J/A+A/630/A106 Stellar pulsators in the eclipsing binaries (Gaulme+, 2019)
Systematic search for stellar pulsators in the eclipsing binaries observed
by Kepler.
Gaulme P., Guzik J.A.
<Astron. Astrophys., 630, A106 (2019)>
=2019A&A...630A.106G 2019A&A...630A.106G (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing ; Asteroseismology
Keywords: binaries: general - binaries: eclipsing - stars: oscillations -
stars: variables: delta Scuti - asteroseismology - catalogs
Abstract:
Eclipsing binaries (EBs) are unique targets for measuring precise
stellar properties and can be used to constrain stellar evolution
models. In particular, it is possible to measure masses and radii of
both components of a double-lined spectroscopic EB at the percent
level. Since the advent of high-precision photometric space missions
(MOST, CoRoT, Kepler, BRITE, TESS), the use of stellar pulsation
properties to infer stellar interiors and dynamics constitutes a
revolution for studies of low-mass stars. The Kepler mission has led
to the discovery of thousands of classical pulsators such as δ
Scuti and solar-like oscillators (main sequence and evolved), but also
almost 3000 EBs with orbital periods shorter than 1100 days. We report
the first systematic search for stellar pulsators in the entire Kepler
EB catalog. The focus is mainly aimed at discovering δ Scuti,
γ Doradus, red giant, and tidally excited pulsators. We
developed a data inspection tool (DIT) that automatically produces a
series of plots from the Kepler light curves that allows us to
visually identify whether stellar oscillations are present in a given
time series. We applied the DIT to the whole Kepler EB database and
identified 303 systems whose light curves display oscillations,
including 163 new discoveries. A total of 149 stars are flagged as
δ Scuti (100 from this paper), 115 as γ Doradus (69 new),
85 as red giants (27 new), and 59 as tidally excited oscillators (29
new). There is some overlap among these groups, as some display
several types of oscillations. Despite the likelihood that many of
these systems are false positives, for example, when an EB light curve
is blended with a pulsator, this catalog gathers a vast sample of
systems that are valuable for a better understanding of stellar
evolution.
Description:
we led the first systematic search for stellar pulsators in the
likely-to-be complete Kepler EB catalog, which includes 2925 systems
among which about 600 are actually ellipsoidal binaries. To this aim,
we developed a dedicated data inspection tool that automatically
processes the Kepler light curves, provided elementary information
about EB properties is fed in (orbital period, epochs, and duration of
eclipses). We focused on three main classes of stellar oscillators:
classical δ Sct and γ Dor pulsators, solar-like
oscillators which happened to be all RGs, and tidal pulsators.
We established a list of 303 pulsators associated with an EB,
including 163 that were reported for the first time as pulsator and
binary candidates. A total of 149 stars are flagged as δ Sct
(100 from this paper), 115 stars as γ Dor (69 new), 85 stars as
RGs (27 new), and 59 as tidally excited oscillators (29 new).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 196 307 Properties of the systems where pulsations are
detected
refs.dat 151 104 References
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 I8 --- KIC KIC number
10- 14 I5 K Teff ? Effective temperature
16- 20 F5.2 mag Kepmag ? Kepler magnitude
22- 24 A3 --- Type Type of binary systems (1)
26- 27 I2 --- Ecl Number of eclipses that are visible per
orbital period (0 for ELL systems,
1 or 2 for the others)
29- 35 F7.2 d Porb Orbital period rounded at two digits
37- 41 F5.2 % Depth ? Eclipse depth of the deepest eclipse
(primary)
43- 46 F4.2 --- Sep ? Orbital phase separation in between the
secondary and the primary eclipse
48- 51 F4.2 --- W2/W1 ? Eclipse duration ratio W2/W1
53- 56 F4.1 --- W1+W2/Porb ? Sum of eclipse duration relative to orbital
period, W1+w2/Porb
58- 97 A40 --- Pulstype Pulsator type (2)
99-139 A41 --- Ref Literature, in refs.dat file
141 A1 --- NewPB [Y] Target identified both as a pulsator and
a binary for first time
143-196 A54 --- Notes Notes (3)
--------------------------------------------------------------------------------
Note (1): type of binary systems as follows:
D = detached
SD = semi-detached
OC = over-contact
ELL = ellipsoidal
Note (2): Pulsator type as δ-Sct for δ Scuti,
γ Dor for γ Doradus, "Rossby", "RG" for RG solar-like oscillator,
"tidal", SPB for slowly pulsating B-type stars, "WD" for white dwarf, or
sdB for subdwarf B. The type "rot" stands for surface stellar "rotation"
that may mimic stellar pulsations.
Note (3): Notes are random relevant specific information regarding each system.
"HB" stands for heartbeat, FP for false positive, KOI for Kepler object of
interest, Porb for orbital period, "Ecl." for eclipse, "harm." for harmonics,
T1 and T2 for star 1 star 2 effective temperatures, Teff refers to the
published KIC effective temperature, "SB1" and "SB2" for single or
double-lined spectroscopic binary. The label "Porb=Porb/2" means that the
actual orbital period is half of what Villanova database reported.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: refs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Ref Reference code
8- 26 A19 --- BibCode BibCode
28- 51 A24 --- Aut Author's name
53-151 A99 --- Com Comments
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 12-Dec-2019