704 Interamnia

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704 Interamnia
704Int-Size.gif
Comparison of Interamnia and Ceres
Discovery
Discovered by Vincenzo Cerulli
Discovery time October 2, 1910
Names
Other names 1910 KU; 1952 MW
Group Main belt
Orbit
Reference date October 22, 2004 (JD 2453300.5)
Longest distance from the Sun 526.464 Gm (3.519 AU)
Shortest distance from the Sun 389.910 Gm (2.606 AU)
Longest distance from the center of its orbital path
("semi-major axis")
458.187 Gm (3.063 AU)
How egg-shaped its orbit is
("eccentricity")
0.149
How long it takes to complete an orbit 1957.827 d (5.36 a)
Average speed 16.92 km/s
Mean anomaly 204.093°
Angle above the reference plane
("inclination")
17.285°
Longitude of where it comes up through the reference plane 280.422°
Angle between its shortest distance from what it orbits around and where it comes up through the reference plane
("argument of periapsis")
95.654°
Size and Other Qualities
Measures 350.4×303.7 km 1
Mass 5.7×1019 kg
Average density 3.6 g/cm³
Gravity at its surface 0.186 m/s²
Slowest speed able to escape into space
("escape velocity")
242.9 m/s
How long it takes to turn around one time 0.364 d 2
How much light it reflects 0.075
Avg. surface temp. ~160 K
Light-band group
("spectral type")
F
True brightness
("absolute magnitude")
5.94

704 Interamnia is a very big asteroid. Scientists think it is 350 kilometers wide. Its mean distance from the Sun is 3.067 (AU). It was found on October 2, 1910 by Vincenzo Cerulli. It is named after the Latin name for Teramo, Italy, which is where Cerulli worked. It is the fifth heaviest asteroid after Ceres, Vesta, Pallas and Hygiea, and scientists think that it makes up 2.0% of the mass of the whole asteroid belt.

Characteristics[change | change source]

Although the biggest asteroid apart from the "big four", Interamnia is not studied a lot. It is easily the biggest of the F-type asteroids, but there exist very few details of what the inside is made of or shape and no lightcurve analysis has yet been done to find out the ecliptic coordinates of Interamnia's poles (and hence its axial tilt). Its apparently high bulk density (though subject to much error) suggests a very solid body entirely without internal porosity or traces of water. This also strongly suggests that Interamnia is big enough to have fully withstood all the collisions that have happened in the asteroid belt since the Solar System was made.

Its very dark surface and fairly far distance form the Sun means Interamnia can never be seen with 10x50 binoculars. At most oppositions its magnitude is around +11.0, which is less than the minimum brightness of Vesta, Ceres or Pallas. Even at a near-perihelion opposition its magnitude is only around +9.9, which is over four magnitudes lower than Vesta.

Its orbit is a bit more eccentric that of Hygiea (15% versus 12%) but is different because Hygiea's orbit is much more inclined and takes a bit shorter to complete one orbit. Another difference is that Interamnia's perihelion is at the other side of the perihelia of the "big four", so that at Interamnia at perihelion is actually closer to the Sun than Ceres and Pallas are at the same longitude. It is unlikely to collide with Pallas because their nodes are located too far apart, whilst although its nodes are located on the opposite side from those of Ceres, it is generally clear of Ceres when both cross the same orbital plane and a collision is again unlikely.

Other websites[change | change source]