GALEX AND OPTICAL OBSERVATIONS OF GW LIBRAE DURING THE LONG DECLINE FROM SUPEROUTBURST

被引：21

作者：

Bullock, Eric ^{[1
]}

Szkody, Paula ^{[1
]}

Mukadam, Anjum S. ^{[1
]}

Borges, Bernardo W. ^{[2
]}

Fraga, Luciano ^{[3
]}

Gaensicke, Boris T. ^{[4
]}

Harrison, Thomas E. ^{[5
]}

Henden, Arne ^{[6
]}

Holtzman, Jon ^{[5
]}

Howell, Steve B. ^{[7
]}

Lawson, Warrick A. ^{[8
]}

Levine, Stephen ^{[9
,10
]}

Plotkin, Richard M. ^{[1
,11
]}

Seibert, Mark ^{[12
]}

Templeton, Matthew ^{[6
]}

Teske, Johanna ^{[13
]}

Vrba, Frederick J. ^{[9
]}

机构：

[1] Univ Washington, Dept Astron, Seattle, WA 98195 USA

[2] Fundacao Univ Fed Grande Dourados, Fac Ciencias Exatas & Tecnol, BR-79804070 Dourados, Brazil

[3] So Observ Astrophys Res, La Serena, Chile

[4] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England

[5] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA

[6] AAVSO, Cambridge, MA 02138 USA

[7] Natl Opt Astron Observ, Tucson, AZ 85726 USA

[8] Univ New S Wales, Australian Def Force Acad, Sch Phys Environm & Math Sci, Canberra, ACT 2600, Australia

[9] USN Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA

[10] Lowell Observ, Flagstaff, AZ 86001 USA

[11] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands

[12] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA

[13] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA

来源：

ASTRONOMICAL JOURNAL | 2011年 / 141卷 / 03期

基金：

美国国家科学基金会;

关键词：

novae; cataclysmic variables; stars: individual (GW Lib); stars: oscillations; HUBBLE-SPACE-TELESCOPE; WHITE-DWARF; SPECTROSCOPIC OBSERVATIONS; PULSATION; NOVAE;

D O I：

10.1088/0004-6256/141/3/84

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The prototype of accreting, pulsating white dwarfs (GW Lib) underwent a large amplitude dwarf nova outburst in 2007. We used ultraviolet data from Galaxy Evolution Explorer and ground-based optical photometry and spectroscopy to follow GW Lib for three years following this outburst. Several variations are apparent during this interval. The optical shows a superhump modulation in the months following outburst, while a 19 minute quasi-periodic modulation lasting for several months is apparent in the year after outburst. A long timescale (about 4 hr) modulation first appears in the UV a year after outburst and increases in amplitude in the following years. This variation also appears in the optical two years after outburst but is not in phase with the UV. The pre-outburst pulsations are not yet visible after three years, likely indicating the white dwarf has not returned to its quiescent state. The prototype

引用

页数：11

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