Pulsed radiation from neutron star winds
| Autor: | Y. A. Gallant, John G. Kirk, O. Skjaeraasen |
|---|---|
| Rok vydání: | 2002 |
| Předmět: |
Physics
Magnetic energy Crab Pulsar Astrophysics::High Energy Astrophysical Phenomena Astrophysics (astro-ph) FOS: Physical sciences Magnetosphere Astronomy and Astrophysics Astrophysics Vela Luminosity Lorentz factor symbols.namesake Neutron star Pulsar Space and Planetary Science symbols Astrophysics::Galaxy Astrophysics |
| Zdroj: | Astronomy & Astrophysics. 388:L29-L32 |
| ISSN: | 1432-0746 0004-6361 |
| DOI: | 10.1051/0004-6361:20020599 |
| Popis: | The radiation of a pulsar wind is computed assuming that at roughly 10 to 100 light cylinder radii from the star, magnetic energy is dissipated into particle energy. The synchrotron emission of heated particles appears periodic, with, in general, both a pulse and an interpulse. The predicted spacing agrees well with the Crab and Vela pulse profiles.Using parameters appropriate for the Crab pulsar (magnetisation parameter at the light cylinder $\sigma=6\times10^4$, Lorentz factor $\Gamma=250$) agreement is found with the observed total pulsed luminosity. This suggests that the high-energy pulses from young pulsars originate not in the corotating magnetosphere within the light cylinder (as in all other models) but from the radially directed wind well outside it. Comment: 4 pages, 2 figures, accepted for publication in A&A Letters |
| Databáze: | OpenAIRE |
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