Volume 401, Number 2, April II 2003
|Page(s)||625 - 630|
|Section||Stellar structure and evolution|
|Published online||21 March 2003|
Point X-ray sources in the SNR G 315.4-2.30 (MSH 14-63, RCW 86)
Sternberg Astronomical Institute, Moscow State University, Universitetskij Pr. 13, Moscow 119992, Russia
2 E.K.Kharadze Abastumani Astrophysical Observatory, Georgian Academy of Sciences, A.Kazbegi ave. 2-a, Tbilisi 380060, Georgia
3 Abdus Salam International Centre for Theoretical Physics, Strada Costiera 11, PO Box 586, 34100 Trieste, Italy
4 Space Research Institute, Russian Academy of Sciences, Profsoyuznaya 84/32, Moscow 117997, Russia
Corresponding author: V. V. Gvaramadze, email@example.com
Accepted: 28 October 2002
We report the results of a search for a point X-ray source (stellar remnant) in the southwest protrusion of the supernova remnant G 315.4-2.30 (MSH 14-63, RCW 86) using the archival data of the Chandra X-ray Observatory. The search was motivated by a hypothesis that G 315.4-2.30 is the result of an off-centered cavity supernova explosion of a moving massive star, which ended its evolution just near the edge of the main-sequence wind-driven bubble. This hypothesis implies that the southwest protrusion in G 315.4-2.30 is the remainder of a pre-existing bow shock-like structure created by the interaction of the supernova progenitor's wind with the interstellar medium and that the actual location of the supernova blast center is near the center of this hemispherical structure. We have discovered two point X-ray sources in the “proper" place. One of the sources has an optical counterpart with the photographic magnitude , while the spectrum of the source can be fitted with an optically thin plasma model. We interpret this source as a foreground active star of late spectral type. The second source has no optical counterpart to a limiting magnitude ~21. The spectrum of this source can be fitted almost equally well with several simple models (power law: photon index ; two-temperature blackbody: keV, km and keV, km; blackbody plus power law: keV, photon index ). We interpret this source as a candidate stellar remnant (neutron star), while the photon index and non-thermal luminosity of the source (almost the same as those of the Vela pulsar and the recently discovered pulsar PSR J 0205+6449 in the supernova remnant 3C 58) suggest that it can be a young “ordinary" pulsar.
Key words: stars: neutron / ISM: bubbles / ISM: individual objects: G 315.4-2.30 (MSH 14-63, RCW 86) / ISM: supernova remnants / X-ray: stars
© ESO, 2003
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