TY - JOUR
T1 - The X-ray emission from Nova V382 Velorum - II. The super-soft component observed with BeppoSAX
AU - Orio, M.
AU - Parmar, A. N.
AU - Greiner, J.
AU - Ögelman, H.
AU - Starrfield, Sumner
AU - Trussoni, E.
PY - 2002/6/11
Y1 - 2002/6/11
N2 - 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.
AB - 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.
KW - Novae, cataclysmic variables
KW - Stars: individual: V382 Vel
KW - X-rays: stars
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U2 - 10.1046/j.1365-8711.2002.05577.x
DO - 10.1046/j.1365-8711.2002.05577.x
M3 - Article
AN - SCOPUS:0043094330
SN - 0035-8711
VL - 333
SP - L11-L15
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 1
ER -