704 Interamnia
 Comparison of Interamnia and Ceres | |
| Discovery | |
|---|---|
| Discovered by | Vincenzo Cerulli |
| Discovery date | October 2, 1910 |
| Designations | |
| 1910 KU; 1952 MW | |
| Main belt | |
| Orbital characteristics | |
| Epoch October 22, 2004 (JD 2453300.5) | |
| Aphelion | 526.464 Gm (3.519 AU) |
| Perihelion | 389.910 Gm (2.606 AU) |
| 458.187 Gm (3.063 AU) | |
| Eccentricity | 0.149 |
| 1957.827 d (5.36 a) | |
Average orbital speed | 16.92 km/s |
| 204.093° | |
| Inclination | 17.285° |
| 280.422° | |
| 95.654° | |
| Physical characteristics | |
| Dimensions | 350.4×303.7 km 1 |
| Mass | 5.7×1019 kg |
Mean density | 3.6 g/cm³ |
| 0.186 m/s² | |
| 242.9 m/s | |
| 0.364 d 2 | |
| Albedo | 0.075 |
| Temperature | ~160 K |
Spectral type | F |
| 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
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
- Orbital simulation from JPL (Java)
- G. Michalak Determination of asteroid masses Astronomy & Astrophysics, Vol. 374, 703 (2001)
- Animation of Asteroid Interamnia taken on April 1st & 2nd, 2003
- Occultation of GSC 23450183 by (704) Interamnia on 1996 December 17 (dia: 329km; rotation period of 8.70 +/- 0.06 hours)
- Interamnia Occultations Observed before 2003
- Occultation of HIP36189 by (704) Interamnia on 2003 March 23 (dia: 350.4×303.7 km) recorded by Isao Ootsuki (graze) and Hideo Takashima and Fujio Ohbain Japan, analysis by Tsutomu Hayamizu