EDP Sciences
First Science with the ODIN satellite
Free Access
Issue
A&A
Volume 402, Number 3, May II 2003
First Science with the ODIN satellite
Page(s) 827 - 836
Section Cosmology
DOI https://doi.org/10.1051/0004-6361:20030279


A&A 402, 827-836 (2003)
DOI: 10.1051/0004-6361:20030279

Signatures of high energy protons in pulsar winds

E. Amato, D. Guetta and P. Blasi

INAF/Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
(Received 4 July 2002 / Accepted 4 February 2003 )

Abstract
The resonant cyclotron absorption model (Hoshino et al. 1992; Gallant & Arons 1994) is very successful in describing particle acceleration in plerions. A prediction of this model is the presence of a substantial amount of relativistic protons in pulsar winds. Although difficult to detect, these protons may show up through their interactions either with the photons in the plerion environment or with the thermal gas in the supernova ejecta. Inelastic proton-proton (p-p) collisions are expected to be very effective in young objects, resulting in a copious production of neutral and charged pions. Charged pions produced during the first few hundred years after the supernova explosion may have time to decay into muons, whose subsequent decay may provide an additional source of electrons and positrons in these nebulae, that adds up to the pulsar input. These secondary leptons evolve just as the pairs in the pulsar wind, and signatures of their presence could be found, in principle, even in the synchrotron spectrum of older objects. p-p collisions may remain fairly efficient even in moderately old objects resulting in the production of TeV $\gamma$-rays and neutrinos. We apply our calculations to the case of the Crab Nebula, the best studied plerion thus far, and find that existing data already allow us to infer interesting constraints on the physical properties of the Crab pulsar wind.


Key words: acceleration of particles -- stars: pulsars: general -- stars: winds, outflows

Offprint request: E. Amato, amato@arcetri.astro.it

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© ESO 2003

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