6533b7d2fe1ef96bd125f7b0
RESEARCH PRODUCT
A TEST of the NATURE of the FE K LINE in the NEUTRON STAR LOW-MASS X-RAY BINARY SERPENS X-1
Jeroen HomanLuciano BurderiSudip BhattacharyyaTiziana Di SalvoChia-ying ChiangMichael ParkerJon M. MillerElise EgronR. IariaAntonino D'aiEdward M. CackettDidier BarretDidier BarretDacheng LinAndrew C. FabianM. Coleman Millersubject
SerpensAstrophysics::High Energy Astrophysical PhenomenaX-ray binaryFOS: Physical sciencesAstrophysicsaccretion accretion disk01 natural sciencesSpectral linestars: neutronSettore FIS/05 - Astronomia E Astrofisica0103 physical sciencesEmission spectrum010303 astronomy & astrophysicsLine (formation)High Energy Astrophysical Phenomena (astro-ph.HE)Physics010308 nuclear & particles physicsAstronomy and Astrophysicsprofiles; stars: neutron; X-rays: binaries; Astronomy and Astrophysics; Space and Planetary Science [accretion accretion disks; line]Astronomy and AstrophysicK-lineX-rays: binarieBlack holeNeutron starline: profileSpace and Planetary ScienceAstrophysics - High Energy Astrophysical Phenomenadescription
Broad Fe K emission lines have been widely observed in the X-ray spectra of black hole systems, and in neutron star systems as well. The intrinsically narrow Fe K fluorescent line is generally believed to be part of the reflection spectrum originating in an illuminated accretion disk, and broadened by strong relativistic effects. However, the nature of the lines in neutron star LMXBs has been under debate. We therefore obtained the longest, high-resolution X-ray spectrum of a neutron star LMXB to date with a 300 ks Chandra HETGS observation of Serpens X-1. The observation was taken under the "continuous clocking" mode and thus free of photon pile-up effects. We carry out a systematic analysis and find that the blurred reflection model fits the Fe line of Serpens X-1 significantly better than a broad Gaussian component does, implying that the relativistic reflection scenario is much preferred. Chandra HETGS also provides highest spectral resolution view of the Fe K region and we find no strong evidence for additional narrow lines.
| year | journal | country | edition | language |
|---|---|---|---|---|
| 2015-09-09 |