凌日时间变分法

动画显示系统内行星-1和行星-2在凌日时间上的差异。创建者：NASA/克卜勒任务。

凌日时间变分法是通过观察凌日时间变化以检测系外行星的一种方法。这提供了一种极其灵敏，可以用来检测地球大小系外行星的方法^[1]^[2]^[3]。"时间变异"需要精确的测量凌发生的时刻，才可以可测量出周期的改变。

第一颗以凌日时间变异检测出的非凌日行星是由NASA的克卜勒任务卫星完成的。凌日的克卜勒-19b显示在300天的周期中有著5分钟的振幅变异，显示有另一颗行星克卜勒-19c存在著，它的合理周期可能接近这颗凌日行星的数倍^[4]^[5]。

在2010年，研究人员依据凌日时间变分法建议WASP-3也有第二颗的行星存在^[6]^[7]，但是在2012年这项建议被否定了^[8]。

凌日时间变分法的技术在2012年被用来发现克卜勒-9d，并被普遍的用于验证系外行星的发现^[9]。

参考资料[编辑]

^ Miralda-Escude. Orbital perturbations on transiting planets: A possible method to measure stellar quadrupoles and to detect Earth-mass planets. The Astrophysical Journal. 2001, 564 (2): 1019. Bibcode:2002ApJ...564.1019M. arXiv:astro-ph/0104034 . doi:10.1086/324279.
^ Holman; Murray. The Use of Transit Timing to Detect Extrasolar Planets with Masses as Small as Earth. Science :-,2005. 2004, 307 (1291). arXiv:astro-ph/0412028 . doi:10.1106/science.1107822.
^ Agol; Sari; Steffen; Clarkson. On detecting terrestrial planets with timing of giant planet transits. Monthly Notices of the Royal Astronomical Society. 2004, 359 (2): 567–579. Bibcode:2005MNRAS.359..567A. arXiv:astro-ph/0412032 . doi:10.1111/j.1365-2966.2005.08922.x.
^ Invisible World Discovered （页面存档备份，存于互联网档案馆）, NASA Kepler News, 8 September 2011
^ Ballard; et. al.; Francois Fressin; David Charbonneau; Jean-Michel Desert; Guillermo Torres; Geoffrey Marcy; Burke; Howard Isaacson. The Kepler-19 System: A Transiting 2.2 R_Earth Planet and a Second Planet Detected via Transit Timing Variations. 2011. arXiv:1109.1561  [astro-ph.EP].
^ Planet found tugging on transits （页面存档备份，存于互联网档案馆）, Astronomy Now, 9 July 2010
^ G.Maciejewski, D.Dimitrov, R.Neuhaeuser, A.Niedzielski, St.Raetz, Ch.Ginski, Ch.Adam, C.Marka, M.Moualla, M.Mugrauer. Transit timing variation in exoplanet WASP-3b. 2010. arXiv:1006.1348v1  [astro-ph.EP].
^ M Montalto; et al. A new analysis of the WASP-3 system: no evidence for an additional companion. MNRAS. Nov 2, 2012. arXiv:1211.0218 .
^ The Transit Timing Variation (TTV) Planet-finding Technique Begins to Flower. [2013-01-12]. （原始内容存档于2017-03-30）.

外部链接[编辑]

TTV papers

[1] Miralda-Escude. Orbital perturbations on transiting planets: A possible method to measure stellar quadrupoles and to detect Earth-mass planets. The Astrophysical Journal. 2001, 564 (2): 1019. Bibcode:2002ApJ...564.1019M. arXiv:astro-ph/0104034 . doi:10.1086/324279.

[2] Holman; Murray. The Use of Transit Timing to Detect Extrasolar Planets with Masses as Small as Earth. Science :-,2005. 2004, 307 (1291). arXiv:astro-ph/0412028 . doi:10.1106/science.1107822.

[3] Agol; Sari; Steffen; Clarkson. On detecting terrestrial planets with timing of giant planet transits. Monthly Notices of the Royal Astronomical Society. 2004, 359 (2): 567–579. Bibcode:2005MNRAS.359..567A. arXiv:astro-ph/0412032 . doi:10.1111/j.1365-2966.2005.08922.x.

[4] Invisible World Discovered （页面存档备份，存于互联网档案馆）, NASA Kepler News, 8 September 2011

[5] Ballard; et. al.; Francois Fressin; David Charbonneau; Jean-Michel Desert; Guillermo Torres; Geoffrey Marcy; Burke; Howard Isaacson. The Kepler-19 System: A Transiting 2.2 R_Earth Planet and a Second Planet Detected via Transit Timing Variations. 2011. arXiv:1109.1561  [astro-ph.EP].

[6] Planet found tugging on transits （页面存档备份，存于互联网档案馆）, Astronomy Now, 9 July 2010

[7] G.Maciejewski, D.Dimitrov, R.Neuhaeuser, A.Niedzielski, St.Raetz, Ch.Ginski, Ch.Adam, C.Marka, M.Moualla, M.Mugrauer. Transit timing variation in exoplanet WASP-3b. 2010. arXiv:1006.1348v1  [astro-ph.EP].

[Montalto-8] M Montalto; et al. A new analysis of the WASP-3 system: no evidence for an additional companion. MNRAS. Nov 2, 2012. arXiv:1211.0218 .

[9] The Transit Timing Variation (TTV) Planet-finding Technique Begins to Flower. [2013-01-12]. （原始内容存档于2017-03-30）.

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