roAp星10 Aql的MOST测光
MOST photometry of the roAp star 10 Aql
摘要：
背景：我们提出了31.2天的近连续MOST测光的roAp星10Aql。目的：目标是为这颗研究较少的恒星提供明确的频率识别，并在磁模型的背景下讨论检测到的频率，分析磁场对脉动的影响。方法：利用传统的傅里叶分析技术，对三个独立的数据进行处理，识别出恒星的固有频率。计算了受极场强度Bp = 0- 5 kG的磁场影响的理论非绝热轴对称模，以将观测结果与理论进行比较。结果：高精度的数据使我们能够识别出三个确定的固有脉动频率和两个低信噪比的其他候选频率。考虑到观测到的间距，只有一个（50.95microHz）符合roAp星的主序星性质。与理论模型的比较产生了一个最适合的1.95 Msun模型具有太阳能金属丰度，抑制信封对流，和均匀的氦丰度。此外，我们的分析证实了怀疑的恒星旋转缓慢，并设定了新的旋转周期（Prot>1个月）和倾角（i>30 \pm 10度）的下限。结论：观察到的频谱不足以明确识别模型。另一方面，由于描述磁场与恒星结构和脉动的相互作用所需的近似，模型很难详细地代表roAp星。因此，只能估计拟合过程所需的模型频率误差。然而，令人鼓舞的是，模型抑制对流，包括太阳金属丰度，与目前的概念的roAp星，最适合的意见。
英文摘要：
Context: We present 31.2 days of nearly continuous MOST photometry of the roAp star 10Aql. Aims: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. Methods: 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. Results: 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 (50.95microHz) is consistent with the main sequence nature of roAp stars. The comparison with theoretical models yields a best fit for a 1.95Msun 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>1 month) and inclination (i>30\pm10deg.). Conclusions: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.
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