Hard X-ray and Infrared Emission from Apparently Single White Dwarfs

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dc.creatorChu, Y. -H.
dc.creatorGruendl, R. A.
dc.creatorGuerrero, M. A.
dc.creatorSu, K. Y. -L.
dc.date2007-01-01
dc.date.accessioned2026-07-07T07:37:48Z
dc.date.available2026-07-07T07:37:48Z
dc.descriptionThe photospheric emission of a white dwarf (WD) is not expected to be detectable in hard X-rays or the mid-IR. Hard X-ray (~1 keV) emission associated with a WD is usually attributed to a binary companion; however, emission at 1 keV has been detected from three WDs without companions: KPD 0005+5106, PG 1159, and WD 2226-210. The origin of their hard X-ray emission is unknown, although it has been suggested that WD 2226-210 has a late-type companion whose coronal activity is responsible for the hard X-rays. Recent Spitzer observations of WD 2226-210 revealed mid-IR excess emission indicative of the existence of a dust disk. It now becomes much less clear whether WD 2226-210's hard X-ray emission originates from the corona of a late-type companion or from the accretion of the disk material. High-quality X-ray observations and mid-IR observations of KPD 0005+5106 and PG 1159 are needed to help us understand the origin of their hard X-ray emission.
dc.description6 pages, 3 figures, 15th European White Dwarf Workshop, held at Leicester on August 7-11, 2006
dc.identifierhttps://arxiv.org/abs/astro-ph/0701025
dc.identifierhttp://arxiv.org/abs/astro-ph/0701025
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/120902
dc.subjectAstrophysics
dc.titleHard X-ray and Infrared Emission from Apparently Single White Dwarfs
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