Stellar Oscillations in Planet Hosting K Giant Stars

该项目将利用精确的恒星径向速度测量研究K巨星星星所在行星的恒星振荡。这些将用于确定基本的恒星参数，特别是恒星质量。太阳系外的行星已经被发现围绕着20多颗巨星。这些发现是重要的，因为主恒星的质量在1.1 - 2.5 M质量之间，比大多数行星的质量要高。径向速度测量已经发现了大多数已知的太阳系外行星，但由于恒星线的缺乏和恒星自转率高，径向速度测量不适合在这种恒星质量的主序星周围进行行星搜索。但巨星恒星质量的确定是困难的，因为覆盖广泛质量范围的主序星演化轨迹都会聚在色星等图的巨分支上。利用我们的研究检测到的脉动模式，我们将获得大样本巨星的准确质量。与合作者的工作将使用干涉测量，以获得准确的恒星半径为我们的计划恒星。对程序恒星的恒星半径和质量的综合测量最终可以用来校准恒星演化等时线，以便将来可以用来确定拥有巨星的行星的精确质量。

This project will study stellar oscillations in planet hosting K giant star using precise stellar radial velocity measurements. These will be used to determine basic stellar parameters, in particular, the stellar mass. Extrasolar planets have been discovered around over 20 giant stars. These discoveries are important because the host stars have masses in the range of 1.1 - 2.5 Mʘ, signficantty higher than the masses of most planet hosting stars. Radial velocity surveys, which have discovered most of the known extrasolar planets, are ill-suited for planet searches around main sequence stars of this stellar mass because of the paucity of stellar lines and high stellar rotation rates. However, the determination of the stellar mass of giant stars is difficult because the evolutionary tracks of main sequence stars covering a wide range of masses all converge on the giant branch of the color magnitude diagram. Using the pulsation modes detected by our study we will derive accurate masses for a large sample of giant stars. Work with collaborators will use interferometric measurements to get accurate stellar radii for our program stars. The combined measurements of the stellar radii and masses for the program stars can ultimately be used to calibrate stellar evolutionary isochrones so that in future these can be used to determine accurate masses of planet hosting giant stars.