Variable O VI and N V Emission from the X-ray Binary LMC X-3: Heating of the Black Hole Companion - Astrophysics > High Energy Astrophysical PhenomenaReportar como inadecuado




Variable O VI and N V Emission from the X-ray Binary LMC X-3: Heating of the Black Hole Companion - Astrophysics > High Energy Astrophysical Phenomena - Descarga este documento en PDF. Documentación en PDF para descargar gratis. Disponible también para leer online.

Abstract: Based on high-resolution ultraviolet spectroscopy obtained with FUSE and COS,we present new detections of O VI and N V emission from the black-hole X-raybinary XRB system LMC X-3. We also update the ephemeris of the XRB usingrecent radial velocity measurements obtained with the echelle spectrograph onthe Magellan-Clay telescope. We observe significant velocity variability of theUV emission, and we find that the O VI and N V emission velocities follow theoptical velocity curve of the XRB. Moreover, the O VI and N V intensitiesregularly decrease between binary phase = 0.5 and 1.0, which suggests that thesource of the UV emission is increasingly occulted as the B star in the XRBmoves from superior to inferior conjunction. These trends suggest thatillumination of the B-star atmosphere by the intense X-ray emission from theaccreting black hole creates a hot spot on one side of the B star, and this hotspot is the origin of the O VI and N V emission. However, the velocitysemiamplitude of the ultraviolet emission, K {UV}~180 km-s, is lower than theoptical semiamplitude; this difference could be due to rotation of the B star.If our hypothesis about the origin of the highly ionized emission is correct,then careful analysis of the emission occultation could, in principle,constrain the inclination of the XRB and the mass of the black hole.



Autor: Limin Song, Todd M. Tripp, Q. Daniel Wang, Yangsen Yao, Wei Cui, Yongquan Xue, Jerome A. Orosz, Danny Steeghs, James F. Steiner,

Fuente: https://arxiv.org/







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