J/A+A/638/A59 delta Scuti stars with TESS (Barcelo Forteza+, 2020)
Unveiling the power spectra of delta Scuti stars with TESS.
The temperature, gravity, and frequency scaling relation.
Barcelo Forteza S., Moya A., Barrado D., Solano E., Martin-Ruiz S.,
Suarez J.C., Garcia Hernandez A.
<Astron. Astrophys. 638, A59 (2020)>
=2020A&A...638A..59B 2020A&A...638A..59B (SIMBAD/NED BibCode)
ADC_Keywords: Stars, A-type ; Stars, F-type; Asteroseismology ;
Effective temperatures
Keywords: asteroseismology - stars: oscillations - stars: variables: delta Scuti
Abstract:
Thanks to high-precision photometric data legacy from space telescopes
like CoRoT and Kepler, the scientific community could detect and
characterize the power spectra of hundreds of thousands of stars.
Using the scaling relations, it is possible to estimate masses and
radii for solar-type pulsators. However, these stars are not the only
kind of stellar objects that follow these rules: delta Scuti stars
seem to be characterized with seismic indexes such as the large
separation. Thanks to long-duration high-cadence TESS light curves, we
analysed more than two thousand of this kind of classical pulsators.
In that way, we propose the frequency at maximum power as a proper
seismic index since it is directly related with the intrinsic
temperature, mass and radius of the star. This parameter seems not to
be affected by rotation, inclination, extinction or resonances, with
the exception of the evolution of the stellar parameters. Furthermore,
we can constrain rotation and inclination using the departure of
temperature produced by the gravity-darkening effect. This is
especially feasible for fast rotators as most of delta Scuti stars
seem to be.
Description:
Characteristics of delta Scuti stars of our sample taking into account
the temperature, surface gravity, and frequency scaling relation and
also the gravity-darkening effect.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 97 2050 Rotation & inclination limits of the sample
table2.dat 52 174 Mean temperature of CoRoT sample
maps/* . 607 Infrared maps for some stars
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See also:
B/corot : CoRoT observation log (N2-4.4) (CoRoT 2016)
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
IV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Name Identifier, KIC for Kepler, TIC for TESS
15- 19 I5 K Teff ? Measured effective temperature (1)
21- 23 I3 K e_Teff ? Error of Teff (1)
25- 29 F5.2 [cm/s2] lofgeff ? Measured surface gravity
31- 33 I3 uHz numax ? Frequency at maximum power
35- 37 I3 uHz e_numax ? Error of frequency at maximum power
39- 42 I4 K <Teff> ? Mean effective temperature
44- 47 I4 K e_<Teff> ? Error of mean effective temperature
49- 52 F4.2 [cm/s2] ? Mean surface gravity
54- 55 A2 --- l_Omin/O-C [>≲ ] Limit flag on rotation rate
56- 58 I3 % Omin/O-C ? Minimum rotation from break-up frequency,
Omega-min/OmegaC
60- 61 A2 --- l_incl [>≲ ] Limit flag on inclination
62- 63 I2 deg incl ? Inclination constraint
65- 90 A26 --- Com Comments (see main text)
92- 95 A4 --- Var Cause of the observed variation of
pulsations over time (2)
97 A1 --- Map [*] * indicates an IR map in
subdirectory maps
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Note (1): From Brown et al. (2011; Cat. J/AJ/142/112) and
Stassun et al. (2019AJ....158..138S 2019AJ....158..138S, Cat. IV/38).
Note (2): Flag as follows:
Cte = Constant
One = Variable (one sidelobe detected)
Sym = Variable (symmetric multiplet)
Asym = Variable (asymmetric multiplet)
Bin = Variable (Binarity)
RMC = Variable (resonant mode coupling)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 9 I9 --- CoRoT CoRoT ID
11- 14 I4 K TeffC Effective temperature from COROTSKY (1)
16- 20 F5.3 mag AV Extinction (2)
22- 26 I5 K TeffV Effective temperature from VOSA (2)
28- 31 I4 K TeffS1 ? Spectroscopic Teff, model 1 (3)
33- 36 I4 K TeffS2 ? Spectroscopic Teff, model 2 (3)
38- 40 I3 uHz numax Frequency at maximum power
42- 44 I3 uHz e_numax Error of frequency at maximum power
46- 49 I4 K <Teff> Mean effective temperature
51- 52 I2 K e_<Teff> Error of mean effective temperature
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Note (1): COROTSKY from Charpinet et al. 2006, in ESA Special Publication,
Vol. 1306, The CoRoT Mission Pre-Launch Status - Stellar Seismology and
Planet Finding, ed. M. Fridlund, A. Baglin, J. Lochard, & L. Conroy, 353.
Note (2): Estimated with VOSA (Bayo et al. 2008, Cat. J/A+A/492/277)
Note (3): Temperatures from Sarro et al. 2013, Cat. J/A+A/550/A120
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Acknowledgements:
Sebastia Barcelo Forteza, sbarcelo(at)cab.inta-csic.es
(End) Sebastia Barcelo Forteza [Spain], Patricia Vannier [CDS] 06-May-2020