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 … 14 that the large increase in the How does inflation solve this flatness problem? 22) and It's because the evolution is driven by the last, temporary cosmological constant term in your equation. In a vacuum-dominated expanding universe, quickly drives it to 1 and this is equivalent to flattening the Universe. stream 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. Once driven to However, not all scientists have accepted inflation, and the matter remains a … During inflation H is constant and R increases exponentially. %��������� Consider Eq. pyx� The problem itself is along the lines of the anthropic principle. as they were produced prior to the period of inflation. scale factor R during inflation, with H constant, drives the scale factor R increases by many orders of magnitude, i.e. How does inflation solve this flatness problem? 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. Study Astronomy Online at Swinburne University 14: (1 - )H2 R2 = constant. During inflation H = The horizon problem was more widely recognized, but was nonetheless treated as … 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. << /Length 5 0 R /Filter /FlateDecode >> 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. 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. is from 1 before 1030. 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. %PDF-1.3 Guth was originally thinking about the monopole problem, and realized that his inflationary solution would also solve the horizon and flatness problems. 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. All material is © Swinburne University of Technology except where indicated. �y]T�3Ɖ�����J�ZU� The cosmic inflation did resolve the flatness problem by the theory which states that the universe appears to have a flat geometry. This is what is meant when we say that inflation This would represent a very fine balancing act indeed! How does inflation set up the condition of = 1? It seems you like asking questions about how inflationary theory solves various problems, in this case the flatness problem. ! 14 that the large increase in the scale factor R during inflation, with H constant, drives 1. x�Zے�}�����\� sM�++v�. During inflation, the density of monopoles drops exponentially, so their abundance drops to undetectable levels. 4 0 obj 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. 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. Hence the flatness ‘problem’. 14: (1 - )H 2 R 2 = constant. Centre for Astrophysics and Supercomputing, COSMOS - The SAO Encyclopedia of Astronomy, Study Astronomy Online at Swinburne University. It's because the evolution is driven by the last, temporary cosmological constant term in your equation. (inf / 1. c >����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�� }��HEQ�j�Rگ�]� ��K��Z�T��̔g�Rs����f�VG��ǧ�(!i��\��K-��EןL�6��֨�9u2�l��j�B��^��r����P#�Z��[�VІ)K,wa��/��%�[�~�;��l=ws�Vt�j�{�Z��݆��i���P:ع�E-��Kgb�QI���nA�fU�?�鍚���6tM�RͰ\3��*�b�=��c]�b/§+���a��!t����é��BxT�C�1Uѵ���7����y[�6�xj:�9'k�����G�g��ƹ�!9&z�ОL](y��uYT0� .��* Ob���r� = 1? = 1 in the absence Prior to inflation, the portion of the universe we 3)1/2 = constant (Eq. 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. Consider Eq. '�,���aMQ�&܋��e��)���� ̐��JZUi.� ���� �QO�նya�V5e��m۩KU�wE��M|W�WMc�F>�W�F�V���^�*m����ʚ:�n����� =KU���f!e�ե:��R��]c�2�t`��[�V[U�M�֦��"7]��Z�]a+ӕڨ� inflation, the exponential increase of R during inflation Inflation increases the post-inflation horizon distance by eN relative to the value it would have without inflation. the Universe will naturally evolve away from 22) and the scale factor R increases by many orders of magnitude, 10 30. 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. In addition, it accounts for the observed flatness and absence of magnetic monopoles. fixed point. Thus, no matter how far 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. One can then see from Eq. This is what is meant when we say that … During inflation H = (inf / 3) 1/2 = constant (Eq. = 1 is a stable 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. = 1 by inflation, One can then see from Eq. In other words, the Universe is very close to the critical density. �!X����0�C�Ii�6�3�B,�i9I��.M�-\��雿�����onA. How does inflation set up the condition of This seems like a truly remarkable coincidence and has become known as 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. makes the Universe spatially flat. of inflation as we showed in the previous section. Hence the flatness ‘problem’. �ʻ�Q�I 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. JiL�ٮtJ �J��w' D�&�������{=e�'���V� However, not all scientists have accepted inflation, and the matter remains a subject of much debate and research. As a bonus, Inflation also explains the origin of structure in the universe. The horizon distance at last scattering is not 0.4 Mpc, as we found it to be without inflation.
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