The X-ray emission from Nova V382 Velorum - II. The super-soft component observed with BeppoSAX

M. Orio, A. N. Parmar, J. Greiner, H. Ögelman, Sumner Starrfield, E. Trussoni

Research output: Contribution to journalArticlepeer-review

38 Scopus citations

Abstract

Nova Velorum 1999 (V382 Vel) was observed by BeppoSAX six months after optical maximum, and was detected as a bright X-ray supersoft source, with a count rate 3.454 ± 0.002 cts-1 in the Low-Energy Concentrator Spectrometer (LECS). It was the softest and most luminous supersoft source observed with this instrument. The flux in the 0.1-0.7 keV range was not constant during the observation. It dropped by a factor of 2 in less than 1.5 hr and then was faint for at least 15 min, without significant spectral changes. The observed spectrum is not well-fitted with atmospheric models of a hot, hydrogen burning white dwarf. This is due mainly to a supersoft excess in the range of 0.1-0.2 keV, but the fit can be significantly improved at higher energy if at least one emission feature is superimposed. We suggest that a 'pseudocontinuum' was detected, consisting of emission lines in the supersoft X-ray range superimposed on the thermal continuum of a white dwarf atmosphere. As a result, an accurate determination of the effective temperature and gravity of the white dwarf at this post-outburst stage is not possible.

Original languageEnglish (US)
Pages (from-to)L11-L15
JournalMonthly Notices of the Royal Astronomical Society
Volume333
Issue number1
DOIs
StatePublished - Jun 11 2002

Keywords

  • Novae, cataclysmic variables
  • Stars: individual: V382 Vel
  • X-rays: stars

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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