TeV cosmic-ray electrons from millisecond pulsars

Kisaka, Shota; Kawanaka, Norita

doi:10.1111/j.1365-2966.2012.20576.x

Cited by 25 publications

(25 citation statements)

References 60 publications

(75 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Alternatively, we note that two of the highest TS MSPs identified in this study (J1023+0038, J1959+2048) are either transient low-mass X-ray binary systems, or black widow pulsars. This could potentially suggest that such objects produce more TeV emission than the remainder of the MSP population [8,27]. On the other hand, J0030+0451 and J0613-0200 each appear to be isolated MSPs, while J0613-0200 is in a non-interacting binary system.…”

Section: Evidence For Tev Halos Around Millisecond Pulsarsmentioning

confidence: 99%

Millisecond pulsars, TeV halos, and implications for the Galactic Center gamma-ray excess

Linden

2018

Phys. Rev. D

View full text Add to dashboard Cite

Observations by HAWC indicate that many young pulsars (including Geminga and Monogem) are surrounded by spatially extended, multi-TeV emitting regions. It is not currently known, however, whether TeV emission is also produced by recycled, millisecond pulsars (MSPs). In this study, we perform a stacked analysis of 24 MSPs within HAWC's field-of-view, finding between 2.6-3.2σ evidence that these sources are, in fact, surrounded by TeV halos. The efficiency with which these MSPs produce TeV halos is similar to that exhibited by young pulsars. This result suggests that several dozen MSPs will ultimately be detectable by HAWC, including many "invisible" pulsars without radio beams oriented in our direction. The TeV halos of unresolved MSPs could also dominate the TeV-scale diffuse emission observed at high galactic latitudes. We also discuss the possibility that TeV and radio observations could be used to constrain the population of MSPs that is present in the inner Milky Way, thereby providing us with a new way to test the hypothesis that MSPs are responsible for the Galactic Center GeV excess.

show abstract

Section: Evidence For Tev Halos Around Millisecond Pulsarsmentioning

confidence: 99%

Millisecond pulsars, TeV halos, and implications for the Galactic Center gamma-ray excess

Linden

2018

Phys. Rev. D

View full text Add to dashboard Cite

show abstract

“…This scenario is also at odds with current estimates of the supernova birth rate. Blum et al (2013) found an upper bound to the positron flux by neglecting energy losses, arguing that the flattening of the PF seen by AMS-02 around several hundred GeV is consistent with a purely secondary Gendelev et al 2010;Yin et al 2013;Feng & Zhang 2015), 'white dwarf pulsars' mainly formed by the merger of two white dwarfs (Kashiyama et al 2011), and millisecond pulsars (MSPs; Kisaka & Kawanaka 2012). In this paper, we investigate the latter source class.…”

Section: Introductionmentioning

confidence: 99%

Cosmic-Ray Positrons From Millisecond Pulsars

Venter

Kopp

Harding

et al. 2015

ApJ

View full text Add to dashboard Cite

Observations by the Fermi Large Area Telescope of γ-ray millisecond pulsar light curves imply copious pair production in their magnetospheres, and not exclusively in those of younger pulsars. Such pair cascades may be a primary source of Galactic electrons and positrons, contributing to the observed enhancement in positron flux above ∼10 GeV. Fermi has also uncovered many new millisecond pulsars, impacting Galactic stellar population models. We investigate the contribution of Galactic millisecond pulsars to the flux of terrestrial cosmic-ray electrons and positrons. Our population synthesis code predicts the source properties of present-day millisecond pulsars. We simulate their pair spectra invoking an offset-dipole magnetic field. We also consider positrons and electrons that have been further accelerated to energies of several TeV by strong intrabinary shocks in black widow and redback systems. Since millisecond pulsars are not surrounded by pulsar wind nebulae or supernova shells, we assume that the pairs freely escape and undergo losses only in the intergalactic medium. We compute the transported pair spectra at Earth, following their diffusion and energy loss through the Galaxy. The predicted particle flux increases for non-zero offsets of the magnetic polar caps. Pair cascades from the magnetospheres of millisecond pulsars are only modest contributors around a few tens of GeV to the lepton fluxes measured by AMS−02, PAMELA, and Fermi, after which this component cuts off. The contribution by black widows and redbacks may, however, reach levels of a few tens of percent at tens of TeV, depending on model parameters.Subject headings: cosmic rays -pulsars: general -stars: neutron 2 Such an additional source of primary positrons may be either of dark matter annihilation origin (e.g., Grasso et al.

show abstract

“…The two alternatives to the origin of excess positrons as secondary CRs are annihilations or decays of dark matter particles (e.g., Silk & Srednicki 1984;Bertone et al 2005;Bergström et al 2008) and the presence of local sources of accelerated electrons and positrons, which are believed to come from energetic pulsars and supernova remnants (Atoyan et al 1995;Hooper et al 2009;Malyshev et al 2009;Yüksel et al 2009;Blasi & Amato 2011;Kisaka & Kawanaka 2012;Profumo 2012).…”

Section: Introductionmentioning

confidence: 99%

GeV–TeV Cosmic-Ray Leptons in the Solar System from the Bow Shock Wind Nebula of the Nearest Millisecond Pulsar J0437–4715

Bykov

Petrov

Krassilchtchikov

et al. 2019

ApJL

View full text Add to dashboard Cite

We consider acceleration of leptons up to GeV-TeV energies in the bow shock wind nebula of PSR J0437-4715 and their subsequent diffusion through the interstellar magnetic fields. The leptons accelerated at the pulsar wind termination surface are injected into re-acceleration in colliding shock flows. Modelled spectra of synchrotron emission from the accelerated electrons and positrons are consistent with the far-ultraviolet and X-ray observations of the nebula carried out with the Hubble Space Telescope and Chandra X-ray Observatory. These observations are employed to constrain the absolute fluxes of relativistic leptons, which are escaping from the nebula and eventually reaching the Solar System after energy-dependent diffusion through the local interstellar medium accompanied by synchrotron and Compton losses. It is shown that accelerated leptons from the nebula of PSR J0437-4715 can be responsible both for the enhancement of the positron fraction above a few GeV detected by PAMELA and AMS-02 spectrometers and for the TeV range lepton fluxes observed with H.E.S.S., VERITAS, Fermi, CALET, and DAMPE. Corresponding author: A.M. Bykov byk@astro.ioffe.ru A.M. Bykov et al.

show abstract

TeV cosmic-ray electrons from millisecond pulsars

Cited by 25 publications

References 60 publications

Millisecond pulsars, TeV halos, and implications for the Galactic Center gamma-ray excess

Millisecond pulsars, TeV halos, and implications for the Galactic Center gamma-ray excess

Cosmic-Ray Positrons From Millisecond Pulsars

GeV–TeV Cosmic-Ray Leptons in the Solar System from the Bow Shock Wind Nebula of the Nearest Millisecond Pulsar J0437–4715

Contact Info

Product

Resources

About