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Title:
The Far-Ultraviolet Spectrum and Short-Timescale Variability of AM Herculis from Observations with the Hopkins Ultraviolet Telescope
Authors:
Greeley, Bradford W.; Blair, William P.; Long, Knox S.; Raymond, John C.
Publication:
The Astrophysical Journal, Volume 513, Issue 1, pp. 491-505. (ApJ Homepage)
Publication Date:
03/1999
Origin:
APJ
ApJ Keywords:
STARS: NOVAE, CATACLYSMIC VARIABLES, STARS: INDIVIDUAL: CONSTELLATION NAME: AM HERCULIS, STARS: MAGNETIC FIELDS
DOI:
10.1086/306853
Bibliographic Code:
1999ApJ...513..491G

Abstract

Using the Hopkins Ultraviolet Telescope (HUT), we have obtained 850-1850 Å spectra of the magnetic cataclysmic variable star AM Her in the high state. These observations provide high time resolution spectra of AM Her in the far-ultraviolet and sample much of the orbital period of the system. The spectra are not well modeled in terms of simple white dwarf (WD) atmospheres, especially at wavelengths shortward of Lyalpha. The continuum flux changes by a factor of 2 near the Lyman limit as a function of orbital phase; the peak fluxes are observed near magnetic phase 0.6 when the accreting pole of the WD is most clearly visible. The spectrum of the hot spot can be modeled in terms of a 100,000 K WD atmosphere covering 2% of the WD surface. The high time resolution of the HUT data allows an analysis of the short-term variability and shows the UV luminosity to change by as much as 50% on timescales as short as 10 s. This rapid variability is shown to be inconsistent with the clumpy accretion model proposed to account for the soft X-ray excess in polars. We see an increase in narrow-line emission during these flares when the heated face of the secondary is in view. The He II narrow-line flux is partially eclipsed at secondary conjunction, implying that the inclination of the system is greater than 45 deg. We also present results from models of the heated face of the secondary. These models show that reprocessing on the face of the secondary star of X-ray/EUV emission from the accretion region near the WD can account for the intensities and kinematics of most of the narrow-line components observed.
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