Damping scales of neutralino cold dark matter

By S. Hofmann, D. Schwarz, H. Stoecker. 2001

232 citations recorded by the source corpus.

The lightest supersymmetric particle, most likely the neutralino, might account for a large fraction of dark matter in the Universe. We show that the primordial spectrum of density fluctuations in neutralino cold dark matter (CDM) has a sharp cutoff due to two damping mechanisms: collisional damping during the kinetic decoupling of the neutralinos at about 30 MeV (for typical neutralino and sfermion masses) and free streaming after the last scattering of neutralinos. The last scattering temperature is lower than the kinetic decoupling temperature by one order of magnitude. The cutoff in the primordial spectrum defines a minimal mass for CDM objects in hierarchical structure formation. For typical neutralino and sfermion masses the first gravitationally bound neutralino clouds have to have masses above ${10}^{\ensuremath{-}7}{M}_{\ensuremath{\bigodot}}.$

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/897583be3743e000f7759f7d33e6ebc881e5469c

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Citations in the corpus

Non-Abelian dark matter and dark radiation (2015, result): “[21] S.”
Hundreds of Milky Way Satellites? Luminosity Bias in the Satellite Luminosity Function (2008, background): “…extreme (larger than a factor of 1010) when compared to the full mass function of CDM subhalos, which is expected to rise as 1/M down to the small-scale clustering cutoff for the dark matter particle,McutT1M (Hofmann et al. 2001; Bertschinger 2006; Profumo et al. 2006; Johnson & Kamionkowski 2008).”
Characterization of subhalo structural properties and implications for dark matter annihilation signals (2016, background): “The minimum halo mass depends on the free-streaming of DM particles from high to low density regions (Zybin et al. 1999; Hofmann et al. 2001; Berezinsky et al. 2003; Green et al. 2005) and on the effect of acoustic oscillations (Loeb & Zaldarriaga 2005; Bertschinger 2006).”
Multi-frequency analysis of neutralino dark matter annihilations in the Coma cluster (2005, methodology): “9s exp [ − ( Ms Mcut )−2/3] , (21) Diemand et al. 2005 where Mcut is the free streaming cutoff mass (Hofmann et al. 2001, Chen et al. 2001, Green et al. 2005, Diemand et al. 2005), while the normalization A(Mvir) is derived imposing that the total mass in subhalos is a fraction fs of the total…”
SEARCH FOR DARK MATTER SATELLITES USING FERMI-LAT (2012, unknown): “…the resolution to recover all satellites down to a mass of "-' 10 6 1\1(,), the minimum mass of a bound satellite orbiting the Milky Way may be as low as the Earth mass ("-' 10-6 1\1(,)), a scale that is roughly set by the WIMP velocity at freeze-out (Hofmann et al. 2001; Loeb & Zaldarriaga 2005).”
The power spectrum of SUSY-CDM on subgalactic scales (2003, background): “Hofmann et al. (2001) calculated the effect of these processes on the primordial density perturbations and found exponential damping with a characteristic comoving wavenumber kd ≈ 1.8 ( m Tkd )1/2 akd a0 Hkd , ≈ 3.8 × 10 7 Mpc ( m 100 GeV )1/2 ( Tkd 30 MeV )1/2 .”
Halo mass function and the free streaming scale (2013, background): “However, for a 100 GeV neutralino with a decoupling temperature of 30 MeV the half-mode mass is M = 2.9 × 10−6h−1M , which roughly corresponds to the mass of the Earth.”
The Aquarius Project: the subhaloes of galactic haloes (2008, background): “Depending on the specific particle physics model, this cut-off lies around an Earth mass, at ∼ 10−6 M⊙, but could be as low as 10−12 M⊙ in certain scenarios (Hofmann et al., 2001; Green et al., 2004).”
Gravitational probes of dark matter physics (2017, background): “This occurs at a temperature Tkd, with the approximate relation [172, 173, 174, 175]”