J/MNRAS/471/2491 delta Scuti stars seismic and physical observables (Moya+ 2017)
Semi-empirical seismic relations of A-F stars from COROT and Kepler legacy data.
Moya A., Suarez J.C., Garcia Hernandez A., Mendoza M.A.
<Mon. Not. R. Astron. Soc., 471, 2491-2497 (2017)>
=2017MNRAS.471.2491M 2017MNRAS.471.2491M (SIMBAD/NED BibCode)
ADC_Keywords: Asteroseismology ; Stars, variable
Keywords: asteroseismology - methods: data analysis - stars: evolution -
stars: fundamental parameters - stars: statistics -
stars: variables: delta Scuti
Abstract:
Asteroseismology is witnessing a revolution, thanks to high-precise
asteroseismic space data (MOST, COROT, Kepler, BRITE) and their large
ground-based follow-up programs. Those instruments have provided an
unprecedented large amount of information, which allows us to
scrutinize its statistical properties in the quest for hidden
relations among pulsational and/or physical observables. This approach
might be particularly useful for stars whose pulsation content is
difficult to interpret. This is the case of intermediate-mass
classical pulsating stars (i.e. γ Dor, δ Scuti, hybrids)
for which current theories do not properly predict the observed
oscillation spectra. Here, we establish a first step in finding such
hidden relations from data mining techniques for these stars. We
searched for those hidden relations in a sample of δ Scuti and
hybrid stars observed by COROT and Kepler (74 and 153, respectively).
No significant correlations between pairs of observables were found.
However, two statistically significant correlations emerged from
multivariable correlations in the observed seismic data, which
describe the total number of observed frequencies and the largest one,
respectively. Moreover, three different sets of stars were found to
cluster according to their frequency density distribution. Such sets
are in apparent agreement with the asteroseismic properties commonly
accepted for A-F pulsating stars.
Description:
The COROT sample is composed of 90 δ Scuti stars observed on the
EXO field during the LRa01 run, i.e. the first long run in the
direction of the galactic anticentre, with a time span of 131d and a
sampling time of 8min.
The Kepler sample contains 153 stars, classified as δ Scuti or
hybrids following a comprehensive analysis of both their fundamental
parameters and their pulsational content (see details in Uytterhoeven
et al., 2011, Cat. J/A+A/534/A125)
For the complete sample we extracted the following asteroseismic
observables defined as: minimum frequency (νmin), maximum frequency
(νmax), frequency of the mode with the largest amplitude
(νmax,a), frequency range (D=νmax-νmin), number of
observed frequencies (Nfreq), maximum amplitude (Amax), frequency with
the largest density of modes (νmax,d) and the large separation
({DELTA}ν).
In addition to those seismic observables, we included the effective
temperature (Teff), surface gravity (g), apparent magnitude at filter
'B' (mB) and two non-compound observables: the convective
efficiency of the outer convection zone and the energy of the
pulsation mode, defined as ε=(Teff3xlog(g))-2/3 and
E=[Axνmax,a]2 (see details in Uytterhoeven et al. 2011, Cat.
J/A+A/534/A125).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 97 227 Seismic and physical observables of the stars used
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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)
J/A+A/534/A125 : Variability of A- & F-stars from Kepler (Uytterhoeven+, 2011)
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 15 A15 --- Star Star name
17- 21 F5.2 d-1 numin Minimum frequency
23- 27 F5.2 d-1 numax Maximum frequency
29- 33 F5.2 d-1 D Frequency range (D=numax-numin)
35- 39 F5.2 d-1 numaxa Frequency of the mode with the largest amplitude
41- 43 I3 --- Nfreq Number of frequency
45- 49 F5.2 mmag Amax ? Maximum magnitude amplitude
51- 54 F4.2 d-1 Dnu ? Large separation
56- 60 F5.2 d-1 numaxd Frequency with the largest density of modes
62- 69 F8.2 K Teff ? Effective temperature
71- 78 F8.2 m/s2 g ? Surface gravity
80- 84 F5.2 mag Bmag ? B magnitude
86- 92 F7.2 mmag/d E Energy of the pulsation mode
94- 97 F4.2 10-9K-2 Eps ? Convective efficiency of the outer
convection zone
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 24-May-2020