Stellar Oscillations in Planet Hosting K Giant Stars

这个项目将使用精确的恒星径向速度测量来研究拥有K巨星的行星上的恒星振荡。这些将被用来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在20多颗巨星周围被发现。这些发现很重要，因为主恒星的质量在1.1M-2.5Mʘ的范围内，显著高于大多数主恒星的质量。径向速度测量已经发现了大多数已知的太阳系外行星，由于缺乏恒星线和较高的恒星自转速度，不适合在这种恒星质量的主序恒星周围进行行星搜索。然而，巨星的恒星质量很难确定，因为覆盖大质量范围的主序恒星的演化轨迹都汇聚在色等图的巨型分支上。利用我们的研究探测到的脉动模式，我们将得到大样本巨型恒星的精确质量。与合作者合作将使用干涉测量来获得我们计划恒星的准确恒星半径。对计划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，以便在未来可以用来确定拥有巨型恒星的行星的准确质量。

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.