704 Interamnia

{{Infobox planet

| minorplanet=yes

| background=#D6D6D6

| name=704 Interamnia

| image=704 Interamnia VLT (2021), deconvolved.pdf

| image_size =

| caption=

| discoverer=Vincenzo Cerulli

| discovered=2 October 1910

| mpc_name=(704) Interamnia

| alt_names=1910 KU; 1952 MW

| pronounced={{IPAc-en|ɪ|n|t|ər|ˈ|æ|m|n|i|ə}}

| adjective=Interamnian {{IPAc-en|ɪ|n|t|ər|ˈ|æ|m|n|i|ə|n}}{{OED|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={{Convert|3.53|AU|Gm|abbr=on|lk=on}}

| perihelion={{Convert|2.58|AU|Gm|abbr=on}}

| semimajor={{Convert|3.056|AU|Gm|abbr=on}}

| 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{{citation needed|date=September 2021}}

| dimensions = {{val|362|x|348|x|310}} ± 8 km

| flattening = 0.14{{efn|1=Flattening derived from the maximum aspect ratio (c/a): $f=1-\frac{c}{a}$ , where (c/a) = {{val|.86|.03}}.}}

| mean_diameter={{val|332|5|u=km}}P. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. Astronomy & Astrophysics 54, A56

|mass={{val|35|5|e=18|u=kg}}
{{val|38|13|e=18|u=kg}}

|density={{val|1.84|.28|u=g/cm3}}
{{val|2.0|0.7|u=g/cm3}}

| rotation=8.71 h
8.727 h

|pole_ecliptic_lat={{val|62|5}}°

|pole_ecliptic_lon={{val|87|5}}°

| spectral_type=F/B

| magnitude=9.9 to 13.0

| abs_magnitude=6.35

| albedo={{val|.067}}
{{val|0.078|0.014}} geometric ({{val|0.645|0.014}} BV, {{val|0.259|0.021}} UB)

| mean_motion={{Deg2DMS|0.1845|sup=ms}} / day

| observation_arc=110.8 yr

| uncertainty=0

}}

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.{{Cite journal|url=http://iau-comm4.jpl.nasa.gov/EPM2004.pdf |doi=10.1007/s11208-005-0033-2 |title=High-Precision Ephemerides of Planets—EPM and Determination of Some Astronomical Constants |journal=Solar System Research |volume=39 |issue=3 |pages=176–186 |date=2005 |last1=Pitjeva |first1=E. V. |s2cid=120467483 |bibcode=2005SoSyR..39..176P |url-status=dead |archive-url=https://web.archive.org/web/20081031065523/http://iau-comm4.jpl.nasa.gov/EPM2004.pdf |archive-date=2008-10-31 }} 15 = 0.0124 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

File:Interamnia medie.gif

File:704 cerulli low.jpg

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,{{cite journal|arxiv=1911.13049|doi=10.1051/0004-6361/201936639|title=(704) Interamnia: A transitional object between a dwarf planet and a typical irregular-shaped minor body|year=2020|last1=Hanuš|first1=J.|last2=Vernazza|first2=P.|last3=Viikinkoski|first3=M.|last4=Ferrais|first4=M.|last5=Rambaux|first5=N.|last6=Podlewska-Gaca|first6=E.|last7=Drouard|first7=A.|last8=Jorda|first8=L.|last9=Jehin|first9=E.|last10=Carry|first10=B.|last11=Marsset|first11=M.|last12=Marchis|first12=F.|last13=Warner|first13=B.|last14=Behrend|first14=R.|last15=Asenjo|first15=V.|last16=Berger|first16=N.|last17=Bronikowska|first17=M.|last18=Brothers|first18=T.|last19=Charbonnel|first19=S.|last20=Colazo|first20=C.|last21=Coliac|first21=J.-F.|last22=Duffard|first22=R.|last23=Jones|first23=A.|last24=Leroy|first24=A.|last25=Marciniak|first25=A.|last26=Melia|first26=R.|last27=Molina|first27=D.|last28=Nadolny|first28=J.|last29=Person|first29=M.|last30=Pejcha|first30=O.|s2cid=208512707|journal=Astronomy & Astrophysics|volume=633|pages=A65|bibcode=2020A&A...633A..65H|display-authors=29}} in contrast to 4 Vesta and 10 Hygiea.{{Cite journal |s2cid = 206541950|doi = 10.1126/science.1223272|title = The Geologically Recent Giant Impact Basins at Vesta's South Pole|year = 2012|last1 = Schenk|first1 = P.|last2 = O'Brien|first2 = D. P.|last3 = Marchi|first3 = S.|last4 = Gaskell|first4 = R.|last5 = Preusker|first5 = F.|last6 = Roatsch|first6 = T.|last7 = Jaumann|first7 = R.|last8 = Buczkowski|first8 = D.|last9 = McCord|first9 = T.|last10 = McSween|first10 = H. Y.|last11 = Williams|first11 = D.|last12 = Yingst|first12 = A.|last13 = Raymond|first13 = C.|last14 = Russell|first14 = C.|journal = Science|volume = 336|issue = 6082|pages = 694–697|pmid = 22582256|bibcode = 2012Sci...336..694S}}{{cite journal |last1=Vernazza |first1=P. |last2=Jorda |first2=L. |last3=Ševeček |first3=P. |last4=Brož |first4=M. |last5=Viikinkoski |first5=M. |last6=Hanuš |first6=J. |last7=Carry |first7=B. |last8=Drouard |first8=A. |last9=Ferrais |first9=M. |last10=Marsset |first10=M. |last11=Marchis |first11=F. |last12=Birlan |first12=M. |last13=Podlewska-Gaca |first13=E. |last14=Jehin |first14=E. |last15=Bartczak |first15=P. |last16=Dudzinski |first16=G. |last17=Berthier |first17=J. |last18=Castillo-Rogez |first18=J. |last19=Cipriani |first19=F. |last20=Colas |first20=F. |last21=DeMeo |first21=F. |last22=Dumas |first22=C. |last23=Durech |first23=J. |last24=Fetick |first24=R. |last25=Fusco |first25=T. |last26=Grice |first26=J. |last27=Kaasalainen |first27=M. |last28=Kryszczynska |first28=A. |last29=Lamy |first29=P. |last30=Le Coroller |first30=H. |last31=Marciniak |first31=A. |last32=Michalowski |first32=T. |last33=Michel |first33=P. |last34=Rambaux |first34=N. |last35=Santana-Ros |first35=T. |last36=Tanga |first36=P. |last37=Vachier |first37=F. |last38=Vigan |first38=A. |last39=Witasse |first39=O. |last40=Yang |first40=B. |last41=Gillon |first41=M. |last42=Benkhaldoun |first42=Z. |last43=Szakats |first43=R. |last44=Hirsch |first44=R. |last45=Duffard |first45=R. |last46=Chapman |first46=A. |last47=Maestre |first47=J. L. |title=A basin-free spherical shape as an outcome of a giant impact on asteroid Hygiea |journal=Nature Astronomy |date=February 2020 |volume=4 |issue=2 |pages=136–141 |doi=10.1038/s41550-019-0915-8 |bibcode=2020NatAs...4..136V |hdl=10261/204968 |s2cid=209938346 |url=https://www.eso.org/public/archives/releases/sciencepapers/eso1918/eso1918a.pdf |access-date=March 30, 2022}}

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.Hanuš et al. 2020

Mass

In 2001, Michalak estimated Interamnia to have a mass of {{val|7|2|e=19|u=kg}}. 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 {{val|3.9|.2|e=19|u=kg}}.

Goffin's 2014 astrometric reanalysis gives an even lower mass of {{val|2.7|0.1|e=19|u=kg}}.{{cite journal|arxiv=1402.4241|last1=Goffin|first1=Edwin|s2cid=118444915|title=Astrometric asteroid masses: A simultaneous determination|date=2014|doi=10.1051/0004-6361/201322766|volume=565|journal=Astronomy & Astrophysics|page=A56|bibcode=2014A&A...565A..56G}}

In 2019, Hanuš et al. consolidated 21 selected prior mass estimates, dating from 1992 to 2017, with a metastatistical result of {{val|3.8|1.3|e=19|u=kg}} (that is, {{val|2.5|to|5.1|e=19|u=kg}} to within 1 sigma uncertainty.

Gallery

File:Animation of 704 Interamnia orbit 2000-2020.gif|Animation of 704 Interamnia{{'s}} orbit 2000–2020
{{legend2|yellow|Sun}}{{·}}{{legend2| RoyalBlue|Earth}}{{·}}{{legend2|Gold|Mars}}{{·}}{{legend2|Lime|Jupiter}}{{·}}{{legend2|Magenta|704 Interamnia}}

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

{{reflist|refs=

{{cite web

|title = Bright Minor Planets 2007

|publisher = Minor Planet Center

|url = http://www.cfa.harvard.edu/iau/Ephemerides/Bright/2007

|access-date = 2008-05-21

}}{{Dead link|date=August 2018 |bot=InternetArchiveBot |fix-attempted=yes }}

{{cite journal

|last=Michalak

|first=G.

|title=Determination of asteroid masses

|journal=Astronomy & Astrophysics

|volume=374

|issue=2

|pages=703–711

|date=2001

|doi=10.1051/0004-6361:20010731

|bibcode=2001A&A...374..703M

|doi-access=free

}}

{{cite web

|date=2010

|title=Recent Asteroid Mass Determinations

|publisher=Personal Website

|first=James

|last=Baer

|url=http://home.earthlink.net/~jimbaer1/astmass.txt

|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

}}

{{cite journal

|display-authors=etal

|first1=J. |last1=Hanuš

|first2=P. |last2=Vernazza

|first3=M. |last3=Viikinkoski

|first4=M. |last4=Ferrais

|first5=N. |last5=Rambaux

|first6=E. |last6=Podlewska-Gaca

|s2cid=208512707 |title=(704) Interamnia: A transitional object between a dwarf planet and a typical irregular-shaped minor body

|bibcode=2020A&A...633A..65H }}

}}

External links

[http://physics.bgsu.edu/~layden/Anim/Asteroids/interamnia.htm Animation of Asteroid Interamnia] taken on 1 & 2 April 2003
[http://iota.jhuapl.edu/mp704d17.htm Interamnia Occultations Observed before 2003]
[http://adsabs.harvard.edu/abs/1997DPS....29.0710B Occultation of GSC 23450183] by {{mp|704 Interamnia}} on 17 December 1996
[https://web.archive.org/web/20070109172809/http://uchukan.satsumasendai.jp/data/occult/limovie/0303intera-study.html Occultation of HIP36189] by {{mp|704 Interamnia}} on 23 March 2003
[https://arxiv.org/abs/1911.13049 (704) Interamnia: A transition object between a dwarf planet and a typical irregular-shaped minor body]
{{AstDys|704}}
{{JPL small body}}

Category:Background asteroids

Interamnia

Category:F-type asteroids (Tholen)

Category:B-type asteroids (SMASS)

19101002

Category:Objects observed by stellar occultation

Category:Possible dwarf planets

704&nbsp;Interamnia