The Weighted Super-Bergman Kernels of $$\mathbb {B}^{m|n}$$ B m | n and Integral Representations of the Invariant Inner Products on $$H^2_{\nu }(\mathbb {B}^m)$$ H ν 2 ( B m )

Feng, Zhiming; Tu, Zhenhan

doi:10.1007/s11785-014-0392-0

Cited by 9 publications

(15 citation statements)

References 13 publications

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“…[357,435]) or analytically by using the Hulthèn potential as an approximation for the true Yukawa potential [434,470,471,472]. This effect has important implications for indirect detection [357,435,442,471,473,474,475,476,477,478]. During freeze-out, the DM velocity is v rel ∼ 0.3 c, while at later timesin DM halos today and during the recombination epoch-the velocity is far smaller.…”

Section: Indirect Detectionmentioning

confidence: 99%

“…For instance, energy injection from DM annihilation may increase the ionization fraction during recombination, resulting in a distorted CMB spectrum [456,458,459,487,488,489,490,491]. Since the DM velocity is very low during the recombination epoch, v rel ∼ 10 −8 c, the predicted Sommerfeld effect is very large at this epoch [22,471].…”

Section: Indirect Detectionmentioning

confidence: 99%

“…To accurately calculate the relic density in DM models with a light mediator, one needs to consider several subtle effects[141,471,479,480,481,482], such as enhanced annihilation after freeze-out, chemical recoupling, and bound state formation. If the two sectors were not in thermal equilibrium during DM freeze-out, the relic abundance also depends on the temperature ratio of the two sectors, see, e.g.,[364].…”

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confidence: 99%

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Dark matter self-interactions and small scale structure

2018

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We review theories of dark matter (DM) beyond the collisionless paradigm, known as self-interacting dark matter (SIDM), and their observable implications for astrophysical structure in the Universe. Selfinteractions are motivated, in part, due to the potential to explain long-standing (and more recent) small scale structure observations that are in tension with collisionless cold DM (CDM) predictions. Simple particle physics models for SIDM can provide a universal explanation for these observations across a wide range of mass scales spanning dwarf galaxies, low and high surface brightness spiral galaxies, and clusters of galaxies. At the same time, SIDM leaves intact the success of ΛCDM cosmology on large scales. This report covers the following topics: (1) small scale structure issues, including the core-cusp problem, the diversity problem for rotation curves, the missing satellites problem, and the too-big-to-fail problem, as well as recent progress in hydrodynamical simulations of galaxy formation; (2) N-body simulations for SIDM, including implications for density profiles, halo shapes, substructure, and the interplay between baryons and selfinteractions;(3) semi-analytic Jeans-based methods that provide a complementary approach for connecting particle models with observations; (4) merging systems, such as cluster mergers (e.g., the Bullet Cluster) and minor infalls, along with recent simulation results for mergers; (5) particle physics models, including light mediator models and composite DM models; and (6) complementary probes for SIDM, including indirect and direct detection experiments, particle collider searches, and cosmological observations. We provide a summary and critical look for all current constraints on DM self-interactions and an outline for future directions.

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Section: Indirect Detectionmentioning

confidence: 99%

Section: Indirect Detectionmentioning

confidence: 99%

mentioning

confidence: 99%

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Dark matter self-interactions and small scale structure

2018

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“…However, further analysis finds that the enhancement of cross section due to the Sommerfeld effect would also affect the thermal history of DM in the early Universe. The calculation of DM relic density with Sommerfeld enhancement depends on several issues, such as the temperature of kinematic decoupling [217][218][219] and the efficiency of self-interactions for persevering thermal velocity distribution [219]. Detailed calculation shows there is a tension between large enhancement factor and correct DM relic density [219,220].…”

Section: Sommerfeld Enhancementmentioning

confidence: 99%

“…The calculation of DM relic density with Sommerfeld enhancement depends on several issues, such as the temperature of kinematic decoupling [217][218][219] and the efficiency of self-interactions for persevering thermal velocity distribution [219]. Detailed calculation shows there is a tension between large enhancement factor and correct DM relic density [219,220]. In order to obtain correct DM relic density for m χ ∼1 TeV and m φ ∼ 1GeV, the maximal value of enhancement factor S for χχ → φφ → µ + µ − µ + µ − is only ∼ O(10 2 ) which is smaller than the required value O(10 3 ).…”

Section: Sommerfeld Enhancementmentioning

confidence: 99%

Status of dark matter detection

Yin

Yuan

2013

Front. Phys.

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The detection of dark matter has made great progresses in recent years. We give a brief review on the status and progress in dark matter detection, including the progresses in direct detection, collider detection at LHC and focus on the indirect detection. The results from PAMELA, ATIC, Fermi-LAT and relevant studies on these results are introduced. Then we give the progress on indirect detection of gamma rays from Fermi-LAT and ground based Cerenkov telescopes. Finally the detection of neutrinos and constraints on the nature of dark matter are reviewed briefly. PACS numbers: 12.60.Jv,14.80.Ly Indirect detection DM DM SM SM New Physics Collider detection Direct detection High energy photon, neutrino, anti-matter Missing transverse energy Nuclear recoil FIG. 1: Schematic plot to show the relation among the direct detection, indirect detection and collider detection of DM. The arrows indicate the direction of reaction.

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Dark Higgs models at the 7 TeV LHC

Weihs¹,

Zurita²

2012

J. High Energ. Phys.

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We study how collider data and electroweak precision observables affect the parameter space of models including a new dark force mediated by a massive U(1) gauge boson. It acquires mass via a Higgs mechanism in the dark sector which is connected to the Standard Model through kinetic mixing of the two U(1) gauge bosons and the Higgs potential.We assess the impact of the 7 TeV LHC and show that most of the parameter space of the model can be probed with an integrated luminosity of 15 fb −1 .

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The Weighted Super-Bergman Kernels of $$\mathbb {B}^{m|n}$$ B m | n and Integral Representations of the Invariant Inner Products on $$H^2_{\nu }(\mathbb {B}^m)$$ H ν 2 ( B m )

Cited by 9 publications

References 13 publications

Dark matter self-interactions and small scale structure

Dark matter self-interactions and small scale structure

Status of dark matter detection

Dark Higgs models at the 7 TeV LHC

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