Abstract
To explore the amount of secondary irradiation and the long-term effects of a superoutburst (SOB) on tremendous outburst amplitude dwarf novae (TOADs), we obtained spectra of EG Cnc for 3-17 months past its SOB, of SW UMa, WX Cet, and USNO 1425.09823278 at 2 months past their SOBs and HV Vir and LL And during their quiescent states at 3 and 5 yr past SOB. The quiescent spectra of EG Cnc, HV Vir, LL And, and USNO 1425 show emission cores surrounded by broad absorption lines from the white dwarf, consistent with very low mass accretion onto low-temperature white dwarfs. SW UMa and WX Cet likely have higher accretion rates and more extensive disks. SW UMa exhibits unusual disk structure, with three zones of emission that persist for 3 days, while EG Cnc and USNO 1425 have a strong orbital modulation of the Balmer lines that may be related to long-lasting irradiation after superoutburst.
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Footnotes
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Based on observations with the Apache Point Observatory (APO) 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium (ARC).