Evolved Pulsar Wind Nebulae as Sources of (Mostly Leptonic) Cosmic Rays
| Autor: | Yves A. Gallant |
|---|---|
| Přispěvatelé: | Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2) |
| Rok vydání: | 2018 |
| Předmět: |
Nuclear and High Energy Physics
Particle physics Astrophysics::High Energy Astrophysical Phenomena Population cosmic radiation: energy Cosmic ray Astrophysics energy loss: adiabatic 01 natural sciences Pulsar wind nebula GLAST particle: acceleration cosmic rays Pulsar PAMELA supernova 0103 physical sciences AMS 010306 general physics education 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics pulsar acceleration of particles supernova remnants Physics electron positron education.field_of_study Astrophysics::Instrumentation and Methods for Astrophysics electron: cosmic radiation Galactic plane gamma rays Particle acceleration Supernova gamma ray pulsars [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] Heliosphere |
| Zdroj: | Nucl.Part.Phys.Proc. 2nd Conference on Cosmic Ray Origin-beyond the standard models 2nd Conference on Cosmic Ray Origin-beyond the standard models, Sep 2016, San Vito di Cadore, Italy. pp.106-113, ⟨10.1016/j.nuclphysbps.2018.07.017⟩ |
| ISSN: | 2405-6014 |
| DOI: | 10.1016/j.nuclphysbps.2018.07.017 |
| Popis: | Pulsars, and more precisely their wind nebulae, are perhaps the most likely astrophysical sources of high-energy cosmic-ray electrons and especially positrons, and in particular of the excess positronic component above ∼20 GeV measured by PAMELA, Fermi-LAT and AMS-02. While e ± pairs are created in pulsar magnetospheres, their acceleration to relevant cosmic-ray energies likely occurs at the pulsar wind termination shock, and they are subsequently confined in the pulsar wind nebula (PWN) until late stages of its evolution. We discuss the implications of radiative and adiabatic energy losses for the likely contributions of different stages of PWN evolution to the observed cosmic-ray e ± spectrum, and highlight the plausibly dominant contribution of late, subsonic expansion and especially bow-shock PWN phases. The most recently opened observational window on PWNe, with implications for accelerated e ± in the relevant energy range, is the domain of TeV γ-rays. I review the properties of the population of PWNe revealed in this energy domain, in particular by the H.E.S.S. array of Cherenkov telescopes and its Galactic Plane Survey, and discuss the constraints which these place on the evolution of middle-aged PWNe. Finally, I briefly review the possibility of hadron acceleration in PWNe, and discuss theoretical and observational constraints which limit a plausible major contribution of these objects to the bulk of the (hadronic) Galactic cosmic-ray spectrum. |
| Databáze: | OpenAIRE |
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