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K. Kaneta, Y. Mambrini and K. A. Olive, Radiative production of nonthermal dark matter , Phys. Rev. D99
Original
1901
Earlier work this paper cites.
K. Harigaya, K. Mukaida and M. Yamada, Dark Matter Production during the Thermalization Era , JHEP 07
Original
1901
Earlier work this paper cites.
C. Maldonado and J. Unwin, Establishing the Dark Matter Relic Density in an Era of Particle Decays , JCAP 1906
Original
1902
Earlier work this paper cites.
F. D’Eramo and K. Schmitz, Imprint of a scalar era on the primordial spectrum of gravitational waves , 1904.07870
Original
1904
Earlier work this paper cites.
A. Banerjee, G. Bhattacharyya, D. Chowdhury and Y. Mambrini, Dark matter seeping through dynamic gauge kinetic mixing , 1905.11407
Original
1905
Earlier work this paper cites.
A. Poulin, Dark matter freeze-out in modified cosmological scenarios , Phys. Rev. D100
Original
1905
Earlier work this paper cites.
T. Tenkanen, The Standard Model Higgs and Hidden Sector Cosmology , 1905.11737
Original
1905
Earlier work this paper cites.
N. Bernal and F. Hajkarim, Primordial Gravitational Waves in Nonstandard Cosmologies , Phys. Rev. D100
Original
1905
Earlier work this paper cites.
D. G. Figueroa and E. H. Tanin, Ability of LIGO and LISA to probe the equation of state of the early Universe , JCAP 2019
Original
1905
Earlier work this paper cites.
P. Arias, N. Bernal, A. Herrera and C. Maldonado, Reconstructing Non-standard Cosmologies with Dark Matter , 1906.04183
Original
1906
Earlier work this paper cites.
R. J. Scherrer and M. S. Turner, Decaying Particles Do Not Heat Up the Universe , Phys. Rev. D31
1985
Earlier work this paper cites.
B. Ratra and P. J. E. Peebles, Cosmological Consequences of a Rolling Homogeneous Scalar Field , Phys. Rev. D37
1988
Earlier work this paper cites.
J. McDonald, WIMP Densities in Decaying Particle Dominated Cosmology , Phys. Rev. D43
1991
Earlier work this paper cites.
B. Spokoiny, Deflationary universe scenario , Phys. Lett. B315
1993
Earlier work this paper cites.
S. Sarkar, Big bang nucleosynthesis and physics beyond the standard model , Rept. Prog. Phys. 59
1996
Earlier work this paper cites.
R. R. Caldwell, R. Dave and P. J. Steinhardt, Cosmological imprint of an energy component with general equation of state , Phys. Rev. Lett. 80
1998
Earlier work this paper cites.
D. J. H. Chung, E. W. Kolb and A. Riotto, Production of massive particles during reheating , Phys. Rev. D60
1999
Earlier work this paper cites.
G. F. Giudice and R. Rattazzi, Theories with gauge mediated supersymmetry breaking , Phys. Rept. 322
1999
Earlier work this paper cites.
K. Choi, String or M theory axion as a quintessence , Phys. Rev. D62
2000
Earlier work this paper cites.
G. R. Dvali, G. Gabadadze and M. Porrati, 4-D gravity on a brane in 5-D Minkowski space , Phys. Lett. B485
2000
Earlier work this paper cites.
G. F. Giudice, E. W. Kolb and A. Riotto, Largest temperature of the radiation era and its cosmological implications , Phys. Rev. D64
2001
Earlier work this paper cites.
R. Allahverdi and M. Drees, Thermalization after inflation and production of massive stable particles , Phys. Rev. D66
2002
Earlier work this paper cites.
R. Allahverdi and M. Drees, Production of massive stable particles in inflaton decay , Phys. Rev. Lett. 89
2002
Earlier work this paper cites.
N. Arkani-Hamed, H. Georgi and M. D. Schwartz, Effective field theory for massive gravitons and gravity in theory space , Annals Phys. 305
2003
Earlier work this paper cites.

Similar

N. Okada and O. Seto, Relic density of dark matter in brane world cosmology , Phys. Rev. D70
2004
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C. L. Gardner, Quintessence and the transition to an accelerating universe , Nucl. Phys. B707
2005
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G. B. Gelmini and P. Gondolo, Neutralino with the right cold dark matter abundance in (almost) any supersymmetric model , Phys. Rev. D74
2006
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2006
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2009
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Then

M. A. G. Garcia, Y. Mambrini, K. A. Olive and M. Peloso, Enhancement of the Dark Matter Abundance Before Reheating: Applications to Gravitino Dark Matter , Phys. Rev. D96
Original
2017
Later among the works it cites.
F. D’Eramo, N. Fernandez and S. Profumo, When the Universe Expands Too Fast: Relentless Dark Matter , JCAP 1705
Original
2017
Later among the works it cites.
J. Bramante and J. Unwin, Superheavy Thermal Dark Matter and Primordial Asymmetries , JHEP 02
Original
2017
Later among the works it cites.
B. Dutta, E. Jimenez and I. Zavala, Dark Matter Relics and the Expansion Rate in Scalar-Tensor Theories , JCAP 1706
Original
2017
Later among the works it cites.
K. Benakli, Y. Chen, E. Dudas and Y. Mambrini, Minimal model of gravitino dark matter , Phys. Rev. D95

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2019

Ultraviolet Freeze-in and Non-Standard Cosmologies

Bernal, Nicolás, Elahi, Fatemeh, Maldonado, Carlos et al.

Understand

A notable feature of UV freeze-in is that the relic density is strongly dependent on the highest temperatures of the thermal bath, and a common assumption is that the relevant 'highest temperature' should be the reheating temperature after inflation $T_\text{RH}$.

However, the temperature of the thermal bath can be significantly higher in certain scenarios, reaching a value denoted T max , a fact which is only apparent away from the instantaneous decay approximation.
Interestingly, it has been shown that if the operators are of sufficiently high mass dimension then the dark matter abundance can be enhanced by a 'boost factor' depending on ($T_\text{max}/T_\text{RH}$) relative to naive estimates assuming instantaneous reheating.
We highlight here that in non-standard cosmological histories the critical mass dimension of the operator above at which the instantaneous decay approximation breaks down, and the exponent of the boost factor, depend on the equation of state $\omega$ prior to reheating.