145 Adeona

145 Adeona
Discovery
Discovered by	Christian Heinrich Friedrich Peters
Discovery date	3 June 1875
Designations
MPC designation	(145) Adeona
Pronunciation	/ædiːˈoʊnə/
Named after	Adeōna
Minor planet category	main-belt · Adeona
Adjectives	Adeonian
Orbital characteristics
	Epoch 31 July 2016 (JD 2457600.5)
	Uncertainty parameter 0
Observation arc	130.60 yr (47700 d)
Aphelion	3.05972 AU (457.728 Gm)
Perihelion	2.28737 AU (342.186 Gm)
Semi-major axis	2.67354 AU (399.956 Gm)
Eccentricity	0.14444
Orbital period (sidereal)	4.37 yr (1596.7 d)
Mean anomaly	233.709°
Mean motion	0° 13m 31.663s / day
Inclination	12.6337°
Longitude of ascending node	77.4206°
Argument of perihelion	44.0233°
Physical characteristics
Mean diameter	144±3 km; 127.783±0.355 km; 149.5±5.5 km
Flattening	0.08
Mass	(2.4±0.3)×1018 kg ; (2.08±0.57)×1018 kg
Mean density	1.52±0.21 g/cm3; 1.18±0.34 g/cm3
Equatorial surface gravity	0.0422 m/s2
Equatorial escape velocity	0.0799 km/s
Synodic rotation period	15.071 h (0.6280 d)
Geometric albedo	0.048 (calculated); 0.061±0.010; 0.0467 ± 0.0116
Spectral type	C (Tholen)
Absolute magnitude (H)	8.43, 8.050

145 Adeona is a large asteroid from the intermediate asteroid belt, approximately 150 kilometers (93 miles) in diameter. Its surface is very dark,^[8] and, based upon its classification as a C-type asteroid, is probably composed of primitive carbonaceous material. The spectra of the asteroid displays evidence of aqueous alteration.^[9] The Adeona family of asteroids is named after it.

It was discovered by C. H. F. Peters on June 3, 1875, from the observatory at Hamilton College, Clinton, New York. Peters named it after Adeona, the Roman goddess of homecoming, because he had recently returned from a journey across the world to observe the transit of Venus. Peters also discovered 144 Vibilia on the same night.^[10]

During 2001, Adeona was observed by radar from the Arecibo Observatory. The returned signal matched an effective diameter of 151 ± 18 km. This is consistent with the asteroid dimensions computed through other means.^[11]

Two stellar occultations by Adeona have been observed: The first one on July 9, 2002 when it occulted an 11.8 mag star, and then again on February 3, 2005 when several observers in Japan recorded the occultation of a 10.4 mag star. The latter was consistent with a diameter of 151 km.^[12]^[13]^[14]

The Dawn mission team discussed performing a flyby of this object, however NASA decided against it in July 2016.^[15] At the time this was considered Dawn was orbiting the large asteroid/dwarf planet 1 Ceres, and went on studying that body later that year.^[16] Dawn had previously orbited asteroid 4 Vesta, before traveling to Ceres.^[16]

Notes

^ Flattening derived from the maximum aspect ratio (c/a): $f=1-{\frac {c}{a}}$ , where (c/a) = 0.92±0.03.^[6]

References

^ "Discovery Circumstances: Numbered Minor Planets". Archived from the original on 10 May 2008. Retrieved 22 June 2004.
^ Noah Webster (1884) A Practical Dictionary of the English Language
^ "Adeona in Lewis & Short". Archived from the original on 20 August 2020. Retrieved 3 February 2018.
^ ^a ^b ^c ^d ^e ^f "145 Adeona". JPL Small-Body Database. NASA/Jet Propulsion Laboratory. Retrieved 12 May 2016.
^ "The Asteroid Orbital Elements Database". astorb. Lowell Observatory.
^ ^a ^b ^c ^d ^e P. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. Astronomy & Astrophysics 54, A56
^ ^a ^b ^c Carry, B. (December 2012), "Density of asteroids", Planetary and Space Science, 73 (1): 98–118, arXiv:1203.4336, Bibcode:2012P&SS...73...98C, doi:10.1016/j.pss.2012.03.009, S2CID 119226456.
^ ^a ^b ^c ^d Pravec, P.; et al. (May 2012), "Absolute Magnitudes of Asteroids and a Revision of Asteroid Albedo Estimates from WISE Thermal Observations", Asteroids, Comets, Meteors 2012, Proceedings of the conference held May 16–20, 2012 in Niigata, Japan, vol. 1667, no. 1667, p. 6089, Bibcode:2012LPICo1667.6089P.
^ Fornasier, S.; et al. (February 1999), "Spectroscopic comparison of aqueous altered asteroids with CM2 carbonaceous chondrite meteorites", Astronomy and Astrophysics Supplement, 135: 65–73, Bibcode:1999A&AS..135...65F, doi:10.1051/aas:1999161.
^ Schmadel, Lutz D. (2003). Dictionary of Minor Planet Names. Springer Science & Business Media. p. 28. ISBN 978-3-540-00238-3.
^ Magri, Christopher; et al. (January 2007), "A radar survey of main-belt asteroids: Arecibo observations of 55 objects during 1999–2003", Icarus, 186 (1): 126–151, Bibcode:2007Icar..186..126M, doi:10.1016/j.icarus.2006.08.018
^ "Observed minor planet occultation events". David Dunham. 26 July 2005. Retrieved 3 June 2017.
^ "Results of Asteroidal occultation". Sendai Space Hall. Retrieved 3 June 2017.
^ "Occultation of (145) Adeona on 2005.2.3". Sendai Space Hall. Retrieved 3 June 2017.
^ "New Horizons Receives Mission Extension to Kuiper Belt, Dawn to Remain". July 2016.
^ ^a ^b Landau, Elizabeth (18 November 2016). "New Ceres Views as Dawn Moves Higher". NASA / Jet Propulsion Laboratory. Retrieved 20 November 2016.

External links

145 Adeona at AstDyS-2, Asteroids—Dynamic Site
- Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
145 Adeona at the JPL Small-Body Database
- Close approach · Discovery · Ephemeris · Orbit viewer · Orbit parameters · Physical parameters

[8] Flattening derived from the maximum aspect ratio (c/a): $f=1-{\frac {c}{a}}$ , where (c/a) = 0.92±0.03.^[6]

[1] "Discovery Circumstances: Numbered Minor Planets". Archived from the original on 10 May 2008. Retrieved 22 June 2004.

[2] Noah Webster (1884) A Practical Dictionary of the English Language

[3] "Adeona in Lewis & Short". Archived from the original on 20 August 2020. Retrieved 3 February 2018.

[jpldata-4] ^ ^a ^b ^c ^d ^e ^f "145 Adeona". JPL Small-Body Database. NASA/Jet Propulsion Laboratory. Retrieved 12 May 2016.

[lowell-5] "The Asteroid Orbital Elements Database". astorb. Lowell Observatory.

[VLT-6] P. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. Astronomy & Astrophysics 54, A56

[Carry2012-7] Carry, B. (December 2012), "Density of asteroids", Planetary and Space Science, 73 (1): 98–118, arXiv:1203.4336, Bibcode:2012P&SS...73...98C, doi:10.1016/j.pss.2012.03.009, S2CID 119226456.

[Pravec2012-9] Pravec, P.; et al. (May 2012), "Absolute Magnitudes of Asteroids and a Revision of Asteroid Albedo Estimates from WISE Thermal Observations", Asteroids, Comets, Meteors 2012, Proceedings of the conference held May 16–20, 2012 in Niigata, Japan, vol. 1667, no. 1667, p. 6089, Bibcode:2012LPICo1667.6089P.

[Fornasier1999-10] Fornasier, S.; et al. (February 1999), "Spectroscopic comparison of aqueous altered asteroids with CM2 carbonaceous chondrite meteorites", Astronomy and Astrophysics Supplement, 135: 65–73, Bibcode:1999A&AS..135...65F, doi:10.1051/aas:1999161.

[11] Schmadel, Lutz D. (2003). Dictionary of Minor Planet Names. Springer Science & Business Media. p. 28. ISBN 978-3-540-00238-3.

[icarus186_1_126-12] Magri, Christopher; et al. (January 2007), "A radar survey of main-belt asteroids: Arecibo observations of 55 objects during 1999–2003", Icarus, 186 (1): 126–151, Bibcode:2007Icar..186..126M, doi:10.1016/j.icarus.2006.08.018

[occult1-13] "Observed minor planet occultation events". David Dunham. 26 July 2005. Retrieved 3 June 2017.

[occult2-14] "Results of Asteroidal occultation". Sendai Space Hall. Retrieved 3 June 2017.

[occult3-15] "Occultation of (145) Adeona on 2005.2.3". Sendai Space Hall. Retrieved 3 June 2017.

[16] "New Horizons Receives Mission Extension to Kuiper Belt, Dawn to Remain". July 2016.

[nasa20161118-17] Landau, Elizabeth (18 November 2016). "New Ceres Views as Dawn Moves Higher". NASA / Jet Propulsion Laboratory. Retrieved 20 November 2016.

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See also

Notes

References

External links