{ "id": "1711.06076", "version": "v1", "published": "2017-11-16T13:19:49.000Z", "updated": "2017-11-16T13:19:49.000Z", "title": "The 2015 superoutburst of QZ Virginis: Detection of growing superhumps between the precursor and main superoutburst", "authors": [ "Akira Imada", "Taichi Kato", "Keisuke Isogai", "Franz-Josef Hambsch", "Pavol A. Dubovsky", "Igor Kudzej", "Roger D. Pickard", "Hidehiko Akazawa", "Kiyoshi Kasai", "Hiroshi Itoh", "Lewis M. Cook", "Seiichiro Kiyota" ], "comment": "12 pages, 6 figures, published for PASJ, 69, 72", "doi": "10.1093/pasj/psx055", "categories": [ "astro-ph.SR" ], "abstract": "We report on time-resolved photometry of the 2015 February-March superoutburst of QZ Virginis. The superoutburst consisted of a separated precursor, main superoutburst, and rebrightening. We detected superhumps with a period of 0.061181(42) d between the precursor and main superoutburst. Based on analyses of period changes and amplitudes of superhumps, the observed superhumps were identified as growing superhumps (stage A superhumps). The duration of stage A superhumps was about 5 d, unusually long for SU UMa-type dwarf novae. Using the obtained stage A superhump period, we estimated the mass ratio of QZ Vir to be 0.108(3). This value suggests that QZ Vir is an SU UMa-type dwarf nova evolving toward the period minimum. Based on the present and the previous observations regarding long-lasting stage A superhumps, a time scale of stage A superhumps is likely to be determined by the mass ratio of the system and the temperature of the accretion disk.", "revisions": [ { "version": "v1", "updated": "2017-11-16T13:19:49.000Z" } ], "analyses": { "keywords": [ "main superoutburst", "qz virginis", "growing superhumps", "mass ratio", "su uma-type dwarf nova evolving" ], "tags": [ "journal article" ], "note": { "typesetting": "TeX", "pages": 12, "language": "en", "license": "arXiv", "status": "editable" } } }