Thermonuclear flash model for long X-ray tails from Aquila X-1

Details Thermonuclear flash model for long X-ray tails from Aquila X-1 Thermonuclear flash model for long X-ray tails from Aquila X-1

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...390..634f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 390, no. 2, May 10, 1992, p. 634-638.

Astronomy and Astrophysics

Astrophysics

15

Neutron Stars, Stellar Radiation, Thermonuclear Reactions, X Ray Stars, Electron Capture, Stellar Envelopes, Stellar Luminosity

Scientific paper

Attention is given to a thermonuclear flash model for long X-ray tails from the recurrent transient Aql X-1, in which the extended phase of nuclear burning is due to the fact that the envelope is out of thermal equilibrium. Only the first X-ray burst emitted by Aql X-1 during its transient outburst exhibits a long X-ray tail. The properties of subsequent bursts are distinguished by a lack of an X-ray tail reflecting the much smaller accumulated masses which result from the effects of thermal inertia in the neutron star envelope. The characteristics of the latter bursts are similar to those of typical X-ray bursters. For a neutron star characterized by a mass and radius of 1.4 solar mass and 9.1 km, respectively, the occurrence of the long X-ray tail requires that the mass of the accumulated layer be less than 10 exp 23 g and that the envelope temperatures of the neutron star be less than 1.5 x 10 exp 7. This interpretation is found to be consistent with the thermal relaxation of the neutron star envelope during the quiescent state of Aql X-1 and with the mass accretion rates inferred for the transient outburst itself.

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