Red component activity in dwarf novae

Details Red component activity in dwarf novae Red component activity in dwarf novae

Jun 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984natur.309..768w&link_type=abstract

Nature (ISSN 0028-0836), vol. 309, June 28, 1984, p. 768-770.

Computer Science

21

Dwarf Novae, Light Emission, Stellar Activity, Stellar Radiation, Accretion Disks, Binary Stars, Starspots

Scientific paper

SU Ursae Majoris systems are short-period binary dwarf novae characterized by two distinct classes of outbursts: "normal outbursts" of duration ≡2 days and less frequent "superoutbursts" which last ≡12 days. During superoutbursts, "superhumps" are observed which modulate the visible light by ⪉40% with a period 3 - 7% longer than the binary period. Measurement of eclipse depths in the two eclipsing SU UMa systems during superoutburst should show whether or not the superhump light is eclipsed and hence make it possible to infer its location either in the eclipsed disk or in the uneclipsed red component. Study of the available eclipse data reported here shows that the superhump light is not eclipsed, so that the red component is the location of the superhump.

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