Supersymmetric dark matter

Jungman, Gerard; Kamionkowski, Marc; Griest, K.

doi:10.1016/0370-1573(95)00058-5

Cited by 4,408 publications

(6,259 citation statements)

References 308 publications

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“…where we have introduced 6) and the derivatives of the delta function that appear above are as usual defined in terms of integration by parts. After these preliminaries, let us now start to calculate the expansion coefficients C j .…”

Section: B the Collision Term For Two-body Scattering Processesmentioning

confidence: 99%

Thermal decoupling of WIMPs from first principles

Bringmann

Hofmann

2007

J. Cosmol. Astropart. Phys.

186

227

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Abstract. Weakly interacting massive particles (WIMPs) are arguably the most natural DM candidates from a particle physics point of view. After their number density has frozen out in the early universe, determining their relic density today, WIMPs are still kept very close to thermal equilibrium by scattering events with standard model particles. The complete decoupling from the thermal bath happens as late as around ∼ 1 − 10 MeV, thereby setting an important cosmological scale that can directly be translated into a small-scale cutoff of the spectrum of matter density fluctuations. We present here a full analytic treatment of the kinetic decoupling process from first principles. This allows an exact determination of the decoupling scale, for an arbitrary WIMP candidate and any scattering amplitude. As an application, we consider the situation of the lightest supersymmetric particle as well as the lightest Kaluza-Klein particle that arises in theories with universal extra dimensions; furthermore, we show that our formalism can also easily be applied to, e.g., the evolution of the non-relativistic electrons into the recombination regime. Finally, we comment on the impacts for the smallest gravitationally bound structures and the prospects for the indirect detection of dark matter.

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Section: B the Collision Term For Two-body Scattering Processesmentioning

confidence: 99%

Thermal decoupling of WIMPs from first principles

Bringmann

Hofmann

2007

J. Cosmol. Astropart. Phys.

186

227

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“…This point, subsequently also recognized in Ref. [13], was usually overlooked in subsequent papers, though the afore mentioned uncertainties still persist. The common practice prevailed of employing, for the relevant couplings, some standard values, which became consolidated more because of their reiterated use, rather than because of confirmation by more refined theoretical analyses.…”

Section: Introductionmentioning

confidence: 81%

“…This has quite significant consequences on the size of σ (nucleon) scalar , because m s < N|ss|N > is the most important term among the m q < N|qq|N >'s [47], unless tan β is very small (see Eqs. (6),(12), (13)). …”

Section: Size Of the Higgs-quark Couplingsmentioning

confidence: 99%

Implications for relic neutralinos of the theoretical uncertainties in the neutralino–nucleon cross section

Bottino

Donato

Fornengo

et al. 2000

Astroparticle Physics

172

179

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We discuss the effect induced on the neutralino-nucleon cross-section by the present uncertainties in the values of the quark masses and of the quark scalar densities in the nucleon. We examine the implications of this aspect on the determination of the neutralino cosmological properties, as derived from measurements of WIMP direct detection. We show that, within current theoretical uncertainties, the DAMA annual modulation data are compatible with a neutralino as a major dark matter component, to an extent which is even larger than the one previously derived. We also comment on implications of the mentioned uncertainties for experiments of indirect dark matter detection. *

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“…WIMPs are stable particles which arise in several extensions of the Standard Model of electroweak interactions. Typically they are presumed to have masses between 10 GeV and a few TeV and interact with ordinary matter only weakly (for reviews, see [6]). …”

Section: Introductionmentioning

confidence: 99%

“…We remind the reader that N−body simulations of the spatial distribution of Cold Dark Matter (which includes WIMPs) seem to be at odds with observations at least in the central region of galaxies [10]; this may have ramifications for f 1 as well. On the theory side, several modifications of the standard "shifted Maxwellian" distribution [6] have been suggested, ranging from co-or counter-rotating halos [11] to scenarios where the threedimensional WIMP velocity distribution gets large contributions from discrete "streams" with (nearly) fixed velocity [12,13].…”

Section: Introductionmentioning

confidence: 99%

Model-independent determination of the WIMP mass from direct dark matter detection data

Drees

Shan

2008

J. Cosmol. Astropart. Phys.

226

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Weakly Interacting Massive Particles (WIMPs) are one of the leading candidates for Dark Matter. We develop a model-independent method for determining the mass m χ of the WIMP by using data (i.e., measured recoil energies) of direct detection experiments. Our method is independent of the as yet unknown WIMP density near the Earth, of the form of the WIMP velocity distribution, as well as of the WIMP-nucleus cross section. However, it requires positive signals from at least two detectors with different target nuclei. In a background-free environment, m χ ∼ 50 GeV could in principle be determined with an error of ∼ 35% with only 2 × 50 events; in practice upper and lower limits on the recoil energy of signal events, imposed to reduce backgrounds, can increase the error. The method also loses precision if m χ significantly exceeds the mass of the heaviest target nucleus used.

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Supersymmetric dark matter

Cited by 4,408 publications

References 308 publications

Thermal decoupling of WIMPs from first principles

Thermal decoupling of WIMPs from first principles

Implications for relic neutralinos of the theoretical uncertainties in the neutralino–nucleon cross section

Model-independent determination of the WIMP mass from direct dark matter detection data

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