The MOST Asteroseismology Mission: Ultraprecise Photometry from Space
The MOST Asteroseismology Mission: Ultraprecise Photometry from Space
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DOI：
10.1086/377358
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发表时间：
2003-07
影响因子：
3.5
通讯作者：
G. Walker;J. Matthews;R. Kuschnig;R. Johnson;S. Rucinski;J. Pazder;G. Burley;A. Walker;K. Skaret;R. Zee;S. Grocott;K. Carroll;P. Sinclair;D. Sturgeon;J. Harron
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文献类型：
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作者：
G. Walker;J. Matthews;R. Kuschnig;R. Johnson;S. Rucinski;J. Pazder;G. Burley;A. Walker;K. Skaret;R. Zee;S. Grocott;K. Carroll;P. Sinclair;D. Sturgeon;J. Harron
恒星微变和振荡（MOST）使命任务是一颗低成本微型卫星，旨在以微量级的精度探测太阳型恒星和贫金属亚矮星中的低度声振荡（以分钟为周期）。还有计划探测从巨大的，短周期的太阳系外行星反射的光，以及roAp恒星的振荡和Wolf-Rayet恒星密集风中的湍流变化。本文介绍了实验，以及我们如何满足超精密光度的挑战，尽管严重的质量，体积和功率的仪器。一个侧视的150 mm口径Rumak-Maksutov望远镜为两个帧传输CCD供电，一个用于跟踪，另一个用于科学。有一个单一的300 nm宽的过滤器，中心在525 nm。微透镜将较亮（V≤10）的目标恒星的法布里图像投射到科学CCD上。较暗的目标星将直接聚焦在CCD的其他地方。MOST于2003年6月30日发射到低地球，太阳同步，极地轨道，允许在-19 °和+36°之间的恒星连续观察长达60天。姿态由反作用轮和磁力矩器控制。望远镜对角线上的太阳能安全快门是唯一的其他活动部件。将使用累积测光来校准目标视场光阑的响应，数据将被压缩并下载到三个专用地面站。
The Microvariablity and Oscillations of Stars (MOST) mission is a low‐cost microsatellite designed to detect low‐degree acoustic oscillations (periods of minutes) with micromagnitude precision in solar‐type stars and metal‐poor subdwarfs. There are also plans to detect light reflected from giant, short‐period, extrasolar planets and the oscillations of roAp stars and the turbulent variability in the dense winds of Wolf‐Rayet stars. This paper describes the experiment and how we met the challenge of ultraprecise photometry despite severe constraints on the mass, volume, and power available for the instrument. A side‐viewing, 150 mm aperture Rumak‐Maksutov telescope feeds two frame‐transfer CCDs, one for tracking and the other for science. There is a single 300 nm wide filter centered at 525 nm. Microlenses project Fabry images of the brighter (V≤10) target stars onto the science CCD. Fainter target stars will be focused directly elsewhere on the CCD. MOST was launched on 2003 June 30 into a low‐Earth, Sun‐synchronous, polar orbit allowing stars between −19° and +36° declination to be viewed continuously for up to 60 days. Attitude is controlled by reaction wheels and magnetotorquers. A solar safety shutter over the telescope diagonal is the only other moving part. Accumulated photometry will be used to calibrate response across the target field stop, and data will be compressed and downloaded to three dedicated ground stations.