TY - JOUR
T1 - KIC 4552982
T2 - Outbursts and asteroseismology from the longest pseudo-continuous light curve of A ZZ Ceti
AU - Bell, Keaton J.
AU - Hermes, J. J.
AU - Bischoff-Kim, A.
AU - Moorhead, Sean
AU - Montgomery, M. H.
AU - �stensen, Roy
AU - Castanheira, Barbara G.
AU - Winget, D. E.
PY - 2015/8/10
Y1 - 2015/8/10
N2 - We present the Kepler light curve of KIC 4552982, the first ZZ Ceti (hydrogen-atmosphere pulsating white dwarf star) discovered in the Kepler field of view. Our data span more than 1.5 years, with a 86% duty cycle, making it the longest pseudo-continuous light curve ever recorded for a ZZ Ceti. This extensive data set provides the most complete coverage to date of amplitude and frequency variations in a cool ZZ Ceti. We detect 20 independent frequencies of variability in the data that we compare with asteroseismic models to demonstrate that this star has a mass . We identify a rotationally split pulsation mode and derive a probable rotation period for this star of 17.47 � 0.04 hr. In addition to pulsation signatures, the Kepler light curve exhibits sporadic, energetic outbursts that increase the star's relative flux by 2%-17%, last 4-25 hr, and recur on an average timescale of 2.7 days. These are the first detections of a new dynamic white dwarf phenomenon that may be related to the pulsations of this relatively cool ( K) ZZ Ceti star near the red edge of the instability strip.
AB - We present the Kepler light curve of KIC 4552982, the first ZZ Ceti (hydrogen-atmosphere pulsating white dwarf star) discovered in the Kepler field of view. Our data span more than 1.5 years, with a 86% duty cycle, making it the longest pseudo-continuous light curve ever recorded for a ZZ Ceti. This extensive data set provides the most complete coverage to date of amplitude and frequency variations in a cool ZZ Ceti. We detect 20 independent frequencies of variability in the data that we compare with asteroseismic models to demonstrate that this star has a mass . We identify a rotationally split pulsation mode and derive a probable rotation period for this star of 17.47 � 0.04 hr. In addition to pulsation signatures, the Kepler light curve exhibits sporadic, energetic outbursts that increase the star's relative flux by 2%-17%, last 4-25 hr, and recur on an average timescale of 2.7 days. These are the first detections of a new dynamic white dwarf phenomenon that may be related to the pulsations of this relatively cool ( K) ZZ Ceti star near the red edge of the instability strip.
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U2 - 10.1088/0004-637X/809/1/14
DO - 10.1088/0004-637X/809/1/14
M3 - Article
SN - 0004-637X
VL - 809
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 14
ER -