Quintessence and the relic density of neutralinos

By P. Salati. 2002

219 citations recorded by the source corpus.

Abstract The archetypal model for the recently discovered dark energy component of the universe is based on the existence of a scalar field whose dynamical evolution comes down today to a non-vanishing cosmological constant. In the past—before big-bang nucleosynthesis for that matter—that scalar field could have gone through a period of kination during which the universe has expanded at a much higher pace than what is currently postulated in the standard radiation dominated cosmology. I examine here the consequences of such a period of kination on the relic abundance of neutralinos and find that the latter could be much higher—by three orders of magnitude—than what is estimated in the canonical derivation. I shortly discuss the implications of this scenario for the dark matter candidates and their astrophysical signatures.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/e887a818f8ed7d8ec2a1e1c0517dc09cae01f283

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. N. Fornengo
2. R. Lineros
3. J. Lavalle
4. T. Delahaye
5. D. Morrissey
6. Yanou Cui
7. F. Donato
8. J. Wells

In Nuclear and High Energy Physics

1. N. Fornengo
2. R. Lineros
3. J. Lavalle
4. T. Delahaye
5. D. Morrissey
6. Yanou Cui
7. F. Donato
8. J. Wells

Citations in the corpus

• Galactic electrons and positrons at the Earth: new estimate of the primary and secondary fluxes (2010, background): “…1998; Lavalle et al. 2008a; Delahaye et al. 2008; Bergström et al. 2008), or the expansion rate is more rapid than expected in the early universe, before the primordial nucleosynthesis (see Salati 2003 for the original idea, and e.g. Catena et al. 2009 more specifically for the positron channel).”
• Probing the pre-BBN universe with gravitational waves from cosmic strings (2018, background): “This behavior arises in models of inflation, quintessence, dark energy, and axions, and is called kination [11, 12, 16].”
• WIMP dark matter candidates and searches—current status and future prospects (2017, unknown): “[90] for a discussion for quintessence).”
• An Introduction to Particle Dark Matter (2019, unknown): “This phase is called Kination [23].”