HST eclipse maps of UX UMa in the CIV lambda 1550 and HeII lambda 1640 regions

Details HST eclipse maps of UX UMa in the CIV lambda 1550 and HeII lambda 1640 regions HST eclipse maps of UX UMa in the CIV lambda 1550 and HeII lambda 1640 regions

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...18312307b&link_type=abstract

American Astronomical Society, 183rd AAS Meeting, #123.07; Bulletin of the American Astronomical Society, Vol. 25, p.1476

Astronomy and Astrophysics

Astronomy

Scientific paper

We present spectrally-resolved eclipse maps of the accretion disk of the nova-like variable UX UMa in the CIV lambda 1550 and HeII lambda 1640 spectral regions. The analysis is based on time-resolved spectroscopy (wavelength range =~ 35 Angstroms) during eclipse, obtained with the HST High Resolution Spectrograph on 1993 Jan 19 - 22. The spectra were divided in a set of narrow passbands (4-5 Angstroms wide) and light curves were constructed for each one. The eclipse mapping method was used to obtain maps of the disk brightness distribution in each passband. The continuum maps show a small disk with radius =~ 20% of the orbital separation. The radial temperature profile derived from these maps closely follows the radial dependence predicted by the stationary disk model (T ~ R(-3/4) ) at large disk radii, but becomes flatter than the theoretical model close to the disk center. The temperatures in the disk range from 30000K to 10000K and the inferred mass accretion rate is M= 10({-8.3+/-) 0.2} \:M_{sun yr}(-1) . Eclipse maps from contemporary R-band photometry are shown for comparison. The HeII map shows an extended brightness distribution which fills most of the primary lobe and whose temperature profile is much flatter than that of the continuum maps. The CIV doublet has a complex structure with absorption components superimposed on a broad emission profile. The line center does not eclipse and was not mapped. The spatially-resolved spectra obtained by combining all maps show the HeII line in absorption at the inner disk which progressively changes to broad emission with increasing disk radius. A similar but weaker effect is seen in the SiII lambda 1527, 1533 absorption lines.

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