The nature of the compact X-ray source in the supernova remnant G27.4+0.0

Details The nature of the compact X-ray source in the supernova remnant G27.4+0.0 The nature of the compact X-ray source in the supernova remnant G27.4+0.0

Oct 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...434..627h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 434, no. 2, p. 627-634

Astronomy and Astrophysics

Astronomy

18

Astronomical Models, Neutron Stars, Radio Sources (Astronomy), Supernova Remnants, X Ray Astronomy, X Ray Binaries, X Ray Spectra, Heao 2, Rosat Mission, Stellar Winds, Very Large Array (Vla), X Ray Imagery

Scientific paper

High-resolution X-ray imaging data obtained with ROSAT is used to constrain the nature of the central compact source in the supernova remnant G27.4+0.0. Diffuse emission is seen from throughout the approximately 4 min diameter radio shell, while the central source remains unresolved at approximately 3 sec. We combine archival data from the Einstein HRI, IPC, and MPC with the ROSAT HRI data to define the X-ray spectra of the diffuse and point-like emission. The bulk of the shell radiation is consistent with that of a approximately 107 K plasma, although a higher temperature component is also suggested by the data; coupled with the remnant's size and distance, we derive an age of between 500 and 2500 yr. The point source has a substantially harder spectrum, with a power-law photon index less than or approximately equal to 1. A search for periodic modulation from the point source yields upper limits ranging from 10%-35% for periods between 0.025 and 1000 s, depending on the assumed pulse shape. No aperiodic variability on timescales of from 103 to 108 s is required, although a factor of approximately 2 change between the Einstein and ROSAT eras is possible. We show that the point source cannot represent thermal emission from the surface of a young neutron star and is unlikely to be explained as nonthermal, Crab-like X-ray pulses or a small synchrotron nebula. The most likely models involve accretion-powered systems -- either a wind-fed neutron star with a massive companion or a low-mass X-ray binary. In all probability, this is the youngest X-ray binary in the Galaxy.

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