107 Camilla

107 Camilla
Discovery
Discovered by	Norman Robert Pogson
Discovery date	November 17, 1868
Designations
Alternative names	A893 QA; 1938 OG; 1949 HD1
Minor planet category	Main belt (Cybele)
Orbital characteristics
	Epoch December 31, 2006 (JD 2454100.5)
Aphelion	560.937 Gm (3.750 AU)
Perihelion	479.343 Gm (3.204 AU)
Semi-major axis	520.140 Gm (3.477 AU)
Eccentricity	0.078
Orbital period	2368.050 d (6.48 a)
Average orbital speed	15.95 km/s
Mean anomaly	1.746°
Inclination	10.048°
Longitude of ascending node	173.132°
Argument of perihelion	309.877°
Physical characteristics
Dimensions	285×205×170 ± 20 km
Mass	1.09±0.04×1019 kg
Mean density	~1.9 g/cm³
Surface gravity	~0.036 m/s²
Escape velocity	0.10 km/s
Rotation period	0.2018 d (4.84393 h)
Albedo	0.0525
Temperature	~151 K; max: 223 K (-52°C)
Spectral type	C
Absolute magnitude (H)	7.08

S/2001 (107) 1
Discovery
Discovered by	A. Storrs, F. Vilas,; R. Landis, E. Wells,; C. Woods, B. Zellner,; and M. Gaffey
Discovery date	1 March 2001
Designations
Minor planet category	Main belt (Cybele)
Orbital characteristics
Semi-major axis	1235 ± 16 km
Eccentricity	0.006 ± 0.002
Orbital period	3.710 ± 0.001 d
Average orbital speed	24.2 m/s
Inclination	< 10°
Satellite of	107 Camilla
Physical characteristics
Dimensions	~ 11 ± 2 km
Mass	~1.5×1015 kg
Equatorial escape velocity	~ 6 m/s
Absolute magnitude (H)	13.18

107 Camilla is one of the biggest main belt asteroids. It orbits within the Cybele Group, beyond most of the main belt asteroids. It has a very dark surface and is made of carbonate. It was found by N. R. Pogson on November 17, 1868, and named after Camilla, Queen of the Volsci in Roman mythology.

Study of its light curve shows that Camilla's pole probably points towards ecliptic coordinates (β, λ) = (+51°, 72°) with a 10° uncertainty,^[1] which gives it an axial tilt of 29°.

Moon (S/2001 (107) I)

On March 1, 2001, a moon of Camilla was found by A. Storrs, F. Vilas, R. Landis, E. Wells, C. Woods, B. Zellner, and M. Gaffey using the Hubble Space Telescope.^[2] It has been labelled S/2001 (107) 1 but it does not yet have an official name.

Later sightings in September 2005 with the VLT allowed scientists to work out its orbit.^[3] Apart from data in infobox, the inclination was found to be 3 ± 1° with respect to an axis pointing towards (β, λ) = (+55°, 75°).^[3] Given the ~10° uncertainty in the actual rotational axis of Camilla, the orbit's inclination probably is less than 10°.

The moon is estimated to be about 11 km in diameter.^[4] If it has the same density as Camilla, this would give it a mass of about ~1.5×10¹⁵ kg. It has a similar colour to Camilla.^[2]

References

↑ ^1.0 ^1.1 ^1.2 J. Torppa; et al. (2003). "Shapes and rotational properties of thirty asteroids from photometric data" (PDF). Icarus. 164 (2): 346. doi:10.1016/S0019-1035(03)00146-5. S2CID 119609765. Archived from the original (PDF) on 2015-11-06. Retrieved 2007-12-24.
↑ ^2.0 ^2.1 ^2.2 "IAUC 7599". Archived from the original on 2006-05-01. Retrieved 2007-12-24.
↑ ^3.0 ^3.1 ^3.2 ^3.3 ^3.4 107 Camilla and S/2001 (107) 1, F. Marchis Archived 2007-07-24 at the Wayback Machine
↑ ^4.0 ^4.1 ^4.2 ^4.3 F. Marchis; et al. (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.
↑ Assuming a similar density to the primary.
↑ ^6.0 ^6.1 ^6.2 "Supplemental IRAS Minor Planet Survey". Archived from the original on 2010-01-17. Retrieved 2007-12-24.{{cite web}}: CS1 maint: bot: original URL status unknown (link)
↑ Axis ratios (rounded to nearest 5 km) based on lightcurve analysis of Torppa et al. (2003), however taking IRAS mean diameter is inconsistent with the maximum value of the short axis obtained in Marchis et al. (2006). Hence, presumably IRAS measurements were taken of a large face. Therefore, anchoring absolute size by reuqiring the shortest axis to be no larger than the maximum allowed by Marchis et al. (2006).
↑ Error estimate derived from consideration of $M\propto a^{3}/P^{2}$ and given errors in a and P. See propagation of uncertainty.
↑ "PDS spectral class data". Archived from the original on 2010-01-17. Retrieved 2007-12-24.{{cite web}}: CS1 maint: bot: original URL status unknown (link)

Other websites

Data on (87) Sylvia from Johnston's archive (maintained by W. R. Johnston)
Hubble Finds New Asteroid Moon (SpaceDaily.com, 21-03-2001), includes discovery image.
107 Camilla and S/2001 (107) 1, orbit data website maintained by F. Marchis. Includes orbit diagrams.

[TorKaaMic03-1] 1.0 ^1.1 ^1.2 J. Torppa; et al. (2003). "Shapes and rotational properties of thirty asteroids from photometric data" (PDF). Icarus. 164 (2): 346. doi:10.1016/S0019-1035(03)00146-5. S2CID 119609765. Archived from the original (PDF) on 2015-11-06. Retrieved 2007-12-24.

[iauc7599-2] 2.0 ^2.1 ^2.2 "IAUC 7599". Archived from the original on 2006-05-01. Retrieved 2007-12-24.

[marchis-3] 3.0 ^3.1 ^3.2 ^3.3 ^3.4 107 Camilla and S/2001 (107) 1, F. Marchis Archived 2007-07-24 at the Wayback Machine

[MarKaaHom06-4] 4.0 ^4.1 ^4.2 ^4.3 F. Marchis; et al. (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.

[mass-5] Assuming a similar density to the primary.

[IRAS-6] 6.0 ^6.1 ^6.2 "Supplemental IRAS Minor Planet Survey". Archived from the original on 2010-01-17. Retrieved 2007-12-24.{{cite web}}: CS1 maint: bot: original URL status unknown (link)

[less-7] Axis ratios (rounded to nearest 5 km) based on lightcurve analysis of Torppa et al. (2003), however taking IRAS mean diameter is inconsistent with the maximum value of the short axis obtained in Marchis et al. (2006). Hence, presumably IRAS measurements were taken of a large face. Therefore, anchoring absolute size by reuqiring the shortest axis to be no larger than the maximum allowed by Marchis et al. (2006).

[error-8] Error estimate derived from consideration of $M\propto a^{3}/P^{2}$ and given errors in a and P. See propagation of uncertainty.

[PDS_tax-9] "PDS spectral class data". Archived from the original on 2010-01-17. Retrieved 2007-12-24.{{cite web}}: CS1 maint: bot: original URL status unknown (link)

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