J/MNRAS/462/1577 Basic properties of Kepler and CoRoT targets (Yildiz+, 2016)
Fundamental properties of Kepler and CoRoT targets.
III. Tuning scaling relations using the first adiabatic exponent.
Yildiz M., Celik Orhan Z., Kayhan C.
<Mon. Not. R. Astron. Soc., 462, 1577-1590 (2016)>
=2016MNRAS.462.1577Y 2016MNRAS.462.1577Y (SIMBAD/NED BibCode)
ADC_Keywords: Stars, late-type ; Stars, masses ; Stars, distances
Keywords: stars: evolution - stars: fundamental parameters - stars: interiors -
stars: late-type - stars: oscillations
Abstract:
So-called scaling relations based on oscillation frequencies have the
potential to reveal the mass and radius of solar-like oscillating
stars. In the derivation of these relations, it is assumed that the
first adiabatic exponent at the surface (Γ1s) of such stars is
constant. However, by constructing interior models for the mass range
0.8-1.6M☉, we show that Γ1s is not constant at stellar
surfaces for the effective temperature range with which we deal.
Furthermore, the well-known relation between large separation and mean
density also depends on Γ1s. Such knowledge is the basis for
our aim of modifying the scaling relations. There are significant
differences between masses and radii found from modified and
conventional scaling relations. However, a comparison of predictions
of these relations with the non-asteroseismic observations of Procyon
A reveals that new scaling relations are effective in determining the
mass and radius of stars. In the present study, solar-like oscillation
frequencies of 89 target stars (mostly Kepler and CoRoT) were
analysed. As well as two new reference frequencies (νmin1 and
νmin2) found in the spacing of solar-like oscillation frequencies
of stellar interior models, we also take into account νmin0. In
addition to the frequency of maximum amplitude, these frequencies have
a very strong diagnostic potential in the determination of fundamental
properties. The present study applies the derived relations from the
models to the solar-like oscillating stars, and computes their
effective temperatures using purely asteroseismic methods. There are
in general very close agreements between effective temperatures from
asteroseismic and non-asteroseismic (spectral and photometric)
methods. For the Sun and Procyon A, for example, the agreement is
almost total.
Description:
The basic data of certain Kepler (79 stars) and CoRoT (seven stars)
target stars, compiled from the literature, are listed in Table A1.
Oscillation frequencies of three stars (Procyon A, HD 2151 and HD
146233) were obtained from ground-based observations (Bedding et al.,
2010ApJ...713..935B 2010ApJ...713..935B; Bedding et al., 2007ApJ...663.1315B 2007ApJ...663.1315B and Bazot et
al. 2012, Cat. J/A+A/544/A106, respectively).
These stars are also listed in this table, with data for the Sun for
comparison. For most stars, we provide B-V and V-K colours
(SIMBAD data base) from photometric observations, and surface gravity
[log(g)], effective temperature (TeS) and metallicity ([Fe/H]) from
spectroscopic observations.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 240 90 Basic properties of target stars
refs.dat 68 53 References
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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)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- Star Star name (1)
15- 20 F6.1 uHz numax Frequency of maximum amplitude
22- 27 F6.1 uHz numin0 ?=- Reference frequencies for min0
29- 34 F6.1 uHz numin1 ?=- Reference frequencies for min1
36- 41 F6.1 uHz numin2 ?=- Reference frequencies for min2
43- 47 F5.1 uHz <Dnu> Mean large separation between oscillation
frequencies
49- 52 F4.1 uHz ?=- Mean small separation between oscillation
frequencies
54- 57 I4 K TeS Effective temperature from spectra
(see Section 2)
59- 62 I4 K TeVK ?=- Effective temperature from V-K colour
index (see Section 2)
64- 67 I4 K TeBV ?=- Effective temperature from B-V colour
index (see Section 2)
69- 72 I4 K Tesis0 ?=- Effective temperature from minima min0
(see Section 3)
74- 77 I4 K Tesis1 ?=- Effective temperature from minima min1
(see Section 3)
79- 82 I4 K Tesis2 ?=- Effective temperature from minima min2
(see Section 3)
85- 88 F4.2 Msun Msca Mass from the new scaling relations
(see Section 3)
90- 93 F4.2 Msun M1sca Mass from the conventional scaling relations
(see Section 3)
95- 98 F4.2 Msun Mlit ? Mass from the literature (see Section 3)
99-103 F5.2 Rsun Rsca Radius from the new scaling relations
(see Section 3)
104-108 F5.2 Rsun R1sca Radius from the conventional scaling
relations (see Section 3)
109-113 F5.2 Rsun Rlit ?=- Radius from the literature
(see Section 3)
115-118 F4.2 [cm/s2] loggsca Surface gravity from the new scaling
relations (see Section 3)
120-123 F4.2 [cm/s2] logg1sca Surface gravity from the conventional scaling
relations (see Section 3)
125-128 F4.2 [cm/s2] loggspc ?=- Surface gravity from spectra
130-146 A17 --- Ref References
148-152 F5.1 uHz e_numax rms uncertainty on numax
154-157 F4.1 uHz e_numin0 ?=- rms uncertainty on numin0
159-162 F4.1 uHz e_numin1 ?=- rms uncertainty on numin1
164-167 F4.1 uHz e_numin2 ?=- rms uncertainty on numin2
169-171 F3.1 uHz e_<Dnu> rms uncertainty on <Dnu>
173-175 I3 K e_TeS rms uncertainty on TeS
177-179 I3 K e_TeVK ?=- rms uncertainty on TeVK
181-183 I3 K e_TeBV ?=- rms uncertainty on TeBV
185-187 I3 K e_Tesis0 ?=- rms uncertainty on Tesis0
189-191 I3 K e_Tesis1 ?=- rms uncertainty on Tesis1
193-195 I3 K e_Tesis2 ?=- rms uncertainty on Tesis2
197-200 F4.2 Msun e_Msca rms uncertainty on Msca
202-205 F4.2 Msun e_M1sca rms uncertainty on M1sca
207-210 F4.2 Msun e_Mlit ?=- rms uncertainty on Mlit
212-215 F4.2 Rsun e_Rsca rms uncertainty on Rsca
217-220 F4.2 Rsun e_R1sca rms uncertainty on R1sca
222-225 F4.2 Rsun e_Rlit ? rms uncertainty on Rlit
227-230 F4.2 [cm/s2] e_loggsca rms uncertainty on loggsca
232-235 F4.2 [cm/s2] e_logg1sca rms uncertainty on logg1sca
237-240 F4.2 [cm/s2] e_loggspc ?=- rms uncertainty on loggspc
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Note (1): Unlike the other stars, for Procyon A, the mass and radius are the
observed values, not the model values in the literature.
Since TeS, TeVK and TeBV of KIC 11771760 are not available, we use Tsis0 in
the scaling relations.
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ref Reference number
4- 22 A19 --- BibCode BibCode
24- 47 A24 --- Aut Author's name
48- 68 A21 --- Com Comments
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History:
From electronic version of the journal
References:
Yildiz et al., Paper I 2014MNRAS.441.2148Y 2014MNRAS.441.2148Y
Yildiz et al., Paper II 2015MNRAS.448.3689Y 2015MNRAS.448.3689Y
(End) Patricia Vannier [CDS] 31-Jan-2018