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0.41369942 日 (極)0日 9時間 55分 29.37秒[6]
0日 9時間 50分 30秒[6]
0日 9時間 55分 43.63秒[6]
土星0.44403 日 (内部)[11]
0.426 日 (赤道)
0.443 日 (極)0日 10時間 39分 24秒[6]
0日 10時間 14分[6]
0日 10時間 38分[6]
天王星?0.71833 日[6][7][11]?0日 17時間 14分 24秒
海王星0.67125 日[6][11]0日 16時間 6分 36秒
冥王星?6.38718 日[6][7]?6日 9時間 17分 32秒
ハウメア0.163145 日[12]0日 3時間 54分 56秒
関連項目
順行・逆行
脚注^ ⇒Leap seconds by USNO
^ a b ⇒IERS EOP Useful constants
^ Aoki, the ultimate source of these figures, uses the term "seconds of UT1" instead of "seconds of mean solar time". Aoki, et al., "The new definition of Universal Time", Astronomy and Astrophysics 105 (1982) 359?361.
^ Explanatory Supplement to the Astronomical Almanac, ed. P. Kenneth Seidelmann, Mill Valley, Cal., University Science Books, 1992, p.48, ISBN 0-935702-68-7.
^ Rotation and pole position for the Sun and planets Rotation period in days is 360° divided by the coefficient of d.
^ a b c d e f g h i j k l m Clabon Walter Allen and Arthur N. Cox (2000). Allen's Astrophysical Quantities. Springer. pp. 296. .mw-parser-output cite.citation{font-style:inherit;word-wrap:break-word}.mw-parser-output .citation q{quotes:"\"""\"""'""'"}.mw-parser-output .citation.cs-ja1 q,.mw-parser-output .citation.cs-ja2 q{quotes:"「""」""『""』"}.mw-parser-output .citation:target{background-color:rgba(0,127,255,0.133)}.mw-parser-output .id-lock-free a,.mw-parser-output .citation .cs1-lock-free a{background:url("//upload.wikimedia.org/wikipedia/commons/6/65/Lock-green.svg")right 0.1em center/9px no-repeat}.mw-parser-output .id-lock-limited a,.mw-parser-output .id-lock-registration a,.mw-parser-output .citation .cs1-lock-limited a,.mw-parser-output .citation .cs1-lock-registration a{background:url("//upload.wikimedia.org/wikipedia/commons/d/d6/Lock-gray-alt-2.svg")right 0.1em center/9px no-repeat}.mw-parser-output .id-lock-subscription a,.mw-parser-output .citation .cs1-lock-subscription a{background:url("//upload.wikimedia.org/wikipedia/commons/a/aa/Lock-red-alt-2.svg")right 0.1em center/9px no-repeat}.mw-parser-output .cs1-ws-icon a{background:url("//upload.wikimedia.org/wikipedia/commons/4/4c/Wikisource-logo.svg")right 0.1em center/12px no-repeat}.mw-parser-output .cs1-code{color:inherit;background:inherit;border:none;padding:inherit}.mw-parser-output .cs1-hidden-error{display:none;color:#d33}.mw-parser-output .cs1-visible-error{color:#d33}.mw-parser-output .cs1-maint{display:none;color:#3a3;margin-left:0.3em}.mw-parser-output .cs1-format{font-size:95%}.mw-parser-output .cs1-kern-left{padding-left:0.2em}.mw-parser-output .cs1-kern-right{padding-right:0.2em}.mw-parser-output .citation .mw-selflink{font-weight:inherit}ISBN 0387987460
^ a b c This rotation is negative because the pole which points north of the ecliptic rotates in the opposite direction to most other planets.
^ Reference adds about 1 ms to Earth's stellar day given in mean solar time to account for the length of Earth's mean solar day in excess of 86400 SI seconds.
^ Clabon Walter Allen and Arthur N. Cox (2000). Allen's Astrophysical Quantities. Springer. pp. 308. ISBN 0387987460
^ Chamberlain, Matthew A.; Sykes, Mark V.; Esquerdo, Gilbert A. (2007). “Ceres lightcurve analysis ? Period determination”. Icarus 188: 451–456. doi:10.1016/j.icarus.2006.11.025. https://ui.adsabs.harvard.edu/abs/2007Icar..188..451C/abstract.
^ a b c d Rotation period of the deep interior is that of the planet's magnetic field.
^ Pedro Lacerda, David Jewitt and Nuno Peixinho (2008-04-02). ⇒“High-Precision Photometry of Extreme KBO 2003 EL61”. The Astronomical Journal 135: 1749?1756. doi:10.1088/0004-6256/135/5/1749. ⇒http://www.iop.org/EJ/abstract/1538-3881/135/5/1749 2008年9月22日閲覧。
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