�y]T�3Ɖ�����J�ZU� How does inflation solve this flatness problem? %PDF-1.3 In addition, it accounts for the observed flatness and absence of magnetic monopoles. = 1 in the absence Hence the flatness ‘problem’. This is what is meant when we say that … Ω0 initially must have been almost exactly: There is no known reason for the density of the Universe to be so close to the critical density, and this appears to be an unacceptably strange coincidence in the view of most astronomers. However, not all scientists have accepted inflation, and the matter remains a … It's because the evolution is driven by the last, temporary cosmological constant term in your equation.
Prior to inflation, the portion of the universe we It seems you like asking questions about how inflationary theory solves various problems, in this case the flatness problem.
To phrase it more scientifically, the flatness problem arises because we appear to live in a Universe that has an observed a density parameter (Ω0) very close to 1.
As discussed here and elsewhere, whether these are problems and whether inflation can solve them satisfactorily are other questions, but it is not just some sort of ad-hoc explanation. pyx� �!X����0�C�Ii�6�3�B,�i9I��.M�-\��雿�����onA. However, not all scientists have accepted inflation, and the matter remains a subject of much debate and research. The cosmic inflation did resolve the flatness problem by the theory which states that the universe appears to have a flat geometry. The cosmic inflation solves the flatness problem because it reverses the evolution | Ω − 1 |: as time goes to the future, | Ω − 1 | is (more precisely, was) decreasing in this case. Guth was originally thinking about the monopole problem, and realized that his inflationary solution would also solve the horizon and flatness problems. Many attempts have been made to explain the flatness problem, and modern theories now include the idea of inflation which predicts the observed flatness of the Universe. This would represent a very fine balancing act indeed! During inflation, the density of monopoles drops exponentially, so their abundance drops to undetectable levels. 3)1/2 = constant (Eq. (inf /
As a bonus, Inflation also explains the origin of structure in the universe. Centre for Astrophysics and Supercomputing, COSMOS - The SAO Encyclopedia of Astronomy, Study Astronomy Online at Swinburne University.
22) and The ‘problem’ is that for the Universe to be so close to critical density after ~ 14 billion years of expansion and evolution, it must have been even closer at earlier times. the Universe will naturally evolve away from
Hence the flatness ‘problem’. ! 14: (1 - )H2 R2 = constant. the scale factor R increases by many orders of magnitude, During inflation H = (inf / 3) 1/2 = constant (Eq. 14 that the large increase in the For instance, it requires the density at the Planck time (within 10-43 seconds of the Big Bang) to be within 1 part in 1057 of the critical density. 22) and the scale factor R increases by many orders of magnitude, 10 30. >����N0W7��Ç�z�ѻ���oȼ1U�975�5��U7(Bnט���-*���
T�t�We�Byx�Ί�� ��s��@�+b���9a�� l�k|��*`�]�N�9p�ǡ�u��8 �s흛 � Q�O ]�!4]1u����e��lB\�PJ�� How does inflation set up the condition of = 1? All material is © Swinburne University of Technology except where indicated. This seems like a truly remarkable coincidence and has become known as the ‘flatness problem’. as they were produced prior to the period of inflation.
%��������� One can then see from Eq. Inflation is a mechanism for realizing the cosmological principle, which is the basis of the standard model of physical cosmology: it accounts for the homogeneity and isotropy of the observable universe. 1. JiL�ٮtJ �J��w' D�&�������{=e�'���V� In other words, the Universe is very close to the critical density.
4 0 obj = 1 by inflation, The horizon distance at last scattering is not 0.4 Mpc, as we found it to be without inflation. How does inflation solve this flatness problem? So what we mean when we say that inflation requires a certain number of e-folds (60 or so) to "solve" the flatness problem is that inflation needs to have lasted that long in order … During inflation H is constant and R increases exponentially. A flat Universe is one in which the amount of matter present is just sufficient to halt its expansion, but insufficient to re-collapse it. of inflation as we showed in the previous section. How does inflation set up the condition of Inflation increases the post-inflation horizon distance by eN relative to the value it would have without inflation. Many attempts have been made to explain the flatness problem, and modern theories now include the idea of inflation which predicts the observed flatness of the Universe.
i.e. If you work out the mathematics, you find that while in a decelerating universe the curvature deviates away from flatness as time goes on, during inflation it deviates towards flatness, even if it started out in some highly curved state.
is from 1 before With inflation it is larger by a factor e100=1043, which is more than enough for the whole last scattering surface to be in causal contact. One can then see from Eq. Once driven to Thus, no matter how far 1030. 14: (1 - )H 2 R 2 = constant.
x�Zے�}�����\� sM�++v�. The cosmic inflation solves the flatness problem because it reverses the evolution | Ω − 1 |: as time goes to the future, | Ω − 1 | is (more precisely, was) decreasing in this case. c
inflation, the exponential increase of R during inflation
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quickly drives it to 1 and this is equivalent to flattening the Universe.
Imagine the surprise of astronomers to find that, as near as we can tell, the Universe has exactly the required density of matter to be flat. This is what is meant when we say that inflation Study Astronomy Online at Swinburne University
The horizon problem was more widely recognized, but was nonetheless treated as … = 1? = 1 is a stable makes the Universe spatially flat. During inflation H = I argue that before the development of the inflationary model, the flatness problem was generally not considered a serious scientific problem by most researchers in the cosmology community.
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It's because the evolution is driven by the last, temporary cosmological constant term in your equation.
Consider Eq. fixed point.
The problem itself is along the lines of the anthropic principle.
14 that the large increase in the scale factor R during inflation, with H constant, drives 1.
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