Wave Atoms

We argue that the cosmic ray positron excess observed in ATIC-2, Fermi LAT, PAMELA, HESS and recently in the precision AMS-02 experiment can be attributed to the production in a local, middle-aged supernova remnant (SNR). Using the prediction of our model of cosmic ray acceleration in SNR we estimate that the SNR responsible for the observed positron excess is located between 250 and 320pc from the Sun and is 170-380 kyear old. The most probable candidate for such a source is the SNR which gave birth to the well-known Geminga pulsar, but is no longer visible. Other contenders are also discussed.Comment: 9 pages, 3 figures, accepted by Astroparticle Physic

show abstract

“…The mechanisms considered can be listed, as follows. a) Nearby pulsars ( eg [29] ). b) Microquasars ( eg [30] ).…”

Section: Comparison With the Results Of Other Workersmentioning

confidence: 99%

Cosmic ray positrons from a local, middle-aged supernova remnant

Erlykin

Wolfendale

2013

Astroparticle Physics

View full text Add to dashboard Cite

show abstract

“…It can be described by a broken power law with an index about -3.1 before ∼ 1 TeV and nearly -4.1 after ∼ 1 TeV [13]. In the past years, much attention has been paid to the excesses of the electron and the positron including both the dark matter ( [19] and references therein) and the astrophysics origin [20][21][22][23][24][25][26][27]. Several studies attribute this spectral break to the acceleration limit or the confinement at source [28][29][30][31], the energy loss during propagation [32,33], or the contribution from nearby pulsars [34].…”

Section: Introductionmentioning

confidence: 99%

On the PeV knee of the cosmic ray spectrum and the TeV cutoff of the electron spectrum

Jin

Liu

et al. 2018

Phys. Rev. D

View full text Add to dashboard Cite

Spectra of Cosmic Rays (CRs), and particularly their features, contain a lot of important information about the astro-particle physics and the fundamental physics. Realizing that the 4 PeV knee of CR nuclei and the 1 TeV spectral cutoff of the electron share almost a same Lorentz factor, we propose that CRs experience a threshold interaction with a new light particle X abundant in the Galaxy. The interaction CR + X −→ CR + X ′ can take place when the effective energy is sufficient to convert it into another heavier unknown particle X ′ (as a representative to all possible threshold inelastic interactions). Under this scenario, we can reproduce the spectral break for both the nuclei and the electron, and predict a zig-zag spectrum for them. Given that there are great uncertainties in experiments, our model accommodates a wide mass range of the X from ultra low value to around 1 eV.

show abstract

“…Both figures show that electrons/positrons ejected from MSPs with high multiplicity partially contribute to the excess from background flux observed by Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics (PAMELA), HESS and Fermi telescopes. In this energy range, other sources such as canonical pulsars (Shen 1970;Atoyan, Aharonian & Völk 1995;Chi, Cheng & Young 1996;Zhang & Cheng 2001;Kobayashi et al 2004;Grimani 2007;Büsching et al 2008a;Grasso et al 2009;Hooper, Blasi & Serpico 2009;Malyshev, Cholis & Gelfand 2009;Yüksel, Kistler & Stanev 2009;Heyl, Gill & Hernquist 2010;Kawanaka et al 2010; Profumo 2012) would also contribute to the observed electron/positron spectrum. Note that even if other sources are dominant for the observed excess, the total spectrum added to the contribution of MSPs with high multiplicity does not significantly exceed the observed electron/positron spectrum.…”

Section: R E S U Lt S a N D Discussionmentioning

confidence: 99%

TeV cosmic-ray electrons from millisecond pulsars

Kisaka¹,

Kawanaka²

2012

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Recent γ‐ray observations by Fermi Gamma‐Ray Space Telescope suggest that the γ‐ray millisecond pulsar (MSP) population is separated into two subclasses with respect to pair multiplicity. Here, we calculate the cosmic‐ray electron/positron spectra from MSPs. Based on the assumption of equipartition in the pulsar‐wind region, the typical energy of electrons/positrons ejected by a MSP with pair multiplicity of the order of unity is ∼50 TeV. In this case, we find that a large peak in the 10–50 TeV energy range would be observed in the cosmic‐ray electron/positron spectrum. Even if the fraction of pair‐starved MSPs is 10 per cent, a large peak would be detectable in future observations. We also calculate the contribution from MSPs with high pair multiplicity to the electron/positron spectrum. We suggest that if the multiplicity of the dominant MSP population is ∼103, electrons/positrons from this population may contribute to the observed excess from the background electron/positron flux and positron fraction.

show abstract

Wave Atoms

Cited by 4 publications

References 0 publications

Cosmic ray positrons from a local, middle-aged supernova remnant

Cosmic ray positrons from a local, middle-aged supernova remnant

On the PeV knee of the cosmic ray spectrum and the TeV cutoff of the electron spectrum

TeV cosmic-ray electrons from millisecond pulsars

Contact Info

Product

Resources

About