Spectrophotometry of the extreme-ultraviolet star Feige 24

Details Spectrophotometry of the extreme-ultraviolet star Feige 24 Spectrophotometry of the extreme-ultraviolet star Feige 24

Aug 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...216...18l&link_type=abstract

Astrophysical Journal, Part 1, vol. 216, Aug. 15, 1977, p. 18-22.

Astronomy and Astrophysics

Astrophysics

28

Binary Stars, Far Ultraviolet Radiation, Hot Stars, Stellar Spectrophotometry, White Dwarf Stars, Emission Spectra, Helium Ions, Line Spectra, Stellar Luminosity, Stellar Spectra, Ultraviolet Spectra

Scientific paper

Spectrophotometry of Feige 24, the second known extrasolar source of extreme-ultraviolet (100-1000 A) radiation, was obtained on six nights in 1975-1976. The data have 8-A resolution and span the region from 3800 to 8200 A. The two components of the system are classified as DAwk and M1-2 V, in agreement with previous inferences. The spectroscopic distance modulus of the system is estimated as + or - 1; the resulting absolute visual magnitude of 7.9 + or - 1 is consistent with the luminosities of either a composite white dwarf-red dwarf or a dwarf nova system. The spectra display strong hydrogen and He I emission which is highly variable on a time scale of days. These data are consistent with flare-star activity on the dM component; however, brief spectroscopic and photometric searches for more rapid emission-line variability were negative. It is more likely that the system is a close binary and that the variable emission is due to heating of the cool star by the intense ionizing flux from the hot white dwarf.

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