History of the Universe History

Черепащук, А. М.

doi:10.3367/ufnr.0183.201305i.0535

Cited by 19 publications

(10 citation statements)

References 73 publications

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“…where Φ i is the gravitational potential at the time the perturbation scale was much larger than the cosmological horizon. The distribution of Φ i can be obtained from (7). The power spectrum of the potential is described by a formula similar to Eqn (7), but with A Φ = (4/9)A R [2].…”

Section: Spherical Model Of the Evolution Of Perturbationsmentioning

confidence: 99%

“…Modern cosmology (see monographs [1][2][3][4][5], review [6], and historical overview [7]) studies the most fundamental problems of the origin of our Universe by combining the physics of elementary particles and quantum field theory, especially as regards studying the very early epochs. The inflationary paradigm as part of quantum cosmology should be specially mentioned here.…”

mentioning

confidence: 99%

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Small scale clumps of dark matter

Berezinsky¹,

Dokuchaev²,

Eroshenko³

2014

Успехи физических наук

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®ÂÔÔÂ M min ÏÑAEÇÎßÐÑ-ÊÂÄËÔËÏÂ, ÒÓÇAEÔÍÂÊÞÄÂÇÏÂâ ÄÇÎËÚËÐÂ M min AEÎâ ÐÇÌÕÓÂÎËÐÑ Ä ®ËÐËÏÂÎßÐÑÌ ÔÖÒÇÓ-ÔËÏÏÇÕÓËÚÐÑÌ ÏÑAEÇÎË ÏÑÉÇÕ ËÊÏÇÐâÕßÔâ ÑÕ 10 À11 M AEÑ 10 À3 M [41,42,46,58,59]. ®ËÐËÏÂÎßÐÂâ ÏÂÔÔÂ ÔÅÖÔÕÍÑÄ (ÑÃÓÇÊÂÐËÇ ÔÒÇÍÕÓÂ ÏÂÔÔ) M min ÑÒÓÇAEÇÎâÇÕÔâ ÔÕÑÎÍÐÑÄË- ØÂÓÂÍÕÇÓËÊÖÇÕÔâ ÔÒÇÍÕÓÑÏ ÏÑÜÐÑÔÕË Pk: ÔÏ., ÐÂÒÓËÏÇÓ, [89, 90]). ¥Îâ ÏÇÎÍÑÏÂÔÛÕÂÃÐÞØ ÏÑAE Ô ÎÑÅÂÓË×ÏËÚÇÔÍÑÌ ÕÑÚ-ÐÑÔÕßá ÔÒÓÂÄÇAEÎËÄÑ ÔÑÑÕÐÑÛÇÐËÇ Tk 9 k eq ak 2 , ÇÔÎË k eq ak 5 1. ³ÓÇAEÐËÌ ÍÄÂAEÓÂÕ ÄÑÊÏÖÜÇÐËâ sR hd 2 i Ä ÏÂÔÛÕÂÃÇ R ÄÞÓÂÉÂÇÕÔâ ÚÇÓÇÊ Pk ÔÎÇAEÖáÜËÏ ÑÃÓÂÊÑÏ: £ËAEÐÑ, ÚÕÑ ÒÓË n s % Tam w p . ±ÖÔÕß dp ì ËÏÒÖÎßÔ, ÒÓËÑÃÓÇÕÂÇÏÞÌ ÐÇÌÕÓÂÎËÐÑ Ä ÑAEÐÑÏ ÓÂÔÔÇâÐËË: dp 2 2o 2 1 À cos y, ÅAEÇ o Ë y ì ÔÑÑÕÄÇÕÔÕÄÇÐÐÑ àÐÇÓÅËâ Ë ÖÅÑÎ ÓÂÔÔÇâÐËâ ×ÇÓÏËÑÐÂ.´ÑÅAEÂ AEÎâ ÄÓÇÏÇÐË ÓÇÎÂÍÔÂÙËË t rel ÏÑÉÐÑ ÊÂÒËÔÂÕß ÅAEÇ f 1 9 0Y2À0Y3. ³ ÍÂÚÇÔÕÄÇÐÐÑÌ ÕÑÚÍË ÊÓÇÐËâ, ÒÇÓÄÞÌ ÏÐÑÉËÕÇÎß n Ä (88) ÔÑÑÕÄÇÕÔÕÄÖÇÕ ÕÑÏÖ ×ÂÍÕÖ, ÚÕÑ ÔÅÖÔÕÍË, ÑÃÓÂÊÑÄÂÄ-ÛËÇÔâ ËÊ ÄÞÔÑÍËØ ÒËÍÑÄ (Ô ÃÑÎßÛÇÌ ÄÇÎËÚËÐÑÌ n), ÖÔÒÇÛ-ÐÇÇ ÒÇÓÇÉËÄÂáÕ ÒÓÑÙÇÔÔÞ ÓÂÊÓÖÛÇÐËâ, ÚÇÏ ÔÅÖÔÕÍË, ÑÃÓÂÊÑÄÂÄÛËÇÔâ ËÊ ÐËÊÍËØ ÒËÍÑÄ (Ô ÏÇÐßÛËÏ n). ªÐÕÇÅ-ÓËÓÖâ (88) ÒÑ n, ÒÑÎÖÚÂÇÏ £ ÒÓÇAEÒÑÎÑÉÇÐËË, ÚÕÑ ÍÑÐÙÇÐÕÓÂÙËâ ÔÅÖÔÕÍÑÄ ÒÓÑ-ÒÑÓÙËÑÐÂÎßÐÂ ÒÎÑÕÐÑÔÕË ÅÂÎÑ, Õ.Ç. n cl l xr DM l aM, AEÎâ ÍÑà××ËÙËÇÐÕÂ ÖÔËÎÇÐËâ ÒÑÎÖÚÂÇÏ ÖAEÑÃÐÖá ÑÙÇÐÍÖ: (2003) [JETP Lett. 77 335 (2003) Small scale clumps of dark matter are gravitationally bounded structures that have masses comparable to or lower than stellar masses and consist of non-or weakly interacting dark matter particles. In this paper the current knowledge of how such structures form and evolve is reviewed, various types of spectra of primordial cosmological perturbations are considered, and various dark matter models are examined. Depending on the particular spectrum type, dark matter clumps may differ considerably in their formation processes and ultimate characteristics. The role of clumps in experiments on dark matter particles indirect detection via their annihilation products is discussed. A number of astrophysical problems and phenomena that are related to dark matter clumps are examined.PACS numbers: 14.80. Nb, 95.35.+d, 98.70.Rz

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Section: Spherical Model Of the Evolution Of Perturbationsmentioning

confidence: 99%

mentioning

confidence: 99%

Small scale clumps of dark matter

Berezinsky¹,

Dokuchaev²,

Eroshenko³

2014

Успехи физических наук

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“…Sketch of the evolution of dark energy with an arbitrary equation of state p(ρ). At each point, the curve p = p(ρ) can be approximated by linear dependence(18).…”

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confidence: 99%

“…Whatever the nature of dark energy, it can be effectively characterized by the pressure and density, and it is possible to introduce their ratio w ≡ p/ρ, also known as the equation-of-state parameter. The notion of the cosmological constant (Λ-term), which was introduced by Einstein [13]) and subsequently rejected by him (see [14,15]) after reading Fiedmann's paper [16] (also see [17]) and recognizing the observational evidence of the expansion of the universe [18], has seen a rebirth due to astronomical observations since the discovery of dark energy.…”

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confidence: 99%

Black holes in the presence of dark energy

Babichev¹,

Dokuchaev²,

Eroshenko³

2013

Успехи физических наук

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The new, rapidly developing field of theoretical research -studies of dark energy interacting with black holes (and, in particular, accreting onto black holes) -is reviewed. The term 'dark energy' is meant to cover a wide range of field theory models, as well as perfect fluids with various equations of state, including cosmological dark energy. Various accretion models are analyzed in terms of the simplest test field approximation or by allowing back reaction on the black-hole metric. The behavior of various types of dark energy in the vicinity of Schwarzschild and electrically charged black holes is examined. Nontrivial effects due to the presence of dark energy in the black hole vicinity are discussed. In particular, a physical explanation is given of why the black hole mass decreases when phantom energy is being accreted, a process in which the basic energy conditions of the famous theorem of nondecreasing horizon area in classical black holes are violated. The theoretical possibility of a signal escaping from beneath the black hole event horizon is discussed for a number of dark energy models. Finally, the violation of the laws of thermodynamics by black holes in the presence of noncanonical fields is considered.

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“…Last decades many attempts have been done to detect the dark matter [1][2][3] as weakly interacting massive particles (WIMPs), but with no result up to now. Other dark matter candidates are topological defects which could bear energy (mass): domain walls, strings 4,5 , vertices, dark atoms, etc.…”

Section: Introductionmentioning

confidence: 99%

Deformed compact extra space as dark matter candidate

Gani

Dmitriev

Rubin

2015

Int. J. Mod. Phys. D

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We elaborate the possibility for a deformed extra space to be considered as the dark matter candidate. To perform calculations a class of two-dimensional extra metrics was considered in the framework of the multidimensional gravity. It was shown that there exists a family of stationary metrics of the extra space possessing point-like defect. Estimation of cross section of scattering of a particle of the ordinary matter on a spatial domain with deformed extra space is in agreement with the observational constraints.Comment: 12 pages, 5 figures; V2: some changes to match version published in IJMP

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History of the Universe History

Cited by 19 publications

References 73 publications

Small scale clumps of dark matter

Small scale clumps of dark matter

Black holes in the presence of dark energy

Deformed compact extra space as dark matter candidate

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