704 Interamnia
Observations of 704 Interamnia carried out at the Observatory of Teramo (founded by the discoverer of the asteroid, Vincenzo Cerulli) for the 101st anniversary since its discovery. The animation shows Interamnia's path over three hours.
|
|
| Discovery | |
|---|---|
| Discovered by | Vincenzo Cerulli |
| Discovery date | 2 October 1910 |
| Designations | |
| MPC designation | (704) Interamnia |
| Pronunciation | /ˌɪntərˈæmniə/ IN-tər-AM-nee-ə |
|
Named after
|
Teramo |
| 1910 KU; 1952 MW | |
| Main belt | |
| Orbital characteristics | |
| Epoch 31 July 2016 (JD 2457600.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 102.38 yr (37395 d) |
| Aphelion | 3.5293 AU (527.98 Gm) |
| Perihelion | 2.5857 AU (386.82 Gm) |
| 3.0575 AU (457.40 Gm) | |
| Eccentricity | 0.15431 |
| 5.35 yr (1952.8 d) | |
|
Average orbital speed
|
16.92 km/s |
| 276.11° | |
| 0° 11m 3.66s / day | |
| Inclination | 17.309° |
| 280.30° | |
| 95.208° | |
| Earth MOID | 1.65761 AU (247.975 Gm) |
| Jupiter MOID | 2.14415 AU (320.760 Gm) |
| Jupiter Tisserand parameter | 3.148 |
| Physical characteristics | |
| Dimensions | (350.3 ± 0.8) × (303.6 ± 1.2) km 326 (mean of 350x304) 317 ± 5 km IRAS |
|
Mean radius
|
158.31±2.6 km |
| Mass | 3.90±0.18×1019 kg 7.49 ×1019 |
|
Mean density
|
2.29 ± 0.48 g/cm³ |
|
Equatorial surface gravity
|
0.186 m/s² |
|
Equatorial escape velocity
|
242.9 m/s |
| 0.364 d 2 (8.727 h (0.3636 d) |
|
| 0.0742±0.002 | |
| Temperature | ~160 K |
| F/B | |
| 9.9 to 13.0 | |
| 5.94 | |
704 Interamnia is a very large asteroid, with an estimated diameter of 350 kilometres. Its mean distance from the Sun is 3.067 (AU). It was discovered on October 2, 1910 by Vincenzo Cerulli, and named after the Latin name for Teramo, Italy, where Cerulli worked. It is probably the fifth-most-massive asteroid after Ceres, Vesta, Pallas, and Hygiea, with a mass estimated to be 1.2% of the mass of the entire asteroid belt.
Although Interamnia is the largest asteroid after the "big four", it is a very little-studied body. It is easily the largest of the F-type asteroids, but there exist very few details of its internal composition or shape, and no light curve analysis has yet been done to determine the ecliptic coordinates of Interamnia's poles (and hence its axial tilt). Its apparently high bulk density (though subject to much error) suggests an extremely solid body entirely without internal porosity or traces of water. This also strongly suggests that Interamnia is large enough to have fully withstood all the collisions that have occurred in the asteroid belt since the Solar System was formed.
Its very dark surface and relatively large distance from 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 perihelic opposition its magnitude is only +9.9, which is over four magnitudes lower than Vesta.
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Wikipedia