J/A+A/650/A115 Seismic global parameters of 2103 KIC (Dreau+, 2021)
Seismic constraints on the internal structure of evolved stars:
From high-luminosity RGB to AGB stars.
Dreau G., Mosser B., Lebreton Y., Gehan C., Kallinger T.
<Astron. Astrophys. 650, A115 (2021)>
=2021A&A...650A.115D 2021A&A...650A.115D (SIMBAD/NED BibCode)
ADC_Keywords: Stars, late-type ; Asteroseismology
Keywords: asteroseismology - stars: evolution - stars: late-type -
stars: interiors - stars: AGB and post-AGB - stars: oscillations
Abstract:
The space-borne missions CoRoT and Kepler opened up a new opportunity
for better understanding stellar evolution by probing stellar
interiors with unrivalled high-precision photometric data. Kepler has
observed stellar oscillation for four years, which gave access to
excellent frequency resolution that enables deciphering the
oscillation spectrum of evolved red giant branch and asymptotic giant
branch stars.
The internal structure of stars in the upper parts of the red and
asymptotic giant branches is poorly constrained, which makes the
distinction between red and asymptotic giants difficult. We perform a
thorough seismic analysis to address the physical conditions inside
these stars and to distinguish them.
We took advantage of what we have learnt from less evolved stars. We
studied the oscillation mode properties of ∼2000 evolved giants in a
model described by the asymptotic pressure-mode pattern of red giants,
which includes the signature of the helium second-ionisation zone.
Mode identification was performed with a maximum cross-correlation
method. Then, the modes were fitted with Lorentzian functions
following a maximum likelihood estimator technique.
We derive a large set of seismic parameters of evolved red and
asymptotic giants. We extracted the mode properties up to the degree
l=3 and investigated their dependence on stellar mass, metallicity,
and evolutionary status. We identify a clear difference in the
signature of the helium second-ionisation zone between red and
asymptotic giants. We also detect a clear shortage of the energy of
l=1 modes after the core-He-burning phase. Furthermore, we note that
the mode damping observed on the asymptotic giant branch is similar to
that observed on the red giant branch.
We highlight that the signature of the helium second-ionisation zone
varies with stellar evolution. This provides us with a physical basis
for distinguishing red giant branch stars from asymptotic giants.
Here, our investigation of stellar oscillations allows us to constrain
the physical processes and the key events that occur during the
advanced stages of stellar evolution, with emphasis on the ascent
along the asymptotic giant branch, including the asymptotic giant
branch bump.
Description:
Global seismic parameters of the stars listed in the paper. Each star
is identified with its KIC number (Kepler Input Catalog).
The stellar mass and the effective temperature are from the APOKASC
catalogue (Pinsonneault et al., 2014ApJS..215...19P 2014ApJS..215...19P, Cat.
J/ApJS/215/19). For some stars, the stellar mass and the effective
temperature are not listed in the APOKASC catalogue. It concerns
roughly 5% of our sample, with half of this fraction being associated
with very low Dnu-values (i.e. Dnu≤0.5uHz). For these stars, we
nevertheless obtained rough estimates of the stellar mass and
effective temperature using semi-empirical and empirical scaling
relations implying both the frequency at the maximum oscillation power
numax and large frequency separation Dnu (Kjeldsen & Bedding,
1995A&A...293...87K 1995A&A...293...87K; Kallinger et al., 2010A&A...509A..77K 2010A&A...509A..77K; Mosser et
al., 2010A&A...517A..22M 2010A&A...517A..22M). The stellar classification is performed
following two methods. The first method relies on the envelope
autocorrelation function denoted eta (Mosser et al.,
2019A&A...622A..76M 2019A&A...622A..76M). A star is classified as red giant when
eta≥0.700 and as helium burning star when eta≤0.700. The second
method relies on the acoustic offset (Kallinger et al.,
2012A&A...541A..51K 2012A&A...541A..51K). The evolutionary status is labelled by the
parameter evo with the following code: 0 - RGB star, 1 - red clump
stars, 2 - secondary clump stars, and 3 - AGB stars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablec1.dat 293 2103 Global seismic parameters of the stars
listed in the paper
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/ApJS/215/19 : APOKASC catalog of Kepler red giants (Pinsonneault+, 2014)
J/A+A/588/A87 : Seismic global parameters of 6111 KIC (Vrard+, 2016)
J/A+A/618/A109 : Seismic global parameters of 372 KIC (Mosser+, 2018)
Byte-by-byte Description of file: tablec1.dat
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Bytes Format Units Label Explanations
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2- 9 I8 --- KIC KIC number
12- 16 F5.3 uHz Dnu Large separation
19- 22 F4.2 Msun M Stellar mass
25- 28 I4 K Teff Effective temperature
30- 35 F6.3 --- eps ?=-9.999 Acoustic offset
37- 42 F6.3 --- e_eps ?=-9.999 Uncertainty in eps
44- 49 F6.3 --- d01 ?=-9.999 Reduced l=1 small separation
51- 56 F6.3 --- e_d01 ?=-9.999 Uncertainty in d01
58- 63 F6.3 --- d02 ?=-9.999 Reduced l=2 small separation
65- 70 F6.3 --- e_d02 ?=-9.999 Uncertainty in d02
72- 77 F6.3 --- d03 ?=-9.999 Reduced l=3 small separation
79- 84 F6.3 --- e_d03 ?=-9.999 Uncertainty in d03
86- 92 F7.4 --- Agl ?=-9.9999 Glitch amplitude
94-100 F7.4 --- e_Agl ?=-9.9999 Uncertainty in Agl
103-107 F5.2 --- Ggl ?=-9.99 Glitch period
110-114 F5.2 --- e_Ggl ?=-9.99 Uncertainty in Ggl
116-120 F5.2 --- Phigl ?=-9.99 Glitch phase
122-126 F5.2 --- e_Phigl ?=-9.99 Uncertainty in Phigl
130-135 F6.3 --- V1 ?=-9.999 Dipole mode visibility
139-144 F6.3 --- e_V1 ?=-9.999 Uncertainty in V1
148-153 F6.3 --- V2 ?=-9.999 Quadrupole mode visibility
157-162 F6.3 --- e_V2 ?=-9.999 Uncertainty in V2
166-171 F6.3 --- V3 ?=-9.999 Octupole mode visibility
175-180 F6.3 --- e_V3 ?=-9.999 Uncertainty in V3
182-187 F6.3 muHz Gamma0 ?=-9.999 Radial mode width
189-194 F6.3 muHz e_Gamma0 ?=-9.999 Uncertainty in Gamma0
196-201 F6.3 muHz Gamma1 ?=-9.999 Dipole mode width
203-208 F6.3 muHz e_Gamma1 ?=-9.999 Uncertainty in Gamma1
210-215 F6.3 muHz Gamma2 ?=-9.999 Quadrupole mode width
217-222 F6.3 muHz e_Gamma2 ?=-9.999 Uncertainty in Gamma2
226-232 F7.1 ppm A0 ?=-9999.9 Radial mode amplitude
236-242 F7.1 ppm e_A0 ?=-9999.9 Uncertainty in A0
246-252 F7.1 ppm A1 ?=-9999.9 Dipole mode amplitude
256-262 F7.1 ppm e_A1 ?=-9999.9 Uncertainty in A1
266-272 F7.1 ppm A2 ?=-9999.9 Quadrupole mode amplitude
276-282 F7.1 ppm e_A2 ?=-9999.9 Uncertainty in A2
284-289 F6.3 --- eta ?=-9.999 Envelope autocorrelation function
291-293 I3 --- evo [0/3]?=-99 Evolutionary status (1)
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Note (1): The evolutionary status as follows:
0 = RGB star
1 = red clump star
2 = secondary clump star
3 = AGB star
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Acknowledgements:
Guillaume Dreau, guillaume.dreau(at)obspm.fr
(End) Patricia Vannier [CDS] 26-Apr-2021