Mass Estimates of the Fast Novae QZ AUR and HER 1991

Details Mass Estimates of the Fast Novae QZ AUR and HER 1991 Mass Estimates of the Fast Novae QZ AUR and HER 1991

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...182.2905i&link_type=abstract

American Astronomical Society, 182nd AAS Meeting, #29.05; Bulletin of the American Astronomical Society, Vol. 25, p.833

Astronomy and Astrophysics

Astronomy

Scientific paper

Theoretical models of nova outbursts predict that the most massive white dwarfs will be associated with the fastest and most luminous novae. The distribution of observed nova outbursts is expected to be weighted toward nova with M > 1.3 Msun. However, of the known novae, very few mass estimates are available. We conducted observations of the fast novae QZ Aurigae (Nova Aur 1964) and Her 1991 with the 4m telescope at KPNO and the 1.8m telescope at Apache Point Observatory. We have obtained Hα radial velocity curves which yield mass estimates for the stellar components. Our results indicate that both systems have massive white dwarfs although the masses are not as high as theoretical models predict. We deduce that the accretion disk is the dominant source of light in both systems, effectively preventing us from detecting the secondary even though the novae have long periods (7.14 hr and 8.58 hr). This work was partially supported by NASA grant NAGW-3158.

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