Discovery of an energetic pulsar associated with SNR G76.9+1.0

Par Conseil national de recherches du Canada

DOI	Trouver le DOI : https://doi.org/10.1088/0004-637X/739/1/39
Auteur	Rechercher : Arzoumanian, Z.; Rechercher : Gotthelf, E. V.; Rechercher : Ransom, S. M.; Rechercher : Safi-Harb, S.; Rechercher : Kothes, R.¹; Rechercher : Landecker, T. L.¹
Affiliation	Conseil national de recherches du Canada. Institut Herzberg d'astrophysique du CNRC
Format	Texte, Article
Sujet	ISM: supernova remnants; pulsars: individual: PSR J2022+3842); stars: neutron; X-rays: stars; stars: neutron; X-rays: stars; X-rays: stars
Résumé	We report the discovery of PSR J2022+3842, a 24 ms radio and X-ray pulsar in the supernova remnant G76.9+1.0, in observations with the Chandra X-ray telescope, the Robert C. Byrd Green Bank Radio Telescope, and the Rossi X-ray Timing Explorer (RXTE). The pulsar's spin-down rate implies a rotation-powered luminosity Edot = 1.2 x 10^{38} erg/s, a surface dipole magnetic field strength B_s = 1.0 x 10^{12} G, and a characteristic age of 8.9 kyr. PSR J2022+3842 is thus the second-most energetic Galactic pulsar known, after the Crab, as well as the most rapidly-rotating young, radio-bright pulsar known. The radio pulsations are highly dispersed and broadened by interstellar scattering, and we find that a large (delta-f / f ~= 1.9 x 10^{-6}) spin glitch must have occurred between our discovery and confirmation observations. The X-ray pulses are narrow (0.06 cycles FWHM) and visible up to 20 keV, consistent with magnetospheric emission from a rotation-powered pulsar. The Chandra X-ray image identifies the pulsar with a hard, unresolved source at the midpoint of the double-lobed radio morphology of SNR G76.9+1.0 and embedded within faint, compact X-ray nebulosity. The spatial relationship of the X-ray and radio emissions is remarkably similar to extended structure seen around the Vela pulsar. The combined Chandra and RXTE pulsar spectrum is well-fitted by an absorbed power-law model with column density N_H = (1.7\pm0.3) x 10^{22} cm^{-2} and photon index Gamma = 1.0\pm0.2; it implies that the Chandra point-source flux is virtually 100% pulsed. For a distance of 10 kpc, the X-ray luminosity of PSR J2022+3842 is L_X(2-10 keV) = 7.0 x 10^{33} erg s^{-1}. Despite being extraordinarily energetic, PSR J2022+3842 lacks a bright X-ray wind nebula and has an unusually low conversion efficiency of spin-down power to X-ray luminosity, L_X/Edot = 5.9 x 10^{-5}.
Date de publication	2011-09-06
Maison d’édition	American Astronomical Society IOP Publishing
Dans	The Astrophysical Journal 739, nº 1 : 1–8.
Langue	anglais
Publications évaluées par des pairs	Oui
Identificateur	arXiv:1105.3185v2
Numéro NPARC	19770590
Exporter la notice	Exporter en format RIS
Signaler une correction	Signaler une correction (s'ouvre dans un nouvel onglet)
Identificateur de l’enregistrement	e62197f8-9256-4d73-b6ad-3c38c65c050d
Enregistrement créé	2012-04-04
Enregistrement modifié	2020-04-21

Date de modification :: 2024-05-20