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Rotation period (astronomy)

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Animated rotation of asteroid 433 Eros

In astronomy, the rotation period of a celestial object (e.g., a star, gas giant, planet, moon, asteroid, etc.) is the time that the object takes to complete a single revolution around its axis of rotation relative to the background stars. It differs from the object's solar day, which may include an extra fractional rotation needed to accommodate the portion of the object's orbital period during one day.

Measuring rotation

For solid objects, such as rocky planets and asteroids, the rotation period is a single value. For gaseous/fluid bodies, such as stars and gas giants, the period of rotation varies from the object's equator to its pole due to a phenomenon called differential rotation. Typically, the stated rotation period for a gas giant (such as Jupiter, Saturn, Uranus, Neptune) is its internal rotation period, as determined from the rotation of the planet's magnetic field. For objects that are not spherically symmetrical, the rotation period is, in general, not fixed, even in the absence of gravitational or tidal forces. This is because, although the rotation axis is fixed in space (by the conservation of angular momentum), it is not necessarily fixed in the body of the object itself.[citation needed] As a result of this, the moment of inertia of the object around the rotation axis can vary, and hence the rate of rotation can vary (because the product of the moment of inertia and the rate of rotation is equal to the angular momentum, which is fixed). For example, Hyperion, a satellite of Saturn, exhibits this behaviour, and its rotation period is described as chaotic.

Earth

Main article: Earth's rotation § Periods
See also: Day § Astronomy

Earth's rotation period relative to the Sun (its mean solar day) consists of 86,400 seconds of mean solar time, by definition. Each of these seconds is slightly longer than an SI second because Earth's solar day is now slightly longer than it was during the 19th century, due to tidal deceleration. The mean solar second between 1750 and 1892 was chosen in 1895 by Simon Newcomb as the independent unit of time in his Tables of the Sun. These tables were used to calculate the world's ephemerides between 1900 and 1983, so this second became known as the ephemeris second. The SI second was made equal to the ephemeris second in 1967.[1]

Earth's rotation period relative to the fixed stars, called its stellar day by the International Earth Rotation and Reference Systems Service (IERS), is 86164.098 903 691 seconds of mean solar time (UT1) (23h 56m 4.098 903 691s).[2][3] Earth's rotation period relative to the precessing or moving mean vernal equinox, its sidereal day, is 86164.090 530 832 88 seconds of mean solar time (UT1) (23h 56m 4.090 530 832 88s).[2] Thus the sidereal day is shorter than the stellar day by about 8.4 ms.[4] The length of the mean solar day in SI seconds is available from the IERS for the periods 1623–2005[5] and 1962–2005.[6] Recently (1999–2005) the average annual length of the mean solar day in excess of 86400 SI seconds has varied between 0.3 ms and 1 ms, which must be added to both the stellar and sidereal days given in mean solar time above to obtain their lengths in SI seconds.

Rotation period of selected objects

Celestial objects Rotation period with respect to distant stars (compared to Earth days) Apparent rotational period
viewed from Earth
Sun 25.379995 days (Carrington rotation)
35 days (high latitude)		 25ᵈ 9ʰ 7ᵐ 11.6ˢ
35ᵈ		 ~28 days at its equator[7]
Mercury 58.6462 days[8] 58ᵈ 15ʰ 30ᵐ 30ˢ
Venus -243.0187 days[8][10] −243ᵈ 0ʰ 26ᵐ
Earth 0.99726968 days[8][11] 0ᵈ 23ʰ 56ᵐ 4.0910ˢ
Moon 27.321661 days[12] (synchronous toward Earth) 27ᵈ 7ʰ 43ᵐ 11.5ˢ
Mars 1.02595675 days[8] 1ᵈ 0ʰ 37ᵐ 22.663ˢ
Ceres 0.37809 days[13] 0ᵈ 9ʰ 4ᵐ 27.0ˢ
Jupiter 0.4135344 days (deep interior)[14]
0.41007 days (equatorial)
0.41369942 days (high latitude)		 0ᵈ 9ʰ 55ᵐ 29.37s[8]
0ᵈ 9ʰ 50ᵐ 30ˢ[8]
0ᵈ 9ʰ 55ᵐ 43.63ˢ[8]
Saturn 0.44403 days (deep interior)[14]
0.426 days (equatorial)
0.443 days (high latitude)		 0ᵈ 10ʰ 39ᵐ 24ˢ[8]
0ᵈ 10ʰ 14ᵐ[8]
0ᵈ 10ʰ 38ᵐ[8]
Uranus −0.71833 days[8][10] −0ᵈ 17ʰ 14ᵐ 24ˢ
Neptune 0.67125 days[8] 0ᵈ 16ʰ 6ᵐ 36ˢ
Pluto −6.38718 days[8][10] (synchronous with Charon) –6ᵈ 9ʰ 17ᵐ 32ˢ
Haumea 0.163145 days[15] 0ᵈ 3ʰ 54ᵐ 56ˢ

See also

References

  1. ^ "Leap Seconds". United States Naval Observatory.
  2. ^ a b "Useful Constants". Earth Orientation Parameters. International Earth Rotation and Reference Systems Service.
  3. ^ 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 & Astrophysics 105 (1982) 359–361.
  4. ^ Explanatory Supplement to the Astronomical Almanac, ed. P. Kenneth Seidelmann, Mill Valley, Cal., United States Naval Observatory University Science Books, 1992, p.48, ISBN 0-935702-68-7.
  5. ^ "Excess of the duration of the day to 86400s … since 1623". Earth Orientation Parameters. International Earth Rotation and Reference Systems Service. Archived from the original on 2008-10-03. Graph at end.
  6. ^ "Variations in the duration of the day 1962–2005". Earth Orientation Parameters. International Earth Rotation and Reference Systems Service. Archived from the original on 2007-08-13.
  7. ^ Phillips, Kenneth J. H. (1995). Guide to the Sun. Cambridge University Press. pp. 78–79. ISBN 978-0-521-39788-9.
  8. ^ a b c d e f g h i j k l m Allen, Clabon Walter; Cox, Arthur N. (2000). Allen's Astrophysical Quantities. Springer. p. 296. ISBN 0-387-98746-0. {{cite book}}: Unknown parameter |last-author-amp= ignored (|name-list-style= suggested) (help)
  9. ^ Archinal, Brent A.; et al. ( ) (2010). "Report of the IAU Working Group on Cartographic Coordinates and Rotational Elements: 2009" (PDF). Celestial Mechanics and Dynamical Astronomy. 109 (2): 101–135. Bibcode:2011CeMDA.109..101A. doi:10.1007/s10569-010-9320-4.{{cite journal}}: CS1 maint: extra punctuation (link)
  10. ^ a b c This rotation is negative because the pole which points north of the invariable plane rotates in the opposite direction to most other planets.[9]
  11. ^ 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.
  12. ^ Allen, Clabon Walter; Cox, Arthur N. (2000). Allen's Astrophysical Quantities. Springer. p. 308. ISBN 0-387-98746-0. {{cite book}}: Unknown parameter |last-author-amp= ignored (|name-list-style= suggested) (help)
  13. ^ Chamberlain, Matthew A.; Sykes, Mark V.; Esquerdo, Gilbert A. (2007). "Ceres lightcurve analysis – Period determination". Icarus. 188 (2): 451–456. Bibcode:2007Icar..188..451C. doi:10.1016/j.icarus.2006.11.025.
  14. ^ a b Rotation period of the deep interior is that of the planet's magnetic field.
  15. ^ Lacerda, Pedro; Jewitt, David; Peixinho, Nuno (2008-04-02). "High-Precision Photometry of Extreme KBO 2003 EL61". The Astronomical Journal. 135 (5): 1,749–1,756. arXiv:0801.4124. Bibcode:2008AJ....135.1749L. doi:10.1088/0004-6256/135/5/1749. Retrieved 2008-09-22. {{cite journal}}: Unknown parameter |last-author-amp= ignored (|name-list-style= suggested) (help)
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