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The Astrophysical Journal 738 (2011) 114
R. W. Romani, M. Kerr, H. A. Craig, S. Johnston, I. Cognard1, 2, D. A. Smith3

Most pulsars observed by the Fermi Large Area Telescope have γ -ray luminosities scaling with spin-down power ˙E as Lγ ≈ ( ˙E × 1033 erg s−1)1/2. However, there exist one detection and several upper limits an order of magnitude or more fainter than this trend. We describe these "sub-luminous" γ -ray pulsars and discuss the case for this being an orientation effect. Of the 12 known young radio pulsars with ˙ E > 1034 erg s−1 and d 2 kpc several are substantially sub-luminous. The limited available geometrical constraints favor aligned geometries for these pulsars, although no one case for alignment is compelling. In this scenario GeV emission detected from such sub-luminous pulsars can be due to a lower altitude, lower-power accelerator gap.
1 :  LPCE - Laboratoire de physique et chimie de l'environnement
2 :  USN - Unité Scientifique de la Station de Nançay
3 :  CENBG - Centre d'Etudes Nucléaires de Bordeaux Gradignan
Physique/Astrophysique/Astrophysique galactique

Planète et Univers/Astrophysique/Astrophysique galactique
gamma rays: stars - pulsars: general