423 Diotima: Difference between revisions

423 Diotima
Discovery
Discovered by	Auguste Charlois
Discovery date	December 7, 1896
Designations
Named after	Diotima of Mantinea
Alternative names	1896 DB
Minor planet category	Main belt (Eos)
Orbital characteristics
	Epoch 30 January 2005 (JD 2453400.5)
Aphelion	477.421 Gm (3.191 AU)
Perihelion	439.945 Gm (2.941 AU)
Semi-major axis	458.683 Gm (3.066 AU)
Eccentricity	0.041
Orbital period (sidereal)	1960.969 d (5.37 a)
Average orbital speed	17.01 km/s
Mean anomaly	179.514°
Inclination	11.24°
Longitude of ascending node	69.564°
Argument of perihelion	207.473°
Physical characteristics
Dimensions	208.7 km (IRAS); 171 x 138 km
Mass	1.6×1019 kg; ≈5.1×1018? kg
Mean density	unknown
Surface gravity	unknown
Escape velocity	unknown
Synodic rotation period	4.775 h
Albedo	0.05
Temperature	unknown
Spectral type	C
Absolute magnitude (H)	7.24

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Revision as of 18:25, 11 July 2010

423 Diotima (Template:Pron-en dye-ə-TYE-mə; or as in Latin Diotīma, from Greek Διοτίμα) is a one of the largest Main belt asteroids. It is classified as a C-type asteroid and is probably composed of primitive carbonaceous material. ^{[citation needed]}

It was discovered by Auguste Charlois on December 7, 1896 in Nice. It is named for a priestess who was one of Socrates's teachers. It is one of seven of Charlois's discoveries that was expressly named by the Astromomisches Rechen-Institut (Astronomical Calculation Institute).^[6]

In the late 1990s, a network of astronomers worldwide gathered lightcurve data that was ultimately used to derive the spin states and shape models of 10 new asteroids, including (423) Diotima.^[7]^[8]

Dunham (2002) used 15 chords and obtained an estimated size of 171 x 138 km.^[2]

References

^ ^a ^b ^c ^d ^e "JPL Small-Body Database Browser: 423 Diotima (1896 DB)". 2008-09-09 last obs. Retrieved 2008-11-10. {{cite web}}: Check date values in: |date= (help)
^ ^a ^b Vasundhara, R (2006). "Occultation of 2UCAC 42376428 by (423) Diotima on 2005 March 06". Astronomical Society of India. 34: 21–26. Retrieved 2008-11-30. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
^ Michalak, G. (2001). "Determination of asteroid masses". Astronomy & Astrophysics. 374: 703–711. doi:10.1051/0004-6361:20010731. Retrieved 2008-11-10.
^ Michalak2001 assumed masses of perturbing asteroids used in calculations of perturbations of the test asteroids.
^ Using the volume of an ellipsoid of 209x171x138km * an assumed density of 2 g/cm³ yields a mass (m=d*v) of 5.1E+18 kg
^ Schmadel Lutz D. Dictionary of Minor Planet Names (fifth edition), Springer, 2003. ISBN 3540002383.
^ Durech., J.; Kaasalainen, M., Marciniak, A.; et al., “Physical models of ten asteroids from an observers' collaboration network”, Astronomy and Astrophysics, Volume 465, Issue 1, April I 2007, pp. 331-337
^ Durech, J.; Kaasalainen, M.; Marciniak, A.; Allen, W. H. et al. “Asteroid brightness and geometry,” Astronomy and Astrophysics, Volume 465, Issue 1, April I 2007, pp. 331-337.

External links

Orbital simulation from JPL (Java) / Ephemeris

This article about a C-type asteroid native to the asteroid belt is a stub. You can help Wikipedia by expanding it.

[jpldata-1] "JPL Small-Body Database Browser: 423 Diotima (1896 DB)". 2008-09-09 last obs. Retrieved 2008-11-10. {{cite web}}: Check date values in: |date= (help)

[Vasundhara2006-2] Vasundhara, R (2006). "Occultation of 2UCAC 42376428 by (423) Diotima on 2005 March 06". Astronomical Society of India. 34: 21–26. Retrieved 2008-11-30. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)

[Michalak2001-3] Michalak, G. (2001). "Determination of asteroid masses". Astronomy & Astrophysics. 374: 703–711. doi:10.1051/0004-6361:20010731. Retrieved 2008-11-10.

[4] Michalak2001 assumed masses of perturbing asteroids used in calculations of perturbations of the test asteroids.

[5] Using the volume of an ellipsoid of 209x171x138km * an assumed density of 2 g/cm³ yields a mass (m=d*v) of 5.1E+18 kg

[6] Schmadel Lutz D. Dictionary of Minor Planet Names (fifth edition), Springer, 2003. ISBN 3540002383.

[7] Durech., J.; Kaasalainen, M., Marciniak, A.; et al., “Physical models of ten asteroids from an observers' collaboration network”, Astronomy and Astrophysics, Volume 465, Issue 1, April I 2007, pp. 331-337

[8] Durech, J.; Kaasalainen, M.; Marciniak, A.; Allen, W. H. et al. “Asteroid brightness and geometry,” Astronomy and Astrophysics, Volume 465, Issue 1, April I 2007, pp. 331-337.

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@@ Line 46: / Line 46: @@
 In the late 1990s, a network of astronomers worldwide gathered lightcurve data that was ultimately used to derive the spin states and shape models of 10 new asteroids, including (423) Diotima.<ref>Durech., J.; Kaasalainen, M., Marciniak, A.; et al., [http://www.foam13.it/new/3D/ten_models.pdf “Physical models of ten asteroids from an observers' collaboration network”,] '' Astronomy and Astrophysics'', Volume 465, Issue 1, April I 2007, pp. 331-337</ref><ref>Durech, J.; Kaasalainen, M.; Marciniak, A.; Allen, W. H. et al. “Asteroid brightness and geometry,” ''Astronomy and Astrophysics'', Volume 465, Issue 1, April I 2007, pp. 331-337.</ref>
-Dunham (2002) used 15 [[Chord (geometry)|chords]] and obtained an estimated size of 171 x 138&nbsp;km.<ref name=Vasundhara2006>{{cite journal
+Dunham (2002) used 15 [[Chord (astronomy)|chords]] and obtained an estimated size of 171 x 138&nbsp;km.<ref name=Vasundhara2006>{{cite journal
   |last=Vasundhara |first=R
   |coauthors=Kuppuswamy, Ramamoorthy, Velu, Venkataramana