Cosmic abundances of stable particles: Improved analysis

Gondolo, Paolo; Gelmini, Graciela B.

doi:10.1016/0550-3213(91)90438-4

Cited by 1,410 publications

(1,821 citation statements)

References 8 publications

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“…In general for WIMP DM x f ≈ 20 − 25 [55]. The precise relation between the WIMP mass and the required Yukawa coupling to attain the relic density condition is shown in Fig.…”

Section: A Constraints From Direct Dm Searchesmentioning

confidence: 97%

Majorana dark matter through the Higgs portal under the vacuum stability lamppost

et al. 2015

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We study the vacuum stability of a minimal Higgs portal model in which the standard model (SM) particle spectrum is extended to include one complex scalar field and one Dirac fermion. These new fields are singlets under the SM gauge group and are charged under a global U (1) symmetry. Breaking of this U (1) symmetry results in a massless Goldstone boson, a massive CPeven scalar, and splits the Dirac fermion into two new mass-eigenstates, corresponding to Majorana fermions. The lightest Majorana fermion (w) is absolutely stable, providing a plausible dark matter (DM) candidate. We show that interactions between the Higgs sector and the lightest Majorana fermion which are strong enough to yield a thermal relic abundance consistent with observation can easily destabilize the electroweak vacuum or drive the theory into a non-perturbative regime at an energy scale well below the Planck mass. However, we also demonstrate that there is a region of the parameter space which develops a stable vacuum (up to the Planck scale), satisfies the relic abundance, and is in agreement with direct DM searches. Such an interesting region of the parameter space corresponds to DM masses 350 GeV mw 1 TeV. The region of interest is within reach of second generation DM direct detection experiments.

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“…In general for WIMP DM x f ≈ 20 − 25 [55]. The precise relation between the WIMP mass and the required Yukawa coupling to attain the relic density condition is shown in Fig.…”

Section: A Constraints From Direct Dm Searchesmentioning

confidence: 97%

Majorana dark matter through the Higgs portal under the vacuum stability lamppost

et al. 2015

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“…We use in DarkSUSY the full cross section and solve the Boltzmann equation numerically with the method given in [25,26]. In this way we automatically take care of thresholds and resonances.…”

Section: Calculation Of Relic Densitymentioning

confidence: 99%

DarkSUSY: computing supersymmetric dark matter properties numerically

Gondolo

Edsjö

Ullio

et al. 2004

J. Cosmol. Astropart. Phys.

909

1,059

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The question of the nature of the dark matter in the Universe remains one of the most outstanding unsolved problems in basic science. One of the best motivated particle physics candidates is the lightest supersymmetric particle, assumed to be the lightest neutralino -a linear combination of the supersymmetric partners of the photon, the Z boson and neutral scalar Higgs particles. Here we describe DarkSUSY, a publicly-available advanced numerical package for neutralino dark matter calculations. In DarkSUSY one can compute the neutralino density in the Universe today using precision methods which include resonances, pair production thresholds and coannihilations. Masses and mixings of supersymmetric particles can be computed within DarkSUSY or with the help of external programs such as FeynHiggs, ISASUGRA and SUSPECT. Accelerator bounds can be checked to identify viable dark matter candidates. DarkSUSY also computes a large variety of astrophysical signals from neutralino dark matter, such as direct detection in low-background counting experiments and indirect detection through antiprotons, antideuterons, gamma-rays and positrons from the Galactic halo or high-energy neutrinos from the center of the Earth or of the Sun. Here we describe the physics behind the package. A detailed manual will be provided with the computer package.

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“…when the LSP is the gravitino and the NLSP is a neutralino. The relic abundance of the NLSP neutralino is determined at the time of chemical decoupling by the standard argument (Gondolo & Gelmini 1991;Griest & Seckel 1991). Eventually, the non-relativistic neutralinos decay into LSP gravitinos that become WDM.…”

Section: Wdm Produced By the Non-relativistic Particle Decaymentioning

confidence: 99%

Structure of dark matter halos in warm dark matter models and in models with long-lived charged massive particles

Kamada

Yoshida

Kohri

et al. 2013

J. Cosmol. Astropart. Phys.

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We study the formation of non-linear structures in Warm Dark Matter (WDM) models and in a Long-Lived Charged Massive Particle (CHAMP) model. CHAMPs with a decay lifetime of about 1 yr induce characteristic suppression in the matter power spectrum at subgalactic scales through acoustic oscillations in the thermal background. We explore structure formation in such a model. We also study three WDM models, where the dark matter particles are produced through the following mechanisms: i) WDM particles are produced in the thermal background and then kinematically decoupled; ii) WDM particles are fermions produced by the decay of thermal heavy bosons; and iii) WDM particles are produced by the decay of non-relativistic heavy particles. We show that the linear matter power spectra for the three models are all characterised by the comoving Jeans scale at the matter-radiation equality. Furthermore, we can also describe the linear matter power spectrum for the Long-Lived CHAMP model in terms of a suitably defined characteristic cut-off scale k Ch , similarly to the WDM models. We perform large cosmological N -body simulations to study the non-linear growth of structures in these four models. We compare the halo mass functions, the subhalo mass functions, and the radial distributions of subhalos in simulated Milky Way-size halos. For the characteristic cut-off scale k cut = 51 h Mpc −1 , the subhalo abundance -2 -(∼ 10 9 M sun ) is suppressed by a factor of ∼ 10 compared with the standard ΛCDM model. We then study the models with k cut ≃ 51, 410, 820 h Mpc −1 , and confirm that the halo and the subhalo abundances and the radial distributions of subhalos are indeed similar between the different WDM models and the Long-Lived CHAMP model. The result suggests that the cut-off scale k cut not only characterises the linear power spectra but also can be used to predict the non-linear clustering properties. The radial distribution of subhalos in Milky Way-size halos is consistent with the observed distribution for k cut ∼ 50 − 800 h Mpc −1 ; such models resolve the so-called "missing satellite problem".

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Cosmic abundances of stable particles: Improved analysis

Cited by 1,410 publications

References 8 publications

Majorana dark matter through the Higgs portal under the vacuum stability lamppost

Majorana dark matter through the Higgs portal under the vacuum stability lamppost

DarkSUSY: computing supersymmetric dark matter properties numerically

Structure of dark matter halos in warm dark matter models and in models with long-lived charged massive particles

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