Other
Scientific paper
Jan 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...300..794h&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 300, Jan. 15, 1986, p. 794-803.
Other
36
Accretion Disks, Balmer Series, Cataclysmic Variables, Dwarf Novae, Stellar Spectra, Absorption Spectra, Emission Spectra, H Lines, Stellar Mass Ejection
Scientific paper
Analyses of spectroscopic observations made during the declining phase of a short, symmetric eruption of SS Cygni in 1981 are presented. The profiles of the broad H-beta and H-gamma absorption lines from the optically thick disk remained constant throughout much of the decline. This behavior is difficult to reconcile with any of the currently accepted theoretical models for dwarf novae eruptions. The equivalent width of the He II 4686 A emission is roughly constant during the decline. A significant fraction of the increased 4686 A emission comes from a disk 'hot spot', implying that the outburst is accompanied by an increased mass flux from the companion star. This conclusion is supported by the phasing and strength of the Balmer emission cores. Other published data indicate that increased mass transfer may be present in all eruptions of SS Cyg. A strong though not dominant component in the emission cores apears to be chromospheric emission from the K5 V companion star.
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