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تسجيل مستخدم جديدStaying star gamma Equ
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We determined rotational period of practically nonrotating Ap star gamma Equ and claim $P_{rm rot}= 97$ years. This period is about 35000 times larger than the average rotational period among stars of the same spectral class. Paper discusses possible mechanism explaining the origin of this phenomenon.
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In this paper we study periodic variability of the magnetic field in the Ap star 33 Lib. We found that its most probable period equals 83.5 years. There exist also possible shorter periods: 11.036 days, 7.649 days and 4.690 days. Analysis of the magn
etic behavior of 33 Lib allows us to conclude, that the star shows the second longest period the slow rotator gamma Equ, the latter star with the period of 97 years.
Aims. Despite photometry and spectroscopy of its oscillations obtained over the past 25 years, the pulsation frequency spectrum of the rapidly oscillating Ap (roAp) star gamma Equ has remained poorly understood. Better time-series photometry, combine
d with recent advances to incorporate interior magnetic field geometry into pulsational models, enable us to perform improved asteroseismology of this roAp star. Methods. We obtained 19 days of continuous high-precision photometry of gamma Equ with the MOST (Microvariability & Oscillations of STars) satellite. The data were reduced with two different reduction techniques and significant frequencies were identified. Those frequencies were fitted by interpolating a grid of pulsation models that include dipole magnetic fields of various polar strengths. Results. We identify 7 frequencies in gamma Equ that we associate with 5 high-overtone p-modes and 1st and 2nd harmonics of the dominant p-mode. One of the modes and both harmonics are new discoveries for this star. Our best model solution (1.8 M_sun, log T_eff ~ 3.882; polar field strength ~8.1 kG) leads to unique mode identifications for these frequencies (ell = 0, 1, 2 and 4). This is the first purely asteroseismic fit to a grid of magnetic models. We measure amplitude and phase modulation of the primary frequency due to beating with a closely spaced frequency which had never been resolved. This casts doubts on theories that such modulation - unrelated to the rotation of the star - is due to a stochastic excitation mechanism.
We investigated magnetic variability of the roAp star gamma Equ (HD 201601) with high time resolution. Measurements of the stellar longitudinal magnetic field B_e were performed with the hydrogen line polarimeter and the 6-m optical telescope of Spec
ial Astrophysical Observatory on 20/21 August 1989. We obtained a single 3-hour series of 1720 rapid B_e measurements for this star with the average time resolution of 6.6 sec. The averaged value of <B_e> on this night equals -750 pm 22 G. Both the power spectrum and the amplitude spectrum of the B_e time series essentially are flat. However, they show the presence of a marginally significant magnetic period at P_B = 3.596 min. which is real with the probability 67 %. The amplitude of the magnetic field variations with this period equals 347 pm 31 G. We did not detect variations of B_e field in gamma Equ with the well-known photometric period, P_phot=12.44 min.
$gamma$ Doradus is the prototype star for the eponymous class of pulsating stars that consists of late A-early F main-sequence stars oscillating in low-frequency gravito-inertial modes. Being among the brightest stars of its kind (V = 4.2), $gamma$ D
or benefits from a large set of observational data that has been recently completed by high-quality space photometry from the TESS mission. With these new data, we propose to study $gamma$ Dor as an example of possibilities offered by synergies between multi-technical ground and space-based observations. Here, we present the preliminary results of our investigations.
Physical processes working in the stellar interiors as well as the evolution of stars depend on some fundamental stellar properties, such as mass, radius, luminosity, and chemical abundances. A classical way to test stellar interior models is to comp
are the predicted and observed location of a star on theoretical evolutionary tracks in a H-R diagram. This requires the best possible determinations of stellar mass, radius, luminosity and abundances. To derive its fundamental parameters, we observed the well-known rapidly oscillating Ap star, $gamma$ Equ, using the visible spectro-interferometer VEGA installed on the optical CHARA array. We computed the calibrated squared visibility and derived the limb-darkened diameter. We used the whole energy flux distribution, the parallax and this angular diameter to determine the luminosity and the effective temperature of the star. We obtained a limb-darkened angular diameter of 0.564~$pm$~0.017~mas and deduced a radius of $R$~=~2.20~$pm$~0.12~${rm R_{odot}}$. Without considering the multiple nature of the system, we derived a bolometric flux of $(3.12pm 0.21)times 10^{-7}$ erg~cm$^{-2}$~s$^{-1}$ and an effective temperature of 7364~$pm$~235~K, which is below the effective temperature that has been previously determined. Under the same conditions we found a luminosity of $L$~=~12.8~$pm$~1.4~${rm L_{odot}}$. When the contribution of the closest companion to the bolometric flux is considered, we found that the effective temperature and luminosity of the primary star can be, respectively, up to $sim$~100~K and up to $sim$~0.8~L$_odot$ smaller than the values mentioned above.These new values of the radius and effective temperature should bring further constraints on the asteroseismic modelling of the star.
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