Photometry of EF Pegasi During Superoutburst

Photometry of EF Pegasi During Superoutburst

EF Pegasi was observed photometrically during a superoutburst in 1991 October. Superhumps seen during these observations were best fit with a period of 2ḥ9. This period is used to determine a likely orbital period of 2ḥ0.5 and a mass ratio(M₂/M₁) of 0.26. Distance estimates for EF Peg give values of...

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Veröffentlicht in:Publications of the Astronomical Society of the Pacific 1993-06, Vol.105 (688), p.579-585
Hauptverfasser: Howell, Steve B., Schmidt, Richard, DeYoung, James A., Fried, Robert, Schmeer, Patrick, Gritz, Larry
Format: Artikel
Sprache:eng
Schlagworte:
Astronomical magnitude
Astronomical objects
Astronomical photometry
Astronomy
Earth, ocean, space
Exact sciences and technology
Light curves
Mass ratio
Novae, dwarf novae, recurrent novae, and other cataclysmic (eruptive) variables
Observatories
Stars
Superhumps
Variable and peculiar stars (including novae)
Variable stars
White dwarfs
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Beschreibung
Zusammenfassung:EF Pegasi was observed photometrically during a superoutburst in 1991 October. Superhumps seen during these observations were best fit with a period of 2ḥ9. This period is used to determine a likely orbital period of 2ḥ0.5 and a mass ratio(M₂/M₁) of 0.26. Distance estimates for EF Peg give values of 250 to 600 pc.
ISSN:0004-6280
1538-3873
DOI:10.1086/133198