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444 Gyptis

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Main-belt asteroid

444 Gyptis
Discovery
Discovered byJ. Coggia
Discovery date31 March 1899
Designations
MPC designation(444) Gyptis
Pronunciation/ˈdʒɪptɪs/
Named afterGyptis
Alternative designations1899 EL
Minor planet categoryMain belt
AdjectivesGyptidian
Orbital characteristics
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc116.54 yr (42568 d)
Aphelion3.25674 AU (487.201 Gm)
Perihelion2.28337 AU (341.587 Gm)
Semi-major axis2.77005 AU (414.394 Gm)
Eccentricity0.17569
Orbital period (sidereal)4.61 yr (1684.0 d)
Mean anomaly11.8852°
Mean motion0° 12 49.615 / day
Inclination10.2775°
Longitude of ascending node195.716°
Argument of perihelion154.984°
Physical characteristics
Dimensions179×150 km
Mean diameter159.331±0.490 km
164.63±2.60 km
Mass1.25×10 kg
(1.06±0.28)×10 kg
Mean density5.53±1.46 g/cm
4.55±1.23 g/cm
Synodic rotation period6.214 h (0.2589 d)
Geometric albedo0.051±0.008
Spectral typeC
Absolute magnitude (H)8.07

444 Gyptis is a main-belt asteroid that was discovered by J. Coggia on March 31, 1899, in Marseilles. It is classified as a C-type asteroid and is probably composed of carbonaceous material. The spectra of the asteroid displays evidence of aqueous alteration.

In 2004, Kochetova estimated Gyptis to have a mass of 1.25×10 kg with a high density of 5.53 g/cm. In 2012 Carry estimated the mass as (1.06±0.28)×10 kg with a high density of 4.55±1.23 g/cm. The adaptive optics instrument at the W. M. Keck Observatory showed an object with a diameter of 129 km, which is much smaller than the estimate of 160 km from the IRAS observatory measurements, indicating an irregular shape. The size ratio between the major and minor axes is estimated at 1.40. Observations of an occultation on October 14, 2007, produced six chords indicating a cross-section ellipsoid of 179×150 km.

Between 1990 and 2021, 444 Gyptis has been observed to occult 17 stars.

References

  1. ^ "JPL Small-Body Database Browser: 444 Gyptis (1899 EL)" (2024-09-25 last obs). Retrieved 19 December 2024.
  2. ^ "2007 European Asteroidal Occultation Results". euraster.net (a website for Asteroidal Occultation Observers in Europe). 14 October 2007. Retrieved 1 December 2008. (Chords)
  3. ^ Carry, B. (December 2012), "Density of asteroids", Planetary and Space Science, vol. 73, pp. 98–118, arXiv:1203.4336, Bibcode:2012P&SS...73...98C, doi:10.1016/j.pss.2012.03.009. See Table 1.
  4. ^ Jim Baer (2008). "Recent Asteroid Mass Determinations". Personal Website. Archived from the original on 2 July 2013. Retrieved 27 November 2008.
  5. 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.
  6. Marchis, F.; et al. (November 2006), "Shape, size and multiplicity of main-belt asteroids. I. Keck Adaptive Optics survey", Icarus, 185 (1): 39–63, Bibcode:2006Icar..185...39M, doi:10.1016/j.icarus.2006.06.001, PMC 2600456, PMID 19081813.

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