Determination of Mass-Loss Rates of PG 1159 Stars from Far-Ultraviolet Spectroscopy

Details Determination of Mass-Loss Rates of PG 1159 Stars from Far-Ultraviolet Spectroscopy Determination of Mass-Loss Rates of PG 1159 Stars from Far-Ultraviolet Spectroscopy

Jun 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...500l..55k&link_type=abstract

Astrophysical Journal Letters v.500, p.L55

Astronomy and Astrophysics

Astronomy

41

Stars: Agb And Post-Agb, Stars: Atmospheres, Stars: Evolution, Stars: Mass Loss, Stars: Chemically Peculiar, Ultraviolet: Stars

Scientific paper

We determine the mass-loss rates of four hot, low-gravity PG 1159 stars that are regarded as immediate descendants of Wolf-Rayet central stars of planetary nebulae (i.e., early spectral type [WCE]). The sample consists of classical hydrogen-deficient PG 1159 stars (K1-16, NGC 246, and RX J2117.1+3412) as well as one object of the very rare "hybrid" subtype, which also exhibits hydrogen lines (NGC 7094). The sample is complemented by the famous [WC]-PG 1159 transition object Abell 78. Our analysis is based on the O VI lambda lambda 1032, 1038 resonance line, which is the strongest wind feature in these objects. Far-UV observations were performed with the Berkeley spectrograph during the ORFEUS-SPAS II mission. One spectrum is taken from archive data of the ORFEUS-SPAS I mission, and another one was obtained with the Hopkins Ultraviolet Telescope during the Astro-2 mission. We find mass-loss rates in the range {log}(M dot /Msolar yr-1 )=-8,...,-7 , as compared to the [WCE] stars that have mass-loss rates of about {log}(M dot /Msolar yr-1 )=-5.5,...,-6.5 . By comparing with theory, we conclude that the wind of PG 1159 stars is driven by radiation pressure.

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