187 Lamberta

187 Lamberta
Discovery
Discovered by	J. Coggia, 1878
Discovery date	11 April 1878
Designations
MPC designation	(187) Lamberta
Pronunciation	/læmˈbɜːrtə/
Alternative designations	A878 GB; 1946 LB;; 1948 XR
Minor planet category	Main belt
Orbital characteristics
	Epoch 31 July 2016 (JD 2457600.5)
	Uncertainty parameter 0
Observation arc	113.41 yr (41424 d)
Aphelion	3.3856 AU (506.48 Gm)
Perihelion	2.0695 AU (309.59 Gm)
Semi-major axis	2.7276 AU (408.04 Gm)
Eccentricity	0.24126
Orbital period (sidereal)	4.50 yr (1645.3 d)
Mean anomaly	217.42°
Mean motion	0° 13m 7.68s / day
Inclination	10.588°
Longitude of ascending node	21.707°
Argument of perihelion	196.93°
Earth MOID	1.07102 AU (160.222 Gm)
Jupiter MOID	1.60105 AU (239.514 Gm)
TJupiter	3.289
Physical characteristics
Mean diameter	141±2 km; 147.294±1.389 km; 131.3±1.1 km
Flattening	0.14
Mass	(1.9±0.3)×1018 kg ; (1.80±0.85)×1018 kg
Mean density	1.28±0.22 g/cm3; 1.51±0.71 g/cm3
Synodic rotation period	10.67 h (0.445 d)
Geometric albedo	0.052 (calculated); 0.044±0.007; 0.0647 ± 0.0135
Spectral type	C (Tholen)
Absolute magnitude (H)	8.40, 7.980

187 Lamberta is a main-belt asteroid that was discovered by Corsican-born French astronomer Jérôme Eugène Coggia on April 11, 1878. It was named after the astronomer Johann Heinrich Lambert. This was the second of Coggia's five asteroid discoveries.

This object is orbiting the Sun at a distance of 2.73 AU with a moderate eccentricity of 0.24 and an orbital period of 4.50 years. The orbital plane is inclined at an angle of 10.6° to the plane of the ecliptic. It is spinning with a rotation period of 10.67 hours.

The spectrum matches a classification of a C-type asteroid, which may mean it has a composition of primitive carbonaceous materials. It is a dark object as indicated by the low albedo and has an estimated size of about 131 km.³

Notes

Flattening derived from the maximum aspect ratio (c/a): $f=1-{\frac {c}{a}}$ , where (c/a) = 0.86±0.07.²

References

"187 Lamberta". JPL Small-Body Database. NASA/Jet Propulsion Laboratory. Retrieved 12 May 2016.
P. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. Astronomy & Astrophysics 54, A56
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.
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, no. 1667, Bibcode:2012LPICo1667.6089P. See Table 4.

External links

187 Lamberta at AstDyS-2, Asteroids—Dynamic Site
- Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
187 Lamberta at the JPL Small-Body Database

[4] Flattening derived from the maximum aspect ratio (c/a): $f=1-{\frac {c}{a}}$ , where (c/a) = 0.86±0.07.²

[jpldata-1] "187 Lamberta". JPL Small-Body Database. NASA/Jet Propulsion Laboratory. Retrieved 12 May 2016.

[VLT-2] P. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. Astronomy & Astrophysics 54, A56

[Carry2012-3] 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.

[Pravec2012-5] 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, no. 1667, Bibcode:2012LPICo1667.6089P. See Table 4.

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