Local fading accelerator and the origin of TeV cosmic ray electrons
| Autor: | Jacco Vink, Stefano Gabici, S. Recchia, Felix Aharonian |
|---|---|
| Přispěvatelé: | AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité) |
| Jazyk: | angličtina |
| Rok vydání: | 2019 |
| Předmět: |
electron: energy
lepton: energy Inverse Astrophysics Electron GeV 01 natural sciences cosmic radiation: TeV Luminosity Positron Diffusion (business) attenuation pulsar Physics High Energy Astrophysical Phenomena (astro-ph.HE) education.field_of_study energy: high cosmic radiation: spectrum Computer Science::Computation and Language (Computational Linguistics and Natural Language and Speech Processing) shock waves electron: spectrum Supernova positron Production (computer science) Astrophysics - High Energy Astrophysical Phenomena Particle physics accelerator Astrophysics::High Energy Astrophysical Phenomena energy loss Population FOS: Physical sciences Cosmic ray cosmic radiation: diffusion energy dependence Pulsar 0103 physical sciences supernova synchrotron positron: acceleration Fading 010306 general physics education 010308 nuclear & particles physics particle: energy electron: cosmic radiation acceleration [PHYS.PHYS.PHYS-GEN-PH]Physics [physics]/Physics [physics]/General Physics [physics.gen-ph] injection Compton scattering: inverse 13. Climate action Physics::Accelerator Physics High Energy Physics::Experiment [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] Energy (signal processing) Astrophysics and astroparticle physics |
| Zdroj: | Phys.Rev.D Phys.Rev.D, 2019, 99 (10), pp.103022. ⟨10.1103/PhysRevD.99.103022⟩ Physical Review D Physical Review D, American Physical Society, 2019, 99 (10), pp.103022. ⟨10.1103/PhysRevD.99.103022⟩ PoS 37th International Cosmic Ray Conference 37th International Cosmic Ray Conference, Jul 2021, Berlin, Germany. pp.168, ⟨10.22323/1.395.0168⟩ |
| ISSN: | 1550-7998 1550-2368 |
| Popis: | The cosmic ray electron spectrum exhibits a break at a particle energy of $\ensuremath{\sim}1\text{ }\text{ }\mathrm{TeV}$ and extends without any attenuation up to $\ensuremath{\sim}20\text{ }\text{ }\mathrm{TeV}$. Synchrotron and inverse Compton energy losses strongly constrain the time of emission of $\ensuremath{\sim}20\text{ }\text{ }\mathrm{TeV}$ electrons to $\ensuremath{\approx}2\ifmmode\times\else\texttimes\fi{}{10}^{4}\text{ }\text{ }\mathrm{yr}$ and the distance of the potential source(s) to $\ensuremath{\approx}100--500\text{ }\text{ }\mathrm{pc}$, depending on the cosmic ray diffusion coefficient. This suggests that maybe one nearby discrete source may explain the observed spectrum of high energy electrons. Given the strong energy dependence ($\ensuremath{\propto}1/E$) of the cooling time of TeV electrons, the spectral shape of the electron spectrum above the $\ensuremath{\sim}1\text{ }\text{ }\mathrm{TeV}$ break strongly depends on the history of injection of these electrons from the source. In this paper we show that a local, continuous (on timescales of $\ensuremath{\sim}{10}^{5}\text{ }\text{ }\mathrm{yr}$) but fading electron accelerator, with a characteristic decay time of $\ensuremath{\sim}{10}^{4}\text{ }\text{ }\mathrm{yr}$, can naturally account for the entire spectrum of cosmic ray electrons in the TeV domain. Although the standard ``nearby pulsar'' scenario naturally meets this time condition, it is (almost) excluded by recent measurements of the positron fraction, which above $\ensuremath{\sim}100\text{ }\text{ }\mathrm{GeV}$ saturates at a level well below 0.5 and drops above $\ensuremath{\sim}400--500\text{ }\text{ }\mathrm{GeV}$. The second potential source population, the supernova remnants, accelerate mostly electrons, rather than positrons. However, they hardly can provide an effective production of multi-TeV electrons via the standard diffusive shock acceleration scenario for $\ensuremath{\sim}{10}^{5}\text{ }\text{ }\mathrm{yr}$. A third possibility are stellar wind shocks, which however are likely to be continuous with nearly constant luminosity on timescales $\ensuremath{\gg}10\text{ }\text{ }\mathrm{kyr}$ and probably cannot match the time requirement of our potential source. Therefore, we face a real challenge in the identification of the origin of the source of multi-TeV electrons. Thus, the link of this source with known particle accelerators would require a dramatic revision of the standard paradigms of acceleration and escape in such objects. |
| Databáze: | OpenAIRE |
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