PLATO 2.0 任务
地球与行星天体物理
2015-06-17 v2
摘要
PLATO 2.0 最近被选为 ESA 的 M3 发射机会（2022/24 年）。它以统计数量提供准确的关键行星参数（半径、质量、密度和年龄），旨在解决诸如以下基本问题：行星系统如何形成和演化？是否存在其他拥有类似地球行星（包括潜在宜居行星）的系统？PLATO 2.0 仪器由 34 台小口径望远镜组成（32 台读出周期为 25 秒，2 台为 2.5 秒），提供广阔的视场（2232 平方度）和巨大的测光星等范围（4-16 等）。它专注于宽视场中的亮星（4-11 等），通过测光凌日法探测并表征小至地球大小的行星，其质量随后可通过地基径向速度后续测量确定。将对这些亮星进行星震学观测，以获得高精度的恒星参数，包括质量和年龄。亮目标与星震学的结合使得行星整体参数具有高精度：行星半径、质量和年龄的精度分别达到 2%、4-10% 和 10%。计划的基础观测策略包括两次长期指向（2-3 年），以探测并整体表征延伸至类太阳恒星宜居区（HZ）的行星，以及额外的步进凝视阶段，总共覆盖约 50% 的天空。PLATO 2.0 将观测多达 1,000,000 颗恒星，探测并表征数百颗小型行星，以及数千颗从海王星到气态巨行星 regime 直至宜居区的行星。因此，它将提供首个具有准确半径、质量、平均密度和年龄的整体表征行星的大规模星表。该星表将包含轨道距离适中、表面温度温和的类地行星。以统计数量覆盖此参数范围的整体表征行星是 PLATO 2.0 独有的特点。
引用
@article{arxiv.1310.0696,
title = {The PLATO 2.0 Mission},
author = {H. Rauer and C. Catala and C. Aerts and T. Appourchaux and W. Benz and A. Brandeker and J. Christensen-Dalsgaard and M. Deleuil and L. Gizon and M. -J. Goupil and M. Güdel and E. Janot-Pacheco and M. Mas-Hesse and I. Pagano and G. Piotto and D. Pollacco and N. C. Santos and A. Smith and J. -C. and Suárez and R. Szabó and S. Udry and V. Adibekyan and Y. Alibert and J. -M. Almenara and P. Amaro-Seoane and M. Ammler-von Eiff and M. Asplund and E. Antonello and W. Ball and S. Barnes and F. Baudin and K. Belkacem and M. Bergemann and G. Bihain and A. C. Birch and X. Bonfils and I. Boisse and A. S. Bonomo and F. Borsa and I. M. Brandão and E. Brocato and S. Brun and M. Burleigh and R. Burston and J. Cabrera and S. Cassisi and W. Chaplin and S. Charpinet and C. Chiappini and R. P. Church and Sz. Csizmadia and M. Cunha and M. Damasso and M. B. Davies and H. J. Deeg and R. F. DÍaz and S. Dreizler and C. Dreyer and P. Eggenberger and D. Ehrenreich and P. Eigmüller and A. Erikson and R. Farmer and S. Feltzing and F. de Oliveira Fialho and P. Figueira and T. Forveille and M. Fridlund and R. A. García and P. Giommi and G. Giuffrida and M. Godolt and J. Gomes da Silva and T. Granzer and J. L. Grenfell and A. Grotsch-Noels and E. Günther and C. A. Haswell and A. P. Hatzes and G. Hébrard and S. Hekker and R. Helled and K. Heng and J. M. Jenkins and A. Johansen and M. L. Khodachenko and K. G. Kislyakova and W. Kley and U. Kolb and N. Krivova and F. Kupka and H. Lammer and A. F. Lanza and Y. Lebreton and D. Magrin and P. Marcos-Arenal and P. M. Marrese and J. P. Marques and J. Martins and S. Mathis and S. Mathur and S. Messina and A. Miglio and J. Montalban and M. Montalto and M. J. P. F. G. Monteiro and H. Moradi and E. Moravveji and C. Mordasini and T. Morel and A. Mortier and V. Nascimbeni and R. P. Nelson and M. B. Nielsen and L. Noack and A. J. Norton and A. Ofir and M. Oshagh and R. -M. Ouazzani and P. Pápics and V. C. Parro and P. Petit and B. Plez and E. Poretti and A. Quirrenbach and R. Ragazzoni and G. Raimondo and M. Rainer and D. R. Reese and R. Redmer and S. Reffert and B. Rojas-Ayala and I. W. Roxburgh and S. Salmon and A. Santerne and J. Schneider and J. Schou and S. Schuh and H. Schunker and A. Silva-Valio and R. Silvotti and I. Skillen and I. Snellen and F. Sohl and S. G. Sousa and A. Sozzetti and D. Stello and K. G. Strassmeier and M. Švanda and Gy. M. Szabó and A. Tkachenko and D. Valencia and V. van Grootel and S. D. Vauclair and P. Ventura and F. W. Wagner and N. A. Walton and J. Weingrill and S. C. Werner and P. J. Wheatley and K. Zwintz},
journal= {arXiv preprint arXiv:1310.0696},
year = {2015}
}
备注
63 pages, 17 figures, submitted to Experimental Astronomy (ExA)