Cooling of the white dwarf in U Geminorum between outbursts

Details Cooling of the white dwarf in U Geminorum between outbursts Cooling of the white dwarf in U Geminorum between outbursts

Mar 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...424l..49l&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 424, no. 1, p. L49-L52

Astronomy and Astrophysics

Astrophysics

45

Accretion Disks, Cataclysmic Variables, Data Processing, Ephemerides, H Alpha Line, Novae, White Dwarf Stars, Faint Object Camera, Hubble Space Telescope, Iue, Line Of Sight, Signal To Noise Ratios

Scientific paper

We have obtained far-ultraviolet (1150-1610 A) spectra of U Gem with the Faint Object Spectrograph on the Hubble Space Telescope approximately 13 and 70 days after the end of a normal dwarf nova outburst of the system. Both spectra appear dominated by the White Dwarf (WD) in U Gem. At 1400 A, the flux from U Gem declined approximately 28% between the two observations. Detailed comparison of the spectra with solar abundance WD models suggest that average surface temperature of the WD surface cooled from approximately 39,400 K to approximately 32,100 K between the two observations. The main features which are not fitted well by WD models are absorption due to N V lambda lambda-1239, 1243 and emission at Lyman-alpha. These observations provide unambiguous confirmation that the WD in U Gem cools during quiescence, as was suggested by analyses of far-ultraviolet spectra obtained with International Ultraviolet Explorer (IUE) and Hopkins Ultraviolet Telescope (HUT).

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