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Title: Twin mechanism for baryon and dark matter asymmetries

Authors:
; ;
Publication Date:
Sponsoring Org.:
USDOE
OSTI Identifier:
1299441
Grant/Contract Number:
DOE-SC0010008
Resource Type:
Journal Article: Publisher's Accepted Manuscript
Journal Name:
Physical Review D
Additional Journal Information:
Journal Volume: 94; Journal Issue: 3; Related Information: CHORUS Timestamp: 2016-08-19 18:09:31; Journal ID: ISSN 2470-0010
Publisher:
American Physical Society
Country of Publication:
United States
Language:
English

Citation Formats

Farina, Marco, Monteux, Angelo, and Shin, Chang Sub. Twin mechanism for baryon and dark matter asymmetries. United States: N. p., 2016. Web. doi:10.1103/PhysRevD.94.035017.
Farina, Marco, Monteux, Angelo, & Shin, Chang Sub. Twin mechanism for baryon and dark matter asymmetries. United States. doi:10.1103/PhysRevD.94.035017.
Farina, Marco, Monteux, Angelo, and Shin, Chang Sub. 2016. "Twin mechanism for baryon and dark matter asymmetries". United States. doi:10.1103/PhysRevD.94.035017.
@article{osti_1299441,
title = {Twin mechanism for baryon and dark matter asymmetries},
author = {Farina, Marco and Monteux, Angelo and Shin, Chang Sub},
abstractNote = {},
doi = {10.1103/PhysRevD.94.035017},
journal = {Physical Review D},
number = 3,
volume = 94,
place = {United States},
year = 2016,
month = 8
}

Journal Article:
Free Publicly Available Full Text
Publisher's Version of Record at 10.1103/PhysRevD.94.035017

Citation Metrics:
Cited by: 4works
Citation information provided by
Web of Science

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  • Cited by 8
  • The growth and virialization of spherical top-hat fluctuations, in coupled dark energy models, causes segregation between dark matter (DM) and baryons, as the gravitational infall into the potential well proceeds more slowly for the baryons than for DM. As a consequence, after attaining their turnaround and before full virialization, halos have outer layers rich of baryons. Accordingly, a natural ambiguity exists on the definition of the virial density contrast. In fact, when the outer baryon layers infall onto the DM-richer core, they carry with them DM materials outside the original fluctuation; hence, no time exists when all materials originally belongingmore » to the fluctuation--and only they--have virialized. Baryon-DM segregation can have various astrophysical consequences on different length scales. The smallest halos may loose up to 50% of the original baryonic contents and become hardly visible. Subhalos in cluster-size halos may loose much baryonic materials, which could then be observed as intracluster light. Isolated halos, in general, can be expected to have a baryon component richer than the cosmological proportions, due to the cosmic enrichement of baryons lost in small halo encounters.« less
  • The dark energy, dark matter and baryon densities in the Universe are observed to be similar, with a factor of no more than 20 between the largest and smallest densities. We show that this coincidence can be understood via superhorizon domains of randomly varying densities when the baryon density at initial collapse of galaxy-forming perturbations is determined by anthropic selection. The baryon and dark matter densities are assumed to be dependent on random variables θ{sub d} and θ{sub b} according to ρ{sub dm}∝θ{sub d}{sup α} and ρ{sub b}∝θ{sub b}{sup β}, while the effectively constant dark energy density is dependent uponmore » a random variable φ{sub Q} according to ρ{sub Q}∝φ{sub Q}{sup n}. The ratio of the baryon density to the dark energy density at initial collapse, r{sub Q}, and the baryon-to-dark matter ratio, r, are then determined purely statistically, with no dependence on the anthropically-preferred baryon density. We compute the probability distribution for r{sub Q} and r and show that the observed values of r{sub Q} and r can be naturally understood within this framework. In particular, for the case α = 2, β = 1 and n = 4, which can be physically realized via a combination of axion dark matter, Affleck-Dine baryogenesis and frozen quintessence with a φ{sub Q}{sup 4} potential, the range of r{sub Q} and r which corresponds to the observed Universe is a quite natural, with a probability which is broadly similar to other ranges of r{sub Q} and r.« less
  • In the left-right twin Higgs model, one of the neutral Higgses is a natural candidate for WIMP dark matter. We analyzed the dark matter relic density in this framework and identified regions of parameter space that provide the right amount of dark matter. We also studied the dark matter in the more general inert Higgs doublet model in which the mass splittings between the dark matter and other particles do not follow the relations in the left-right twin Higgs model.