Astronomy and Astrophysics – Astronomy
Scientific paper
May 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...196.5904s&link_type=abstract
American Astronomical Society, 196th AAS Meeting, #59.04; Bulletin of the American Astronomical Society, Vol. 32, p.766
Astronomy and Astrophysics
Astronomy
Scientific paper
We present evidence indicating the presence of a 6.4 keV emission line during a burst from the soft gamma-ray repeater SGR 1900+14. The Rossi X-ray Timing Explorer (RXTE) monitored this source extensively during its outburst in the summer of 1998. A strong burst observed on August 29, 1998 revealed a number of unique properties. The burst exhibits a precursor and is followed by a long ( ~ 103 s) tail modulated at the 5.16 s stellar rotation period. The precursor has a duration of ~ 0.85 s and shows both significant spectral evolution as well as an emission feature centered near 6.4 keV during the first 0.3 s of the event, when the X-ray spectrum was hardest. The continuum during the burst is well fit with an optically thin thermal bremsstrahlung (OTTB) spectrum with the temperature ranging from as high as ~ 40 to as low as 10 keV. The line is strong, with an equivalent width of ~ 400 eV, and the centroid is consistent with Fe K-α fluorescence from relatively cool material. If the rest-frame energy is indeed 6.4 keV, then the lack of an observed redshift indicates that the source of the line is at least ~ 80 km above the surface of the neutron star. We briefly discuss the implications of the line detection in the context of models for SGRs.
Ibrahim Alaa I.
Strohmayer Tod E.
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