Following the Accreting Pulsating White Dwarfs in GW Lib and V455 And After their Superoutbursts

Details Following the Accreting Pulsating White Dwarfs in GW Lib and V455 And After their Superoutbursts Following the Accreting Pulsating White Dwarfs in GW Lib and V455 And After their Superoutbursts

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21712606s&link_type=abstract

American Astronomical Society, AAS Meeting #217, #126.06; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

Accreting pulsating white dwarfs offer the opportunity to study the effects of mass transfer, rotation and accretion on the internal structure of white dwarfs, as pulsation modes in white dwarfs penetrate deep into the stars. Thirteen of these systems are now known to reside in cataclysmic variables. These objects undergo large amplitude outbursts on 20-30 yr timescales which heat the white dwarfs and move them out of their instability zones for 2-3 yrs. Following the white dwarfs as they re-enter the instability strip thus allows an unprecedented opportunity to glean information about the modes and depth of heating.
GW Lib and V455 And are two objects with accreting pulsating white dwarfs that underwent superoutbursts in 2007. We have followed these systems with ultraviolet data from GALEX and HST, and ground-based optical data. These 2 systems show different behavior, with GW Lib remaining hot and lacking pulsations 3 yrs post outburst, while V455 And shows a return of a group of periodicities present at shorter periods than pre-outburst. These differences are being studied on the basis of the masses and rotation rates derived from the COS data.
Support for this work was provided by NASA GALEX grants NNX08AU43G, NNX09AF87G, HST grants GO-11638, GO-11639, and NSF grant AST-0607840.

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