2008A&A...483..239H


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST21:58:21

2008A&A...483..239H - Astronomy and Astrophysics, volume 483, 239-248 (2008/5-3)

MOST photometry of the roAp star 10 Aquilae.

HUBER D., SAIO H., GRUBERBAUER M., WEISS W.W., ROWE J.F., HARETER M., KALLINGER T., REEGEN P., MATTHEWS J.M., KUSCHNIG R., GUENTHER D.B., MOFFAT A.F.J., RUCINSKI S., SASSELOV D. and WALKER G.A.H.

Abstract (from CDS):

We present 31.2-days of nearly continuous MOST photometry of the rapidly oscillating Ap star 10Aql. The goal was to provide an unambiguous frequency identification for this little studied star, as well as to discuss the detected frequencies in the context of magnetic models and analyze the influence of the magnetic field on the pulsation. Using traditional Fourier analysis techniques on three independent data reductions, intrinsic frequencies for the star are identified. Theoretical non-adiabatic axisymmetric modes influenced by a magnetic field having polar field strengths BP=0-5kG were computed to compare the observations to theory. The high-precision data allow us to identify three definite intrinsic pulsation frequencies and two other candidate frequencies with low S/N. Considering the observed spacings, only one (Δν=50.95µHz) is consistent with the main sequence nature of roAp stars. The comparison with theoretical models yields a best fit for a 1.95M model having solar metallicity, suppressed envelope convection, and homogenous helium abundance. Furthermore, our analysis confirms the suspected slow rotation of the star and sets new lower limits to the rotation period (Prot≥1month) and inclination (i>30±10°). The observed frequency spectrum is not rich enough to unambiguously identify a model. On the other hand, the models hardly represent roAp stars in detail due to the approximations needed to describe the interactions of the magnetic field with stellar structure and pulsation. Consequently, errors in the model frequencies needed for the fitting procedure can only be estimated. Nevertheless, it is encouraging that models which suppress convection and include solar metallicity, in agreement with current concepts of roAp stars, fit the observations best.

Abstract Copyright:

Journal keyword(s): techniques: photometric - stars: chemically peculiar - stars: individual: 10 Aql - stars: individual: HD176232 - stars: magnetic fields - stars: oscillations

Simbad objects: 5

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Number of rows : 5

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 V* DO Eri a2* 03 55 16.1314636284 -12 05 56.729555672 6.35 6.32 6.00     A9VpSrEuCr 374 0
2 HD 83368 a2* 09 36 25.40686 -48 45 04.2549   6.480 6.232     A8VSrCrEu+F9V 256 0
3 HD 175922 * 18 57 12.5434811783 +13 22 20.990201933   7.54 7.21     Am 24 0
4 * 10 Aql a2* 18 58 46.9239770705 +13 54 23.944546333 6.23 6.14 5.89     A7VpSrEu_Ksn 268 0
5 * gam Equ a2* 21 10 20.5001160337 +10 07 53.682085548 5.03 4.94 4.68 4.43 4.32 A9VpSrCrEu 513 0

    Equat.    Gal    SGal    Ecl

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2020.07.04-21:58:21

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