87 Sylvia

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87 Sylvia

Discovery
Discovered by:	Norman Robert Pogson
Discovery date:	May 16, 1866
Orbital characteristics
Epoch July 14, 2004 (JD 2453200.5)
Aphelion	563.679 Gm (3.768 AU)
Perihelion:	480.594 Gm (3.213 AU)
Semi-major axis:	522.137 Gm (3.490 AU)
Eccentricity:	0.080
Orbital period:	2381.697 d (6.52 a)
Avg. orbital speed:	15.94 km/s
Mean anomaly:	352.763°
Inclination:	10.855°
Longitude of ascending node:	73.342°
Argument of perihelion:	266.195°
Physical characteristics
Dimensions:	385×265×230 ± 10 km[1][2]
Mass:	1.478±0.006×1019 kg[1]
Mean density:	1.2 ± 0.1 g/cm³[1]
Equatorial surface gravity:	0.027 m/s²
Escape velocity:	0.10 km/s
Rotation period:	0.2160 d (5.183642 h)[3][4]
Albedo:	0.0435[5]
Temperature:	~151 K max: 223 K (-52°C)
Spectral type:	X[6]
Absolute magnitude:	6.94

87 Sylvia is one of the biggest main-belt asteroids. It is a member of the Cybele group located beyond the middle of the belt. Sylvia is famous for being the first asteroid known to have more than one moon.

Contents 1 Discovery and naming 2 Physical characteristics 3 Moons 4 Other websites 5 References

[change] Discovery and naming

Sylvia was found by N. R. Pogson on May 16, 1866 from Madras (Chennai), India.^[7] Paul Herget, in his The Names of the Minor Planets (1955), attributes the name as honouring the first wife of astronomer Camille Flammarion, Sylvie Petiaux-Hugo Flammarion (this entry is signed by A. Paluzie-Borrell). However in the article announcing the discovery of this asteroid (MNRAS, 1866), Pogson explained that he selected the name in reference to Rhea Silvia, mother of Romulus and Remus.

[change] Physical characteristics

Sylvia is very dark in color and probably made of primitive. The discovery of its moons made possible an accurate measurement of the asteroid's mass and density. Its density was found to be very low (around 1.2 times the density of water), indicating that the asteroid has a lot of empty spaces; From 25% to as much as 60% of it may be empty space,^[1] depending on the details of what it's made of. However, the mineralogy of the X-type asteroids is not known well enough to force this further. Either way, this suggests a loose rubble pile (an asteroid that has been broken up in a collision and pulled back together by gravity) structure. Sylvia is also a fairly fast rotator, turning about its axis every 5.18 hours (giving an equatorial rotation speed of about 230 km/h or 145 mph). The short axis is the rotation axis.^[3] Direct images^[1] indicate that Sylvia's pole points towards ecliptic coordinates (β, λ) = (+62.6°, 72.4°) with only a 0.5° uncertainty, which gives it an axial tilt of around 29.1°. Sylvia's shape is very stretched.

[change] Moons

Sylvia is orbited by two small moons. They have been named Romulus and Remus (the formal names are (87) Sylvia I Romulus and (87) Sylvia II Remus, respectively), after the children of the mythological Rhea Silvia.

Romulus, the first moon, was found on February 18, 2001 from the Keck II telescope by Michael E. Brown and Jean-Luc Margot. It is about 18 km in diameter and orbits at a distance of 1356±5 km, taking 3.6496±0.0007 days (87.59 h) to complete an orbit of Sylvia.

Remus, the second moon, was found over three years later on August 9, 2004 by Franck Marchis of UC Berkeley, and Pascal Descamps, Daniel Hestroffer, and Jérôme Berthier of the Observatoire de Paris, France. It is 7±2 km in diameter and orbits at a distance of 706±5 km, taking 1.3788±0.0007 days (33.09 h) to complete an orbit of Sylvia.

It is thought likely that both Sylvia and its moons are rubble piles from a past asteroid collision^[1] Other, smaller moons formed in a similar way may also be found.

From the surface of Sylvia, Romulus and Remus would appear about the same size. Romulus, the farthest moon, would be about 0.89° across, a bit bigger than the closer but smaller Remus, which would be about 0.78° across. Because Sylvia is far from spherical, these values may vary by a little more than 10%, depending on where the observer is on Sylvia's surface. Since the two asteroid moons appear to orbit (as best we can tell) in the same plane, they would occult each other once every 2.2 days. When the season is right, twice during Sylvia's 6.52 year orbital period, they would eclipse the Sun, which, at 0.15° across, is much smaller than when seen from Earth (0.53°). From Remus, the closer moon, Sylvia appears very big, about 30°×18° across, while its view of Romulus varies between 1.59 and 0.50° across. From Romulus, Sylvia measures 16°×10° across, while Remus varies between 0.62° and 0.19°.

[change] Other websites

• Pogson, N. R. (1866), Minor Planet (87) Sylvia, Monthly Notices of the Royal Astronomical Society, Vol. 26, p. 311 (June 1866)
• Data on (87) Sylvia from Johnston's archive (maintained by W. R. Johnston)
• Rubble-Pile Minor Planet Sylvia and Her Twins (ESO news release, August 2005) Includes images and artists impressions
• Adaptive Optics System Reveals New Asteroidal Satellite (SpaceDaily.com, March 2001) Includes a discovery image.
• Space.com: First asteroid trio discovered
• IAUC 7588, reporting discovery of S/2001 (87) 1
• IAUC 7590, confirming the discovery
• IAUC 8582, reporting discovery of S/2004 (87) 1 and naming Romulus and Remus
• An animation of (87) Sylvia and its moons (23 MB, DivX)
• Shape model derived from lightcurve (on page 19)

[change] References

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