J/AJ/161/27 O-C values of KIC10975348 with Kepler Space Telescope (Yang+, 2021)
KIC 10975348: a double-mode or triple-mode high-amplitude δ scuti Star?
Yang T.-Z., Sun X.-Y., Zuo Z.-Y., Liu H.-W.
<Astron. J., 161, 27 (2021)>
=2021AJ....161...27Y 2021AJ....161...27Y
ADC_Keywords: Stars, variable; Stars, faint; Optical
Keywords: Stellar oscillations ; Delta Scuti variable stars ;
Short period variable stars
Abstract:
In this paper, we analyze the light variations of KIC10975348 using
photometric data delivered from the Kepler mission. This star is
exceptionally faint (Kp=18.6mag) compared to most well-studied
δScuti stars. The Fourier analysis of the short-cadence data
(i.e., Q14, Q15, and Q16, spanning 220days) reveals that the
variations are dominated by the strongest mode with a frequency of
F0=10.231899/day, which is compatible with that obtained from
RATS-Kepler. The other two independent modes with F1(=13.4988/day) and
F2(=19.0002/day) are newly detected and have amplitudes two orders of
magnitude smaller than F0. We note that, for the first time, this star
is identified to be a high-amplitude δSct (HADS) star with an
amplitude of about 0.7mag, and the lower ratio of F0/F1=0.758 suggests
that it might be a metal-rich variable star. The frequency F2 may be a
third overtone mode, suggesting that this target might be a new radial
triple-mode HADS star. We perform an O-C analysis using 1018 newly
determined times of maximum light and derive an ephemeris formula of
Tmax=2456170.241912(0)+0.097734(1)xE. The O-C diagram shows that the
pulsation period of KIC10975348 seems to show no obvious change, which
is in contrast to that of the majority of HADS stars. The possible
cause of that may be due to the current short time span of the
observations. To verify its possible period variations, regular
observation from space with a longer time span in the future is
needed.
Description:
KIC10975348 was observed by the Kepler space telescope from
BJD2456107.139 to 2456424.001, including three quarters (i.e., Q14,
Q15, and Q16). There are two observation strategies for this star:
long-cadence (LC; 29.5minutes integration time) mode and short-cadence
(SC; 58.5s integration time) mode. To avoid the Nyquist alias peaks,
we only used the SC data, i.e., Q14.3, Q15.3, and Q16.3 in this work.
All the SC data are available in the Kepler Asteroseismic Science
Operations Center (KASOC) database (http://kasoc.phys.au.dk/).
Objects:
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RA (2000) DE Designation(s)
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19 26 46.11 +48 25 30.7 KIC 10975348 = KIC 10975348
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 27 343 345 Times of Maximum Light and O-C Values of Q14.3
table4.dat 27 348 351 Times of Maximum Light and O-C Values of Q15.3
table5.dat 27 322 322 Times of Maximum Light and O-C Values of Q16.3
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See also:
J/A+A/445/617 : V823 Cas BV(RI)c differential photometry (Jurcsik+, 2006)
J/A+A/478/865 : BVIc differential photometry of GSC 0762-110 (Wils+, 2008)
J/A+A/528/A147 : CoRoT 101155310 light curve (Poretti+, 2011)
J/AJ/144/92 : Times of maximum light for SX Phe star XX Cyg (Yang+, 2012)
J/MNRAS/460/1970 : Kepler δ Sct stars amplitude modulation (Bowman+,2016)
http://kasoc.phys.au.dk/ : KASOC database
Byte-by-byte Description of file: table[345].dat
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Bytes Format Units Label Explanations
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1- 12 F12.6 d BJD Barycentric Julian Date; JD-2400000
14- 17 I4 --- E Cycle number (1)
19- 27 F9.6 d O-C O-C value (1)
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Note (1): E and O-C are based on the ephemeris formula
Tmax=T0+PxE=2456170.241912(0)+0.097734(1)xE
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History:
From electronic version of the journal
(End) Prepared by Coralie Fix [CDS], 15-Mar-2021