hartmut. "Does standard cosmology really predict the cosmic microwave background?" F1000Research 9 (July 7, 2020): 261. http://dx.doi.org/10.12688/f1000research.22432.3.

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In standard Big Bang cosmology, the universe expanded from a very dense, hot and opaque initial state. The light that was last scattered about 380,000 years later, when the universe had become transparent, has been redshifted and is now seen as thermal radiation with a temperature of 2.7 K, the cosmic microwave background (CMB). However, since light escapes faster than matter can move, it is prudent to ask how we, made of matter from this very source, can still see the light. In order for this to be possible, the light must take a return path of the right length. A curved return path is possible in spatially closed, balloon-like models, but in standard cosmology, the universe is “flat” rather than balloon-like, and it lacks a boundary surface that might function as a reflector. Under these premises, radiation that once filled the universe homogeneously cannot do so permanently after expansion, and we cannot see the last scattering event. It is shown that the traditional calculation of the CMB temperature is flawed and that light emitted by any source inside the Big Bang universe earlier than half its “conformal age”, also by distant galaxies, can only become visible to us via a return path. Although often advanced as the best evidence for a hot Big Bang, the CMB actually tells against a formerly smaller universe and so do the most distant galaxies. An attempt to invoke a model in which only time had a beginning, rather than spacetime, has also failed.

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15

TURNER, MICHAEL S. "THE NEW COSMOLOGY." International Journal of Modern Physics A 17, no. 24 (September 30, 2002): 3446–57. http://dx.doi.org/10.1142/s0217751x02012843.

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Over the past three years we have determined the basic features of our Universe. It is spatially flat; accelerating; comprised of 1/3 a new form of matter, 2/3 a new form of energy, with some ordinary matter and a dash of massive neutrinos; and it apparently began from a great burst of expansion (inflation) during which quantum noise was stretched to astrophysical size seeding cosmic structure. This "New Cosmology" greatly extends the highly successful hot big-bang model. Now we have to make sense of it. What is the dark matter particle? What is the nature of the dark energy? Why this mixture? How did the matter – antimatter asymmetry arise? What is the underlying cause of inflation (if it indeed occurred)?

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16

Shojaie, H., and M. Farhoudi. "A cosmology with variable c." Canadian Journal of Physics 84, no. 10 (October 1, 2006): 933–44. http://dx.doi.org/10.1139/p06-070.

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A new varying-c cosmological model, constructed using two additional assumptions, which was introduced in our previous work, is briefly reviewed and the dynamic equation of the model is derived distinctly from a semi-Newtonian approach. The results of this model, using a [Formula: see text] term and an extra energy-momentum tensor, are considered separately. It is shown that the Universe began from a hot Big Bang and expands forever with a constant deceleration parameter regardless of its curvature. Finally, the age, the radius, and the energy content of the Universe are estimated and some discussion about the type of the geometry of the Universe is provided. PACS Nos.: 98.80.Bp, 98.80.Jk

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17

Burbidge, G. "Explosive Cosmogony and the Quasi-Steady State Cosmology." Symposium - International Astronomical Union 183 (1999): 286–89. http://dx.doi.org/10.1017/s0074180900132954.

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Modern cosmology began with the realization that there were solutions to Einstein's theory of gravity discovered by Friedmann and Lemaitre which when combined with the redshift distance relation of Hubble and others could be interpreted as showing that we live in an expanding universe. By 1930, the scientific establishment and many of the lay public believed this. It was then only elementary logic to argue that if time reversal was applied, the universe must originally have been so compact that we could talk of a beginning. Lemaitre tried to describe this state as the “Primeval Atom.” For a decade or so after the war, Gamow, Alpher and Herman and other leading physicists explored this dense configuration trying to make the chemical elements from protons and neutrons. They soon learned that this was not possible because of the absence of stable masses of five and eight, but they also realized that if such an early stage had occurred the universe would contain an expanding cloud of radiation which would preserve its black body form. Dicke and his colleagues in Princeton rediscovered this idea and decided to try and detect the radiation. Penzias and Wilson found such a radiation field, and COBE has demonstrated that it has a perfect black body form out to radio wavelengths. This history of the discovery together with the fact that the light elements D, He3 and He4 in about the right amounts can be made in a hot big bang has led to the widely held, but simplistic view, that the standard cosmology - the hot big bang - is correct.

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18

Peng, Qiu-He, Jing-Jing Liu, and Chi-Kang Chou. "A magnetic-monopole-based mechanism to the formation of the Hot Big Bang modeled Universe." Modern Physics Letters A 35, no. 07 (November 20, 2019): 2050030. http://dx.doi.org/10.1142/s0217732320500303.

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There are some particle physics theories that go beyond the so-called “standard cosmological model” to predict the existence of magnetic monopoles (MMs). The discovery of MMs would be an incredible breakthrough in high-energy physics. The existence of MMs in the early Universe has been speculated and anticipated from Grand Unified Theory. If MMs exist, the inverse powers of the unification mass will not suppress the baryon number violating effects of grand unified gauge theories. Therefore, MM catalyzing nucleon decay is a typical strong interaction. This phenomenon is due to the boundary conditions that must be imposed on the core of MM fermion fields. We present a possible mechanism to explain the formation of the Hot Big Bang Cosmology. The main ingredient in our model is nucleon decay catalyzed by MMs (i.e. the Rubakov–Callan effect). It is shown that Hot Big Bang developed naturally because the luminosity due to the Rubakov–Callan effect is much greater than the Eddington luminosity (i.e. [Formula: see text]).

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19

TURNER, MICHAEL S. "MAKING SENSE OF THE NEW COSMOLOGY." International Journal of Modern Physics A 17, supp01 (October 2002): 180–96. http://dx.doi.org/10.1142/s0217751x02013113.

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Over the past three years we have determined the basic features of the Universe — spatially flat; accelerating; comprised of 1/3 a new form of matter, 2/3 a new form of energy, with some ordinary matter and a dash of massive neutrinos; and apparently born from a burst of rapid expansion during which quantum noise was stretched to astrophysical size seeding cosmic structure. The New Cosmology greatly extends the highly successful hot big-bang model. Now we have to make sense of all this: What is the dark matter particle? What is the nature of the dark energy? Why this mixture? How did the matter — antimatter asymmetry arise? What is the underlying cause of inflation (if it indeed occurred)?

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20

Peebles, P. James E. "Dark matter." Proceedings of the National Academy of Sciences 112, no. 40 (May 2, 2014): 12246–48. http://dx.doi.org/10.1073/pnas.1308786111.

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The evidence for the dark matter (DM) of the hot big bang cosmology is about as good as it gets in natural science. The exploration of its nature is now led by direct and indirect detection experiments, to be complemented by advances in the full range of cosmological tests, including judicious consideration of the rich phenomenology of galaxies. The results may confirm ideas about DM already under discussion. If we are lucky, we also will be surprised once again.

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21

Okada, Nobuchika, and Osamu Yasuda. "A Sterile Neutrino Scenario Constrained By Experiments and Cosmology." International Journal of Modern Physics A 12, no. 21 (August 20, 1997): 3669–94. http://dx.doi.org/10.1142/s0217751x97001894.

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We analyze a scheme in which three active neutrinos and one sterile neutrino account for the solar, the atmospheric and the LSND neutrino anomalies in a model-independent way. It is shown that if the equivalent number, Nν, of the light neutrino species is less than 4, then the constraints from these anomalies, accelerator and reactor experiments and big bang nucleosynthesis force a general 4 × 4 mixing matrix to be effectively split into two 2 × 2 matrices. If these neutrinos are of the Majorana type, then negative results of neutrinoless double beta decay experiments imply that the total mass of neutrinos is not sufficient to account for all the hot dark matter components.

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22

Steigman, G. "Primordial Nucleosynthesis For The New Millennium." Symposium - International Astronomical Union 198 (2000): 13–24. http://dx.doi.org/10.1017/s0074180900166355.

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The physics of the standard hot big bang cosmology ensures that the early Universe was a primordial nuclear reactor, synthesizing the light nuclides (D, 3He, 4He, and 7Li) in the first 20 minutes of its evolution. After an overview of nucleosynthesis in the standard model (SBBN), the primordial abundance yields will be presented, followed by a status report (intended to stimulate further discussion during this symposium) on the progress along the road from observational data to inferred primordial abundances. Theory will be confronted with observations to assess the consistency of SBBN and to constrain cosmology and particle physics. Some of the issues/problems key to SBBN in the new millenium will be highlighted, along with a wish list to challenge theorists and observers alike.

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23

Pitrou, Cyril, Alain Coc, Jean-Philippe Uzan, and Elisabeth Vangioni. "A new tension in the cosmological model from primordial deuterium?" Monthly Notices of the Royal Astronomical Society 502, no. 2 (January 20, 2021): 2474–81. http://dx.doi.org/10.1093/mnras/stab135.

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ABSTRACT Recent measurements of the D(p,γ)3He nuclear reaction cross-section and of the neutron lifetime, along with the reevaluation of the cosmological baryon abundance from cosmic microwave background (CMB) analysis, call for an update of abundance predictions for light elements produced during the big-bang nucleosynthesis (BBN). While considered as a pillar of the hot big-bang model in its early days, BBN constraining power mostly rests on deuterium abundance. We point out a new ≃1.8σ tension on the baryonic density, or equivalently on the D/H abundance, between the value inferred on one hand from the analysis of the primordial abundances of light elements and, on the other hand, from the combination of CMB and baryonic oscillation data. This draws the attention on this sector of the theory and gives us the opportunity to reevaluate the status of BBN in the context of precision cosmology. Finally, this paper presents an upgrade of the BBN code primat.

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24

BURGESS, C. P. "BRANE–ANTIBRANE INFLATION." International Journal of Modern Physics D 11, no. 10 (December 2002): 1597–601. http://dx.doi.org/10.1142/s0218271802002955.

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Inflationary cosmology has become central to our understanding of the initial conditions on whose foundations the current successes of the Hot Big Bang model rest. This is despite the well-known difficulties in finding systems whose dynamics naturally provide all of the features which successful inflation demands. Although string theory provides our best description of the physics of the relevant energy scales, it has only recently begun to shed insight into what the inflationary dynamics might be: the physics of brane-antibrane collisions. This essay is meant to summarize the difficulties which have blocked this realization until now, as well as the new insights about inflation which are now beginning to emerge.

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BASILAKOS, SPYROS, JOSÉ ADEMIR SALES LIMA, and JOAN SOLÀ. "FROM INFLATION TO DARK ENERGY THROUGH A DYNAMICAL Λ: AN ATTEMPT AT ALLEVIATING FUNDAMENTAL COSMIC PUZZLES." International Journal of Modern Physics D 22, no. 12 (October 2013): 1342008. http://dx.doi.org/10.1142/s021827181342008x.

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After decades of successful hot big-bang paradigm, cosmology still lacks a framework in which the early inflationary phase of the universe smoothly matches the radiation epoch and evolves to the present "quasi" de Sitter spacetime. No less intriguing is that the current value of the effective vacuum energy density is vastly smaller than the value that triggered inflation. In this paper, we propose a new class of cosmologies capable of overcoming, or highly alleviating, some of these acute cosmic puzzles. Powered by a decaying vacuum energy density, the spacetime emerges from a pure nonsingular de Sitter vacuum stage, "gracefully" exits from inflation to a radiation phase followed by dark matter and vacuum regimes, and, finally, evolves to a late-time de Sitter phase.

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26

Eremeeva, A. I. "Ancient prototypes of the big bang and the Hot Universe (to the prehistory of some fundamental ideas in cosmology)." Astronomical & Astrophysical Transactions 11, no. 2 (November 1996): 193–96. http://dx.doi.org/10.1080/10556799608205465.

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27

Smoot, George F. "Antarctic observations of the cosmic microwave background." Highlights of Astronomy 9 (1992): 589. http://dx.doi.org/10.1017/s1539299600022607.

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In the standard cosmology of the Big Bang theory the cosmic microwave background (CMB) is the remnant radiation from the hot early universe. The sky signal is comprised of radiation from the CMB, from Galactic emission, from atmospheric emission, and from instrument sidelobes seeing the ground and man-made interference. One observes in directions of minimum galactic signal. The antarctic polar plateau provides the best site in the world for low atmospheric emission, low horizons, low man-made interference, and reasonable accessibility. The low column density of precipitable water and extreme stability for periods exceeding a week, combined with low RFI are critical. A very important secondary benefit for anisotropy experiments is the ability to observe the same part of the sky continuously at a high elevation angle.

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28

Read, J. I., and Neil Trentham. "The baryonic mass function of galaxies." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 363, no. 1837 (October 24, 2005): 2693–710. http://dx.doi.org/10.1098/rsta.2005.1648.

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In the Big Bang about 5% of the mass that was created was in the form of normal baryonic matter (neutrons and protons). Of this about 10% ended up in galaxies in the form of stars or of gas (that can be in molecules, can be atomic, or can be ionized). In this work, we measure the baryonic mass function of galaxies, which describes how the baryonic mass is distributed within galaxies of different types (e.g. spiral or elliptical) and of different sizes. This can provide useful constraints on our current cosmology, convolved with our understanding of how galaxies form. This work relies on various large astronomical surveys, e.g. the optical Sloan Digital Sky Survey (to observe stars) and the HIPASS radio survey (to observe atomic gas). We then perform an integral over our mass function to determine the cosmological density of baryons in galaxies: Ω b,gal =0.0035. Most of these baryons are in stars: Ω * =0.0028. Only about 20% are in gas. The error on the quantities, as determined from the range obtained between different methods, is ca 10%; systematic errors may be much larger. Most ( ca 90%) of the baryons in the Universe are not in galaxies. They probably exist in a warm/hot intergalactic medium. Searching for direct observational evidence and deeper theoretical understanding for this will form one of the major challenges for astronomy in the next decade.

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Chernoff, David F., and S. H. Henry Tye. "Inflation, string theory and cosmic strings." International Journal of Modern Physics D 24, no. 03 (February 23, 2015): 1530010. http://dx.doi.org/10.1142/s0218271815300104.

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At its very beginning, the universe is believed to have grown exponentially in size via the mechanism of inflation. The almost scale-invariant density perturbation spectrum predicted by inflation is strongly supported by cosmological observations, in particular the cosmic microwave background (MB) radiation. However, the universe's precise inflationary scenario remains a profound problem for cosmology and for fundamental physics. String theory, the most-studied theory as the final physical theory of nature, should provide an answer to this question. Some of the proposals on how inflation is realized in string theory are reviewed. Since everything is made of strings, some string loops of cosmological sizes are likely to survive in the hot big bang that followed inflation. They appear as cosmic strings, which can have intricate properties. Because of the warped geometry in flux compactification of the extra spatial dimensions in string theory, some of the cosmic strings may have tensions substantially below the Planck or string scale. Such strings cluster in a manner similar to dark matter leading to hugely enhanced densities. As a result, numerous fossil remnants of the low tension cosmic strings may exist within the galaxy. They can be revealed through the optical lensing of background stars in the near future and studied in detail through gravitational wave emission. We anticipate that these cosmic strings will permit us to address central questions about the properties of string theory as well as the birth of our universe.

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30

Craig, William Lane. "Theism and Big Bang cosmology." Australasian Journal of Philosophy 69, no. 4 (December 1991): 492–503. http://dx.doi.org/10.1080/00048409112344901.

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31

Jha, Ramanand. "A cosmology without big bang." General Relativity and Gravitation 26, no. 11 (November 1994): 1067–73. http://dx.doi.org/10.1007/bf02108933.

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32

Kragh, Helge. "Book Review: Recollections of Big Bang Cosmology: Finding the Big Bang." Journal for the History of Astronomy 41, no. 1 (February 2010): 137–38. http://dx.doi.org/10.1177/002182861004100117.

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33

Hodgson, Peter E. "Theism, Atheism and Big Bang Cosmology." International Philosophical Quarterly 35, no. 1 (1995): 105–7. http://dx.doi.org/10.5840/ipq199535167.

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34

Oppy, Graham. "Theism, Atheism, and Big Bang Cosmology." Faith and Philosophy 13, no. 1 (1996): 125–33. http://dx.doi.org/10.5840/faithphil199613115.

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35

Quinn, Philip L., William Lane Craig, and Quentin Smith. "Theism, Atheism, and Big Bang Cosmology." Philosophy and Phenomenological Research 56, no. 3 (September 1996): 733. http://dx.doi.org/10.2307/2108402.

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36

Wilson, Patrick A. "Theism, Atheism, and Big Bang Cosmology." American Catholic Philosophical Quarterly 70, no. 2 (1996): 291–95. http://dx.doi.org/10.5840/acpq19967022.

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37

Swinburne, Richard, William Lane Craig, and Quentin Smith. "Theism, Atheism, and Big Bang Cosmology." Philosophical Review 104, no. 2 (April 1995): 337. http://dx.doi.org/10.2307/2186006.

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38

Stroh, M. "COBE Causes Big Bang in Cosmology." Science News 141, no. 18 (May 2, 1992): 292. http://dx.doi.org/10.2307/3976173.

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39

Gasperini, M., and G. Veneziano. "Pre-big-bang in string cosmology." Astroparticle Physics 1, no. 3 (July 1993): 317–39. http://dx.doi.org/10.1016/0927-6505(93)90017-8.

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40

Veneziano, G. "Inhomogeneous pre-Big Bang string cosmology." Physics Letters B 406, no. 4 (August 1997): 297–303. http://dx.doi.org/10.1016/s0370-2693(97)00688-6.

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41

Wichoski, U. F., and J. A. S. Lima. "Big-bang cosmology with photon creation." Physics Letters A 262, no. 2-3 (November 1999): 103–9. http://dx.doi.org/10.1016/s0375-9601(99)00681-7.

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42

Turner, Michael S. "Cosmology: going beyond the big bang." Physics World 9, no. 9 (September 1996): 31–40. http://dx.doi.org/10.1088/2058-7058/9/9/22.

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43

Voss, David. "Cosmology: Big bang passes COBE test ..." Physics World 5, no. 5 (May 1992): 6. http://dx.doi.org/10.1088/2058-7058/5/5/3.

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44

Lukas, André, and Rudolf Poppe. "Decoherence in Pre-Big-Bang Cosmology." Modern Physics Letters A 12, no. 09 (March 21, 1997): 597–612. http://dx.doi.org/10.1142/s0217732397000625.

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We analyze the quantum cosmology of the simplest pre-big-bang model without dilaton potential. In addition to the minisuperspace variables we include inhomogeneous dilaton fluctuations and determine their wave function on a semiclassical background. This wave function is used to calculate the reduced density matrix and to find criteria for the loss of decoherence. It is shown that coherence between different backgrounds can always be achieved by a specific choice of vacua. Their exact expressions as functions of the wave number and the background quantities are given. Generically, however, decoherence can be expected. In particular, we discuss the implications of these results on the "exit problem" of pre-big-bang cosmology.

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45

Smith, Quentin. "Atheism, theism and big bang cosmology." Australasian Journal of Philosophy 69, no. 1 (March 1991): 48–66. http://dx.doi.org/10.1080/00048409112344511.

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46

Kajantie, K. "Big Bang and Little Bang, Cosmology in the Laboratory." Physica Scripta T23 (January 1, 1988): 7–11. http://dx.doi.org/10.1088/0031-8949/1988/t23/001.

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47

Burbidge, G., F. Hoyle, and J. V. Narlikar. "Quasi-Steady State Cosmology." Symposium - International Astronomical Union 159 (1994): 293–99. http://dx.doi.org/10.1017/s0074180900175199.

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The standard big bang cosmology has the universe created out of a primeval explosion that not only created matter and radiation but also spacetime itself. The big bang event itself cannot be discussed within the framework of a physical theory but the events following it are in principle considered within the scope of science. The recent developments on the frontier between particle physics and cosmology highlight the attempts to chart the history of the very early universe.

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Troitskii, V. S. "Experimental evidence against the Big Bang cosmology." Uspekhi Fizicheskih Nauk 165, no. 6 (1995): 703. http://dx.doi.org/10.3367/ufnr.0165.199506f.0703.

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49

Durrer, R., K. E. Kunze, and M. Sakellariadou. "Particle creation in pre-big-bang cosmology." New Astronomy Reviews 46, no. 11 (October 2002): 659–80. http://dx.doi.org/10.1016/s1387-6473(02)00235-x.

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50

Fields, B. D. "Big bang nucleosynthesis in the new cosmology." European Physical Journal A 27, S1 (February 13, 2006): 3–14. http://dx.doi.org/10.1140/epja/i2006-08-001-2.

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