KEPLER MISSION DESIGN, REALIZED PHOTOMETRIC PERFORMANCE, AND EARLY SCIENCE
KEPLER MISSION DESIGN, REALIZED PHOTOMETRIC PERFORMANCE, AND EARLY SCIENCE
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DOI：
10.1088/2041-8205/713/2/l79
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发表时间：
2010-04-20
影响因子：
7.9
通讯作者：
Wu, Hayley
中科院分区：
文献类型：
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作者：
Koch, David G.;Borucki, William J.;Wu, Hayley
开普勒使命于2009年3月6日发射，其设计目的是利用凌日测光方法在类太阳恒星的宜居带中探测地球大小的行星。从仅仅43天的数据沿着和地面跟踪观测的结果已经确定了五个新的凌日行星，测量了它们的质量，半径和轨道周期。恒星天体物理学的许多方面也受益于大量和各种恒星的独特，精确，扩展和几乎连续的数据集。经典变星和食星的早期结果显示出很大的希望。为了充分理解该方法、过程以及最终的使命结果，我们提出了最终导致用于实现精密测光性能的飞行和地面系统设计的基本原理。作为一个例子，最初的光度测量结果，我们提出的可变性测量，可用于区分矮星红巨星。
The Kepler Mission, launched on 2009 March 6, was designed with the explicit capability to detect Earth-size planets in the habitable zone of solar-like stars using the transit photometry method. Results from just 43 days of data along with ground-based follow-up observations have identified five new transiting planets with measurements of their masses, radii, and orbital periods. Many aspects of stellar astrophysics also benefit from the unique, precise, extended, and nearly continuous data set for a large number and variety of stars. Early results for classical variables and eclipsing stars show great promise. To fully understand the methodology, processes, and eventually the results from the mission, we present the underlying rationale that ultimately led to the flight and ground system designs used to achieve the exquisite photometric performance. As an example of the initial photometric results, we present variability measurements that can be used to distinguish dwarf stars from red giants.