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704 Interamnia

Large asteroid in the asteroid belt

Field	Value
minorplanet	yes
background	#D6D6D6
name	704 Interamnia
image	704 Interamnia VLT (2021), deconvolved.pdf
discoverer	Vincenzo Cerulli
discovered	2 October 1910
mpc_name	(704) Interamnia
alt_names	1910 KU; 1952 MW
pronounced
adjective	Interamnian
named_after	Teramo
mp_category	Main belt
orbit_ref	{{cite web
type	2024-06-21 last obs
title	JPL Small-Body Database Browser: 704 Interamnia (1910 KU)
url	https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=704
access-date	19 Dec 2024}}
epoch	July 01, 2021
(JD 2459396.5, heliocentric)
aphelion	3.53 AU
perihelion	2.58 AU
semimajor	3.056 AU
eccentricity	0.155
period	5.34 yr (1951 d)
inclination	17.31°
asc_node	280.3°
arg_peri	94.8°
mean_anomaly	248°
avg_speed	16.92 km/s
dimensions	± 8 km
flattening	0.14
mean_diameter
<br />{{val	332	6	u	km}} (volume equivalent)
mass

density

rotation	8.71 h
8.727 h
pole_ecliptic_lat	°
pole_ecliptic_lon	°
spectral_type	F/B
magnitude	9.9 to 13.0
abs_magnitude	6.35
albedo
geometric ( BV, UB)
mean_motion	/ day
observation_arc	110.8 yr
uncertainty	0

|access-date=19 Dec 2024}} (JD 2459396.5, heliocentric)

(volume equivalent)

8.727 h geometric ( BV, UB)

704 Interamnia is a large F-type asteroid. With a mean diameter of around 330 kilometres, it is the fifth-largest asteroid, after Ceres, Vesta, Pallas and Hygiea. Its mean distance from the Sun is 3.067 AU. It was discovered on 2 October 1910 by Vincenzo Cerulli, and named after the Latin name for Teramo, Italy, where Cerulli worked. Its mass is probably between fifth and tenth highest in the asteroid belt, with a mass estimated to be 1.2% of the mass of the entire asteroid belt. Observations by the Very Large Telescope's SPHERE imager in 2017–2019, combined with occultation results, indicate that the shape of Interamnia may be consistent with hydrostatic equilibrium for a body of its density with a rotational period of 7.6 hours. (Its current period is 8.7 hours.) This suggests that Interamnia may have formed as an equilibrium body, and that impacts changed its rotational period after it fully solidified.

Characteristics

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.

One of the first photographic plates of 704 Interamnia. The image was taken in Oct. 1910; the path of the asteroid is shown in the zoom.

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 until 2017–2019 there existed 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). Studies by the Very Large Telescope give an average diameter of about 332 km and found an ellipsoidal shape for Interamnia, similar to 4 Vesta; the resulting density calculation (1.98 ± 0.68 g·cm−3) is not precise enough to definitely infer Interamnia's composition, but the presence of hydrated materials at the surface and its overall spectral similarities to Ceres suggest that it is likely an icy body. The absence of an affiliated asteroid family implies that Interamnia has not suffered a giant impact within the past 3 billion years, in contrast to 4 Vesta and 10 Hygiea.

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.

Surface

There are no deep basins visible in the VLT images. Any large craters must have flat floors, consistent with an icy C/F-type composition.

Mass

In 2001, Michalak estimated Interamnia to have a mass of . Michalak's estimate depends on the masses of 19 Fortuna, 29 Amphitrite, and 16 Psyche; thus this mass was obtained assuming an incomplete dynamical model.

In 2011, Baer calculated Interamnia had a mass of .

Goffin's 2014 astrometric reanalysis gives an even lower mass of .

In 2019, Hanuš et al. consolidated 21 selected prior mass estimates, dating from 1992 to 2017, with a metastatistical result of (that is, to within 1 sigma uncertainty.

Gallery

File:Animation of 704 Interamnia orbit 2000-2020.gif|Animation of 704 Interamnia orbit 2000–2020

File:TESS observation of Interamnia.gif|The Transiting Exoplanet Survey Satellite (TESS) observed 704 Interamnia passing close to a target star, TIC 14802783, on 18/01/19.

Notes

References

|access-date = 2008-05-21

|doi-access=free

|access-date=2011-02-13 |archive-url=https://web.archive.org/web/20130702212735/http://home.earthlink.net/~jimbaer1/astmass.txt |archive-date=2013-07-02 |url-status=dead

|display-authors=etal

References

{{OED. interamnian
P. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. ''Astronomy & Astrophysics'' 54, A56
(2005). "High-Precision Ephemerides of Planets—EPM and Determination of Some Astronomical Constants". Solar System Research.
(2020). "(704) Interamnia: A transitional object between a dwarf planet and a typical irregular-shaped minor body". Astronomy & Astrophysics.
(2012). "The Geologically Recent Giant Impact Basins at Vesta's South Pole". Science.
(February 2020). "A basin-free spherical shape as an outcome of a giant impact on asteroid Hygiea". Nature Astronomy.
Hanuš et al. 2020
(2014). "Astrometric asteroid masses: A simultaneous determination". Astronomy & Astrophysics.

Info: Wikipedia Source

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