论文标题
使用后续极化微透镜观测值测量恒星大气参数
Measuring the stellar atmosphere parameters using follow-up polarimetry microlensing observations
论文作者
论文摘要
我们对潜在的随访微晶观测进行了分析，以研究远处恒星的恒星气氛。首先，我们使用银河系模型，恒星种群和星际灰尘朝银河凸起产生合成的微透析事件。我们模拟了极化光曲线，并通过非常大的望远镜（VLT）的焦点还原光谱仪（fors2）极化计的仪器规范传递。我们发现，VLT望远镜的准确性使我们可以限制凉爽的RGB恒星的大气。假设Ogle望远镜每年检测到约3000美元的微验证事件，我们希望在四个连续的极化数据点上的四个不同标准，即$1σ$，$2σ$，$2σ$，$3σ$，以及相应地相应地相应地相差，我们预计将近$ 20，〜10，〜8，〜8，$和5美元的极化微光泽事件。我们概括了协方差矩阵公式，并列出了极化法和光度法信息的组合，从而使我们测量了大气的散射光学深度以及红色巨型恒星的恒星包膜的内半径。这两个参数可以确定凉爽的RGB源星和可以形成灰尘的半径的大气的灰尘不透明度。
We present an analysis of the potential follow-up polarimetry microlensing observation to study the stellar atmospheres of the distant stars. First, we produce synthetic microlensing events using the Galactic model, stellar population, and interstellar dust toward the Galactic Bulge. We simulate the polarization microlensing light curves and pass them through the instrument specifications of FOcal Reducer and low dispersion Spectrograph (FORS2) polarimeter at Very Large Telescope (VLT), and then analyze them. We find that the accuracy of the VLT telescope lets us constrain the atmosphere of cool RGB stars. Assuming detection of about $3000$ microlensing events per year by the OGLE telescope, we expect to detect almost $20,~10,~8, $ and $5$ of polarization microlensig events for the four different criteria of being three consecutive polarimetry data points above the baseline with $1σ$, $2σ$, $3σ$, and $4σ$, respectively in the polarimetry light curves. We generalize the covariance matrix formulation and present the combination of polarimetry and photometry information that leads us to measure the scattering optical depth of the atmosphere and the inner radius of the stellar envelope of red giant stars. These two parameters could determine the dust opacity of the atmosphere of cool RGB source stars and the radius where dust can be formed.
