Status of dark matter detection

Bi, Xiao-Jun; Yin, Peng-Fei; Yuan, Qiang

doi:10.1007/s11467-013-0330-z

Cited by 35 publications

(38 citation statements)

References 466 publications

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“…The proposed models of the extra sources include the astrophysical sources such as pulsars [15][16][17][18][19], interaction occurring around the CR acceleration sources [20][21][22], as well as the dark matter (DM) annihilation/decay [23][24][25][26][27][28]. One can refer to the reviews for detailed description of the relevant models to explain the electron/positron excesses [29][30][31][32][33].…”

Section: Introductionmentioning

confidence: 99%

Quantitative study of the AMS-02 electron/positron spectra: Implications for pulsars and dark matter properties

2015

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The AMS-02 has just published the unprecedentedly precise measurement of the cosmic electron and positron spectra. In this paper we try to give a quantitative study on the AMS-02 results by a global fitting to the electron and positron spectra, together with the updated positron fraction data. The Markov Chain Monte Carlo algorithm is adopted to do the fitting. The primary electron spectrum and the parameters for pulsars or dark matter which contribute extra positrons are determined simultaneously. We find that there is a hardening of the primary electron spectrum at ∼ 60 GeV. With such a new feature at the background spectrum both the pulsars and dark matter can explain the AMS-02 results very well. The dark matter scenario shows a drop at positron fraction at ∼ 300 GeV, however, suffers very strong constraints from Fermi γ-ray observations. The fitting results also suggest that the propagation model with convection may be more favored by the lepton data than the reacceleration model. PACS numbers:

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Section: Introductionmentioning

confidence: 99%

Quantitative study of the AMS-02 electron/positron spectra: Implications for pulsars and dark matter properties

2015

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“…Bi, P.-F. Chen, and Q. Yuan) [10] and dark energy (M. Li, X.-D. Li, S. Wang, and Y. Wang) [11]. These two subjects are not limited to high energy astrophysics, having a large impact on astrophysics as whole (especially cosmology), as well as being major problems of fundamental physics.…”

Section: Pacs Numbersmentioning

confidence: 99%

Preface: High energy astrophysics

Zhang

Mésáros

2013

Front. Phys.

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High energy astrophysics is one of the most active branches in the contemporary astrophysics. It studies astrophysical objects that emit X-ray and γ-ray photons, such as accreting super-massive and stellar-size black holes, and various species of neutron stars. With the operations of many space-borne and ground-based observational facilities, high energy astrophysics has enjoyed rapid development in the past decades. It is foreseen that the field will continue to advance rapidly in the coming decade, with possible ground-breaking discoveries of astrophysical sources in the high-energy neutrino and gravitational wave channels. This Special Issue of Frontiers of Physics is dedicated to a systematic survey of the field of high energy astrophysics as it stands in 2013. 95.85.Nv, 95.85.Pw, 95.85.Ry, 95.85.Sz, 97.60.Lf, 97.60.Jd, 97.80.Jp, 98.62.Js High energy astrophysics is the branch of astrophysics that studies astrophysical objects that emit high energy photons (X-rays and γ-rays), and more generally, emit non-thermal photons outside the traditional optical wavelengths. By studying non-thermal emission in the universe, one can unveil the part of universe that is not in a steady state, usually originating in violent environments near compact objects, such as neutron stars and black holes of different scales. These objects, besides emitting the broad-band non-thermal electromagnetic radiation, are also believed to be emitters of other signals outside the electromagnetic channel. These multi-messenger signals include cosmic rays, neutrinos, and gravitational waves. The field of high energy astrophysics, along with cosmology and planetary sciences, is one of the three most active branches in the contemporary astrophysics. PACS numbersDuring the past decades, the field of high energy astrophysics has enjoyed a rapid development, thanks to an impressive list of space-borne and ground-based observational facilities. The currently operating space missions dedicated to high energy astrophysics include the Chandra X-ray Observatory, the X-ray Multi-Mirror Mission (XMM)-Newton, Suzaku, and the Nuclear

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“…The CDM model solves this problem by assuming a much larger dark form of matter present in every galaxy and cluster of galaxies. However, over the decades no observation has confirmed the existence of this material either way [3][4][5]. a e-mail: andrew.finch.12@um.edu.mt b e-mail: jackson.said@um.edu.mt…”

Section: Introductionmentioning

confidence: 99%

Galactic rotation dynamics in f(T) gravity

Finch

Said

2018

Eur. Phys. J. C

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We investigate galactic rotation curves in f (T ) gravity, where T represents a torsional quantity. Our study centers on the particular Lagrangian f (T ) = T +αT n , where |n| = 1 and α is a small unknown constant. To do this we treat galactic rotation curves as being composed from two distinct features of galaxies, namely the disk and the bulge. This process is carried out for several values of the index n. The resulting curve is then compared with Milky Way profile data to constrain the value of the index n while fitting for the parameter α. These values are then further tested on three other galaxies with different morphologies. On the galactic scale we find that f (T ) gravity departs from standard Newtonian theory in an important way. For a small range of values of n we find good agreement with data without the need for exotic matter components to be introduced.

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Status of dark matter detection

Cited by 35 publications

References 466 publications

Quantitative study of the AMS-02 electron/positron spectra: Implications for pulsars and dark matter properties

Quantitative study of the AMS-02 electron/positron spectra: Implications for pulsars and dark matter properties

Preface: High energy astrophysics

Galactic rotation dynamics in f(T) gravity

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