English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We present results of 32 nights of CCD photometry of V1974 Cygni, from theyears 1994 and 1995. We verify the presence of two distinct periodicities inthe light curve: 0.0812585 day~1.95 hours and 0.0849767 d~2.04 hr. We establishthat the shorter periodicity is the orbital period of the underlying binarysystem. The longer period oscillates with an average value of |dot(P)| ~3x10^(7)--typical to permanent superhumps. The two periods obey the linearrelation between the orbital and superhump periods that holds among members ofthe SU Ursae Majoris class of dwarf novae. A third periodicity of 0.083204d~2.00 hr appeared in 1994 but not in 1995. It may be related to the recentlydiscovered anti-superhump phenomenon. These results suggest a linkage betweenthe classical nova V1974 Cyg and the SU UMa stars, and indicate the existenceof an accretion disk and permanent superhumps in the system no later than 30months after the nova outburst. From the precessing disk model of the superhumpphenomenon we estimate that the mass ratio in the binary system is between 2.2and 3.6. Combined with previous results this implies a white dwarf mass of0.75-1.07 M sun.Comment: 11 pages, 10 eps. figures, Latex, accepted for publication in MNRA

Permanent Superhumps in Nova V1974 Cygni 1992