2013A&A...559A..63G


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.03CEST22:57:23

2013A&A...559A..63G - Astronomy and Astrophysics, volume 559A, 63-63 (2013/11-1)

An in-depth study of HD 174966 with CoRoT photometry and HARPS spectroscopy. Large separation as a new observable for δ Scuti stars.

GARCIA HERNANDEZ A., MOYA A., MICHEL E., SUAREZ J.C., PORETTI E., MARTIN-RUIZ S., AMADO P.J., GARRIDO R., RODRIGUEZ E., RAINER M., UYTTERHOEVEN K., RODRIGO C., SOLANO E., RODON J.R., MATHIAS P., ROLLAND A., AUVERGNE M., BAGLIN A., BAUDIN F., CATALA C. and SAMADI R.

Abstract (from CDS):

The aim of this work was to use a multi-approach technique to derive the most accurate values possible of the physical parameters of the δ Sct star HD174966, which was observed with the CoRoT satellite. In addition, we searched for a periodic pattern in the frequency spectra with the goal of using it to determine the mean density of the star. First, we extracted the frequency content from the CoRoT light curve. Then, we derived the physical parameters of HD174966 and carried a mode identification out from the spectroscopic and photometric observations. We used this information to look for the models fulfilling all the conditions and discussed the inaccuracies of the method because of the rotation effects. In a final step, we searched for patterns in the frequency set using a Fourier transform, discussed its origin, and studied the possibility of using the periodicity to obtain information about the physical parameters of the star.A total of 185 peaks were obtained from the Fourier analysis of the CoRoT light curve, all of which were reliable pulsating frequencies. From the spectroscopic observations, 18 oscillation modes were detected and identified, and the inclination angle (62.5°+7.5–17.5) and the rotational velocity of the star (142km/s) were estimated. From the multi-colour photometric observations, only three frequencies were detected that correspond to the main ones in the CoRoT light curve. We looked for periodicities within the 185 frequencies and found a quasiperiodic pattern Δν ∼ 64 µHz. Using the inclination angle, the rotational velocity, and an Echelle diagram (showing a double comb outside the asymptotic regime), we concluded that the periodicity corresponds to a large separation structure. The quasiperiodic pattern allowed us to discriminate models from a grid. As a result, the value of the mean density is achieved with a 6% uncertainty. So, the Δν pattern could be used as a new observable for A-F type stars.

Abstract Copyright:

Journal keyword(s): asteroseismology - stars: oscillations - stars: variables: delta Scuti - stars: interiors - stars: fundamental parameters - stars: rotation

VizieR on-line data: <Available at CDS (J/A+A/559/A63): freqs.dat>

Simbad objects: 8

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Number of rows : 8

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 HD 49434 gD* 06 48 19.0657567870 -01 19 08.128922715   6.015 5.731     F0V+ 83 0
2 HD 50844 dS* 06 54 50.1144837501 -01 04 14.775133434   9.28 9.09     A2II 44 0
3 HD 50870 dS* 06 54 56.7572009816 -03 20 21.929661395   9.17 8.85     F0IV 24 0
4 V* FG Vir dS* 12 14 15.4567370777 -05 42 59.750421714   6.807 6.558     A8/9V 207 0
5 HD 173369 * 18 44 37.3774195900 +07 58 39.417960599   8.20 7.97     A2 8 0
6 HD 174936 dS* 18 52 58.8981062609 +02 49 50.855520043   8.79 8.56     A3IV 28 0
7 HD 174966 dS* 18 53 07.8279297091 +01 45 19.690545825   7.95 7.69     A7III/IV 26 0
8 HD 181414 PM* 19 20 19.4881180741 +04 46 40.401978148 7.310 7.180 7.060     A2V 20 0

    Equat.    Gal    SGal    Ecl

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2020.07.03-22:57:23

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