View source for 704 Interamnia

<!-- Additional parameters for this template  are available at [[Template:Infobox Planet]]. -->{{Infobox Planet   | bgcolour=#FFFFC0 |
 name=704 Interamnia
 | discoverer=[[Vincenzo Cerulli]]
 | discovered=[[October 2]], [[1910]]
 | image=704 Interamnia VLT (2021), deconvolved.pdf
 | caption=
 | alt_names=1910 KU; 1952 MW
 | mp_category=[[Main belt]]
 | epoch=[[October 22]], [[2004]] ([[Julian day|JD]] 2453300.5)
 | semimajor=458.187 [[Giga|G]][[metre|m]] (3.063 [[Astronomical unit|AU]])
 | perihelion=389.910 Gm (2.606 AU)
 | aphelion=526.464 Gm (3.519 AU)
 | eccentricity=0.149
 | period=1957.827 [[day|d]] (5.36 [[Julian year (astronomy)|a]])
 | inclination=17.285[[degree (angle)|°]]
 | asc_node=280.422°
 | arg_peri=95.654°
 | mean_anomaly=204.093°
 | avg_speed=16.92 km/[[second|s]]
 | dimensions=350.4×303.7 km <sup>[http://uchukan.satsumasendai.jp/data/occult/0303intera.html 1]</sup>
 | mass=5.7×10<sup>19</sup> [[kilogram|kg]]
 | density=3.6 g/[[cubic centimetre|cm³]]
 | surface_grav=0.186 m/s²
 | escape_velocity=242.9 m/s
 | rotation=0.364 d <sup>[http://obswww.unige.ch/~behrend/page2cou.html 2]</sup>
 | spectral_type=[[F-type asteroid|F]]
 | abs_magnitude=5.94
 | albedo=0.075
 | single_temperature=~160 [[kelvin|K]]}}
'''704 Interamnia''' is a very big [[asteroid]]. Scientists think it is 350 [[kilometer]]s wide. Its mean distance from the [[Sun]] is 3.067 ([[astronomical unit|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 (dwarf planet)|Ceres]], [[4 Vesta|Vesta]], [[2 Pallas|Pallas]] and [[10 Hygiea|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 asteroid]]s, but there are few details of what the inside is made of or shape and no lightcurve analysis has been done to find out the ecliptic coordinates of Interamnia's poles (and 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 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 from the Sun means Interamnia can never be seen with 10x50 [[binoculars]]. At most oppositions its [[apparent magnitude|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 more eccentric than Hygiea (15% versus 12%) but is different because Hygiea's orbit is much more [[inclination|inclined]] and takes less time 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 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. Although its nodes are located on the opposite side from those of Ceres, it is generally far from Ceres when both cross the same orbital plane and a collision is again unlikely.

== Other websites ==
* [http://neo.jpl.nasa.gov/cgi-bin/db?sstr=704 Orbital simulation] {{Webarchive|url=https://archive.today/20121213103003/http://neo.jpl.nasa.gov/cgi-bin/db?sstr=704 |date=2012-12-13 }} from JPL (Java)
* G. Michalak [http://www.aanda.org/index.php?option=com_base_ora&access=standard&Itemid=39&url=articles/aa/pdf/2001/29/aa10228.pdf Determination of asteroid masses] Astronomy & Astrophysics, Vol. 374, 703 (2001)
* [http://physics.bgsu.edu/~layden/Anim/Asteroids/interamnia.htm Animation of Asteroid Interamnia] taken on April 1—2nd, 2003
* [http://adsabs.harvard.edu/abs/1997DPS....29.0710B Occultation] of GSC 23450183 by (704) Interamnia on 1996 December 17 (dia: 329&nbsp;km; rotation period of 8.70 +/- 0.06 hours)
* [http://iota.jhuapl.edu/mp704d17.htm Interamnia Occultations Observed before 2003]
* [http://uchukan.satsumasendai.jp/data/occult/limovie/0303intera-study.html Occultation] {{Webarchive|url=https://web.archive.org/web/20070109172809/http://uchukan.satsumasendai.jp/data/occult/limovie/0303intera-study.html |date=2007-01-09 }} of HIP36189 by (704) Interamnia on 2003 March 23 (dia: 350.4×303.7&nbsp;km) recorded by Isao Ootsuki (graze) and Hideo Takashima and Fujio Ohbain Japan, analysis by Tsutomu Hayamizu

{{MinorPlanets Navigator|703 Noëmi|705 Erminia}}
{{Small Solar System bodies}}

{{DEFAULTSORT:Interamnia}}
[[Category:Asteroids]]