A three-dimensional model of 29 Amphitrite based on its light curve.
|Discovered by||A. Marth|
|Discovery date||March 1, 1854|
|Alternative names||A899 NG|
|Minor planet category||Main belt|
|Epoch June 14, 2006 (JD 2453900.5)|
|Aphelion||409.809 Gm (2.739 AU)|
|Perihelion||354.398 Gm (2.369 AU)|
|Semi-major axis||382.103 Gm (2.554 AU)|
|Orbital period||1491.013 d (4.08 a)|
|Average orbital speed||18.61 km/s|
|Longitude of ascending node||356.501°|
|Argument of perihelion||63.433°|
212.2 ± 6.8 km (IRAS)
|Mean density||2.36 ± 0.26 g/cm³|
|Equatorial surface gravity||0.0593 m/s²|
|Escape velocity||0.1122 km/s|
|Rotation period||0.2246 d (5.390 h)|
|Albedo||0.1793 (geometric) |
|Apparent magnitude||8.65 to 11.46|
|Absolute magnitude (H)||5.85|
|Angular diameter||0.21" to 0.078"|
Amphitrite was discovered by Albert Marth on March 1, 1854, at the private South Villa Observatory, in Regent's Park, London. It was Marth's only asteroid discovery. Its name was chosen by George Bishop, the owner of the observatory, who named it after Amphitrite, a sea goddess in Greek mythology.
Amphirite's orbit is less eccentric and inclined than those of its larger cousins; indeed, it is the most circular of any asteroid discovered up to that point. As a consequence, it never becomes as bright as Iris or Hebe, especially as it is much further from the Sun than those asteroids. It can reach magnitudes of around +8.6 at a favorable opposition, but usually is around the binocular limit of +9.5.
A satellite of the asteroid is suspected to exist, based on lightcurve data collected by Edward F. Tedesco. In 1988 a search for satellites or dust orbiting this asteroid was performed using the UH88 telescope at the Mauna Kea Observatories, but the effort came up empty.
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- "AstDys (29) Amphitrite Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2010-06-26.
- Lutz D. Schmadel, Dictionary of Minor Planet Names: Addendum to Fifth Edition: 2006 - 2008.
- Baer, James; Steven R. Chesley (2008). "Astrometric masses of 21 asteroids, and an integrated asteroid ephemeris" (PDF). Celestial Mechanics and Dynamical Astronomy (Springer Science+Business Media B.V. 2007) 100 (2008): 27–42. Bibcode:2008CeMDA.100...27B. doi:10.1007/s10569-007-9103-8. Retrieved 2008-11-10.
- Tedesco, E. F. (March 1979). "Binary Asteroids: Evidence for Their Existence from Lightcurves". Science, New Series 203 (4383): 905–907. Bibcode:1979Sci...203..905T. doi:10.1126/science.203.4383.905. PMID 17771729.
- van Flandern, T. C.; Tedesco, E. F.; Binzel, R. P. (1979). "Satellites of asteroids". Asteroids. Tucson, AZ: University of Arizona Press. pp. 443–465.
- Gradie, J.; Flynn, L. (March 1988), "A Search for Satellites and Dust Belts Around Asteroids: Negative Results", Abstracts of the Lunar and Planetary Science Conference 19: 405–406, Bibcode:1988LPI....19..405G.