Dissecting cosmic-ray electron-positron data with Occam’s razor: the role of known pulsars

Profumo, Stefano

doi:10.2478/s11534-011-0099-z

Cited by 182 publications

(171 citation statements)

References 199 publications

(173 reference statements)

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“…The pulsars are potential sources which could produce primary e ± at high energy [29][30][31][32]38]. Electrons can be accelerated by the strong magnetosphere of the pulsars, and this acceleration produces photons.…”

Section: E ± From a Single Pulsarmentioning

confidence: 99%

“…Recent studies have proposed some interpretations, such as dark matter annihilation or decay [9][10][11][12][13][14][15][16][17], supernova remnants (SNRs) [18][19][20][21][22][23], secondary production in the interstellar medium (ISM) [24], and pulsars [16,17,[25][26][27][28][29][30][31][32][33][34][35][36][37][38][39]. Cosmicray flux data can also be taken together with other observations (like the dark matter relic density and the direct detection experimental results etc.)…”

Section: Introductionmentioning

confidence: 99%

“…boronto-carbon). The pioneering work on a pulsar interpretation of the positron fraction has been performed [29,31,38] a few years ago. Combined analyses of the recent AMS-02 lepton data have been performed by [16,23], with a global fit on the positron fraction [1], e + flux, e − flux and (e − + e + ) flux.…”

Section: Introductionmentioning

confidence: 99%

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Pulsar interpretation of lepton spectra measured by AMS-02

Feng

Zhang

2016

Eur. Phys. J. C

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Alpha Magnetic Spectrometer (AMS-02) recently published its lepton spectra measurement. The results show that the positron fraction no longer increases above ∼200 GeV. The aim of this work is to investigate the possibility that the excess of positron fraction is due to pulsars. Nearby known pulsars from the ATNF catalog are considered to be a possible primary positron source of the high energy positrons. We find that the pulsars with age T (0.45−4.5) × 10 5 year and distance d < 0.5 kpc can explain the behavior of positron fraction of AMS-02 in the range of high energy. We show that each of the four pulsars-Geminga, J1741-2054, Monogem, and J0942-5552-is able to be a single source satisfying all considered physical requirements. We also discuss the possibility that these high energy e ± are from multiple pulsars. The multiple pulsar contribution predicts a positron fraction with some structures at higher energies.

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Section: E ± From a Single Pulsarmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Pulsar interpretation of lepton spectra measured by AMS-02

Feng

Zhang

2016

Eur. Phys. J. C

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“…There are some tantalizing excesses in the mono-energetic gamma ray signal around 135 GeV observed by the Fermi-LAT [70][71][72][73][74][75] and in the positron excesses at a few GeV ∼ TeV scale observed by PAMELA, Fermi, and AMS02 Collaborations [76][77][78]. However, it is still unclear that the origin of the excesses comes from annihilation or decay of dark matter or astrophysical backgrounds [79,80]. In this paper, we assume that the excesses are originated in the astrophysical phenomena.…”

Section: Constraints From Indirect Detectionmentioning

confidence: 99%

Dark matter and dark force in the type-I inert 2HDM with local U(1) H gauge symmetry

Ko¹,

Omura

Yu³

2014

J. High Energ. Phys.

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We discuss dark matter (DM) physics in the Type-I inert two-Higgs-doublet model (2HDM) with local U(1) H Higgs gauge symmetry, which is assigned to the extra Higgs doublet in order to avoid the Higgs-mediated flavor problems. In this gauged inert DM setup, a U(1) H -charged scalar Φ is also introduced to break U(1) H spontaneously through its nonzero vacuum expectation value (VEV), Φ , and then the remnant discrete subgroup appears according to the U(1) H charge assignment of Φ. The U(1) H -charged Higgs doublet does not have Yukawa couplings with the Standard-Model (SM) fermions, and its lightest neutral scalar component H is stable because of the remnant discrete symmetry. In order to suppress a too large Z-exchange diagram contribution in DM direct detection experiments, we have to introduce a non-renormalizable operator which can be generated by integrating out an extra heavy scalar. With these new particles contents, we first investigate the constraint on the U(1) H gauge interaction, especially through the kinetic and mass mixing between the SM gauge bosons and the extra gauge boson. Then we discuss dark matter physics in our 2HDM: thermal relic density, and direct/indirect detections of dark matter. The additional U(1) H gauge interaction plays a crucial role in reducing the DM thermal relic density. The most important result within the inert DM model with local U(1) H symmetry is that ∼ O(10) GeV dark matter scenario, which is strongly disfavored in the usual Inert Doublet Model (IDM) with Z 2 symmetry, is revived in our model because of newly open channels, HH → Z H Z H , Z H Z. Exotic Higgs decays, h → Z H Z H , ZZ H , would be distinctive signatures of the inert 2HDM with local U(1) H symmetry.

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“…The fact that the measured PF rises with energy may therefore point to nearby sources of primary positrons, either from dark matter annihilation (e.g., [8]), or of astrophysical origin. The latter class of sources may include supernovae (e.g., [9]), pulsar wind nebulae (e.g., [10]), young or mature pulsars (e.g., [11,12]), and millisecond pulsars (MSPs; [13]). In this paper, we investigate the cosmic-ray flux contribution of the latter source class.…”

Section: Introductionmentioning

confidence: 99%

The millisecond pulsar contribution to the rising positron fraction

Venter¹,

Kopp²,

Harding³

et al. 2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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Pair cascades from millisecond pulsars (MSPs) may be a primary source of Galactic electrons and positrons that contribute to the increase in positron flux above 10 GeV as observed by PAMELA and AMS−02. The Fermi Large Area Telescope (LAT) has increased the number of detected γ-ray MSPs tremendously. Light curve modelling furthermore favours abundant pair production in MSP magnetospheres, so that models of primary cosmic-ray positrons from pulsars should include the contribution from the larger numbers of MSPs and their potentially higher positron output per source. We model the contribution of Galactic MSPs to the terrestrial cosmic-ray electron / positron flux by using a population synthesis code to predict the source properties of presentday MSPs. We simulate pair spectra assuming an offset-dipole magnetic field which boosts pair creation rates. We also consider positrons and electrons that have additionally been accelerated to very high energies in the strong intrabinary shocks in black widow (BW) and redback (RB) binary systems. We transport these particles to Earth by calculating their diffusion and the radiative energy losses they suffer in the Galaxy using a model. Our model particle flux increases for nonzero offsets of the magnetic polar caps. We find that pair cascades from MSP magnetospheres contribute only modestly around a few tens of GeV to the measured fluxes. BW and RB fluxes may reach a few tens of percent of the observed flux up to a few TeV. Future observations should constrain the source properties in this case.

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Dissecting cosmic-ray electron-positron data with Occam’s razor: the role of known pulsars

Cited by 182 publications

References 199 publications

Pulsar interpretation of lepton spectra measured by AMS-02

Pulsar interpretation of lepton spectra measured by AMS-02

Dark matter and dark force in the type-I inert 2HDM with local U(1) H gauge symmetry

The millisecond pulsar contribution to the rising positron fraction

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