Cyclic Period Oscillation of the Eclipsing Dwarf Nova DV UMa

• Published in: The Astronomical journal Vol. 153; no. 5; pp. 238 - 245
• Main Authors: Han, Z.-T, Qian, S.-B, Irina, Voloshina, Zhu, L.-Y
• Format: Journal Article
• Language: English
• Published: The American Astronomical Society 01.05.2017
• Subjects: binaries: close; binaries: eclipsing; stars: dwarf novae; stars: individual (DV UMa)
• ISSN: 0004-6256; 1538-3881
• DOI: 10.3847/1538-3881/aa6c2a

DV UMa is an eclipsing dwarf nova with an orbital period of ∼2.06 hr, which lies just at the bottom edge of the period gap. To detect its orbital period changes, we present 12 new mid-eclipse times by using our CCD photometric data and archival data. The latest version of the O-C diagram, combined with the published mid-eclipse times in quiescence, and spanning ∼30 years, was obtained and analyzed. The best fit to those available eclipse timings shows that the orbital period of DV UMa is undergoing a cyclic oscillation with a period of years and an amplitude of s. The periodic variation most likely arises from the light-travel-time effect via the presence of a circumbinary object, because the required energy to drive the Applegate mechanism is too high in this system. The mass of the unseen companion was derived as . If the third body is in the orbital plane (i.e., ) of the eclipsing pair, this would indicate it is a brown dwarf. This hypothetical brown dwarf is orbiting its host star at a separation of ∼8.6 au in an eccentric orbit (e = 0.44).