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{{Short description|Large asteroid in the asteroid belt}}
⚫
{{Use dmy dates|date=October 2019}}
{{Infobox planet
{{Infobox planet
| minorplanet=yes
| minorplanet=yes
| background=#D6D6D6
| background=#D6D6D6
| name=704 Interamnia
| name=704 Interamnia
| image=SPHERE image of Interamnia.jpg
| image=704 Interamnia VLT (2021), deconvolved.pdf
| image_size = 250
| image_size =
| caption=[[VLT-SPHERE]] image of Interamnia
| caption=
| discoverer=[[Vincenzo Cerulli]]
| discoverer=[[Vincenzo Cerulli]]
| discovered=2 October 1910
| discovered=2 October 1910
Line 14: Line 16:
| named_after=[[Teramo]]
| named_after=[[Teramo]]
| mp_category=[[Asteroid belt|Main belt]]
| mp_category=[[Asteroid belt|Main belt]]
| orbit_ref=<ref name=jpldata/>
| orbit_ref = <ref name=JPL>[https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=Interamnia JPL data] Retrieved 2021-09-29</ref>
| epoch=31 July 2016 ([[Julian day|JD]] 2457600.5)
| epoch=July 01, 2021 <br />([[Julian day|JD]] 2459396.5, heliocentric)
| aphelion={{Convert|3.5293|AU|Gm|abbr=on|lk=on}}
| aphelion={{Convert|3.53|AU|Gm|abbr=on|lk=on}}
| perihelion={{Convert|2.5857|AU|Gm|abbr=on}}
| perihelion={{Convert|2.58|AU|Gm|abbr=on}}
| semimajor={{Convert|3.0575|AU|Gm|abbr=on}}
| semimajor={{Convert|3.056|AU|Gm|abbr=on}}
| eccentricity=0.15431
| eccentricity=0.155
| period=5.35 [[Julian year (astronomy)|yr]] (1952.8 [[Julian year (astronomy)|d]])
| period=5.34 [[Julian year (astronomy)|yr]] (1951 [[Julian year (astronomy)|d]])
| inclination=17.309°
| inclination=17.31°
| asc_node=280.30°
| asc_node=280.3°
| arg_peri=95.208°
| arg_peri=94.8°
| mean_anomaly=276.11[[Degree (angle)|°]]
| mean_anomaly=248°
| avg_speed=16.92 km/s
| avg_speed=16.92 km/s{{citation needed|date=September 2021}}
| dimensions={{val|362|x|348|x|310}} ± 8 km<ref name="Hanus2019"/>
| dimensions=c/a = {{val|.86|.03}}<ref name=VLT/><br />{{val|362|x|348|x|310}} ± 8 km<ref name="Hanus2019"/>
| mean_diameter={{val|332|5|u=km}}<ref name=VLT>P. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. ''Astronomy & Astrophysics'' 54, A56</ref>
| mean_diameter={{val|332|6|u=km}} {{small|(volume equivalent)}}<ref name="Hanus2019"/>
|mass={{val|3.79|1.28|e=19|u=kg}}<ref name="Hanus2019"/>
<br />{{val|332|6|u=km}} {{small|(volume equivalent)}}<ref name="Hanus2019"/>
|density={{val|1.98|0.68|u=g/cm3}}<ref name="Hanus2019"/>
|mass={{val|35|5|e=18|u=kg}}<ref name=VLT/><br />{{val|38|13|e=18|u=kg}}<ref name="Hanus2019"/>
| rotation=8.712336 [[hour|h]]<ref name="Hanus2019"/>
|density={{val|1.84|.28|u=g/cm3}}<ref name=VLT/><br />{{val|2.0|0.7|u=g/cm3}}<ref name="Hanus2019"/>
| rotation=8.71 [[hour|h]]<ref name="Hanus2019"/>
|pole_ecliptic_lat={{val|62|5}}°
|pole_ecliptic_lat={{val|62|5}}°
|pole_ecliptic_lon={{val|87|5}}°
|pole_ecliptic_lon={{val|87|5}}°
| spectral_type=[[F-type asteroid|F]]/[[B-type asteroid|B]]<ref name=jpldata/>
| spectral_type=[[F-type asteroid|F]]/[[B-type asteroid|B]]<ref name=JPL/>
| magnitude=9.9 to 13.0<ref name=bright2007/>
| magnitude=9.9 to 13.0<ref name=bright2007/>
| abs_magnitude=5.94<ref name=jpldata/>
| abs_magnitude=6.38<ref name=JPL/>
| albedo={{val|0.0742|0.002}}<ref name=jpldata/>
| albedo={{val|.067}}<ref name=VLT/><br />{{val|0.078|0.014}} geometric ({{val|0.645|0.014}} BV, {{val|0.259|0.021}} UB)<ref name=JPL/>
| mean_motion={{Deg2DMS|0.18435|sup=ms}} / day
| mean_motion={{Deg2DMS|0.1845|sup=ms}} / day
| observation_arc=102.38 yr (37395 d)
| observation_arc=110.8 yr
| uncertainty=0
| uncertainty=0
}}
}}


'''704 Interamnia''' is a large [[F-type asteroid]]. With an estimated mean diameter of 330 kilometres, it is the [[List_of_exceptional_asteroids|fifth-largest asteroid]] after [[Ceres (dwarf planet)|Ceres]], [[4 Vesta|Vesta]], [[2 Pallas|Pallas]], and [[10 Hygiea|Hygiea]]. Its mean distance from the [[Sun]] is 3.067 ([[astronomical unit|AU]]). It was discovered on 2 October 1910 by [[Vincenzo Cerulli]], and named after the [[Latin]] name for [[Teramo]], [[Italy]], where Cerulli worked. It is probably the fifth-to-eighth-[[List of exceptional asteroids#Largest by mass|most-massive asteroid]], with a mass estimated to be 1.2% of the mass of the entire asteroid belt.<ref>{{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 |archiveurl=https://web.archive.org/web/20081031065523/http://iau-comm4.jpl.nasa.gov/EPM2004.pdf |archivedate=2008-10-31 }} 15 = 0.0124</ref> Observations by the [[Very Large Telescope]]'s [[VLT-SPHERE|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 equilibrim body, and that impacts changed its rotational period after it fully solidified.<ref name="Hanus2019"/>
'''704 Interamnia''' is a large [[F-type asteroid]]. With a [[mean diameter]] of around 330 kilometres, it is the [[List of exceptional asteroids|fifth-largest asteroid]], after [[Ceres (dwarf planet)|Ceres]], [[4 Vesta|Vesta]], [[2 Pallas|Pallas]] and [[10 Hygiea|Hygiea]]. Its mean distance from the [[Sun]] is 3.067 [[astronomical unit|AU]]. It was discovered on 2 October 1910 by [[Vincenzo Cerulli]], and named after the [[Latin]] name for [[Teramo]], [[Italy]], where Cerulli worked. Its [[List of exceptional asteroids#Largest by mass|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.<ref>{{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</ref> Observations by the [[Very Large Telescope]]'s [[VLT-SPHERE|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.<ref name="Hanus2019"/>


==Characteristics==
==Characteristics==
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[[File:704 cerulli low.jpg|thumb|left|upright|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.]]
[[File:704 cerulli low.jpg|thumb|left|upright|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 [[List of exceptional asteroids#Largest by diameter|"big four"]], it is a very little-studied body. It is easily the largest of the [[F-type asteroid]]s, 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,<ref>{{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}}</ref> in contrast to 4 Vesta and 10 Hygeia.<ref>{{Cite journal | url=https://www.semanticscholar.org/paper/The-geologically-recent-giant-impact-basins-at-Schenk-O'brien/c4022b20a7042ae75992b87a27cfa1e853cfbbb1 |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}}</ref><ref>https://www.eso.org/public/archives/releases/sciencepapers/eso1918/eso1918a.pdf</ref>
Although Interamnia is the largest asteroid after the [[List of exceptional asteroids#Largest by diameter|"big four"]], it is a very little-studied body. It is easily the largest of the [[F-type asteroid]]s, 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&nbsp;km and found an ellipsoidal shape for Interamnia, similar to 4 Vesta; the resulting density calculation (1.98 ± 0.68 g·cm<sup>−3</sup>) 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,<ref>{{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}}</ref> in contrast to 4 Vesta and 10 Hygiea.<ref>{{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}}</ref><ref>{{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}}</ref>


Its very dark surface and relatively large distance from the Sun means Interamnia can never be seen with 10x50 [[binoculars]]. At most [[opposition (astronomy and astrology)|oppositions]] its [[apparent magnitude|magnitude]] is around +11.0, which is less than the ''minimum'' brightness of Vesta, Ceres or Pallas. Even at a [[Apsis|perihelic]] opposition its magnitude is only +9.9,<ref name=bright2007/> which is over four magnitudes lower than Vesta.
Its very dark surface and relatively large distance from the Sun means Interamnia can never be seen with 10x50 [[binoculars]]. At most [[opposition (astronomy and astrology)|oppositions]] its [[apparent magnitude|magnitude]] is around +11.0, which is less than the ''minimum'' brightness of Vesta, Ceres or Pallas. Even at a [[Apsis|perihelic]] opposition its magnitude is only +9.9,<ref name=bright2007/> which is over four magnitudes lower than Vesta.

Its orbit is slightly more eccentric than that of Hygiea (15% versus 12%) but differs from Hygiea's in its much greater [[inclination]] and slightly shorter period. Another difference is that Interamnia's perihelion is located on the opposite side from 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, 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.


==Surface==
==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.<ref>Hanuš et al. 2020</ref>
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.<ref>Hanuš et al. 2020</ref>


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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.<ref name=Michalak2001/>
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.<ref name=Michalak2001/>


In 2011, Baer calculated Interamnia had a mass of {{val|3.9|.2|e=19|u=kg}}.<ref name=Baer/>
In 2011, Baer calculated Interamnia had a mass of {{val|3.9|.2|e=19|u=kg}}.<ref name=Baer/>


Goffin's 2014 astrometric reanalysis gives an even lower mass of {{val|2.7|0.1|e=19|u=kg}}.<ref>{{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}}</ref>
Goffin's 2014 astrometric reanalysis gives an even lower mass of {{val|2.7|0.1|e=19|u=kg}}.<ref>{{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}}</ref>
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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.<ref name="Hanus2019"/>
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.<ref name="Hanus2019"/>


==Gallery==
⚫
[[File:Animation of 704 Interamnia orbit 2000-2020.gif|thumb|left|Animation of 704 Interamnia{{'s}} orbit 2000-2020<br>{{legend2| yellow| Sun}}{{legend2| RoyalBlue| Earth}}{{·}}{{legend2| Gold| Mars}}{{·}}{{legend2| Lime|Jupiter}}{{·}}{{legend2| Magenta| 704 Interamnia}}]]
<gallery mode="packed" heights="150px">

⚫
File:Animation of 704 Interamnia orbit 2000-2020.gif|Animation of 704 Interamnia{{'s}} orbit 2000-2020<br />{{legend2|yellow|Sun}}{{·}}{{legend2| RoyalBlue|Earth}}{{·}}{{legend2|Gold|Mars}}{{·}}{{legend2|Lime|Jupiter}}{{·}}{{legend2|Magenta|704 Interamnia}}
[[File:TESS observation of Interamnia.gif|thumb|right|The Transiting Exoplanet Survey Satellite (TESS) observed 704 Interamnia passing close to a target star, TIC 14802783, on 18/01/19.]]
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.

</gallery>
{{clear}}


==See also==
==See also==
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{{reflist|refs=
{{reflist|refs=


<!-- Not in use
<ref name=jpldata>{{cite web
<ref name=jpldata>{{cite web
|type=2008-04-14 last obs
|type=2008-04-14 last obs
|title=JPL Small-Body Database Browser: 704 Interamnia (1910 KU)
|title=JPL Small-Body Database Browser: 704 Interamnia (1910 KU)
|url=https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=704
|url=https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=704
|accessdate=7 May 2016}}</ref>
|access-date=7 May 2016}}</ref>
Not in use-->


<ref name=bright2007>{{cite web
<ref name=bright2007>{{cite web
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|publisher = [[Minor Planet Center]]
|publisher = [[Minor Planet Center]]
|url = http://www.cfa.harvard.edu/iau/Ephemerides/Bright/2007
|url = http://www.cfa.harvard.edu/iau/Ephemerides/Bright/2007
|accessdate = 2008-05-21
|access-date = 2008-05-21
}}{{Dead link|date=August 2018 |bot=InternetArchiveBot |fix-attempted=yes }}</ref>
}}{{Dead link|date=August 2018 |bot=InternetArchiveBot |fix-attempted=yes }}</ref>


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|doi-access=free
|doi-access=free
}}</ref>
}}</ref>




<ref name=Baer>
<ref name=Baer>
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|last=Baer
|last=Baer
|url=http://home.earthlink.net/~jimbaer1/astmass.txt
|url=http://home.earthlink.net/~jimbaer1/astmass.txt
|accessdate=2011-02-13
|access-date=2011-02-13
|archive-url=https://web.archive.org/web/20130702212735/http://home.earthlink.net/~jimbaer1/astmass.txt
|archive-url=https://web.archive.org/web/20130702212735/http://home.earthlink.net/~jimbaer1/astmass.txt
|archive-date=2013-07-02
|archive-date=2013-07-02
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== External links ==
== External links ==
* [http://physics.bgsu.edu/~layden/Anim/Asteroids/interamnia.htm Animation of Asteroid Interamnia] taken on April 1 & 2, 2003
* [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://iota.jhuapl.edu/mp704d17.htm Interamnia Occultations Observed before 2003]
* [http://adsabs.harvard.edu/abs/1997DPS....29.0710B Occultation of GSC 23450183] by {{|704 Interamnia}} on 17 December 1996
* [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 {{|704 Interamnia}} on 23 March 2003
* [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]
* [https://arxiv.org/abs/1911.13049 (704) Interamnia: A transition object between a dwarf planet and a typical irregular-shaped minor body]
* {{AstDys|704}}
* {{AstDys|704}}
* {{JPL small body}}
* {{JPL small body}}


⚫
{{Use day dates|date=October 2019}}
{{Minor planets navigator |703 Noëmi |number=704 |705 Erminia}}
{{Minor planets navigator |703 Noëmi |number=704 |705 Erminia}}
{{Large asteroids}}
{{Small Solar System bodies}}
{{Small Solar System bodies}}
{{Authority control}}


{{DEFAULTSORT 000704}}
{{DEFAULTSORT:000704}}
[[Category Background asteroids]]
[[Category:Background asteroids]]
[[Category Discoveries by Vincenzo Cerulli|Interamnia]]
[[Category:Discoveries by Vincenzo Cerulli|Interamnia]]
[[Category Minor planets named for places|Interamnia]]
[[Category:Named minor planets|Interamnia]]
[[Category Named minor planets|Interamnia]]
[[Category:F-type asteroids (Tholen)]]
[[Category F-type asteroids (Tholen)]]
[[Category:B-type asteroids (SMASS)]]
[[Category B-type asteroids (SMASS)]]
[[Category:1910 in science|19101002]]
[[Category:1910 in science|19101002]]
[[Category Astronomical objects discovered in 1910|19101002]]
[[Category:Astronomical objects discovered in 1910|19101002]]
[[Category Objects observed by stellar occultation]]
[[Category:Objects observed by stellar occultation]]
[[Category:Possible dwarf planets]]
[[Category:Possible dwarf planets]]

Latest revision as of 23:36, 25 July 2024

704 Interamnia
Discovery
Discovered byVincenzo Cerulli
Discovery date2 October 1910
Designations
(704) Interamnia
Pronunciation/ɪntərˈæmniə/[1]
Named after
Teramo
1910 KU; 1952 MW
Main belt
AdjectivesInteramnian /ɪntərˈæmniən/[1]
Orbital characteristics[2]
Epoch July 01, 2021
(JD 2459396.5, heliocentric)
Uncertainty parameter 0
Observation arc110.8 yr
Aphelion3.53 AU (528 Gm)
Perihelion2.58 AU (386 Gm)
3.056 AU (457.2 Gm)
Eccentricity0.155
5.34 yr (1951 d)
16.92 km/s[citation needed]
248°
0° 11m 4.2s / day
Inclination17.31°
280.3°
94.8°
Physical characteristics
Dimensionsc/a = 0.86±0.03[3]
362 × 348 × 310 ± 8 km[4]
332±5 km[3]
332±6 km (volume equivalent)[4]
Mass(35±5)×1018 kg[3]
(38±13)×1018 kg[4]
Mean density
1.84±0.28 g/cm3[3]
2.0±0.7 g/cm3[4]
8.71 h[4]
62±5°
87±5°
0.067[3]
0.078±0.014 geometric (0.645±0.014 BV, 0.259±0.021 UB)[2]
F/B[2]
9.9 to 13.0[5]
6.38[2]

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.[6] 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.[4]

Characteristics

[edit]
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,[7] in contrast to 4 Vesta and 10 Hygiea.[8][9]

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,[5] which is over four magnitudes lower than Vesta.

Surface

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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.[10]

Mass

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In 2001, Michalak estimated Interamnia to have a mass of (7±2)×1019 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.[11]

In 2011, Baer calculated Interamnia had a mass of (3.9±0.2)×1019 kg.[12]

Goffin's 2014 astrometric reanalysis gives an even lower mass of (2.7±0.1)×1019 kg.[13]

In 2019, Hanuš et al. consolidated 21 selected prior mass estimates, dating from 1992 to 2017, with a metastatistical result of (3.8±1.3)×1019 kg (that is, (2.5 to 5.1)×1019 kg to within 1 sigma uncertainty.[4]

[edit]
  • Animation of 704 Interamnia's orbit 2000-2020   Sun ·   Earth ·   Mars ·   Jupiter ·   704 Interamnia
    Animation of 704 Interamnia's orbit 2000-2020
      Sun ·   Earth ·   Mars ·   Jupiter ·   704 Interamnia
  • The Transiting Exoplanet Survey Satellite (TESS) observed 704 Interamnia passing close to a target star, TIC 14802783, on 18/01/19.
    The Transiting Exoplanet Survey Satellite (TESS) observed 704 Interamnia passing close to a target star, TIC 14802783, on 18/01/19.

See also

[edit]

References

[edit]
  1. ^ a b "interamnian". Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
  2. ^ a b c d JPL data Retrieved 2021-09-29
  3. ^ a b c d e P. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. Astronomy & Astrophysics 54, A56
  4. ^ a b c d e f g Hanuš, J.; Vernazza, P.; Viikinkoski, M.; Ferrais, M.; Rambaux, N.; Podlewska-Gaca, E.; et al. (2020). "(704) Interamnia: A transitional object between a dwarf planet and a typical irregular-shaped minor body". Astronomy & Astrophysics. 633: A65. arXiv:1911.13049. Bibcode:2020A&A...633A..65H. doi:10.1051/0004-6361/201936639. S2CID 208512707.
  5. ^ a b "Bright Minor Planets 2007". Minor Planet Center. Retrieved 21 May 2008.[permanent dead link]
  6. ^ Pitjeva, E. V. (2005). "High-Precision Ephemerides of Planets—EPM and Determination of Some Astronomical Constants" (PDF). Solar System Research. 39 (3): 176–186. Bibcode:2005SoSyR..39..176P. doi:10.1007/s11208-005-0033-2. S2CID 120467483. Archived from the original (PDF) on 31 October 2008. 15 = 0.0124
  7. ^ Hanuš, J.; Vernazza, P.; Viikinkoski, M.; Ferrais, M.; Rambaux, N.; Podlewska-Gaca, E.; Drouard, A.; Jorda, L.; Jehin, E.; Carry, B.; Marsset, M.; Marchis, F.; Warner, B.; Behrend, R.; Asenjo, V.; Berger, N.; Bronikowska, M.; Brothers, T.; Charbonnel, S.; Colazo, C.; Coliac, J.-F.; Duffard, R.; Jones, A.; Leroy, A.; Marciniak, A.; Melia, R.; Molina, D.; Nadolny, J.; Person, M.; et al. (2020). "(704) Interamnia: A transitional object between a dwarf planet and a typical irregular-shaped minor body". Astronomy & Astrophysics. 633: A65. arXiv:1911.13049. Bibcode:2020A&A...633A..65H. doi:10.1051/0004-6361/201936639. S2CID 208512707.
  8. ^ Schenk, P.; O'Brien, D. P.; Marchi, S.; Gaskell, R.; Preusker, F.; Roatsch, T.; Jaumann, R.; Buczkowski, D.; McCord, T.; McSween, H. Y.; Williams, D.; Yingst, A.; Raymond, C.; Russell, C. (2012). "The Geologically Recent Giant Impact Basins at Vesta's South Pole". Science. 336 (6082): 694–697. Bibcode:2012Sci...336..694S. doi:10.1126/science.1223272. PMID 22582256. S2CID 206541950.
  9. ^ Vernazza, P.; Jorda, L.; Ševeček, P.; Brož, M.; Viikinkoski, M.; Hanuš, J.; Carry, B.; Drouard, A.; Ferrais, M.; Marsset, M.; Marchis, F.; Birlan, M.; Podlewska-Gaca, E.; Jehin, E.; Bartczak, P.; Dudzinski, G.; Berthier, J.; Castillo-Rogez, J.; Cipriani, F.; Colas, F.; DeMeo, F.; Dumas, C.; Durech, J.; Fetick, R.; Fusco, T.; Grice, J.; Kaasalainen, M.; Kryszczynska, A.; Lamy, P.; Le Coroller, H.; Marciniak, A.; Michalowski, T.; Michel, P.; Rambaux, N.; Santana-Ros, T.; Tanga, P.; Vachier, F.; Vigan, A.; Witasse, O.; Yang, B.; Gillon, M.; Benkhaldoun, Z.; Szakats, R.; Hirsch, R.; Duffard, R.; Chapman, A.; Maestre, J. L. (February 2020). "A basin-free spherical shape as an outcome of a giant impact on asteroid Hygiea" (PDF). Nature Astronomy. 4 (2): 136–141. Bibcode:2020NatAs...4..136V. doi:10.1038/s41550-019-0915-8. hdl:10261/204968. S2CID 209938346. Retrieved 30 March 2022.
  10. ^ Hanuš et al. 2020
  11. ^ Michalak, G. (2001). "Determination of asteroid masses". Astronomy & Astrophysics. 374 (2): 703–711. Bibcode:2001A&A...374..703M. doi:10.1051/0004-6361:20010731.
  12. ^ Baer, James (2010). "Recent Asteroid Mass Determinations". Personal Website. Archived from the original on 2 July 2013. Retrieved 13 February 2011.
  13. ^ Goffin, Edwin (2014). "Astrometric asteroid masses: A simultaneous determination". Astronomy & Astrophysics. 565: A56. arXiv:1402.4241. Bibcode:2014A&A...565A..56G. doi:10.1051/0004-6361/201322766. S2CID 118444915.
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