3 Juno: Difference between revisions

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{{Short description|Asteroid in the asteroid belt}}
{{Short description|Stony main-belt asteroid}}
{{Other uses|Juno (disambiguation){{!}}Juno}}
{{Other uses|Juno (disambiguation){{!}}Juno}}
{{Use dmy dates|date=September 2025}}
{{Infobox planet
{{Infobox planet
| minorplanet = yes
| minorplanet = yes
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| symbol = [[File:Juno symbol (bold).svg|24px|⚵]] (historically astronomical, now astrological)
| symbol = [[File:Juno symbol (bold).svg|24px|⚵]] (historically astronomical, now astrological)
| image = 3 Juno VLT (2021).png
| image = 3 Juno VLT (2021).png
| image_size =
| caption =  
| caption =  
| discoverer = [[Karl Ludwig Harding]]
| discoverer = [[Karl Ludwig Harding]]
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| alt_names =  
| alt_names =  
| pronounced = {{IPAc-en|ˈ|dʒ|uː|n|oʊ}} {{respell|JOO|noh}}<ref>{{dict.com|Juno}}</ref>
| pronounced = {{IPAc-en|ˈ|dʒ|uː|n|oʊ}} {{respell|JOO|noh}}<ref>{{dict.com|Juno}}</ref>
| adjectives = Junonian {{IPAc-en|dʒ|uː|ˈ|n|oʊ|n|i|ə|n}}<ref name=OED>{{OED|Junonian}}</ref>
| adjectives = Junonian {{IPAc-en|dʒ|uː|ˈ|n|oʊ|n|i|ə|n}}<ref name="OED">{{OED|Junonian}}</ref>
| named_after = [[Juno (mythology)|Juno]] ({{langx|la|Iūno}})
| named_after = [[Juno (mythology)|Juno]] ({{langx|la|Iūno}})
| mp_category = [[Main belt]] ([[Juno clump]])
| mp_category = [[Main belt]] ([[Juno clump]])
| orbit_ref = <ref name="jpldata" />
| orbit_ref = <ref name="jpldata" />
| epoch = 13&nbsp;September 2023<br/>([[Julian day|JD]]&nbsp;2453300.5)
| epoch = 13&nbsp;September 2023<br>([[Julian day|JD]]&nbsp;2453300.5)
| semimajor = {{Convert|2.67|AU|e6km|abbr=unit}}
| semimajor = {{Convert|2.67|AU|e6km|abbr=unit}}
| perihelion = {{Convert|1.985|AU|e6km|abbr=unit}}
| perihelion = {{Convert|1.985|AU|e6km|abbr=unit}}
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| perihelion_rate = 43.635655
| perihelion_rate = 43.635655
| node_rate = −61.222138
| node_rate = −61.222138
| dimensions = (288 × 250 × 225) ± 5&nbsp;km<ref name=VLT/><br>(320 × 267 × 200) ± 6&nbsp;km<ref name="Baer">
| dimensions = (288 × 250 × 225) ± 5&nbsp;km<ref name="VLT" /><br>(320 × 267 × 200) ± 6&nbsp;km<ref name="Baer">
{{cite web
{{cite web
   |date=2008
   |date=2008
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   }}
   }}
</ref>
</ref>
| mean_diameter = {{val|254|2|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><br>{{val|246.596|10.594|u=km}}<ref name="jpldata"/>
| mean_diameter = {{val|254|2|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><br>{{val|246.596|10.594|u=km}}<ref name="jpldata" />
| mass = {{val|2.7|0.24|e=19|u=kg}}{{efn|Composite estimate.}}<ref name=VLT/><br>{{val|2.86|0.46|e=19|u=kg}}<ref name="Baer2011">James Baer, Steven Chesley & Robert Matson (2011) "Astrometric masses of 26 asteroids and observations on asteroid porosity." ''The Astronomical Journal'', Volume 141, Number 5</ref>{{refn|group=lower-alpha|(1.44 ± 0.23){{e|−11}} {{Solar mass}}}}
| mass = {{val|2.7|0.24|e=19|u=kg}}{{efn|Composite estimate.}}<ref name="VLT" /><br>{{val|2.86|0.46|e=19|u=kg}}<ref name="Baer2011">James Baer, Steven Chesley & Robert Matson (2011) "Astrometric masses of 26 asteroids and observations on asteroid porosity." ''The Astronomical Journal'', Volume 141, Number 5</ref>{{refn|group=lower-alpha|(1.44 ± 0.23){{e|−11}} {{Solar mass}}}}
| density = {{val|3.15|0.28|u=g/cm3}}<ref name=VLT/><br>{{val|3.20|0.56|u=g/cm3}}<ref name="Baer2011"/>
| density = {{val|3.15|0.28|u=g/cm3}}<ref name="VLT" /><br>{{val|3.20|0.56|u=g/cm3}}<ref name="Baer2011" />
| surface_grav = {{cvt|0.112|m/s2|g0|lk=out}}
| surface_grav = {{cvt|0.112|m/s2|g0|lk=out}}
| escape_velocity = {{V2|0.027|127}}&nbsp;km/s
| escape_velocity = {{V2|0.027|127}}&nbsp;km/s
| rotation = 7.21 hr<ref name="jpldata"/> (0.3004 d)<ref name="lc">
| rotation = 7.21 hr<ref name="jpldata" /> (0.3004 d)<ref name="lc">
  {{cite web
  {{cite web
  |editor-last=Harris  
  |editor-last=Harris  
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  |url-status=dead
  |url-status=dead
}}</ref>
}}</ref>
| spectral_type = [[S-type asteroid|S]]<ref name="jpldata"/><ref name="tax">{{cite web | editor-last= Neese | editor-first= C. | title= Asteroid Taxonomy.EAR-A-5-DDR-TAXONOMY-V5.0. |  publisher= [[Planetary Data System|NASA Planetary Data System]] | date= 2005 | url= http://www.psi.edu/pds/asteroid/EAR_A_5_DDR_TAXONOMY_V5_0/data/taxonomy05.tab | archive-url= https://web.archive.org/web/20060905083536/http://www.psi.edu/pds/asteroid/EAR_A_5_DDR_TAXONOMY_V5_0/data/taxonomy05.tab | url-status= dead | archive-date= 2006-09-05 | access-date= 2013-12-24}}</ref>
| spectral_type = [[S-type asteroid|S]]<ref name="jpldata" /><ref name="tax">{{cite web | editor-last= Neese | editor-first= C. | title= Asteroid Taxonomy. EAR-A-5-DDR-TAXONOMY-V5.0. |  publisher= [[Planetary Data System|NASA Planetary Data System]] | date= 2005 | url= http://www.psi.edu/pds/asteroid/EAR_A_5_DDR_TAXONOMY_V5_0/data/taxonomy05.tab | archive-url= https://web.archive.org/web/20060905083536/http://www.psi.edu/pds/asteroid/EAR_A_5_DDR_TAXONOMY_V5_0/data/taxonomy05.tab | url-status= dead | archive-date= 2006-09-05 | access-date= 2013-12-24}}</ref>
| rot_velocity = 31.75 m/s{{efn|name="fact2"|Calculated based on the known parameters}}
| rot_velocity = 31.75 m/s{{efn|name="fact2"|Calculated based on the known parameters}}
| magnitude = 7.4<ref name="AstDys-Juno">{{cite web
| magnitude = 7.4<ref name="AstDys-Juno">{{cite web
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  |url-status=live
  |url-status=live
  }}</ref><ref name="bright2005">{{cite web |title=Bright Minor Planets 2005 |publisher=[[Minor Planet Center]]|url=http://www.cfa.harvard.edu/iau/Ephemerides/Bright/2005 |url-status=dead |archive-url=https://web.archive.org/web/20080929074506/http://www.cfa.harvard.edu/iau/Ephemerides/Bright/2005/ |archive-date=2008-09-29}}</ref> to 11.55
  }}</ref><ref name="bright2005">{{cite web |title=Bright Minor Planets 2005 |publisher=[[Minor Planet Center]]|url=http://www.cfa.harvard.edu/iau/Ephemerides/Bright/2005 |url-status=dead |archive-url=https://web.archive.org/web/20080929074506/http://www.cfa.harvard.edu/iau/Ephemerides/Bright/2005/ |archive-date=2008-09-29}}</ref> to 11.55
| abs_magnitude = 5.33<ref name="jpldata"/><ref name="iras">
| abs_magnitude = 5.33<ref name="jpldata" /><ref name="iras">
  {{cite web
  {{cite web
  |editor-last=Davis  
  |editor-last=Davis  
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  |url-status=dead
  |url-status=dead
}}</ref>
}}</ref>
| pole_ecliptic_lat = 27° ± 5°<ref name="kaasalainen2002"/>
| pole_ecliptic_lat = 27° ± 5°<ref name="kaasalainen2002" />
| pole_ecliptic_lon = 103° ± 5°<ref name="kaasalainen2002"/>
| pole_ecliptic_lon = 103° ± 5°<ref name="kaasalainen2002" />
| albedo = 0.202<ref name=VLT/><br>0.238<ref name="jpldata"/><ref name="iras" />
| albedo = 0.202<ref name="VLT" /><br>0.238<ref name="jpldata" /><ref name="iras" />
| angular_size = 0.30" <!-- Horizons 2018-Oct-28 --> to 0.07"
| angular_size = 0.30" <!-- Horizons 2018-Oct-28 --> to 0.07"
| single_temperature = ~163 [[kelvin|K]]<br />''max:'' 301 K (+28°C)<ref name="lim2005">
| single_temperature = ~163 [[kelvin|K]]<br>''max:'' 301 K (+28°C)<ref name="lim2005">
  {{cite journal
  {{cite journal
  | last= Lim | first= Lucy F.
  | last= Lim | first= Lucy F.
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}}
}}


'''Juno''' ([[minor-planet designation]]: '''3 Juno''') is a large [[asteroid]] in the [[asteroid belt]]. Juno was the third asteroid discovered, in 1804, by German astronomer [[Karl Ludwig Harding|Karl Harding]].<ref>{{Citation | author1=Cunningham, Clifford J | title=Bode's Law and the discovery of Juno : historical studies in asteroid research | date=2017 | publisher=Springer | isbn=978-3-319-32875-1 }}</ref> It is [[List of exceptional asteroids|tied with three other asteroids as the thirteenth largest asteroid]], and it is one of the two largest stony ([[S-type asteroid|S-type]]) asteroids, along with [[15 Eunomia]]. ([[1 Ceres|Ceres]] is the largest asteroid.) It is estimated to contain 1% of the total mass of the asteroid belt.<ref name="Pitjeva05">
'''Juno''' ([[minor-planet designation]]: '''3 Juno''') is a large [[asteroid]] in the [[asteroid belt]]. Juno was the third asteroid discovered, in 1804, by German astronomer [[Karl Ludwig Harding|Karl Harding]].<ref>{{Citation |author1=Cunningham |first=Clifford J |title=Bode's Law and the Discovery of Juno: Historical Studies in Asteroid Research |date=2017 |publisher=Springer |isbn=978-3-319-32875-1}}</ref> It is [[List of exceptional asteroids|tied with three other asteroids as the thirteenth largest asteroid]], and it is one of the two largest stony ([[S-type asteroid|S-type]]) asteroids, along with [[15 Eunomia]]. It is estimated to contain 1% of the total mass of the asteroid belt.<ref name="Pitjeva05">
  {{cite journal
  {{cite journal
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  |last=Pitjeva  
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=== Discovery ===
=== Discovery ===


Juno was discovered on 1 September 1804, by [[Karl Ludwig Harding]].<ref>{{cite book|title=Bode's Law and the Discovery of Juno|series=Historical Studies in Asteroid Research|publisher=[[Springer Publishing]]|chapter=The Discovery of Juno|last1=Cunningham|first1=Clifford J.|author-link=Clifford Cunningham|page=37|year=2017|isbn=978-3-319-32875-1|doi=10.1007/978-3-319-32875-1|bibcode=2017blsj.book.....C }}</ref> It was the third [[asteroid]] found, but was initially considered to be a [[planet]]; it was reclassified as an asteroid and [[minor planet]] during the 1850s.<ref>{{cite web | author=Hilton, James L. |title=When did the asteroids become minor planets? |work=U.S. Naval Observatory |url=http://aa.usno.navy.mil/faq/docs/minorplanets.php |access-date=2008-05-08 |archive-url = https://web.archive.org/web/20080324182332/http://aa.usno.navy.mil/faq/docs/minorplanets.php |archive-date = 2008-03-24}}</ref>
Juno was discovered on 1 September 1804, by [[Karl Ludwig Harding]].<ref>{{cite book|title=Bode's Law and the Discovery of Juno|series=Historical Studies in Asteroid Research|publisher=[[Springer Publishing]]|chapter=The Discovery of Juno|last1=Cunningham|first1=Clifford J.|author-link=Clifford Cunningham|page=37|year=2017|isbn=978-3-319-32875-1|doi=10.1007/978-3-319-32875-1|bibcode=2017blsj.book.....C }}</ref> It was the third [[asteroid]] found, but was initially considered to be a [[planet]]; it was reclassified as an asteroid and [[minor planet]] during the 1850s.<ref name="Hilton" />


=== Name and symbol ===
=== Name and symbol ===


Juno is named after the mythological [[Juno (mythology)|Juno]], the highest Roman goddess. The adjectival form is Junonian (from Latin ''jūnōnius''), with the historical final ''n'' of the name (still seen in the French form, ''Junon'') reappearing, analogous to Pluto ~ Plutonian.<ref name=OED/>
Juno is named after the mythological [[Juno (mythology)|Juno]], the highest Roman goddess. The adjectival form is ''Junonian'' (from {{Langx|la|jūnōnius}}), with the historical final ''n'' of the name (still seen in the [[French language|French]] form, {{Lang|fr|Junon}}) reappearing, analogous to Pluto: Plutonian.<ref name="OED" /> ''Juno'' is the international name for the asteroid, subject to local variations, such as [[Italian language|Italian]] {{Lang|it|Giunone}}, French {{Lang|fr|Junon}}, and [[Russian language|Russian]] {{Lang|ru|Юнона}} ({{Lang|ru-Latn|Yunona}}).{{#tag:ref|There are two exceptions: [[Greek language|Greek]], where the name was translated to its Hellenic equivalent, [[Hera]] (3 {{lang|el|Ήρα}}), as in the cases of [[1 Ceres]] and [[4 Vesta]]; and Chinese, where it is called the 'marriage-god(dess) star' ({{zh|c=婚神星|p=hūnshénxīng}}). This contrasts with the goddess Juno, for which Chinese uses the transliterated Latin name ({{zh|c=朱諾|p=zhūnuò|labels=no}}).|group=lower-alpha}}
'Juno' is the international name for the asteroid, subject to local variation: Italian ''Giunone'', French ''Junon'', Russian ''Юнона'' (''Yunona''), etc.{{#tag:ref|There are two exceptions: Greek, where the name was translated to its Hellenic equivalent, [[Hera]] (3 Ήρα), as in the cases of [[1 Ceres]] and [[4 Vesta]]; and Chinese, where it is called the 'marriage-god(dess) star' (婚神星 ''hūnshénxīng''). This contrasts with the goddess Juno, for which Chinese uses the transliterated Latin name (朱諾 ''zhūnuò'').|group=lower-alpha}}


The old [[astronomical symbol]] of Juno, still used in astrology, is a scepter topped by a star, {{angbr|[[File:Juno symbol (fixed width).svg|16px|⚵]]}}. There were many graphic variants with a more elaborated scepter, such as [[file:Juno orb symbol (fixed width).svg|16px|orbed symbol of Juno]], sometimes tilted at an angle to provide more room for decoration.
The old [[astronomical symbol]] of Juno, still used in astrology, is a scepter topped by a star: [[File:Juno_symbol_(fixed_width).svg|16px|⚵]]. There are many graphic variants with more elaborate scepters, such as [[File:Juno orb symbol (fixed width).svg|16px|orbed symbol of Juno]], sometimes tilted at an angle to provide more room for decoration. The generic asteroid symbol of a disk with its discovery number (③ for Juno) was introduced in 1852 and quickly became the norm.<ref name="Forbes1971">{{cite journal |last=Forbes |first=Eric G. |title=Gauss and the Discovery of Ceres |journal=Journal for the History of Astronomy |volume=2 |issue=3 |pages=195–199 |year=1971 |bibcode=1971JHA.....2..195F |doi=10.1177/002182867100200305 |s2cid=125888612 |url=http://adsabs.harvard.edu/full/1971JHA.....2..195F |access-date=18 July 2021 |archive-date=18 July 2021 |archive-url=https://web.archive.org/web/20210718200510/http://adsabs.harvard.edu/full/1971JHA.....2..195F |url-status=live }}</ref><ref>{{cite journal |last=Gould |first=B. A. |author-link=Benjamin Apthorp Gould |title=On the symbolic notation of the asteroids |journal=Astronomical Journal |year=1852 |volume=2 |issue=34 |page=80 |bibcode=1852AJ......2...80G |doi=10.1086/100212 }}</ref> The scepter symbol was resurrected for astrological use in 1973.<ref>Eleanor Bach (1973). ''Ephemerides of the asteroids: Ceres, Pallas, Juno, Vesta, 1900&ndash;2000''. Celestial Communications.</ref>
The generic asteroid symbol of a disk with its discovery number, {{angbr|③}}, was introduced in 1852 and quickly became the norm.<ref name="Forbes1971">{{cite journal |last=Forbes |first=Eric G. |title=Gauss and the Discovery of Ceres |journal=Journal for the History of Astronomy |volume=2 |issue=3 |pages=195–199 |year=1971 |bibcode=1971JHA.....2..195F |doi=10.1177/002182867100200305 |s2cid=125888612 |url=http://adsabs.harvard.edu/full/1971JHA.....2..195F |access-date=18 July 2021 |archive-date=18 July 2021 |archive-url=https://web.archive.org/web/20210718200510/http://adsabs.harvard.edu/full/1971JHA.....2..195F |url-status=live }}</ref><ref>{{cite journal |last=Gould |first=B. A. |author-link=Benjamin Apthorp Gould |title=On the symbolic notation of the asteroids |journal=Astronomical Journal |year=1852 |volume=2 |issue=34 |page=80 |bibcode=1852AJ......2...80G |doi=10.1086/100212 }}</ref> The scepter symbol was resurrected for astrological use in 1973.<ref>Eleanor Bach (1973) ''Ephemerides of the asteroids: Ceres, Pallas, Juno, Vesta, 1900&ndash;2000''. Celestial Communications.</ref>


==Characteristics==
==Characteristics==
Juno is one of the larger asteroids, perhaps tenth by size and containing approximately 1% the mass of the entire [[asteroid belt]].<ref name="Pitjeva04b">Pitjeva, E. V.; [http://journals.cambridge.org/production/action/cjoGetFulltext?fulltextid=303499 ''Precise determination of the motion of planets and some astronomical constants from modern observations''] {{Webarchive|url=https://web.archive.org/web/20231214154827/https://www.cambridge.org/core/redirect-support |date=14 December 2023 }}, in Kurtz, D. W. (Ed.), ''Proceedings of IAU Colloquium No. 196: Transits of Venus: New Views of the Solar System and Galaxy'', 2004</ref> It is the second-most-massive S-type asteroid after 15 Eunomia.<ref name="Baer"/> Even so, Juno has only 3% the mass of [[Ceres (dwarf planet)|Ceres]].<ref name="Baer"/> The orbital period of Juno is 4.36578 years.<ref>{{cite web|title=Comets Asteroids |url=http://comets-asteroids.findthedata.org/l/3015/3-Juno |archive-url=https://archive.today/20140514074257/http://comets-asteroids.findthedata.org/l/3015/3-Juno |url-status=dead |archive-date=14 May 2014 |publisher=Find The Data.org |access-date=14 May 2014 }}</ref>
Juno is one of the larger asteroids, perhaps tenth by size and containing approximately 1% the mass of the entire [[asteroid belt]].<ref name="Pitjeva04b">Pitjeva, E. V.; [http://journals.cambridge.org/production/action/cjoGetFulltext?fulltextid=303499 ''Precise determination of the motion of planets and some astronomical constants from modern observations''] {{Webarchive|url=https://web.archive.org/web/20231214154827/https://www.cambridge.org/core/redirect-support |date=14 December 2023 }}, in Kurtz, D. W. (Ed.), ''Proceedings of IAU Colloquium No. 196: Transits of Venus: New Views of the Solar System and Galaxy'', 2004</ref> It is the second-most-massive [[S-type asteroid]] after 15 Eunomia.<ref name="Baer" /> Even so, Juno has only 3% the mass of the largest asteroid, [[Ceres (dwarf planet)|Ceres]].<ref name="Baer" /> The orbital period of Juno is 4.36578 years.<ref>{{cite web|title=Comets Asteroids |url=http://comets-asteroids.findthedata.org/l/3015/3-Juno |archive-url=https://archive.today/20140514074257/http://comets-asteroids.findthedata.org/l/3015/3-Juno |url-status=dead |archive-date=14 May 2014 |publisher=Find The Data.org |access-date=14 May 2014 }}</ref>


Amongst S-type asteroids, Juno is unusually reflective, which may be indicative of distinct surface properties. This high albedo explains its relatively high [[apparent magnitude]] for a small object not near the inner edge of the asteroid belt. Juno can reach +7.5 at a favourable opposition, which is brighter than [[Neptune#Observation|Neptune]] or [[Exploration of Titan|Titan]], and is the reason for it being discovered before the larger asteroids [[10 Hygiea|Hygiea]], [[52 Europa|Europa]], [[511 Davida|Davida]], and [[704 Interamnia|Interamnia]]. At most oppositions, however, Juno only reaches a magnitude of around +8.7<ref name="brightestasteroids">
Amongst S-type asteroids, Juno is unusually reflective, which may be indicative of distinct surface properties. This high [[albedo]] explains its relatively high [[apparent magnitude]] for a small object not near the inner edge of the asteroid belt. Juno can reach +7.5 at a favourable [[Opposition (astronomy)|opposition]], which is brighter than [[Neptune#Observation|Neptune]] or [[Exploration of Titan|Titan]], and is the reason for it being discovered before the larger asteroids [[10 Hygiea|Hygiea]], [[52 Europa|Europa]], [[511 Davida|Davida]], and [[704 Interamnia|Interamnia]]. At most oppositions, however, Juno only reaches a magnitude of around +8.7<ref name="brightestasteroids">
  {{cite web
  {{cite web
  |title=The Brightest Asteroids  
  |title=The Brightest Asteroids  
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}}
}}
</ref>—only just visible with [[binoculars]]—and at smaller [[Elongation (astronomy)|elongation]]s a {{convert|3|in|mm|adj=on}} [[telescope]] will be required to resolve it.<ref name="telescope">
</ref>—only just visible with [[binoculars]]—and at smaller [[Elongation (astronomy)|elongation]]s a {{convert|3|in|mm|adj=on}} [[telescope]] is required to resolve it.<ref name="telescope">
  {{cite web|date=2004 |title=What Can I See Through My Scope? |publisher=Ballauer Observatory |url=http://www.allaboutastro.com/Articlepages/whatcanisee.html |access-date=2008-07-20 |url-status=dead |archive-url=https://web.archive.org/web/20110726123615/http://www.allaboutastro.com/Articlepages/whatcanisee.html |archive-date=26 July 2011 }} (archived)
  {{cite web|date=2004 |title=What Can I See Through My Scope? |publisher=Ballauer Observatory |url=http://www.allaboutastro.com/Articlepages/whatcanisee.html |access-date=2008-07-20 |url-status=dead |archive-url=https://web.archive.org/web/20110726123615/http://www.allaboutastro.com/Articlepages/whatcanisee.html |archive-date=26 July 2011 }} (archived)
</ref> It is the main body in the [[Juno family]].
</ref> It is the main body in the [[Juno family]].


Juno was originally considered a planet, along with [[Ceres (dwarf planet)|1 Ceres]], [[2 Pallas]], and [[4 Vesta]].<ref name="Hilton"/> In 1811, [[Johann Hieronymus Schröter|Schröter]] estimated Juno to be as large as 2290&nbsp;km in diameter.<ref name="Hilton">
Juno was originally considered a planet, along with 1 Ceres, [[2 Pallas]], and [[4 Vesta]].<ref name="Hilton" /> In 1811, [[Johann Hieronymus Schröter|Johann Schröter]] estimated Juno to be as large as 2290&nbsp;km in diameter.<ref name="Hilton">
  {{cite web
  {{cite web
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   |date=2007-11-16
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</ref> All four were reclassified as asteroids as additional asteroids were discovered. Juno's small size and irregular shape preclude it from being designated a [[dwarf planet]].
</ref> All four were reclassified as asteroids as additional asteroids were discovered. Juno's small size and irregular shape preclude it from being designated a [[dwarf planet]].
[[File:Moon_and_Asteroids_1_to_10.svg|center|thumb|400x400px|Size comparison: the first 10 asteroids discovered, profiled against Earth's [[Moon]]. Juno is third from the left.]]
[[File:Moon_and_Asteroids_1_to_10.svg|center|thumb|400x400px|Size comparison: the first 10 asteroids discovered, profiled against Earth's [[Moon]]. Juno is third from the left.]]
Juno orbits at a slightly closer mean distance to the [[Sun]] than Ceres or Pallas. Its orbit is moderately inclined at around 12° to the [[ecliptic]], but has an extreme [[orbital eccentricity|eccentricity]], greater than that of [[Pluto]]. This high eccentricity brings Juno closer to the Sun at [[perihelion]] than Vesta and further out at [[aphelion]] than Ceres. Juno had the most eccentric orbit of any known body until [[33 Polyhymnia]] was discovered in 1854, and of asteroids over 200&nbsp;km in diameter only [[324 Bamberga]] has a more eccentric orbit.<ref name="ecc">{{cite web|title=MBA Eccentricity Screen Capture |publisher=JPL Small-Body Database Search Engine |url=http://home.comcast.net/~kpheider/3Juno-ecc.jpg |access-date=2008-11-01 |url-status=dead |archive-url=https://web.archive.org/web/20090327111705/http://home.comcast.net/~kpheider/3Juno-ecc.jpg |archive-date=27 March 2009 }}</ref>
Juno orbits at a slightly closer mean distance to the [[Sun]] than Ceres or Pallas. Its orbit is moderately inclined at around 12° to the [[ecliptic]], but has an extreme [[orbital eccentricity|eccentricity]], greater than that of [[Pluto]]. This high eccentricity brings Juno closer to the Sun at [[perihelion]] than Vesta and further out at [[aphelion]] than Ceres. It had the most eccentric orbit of any known body until [[33 Polyhymnia]] was discovered in 1854, and of asteroids over 200&nbsp;km in diameter only [[324 Bamberga]] has a more eccentric orbit.<ref name="ecc">{{cite web|title=MBA Eccentricity Screen Capture |publisher=JPL Small-Body Database Search Engine |url=http://home.comcast.net/~kpheider/3Juno-ecc.jpg |access-date=2008-11-01 |url-status=dead |archive-url=https://web.archive.org/web/20090327111705/http://home.comcast.net/~kpheider/3Juno-ecc.jpg |archive-date=27 March 2009 }}</ref>


Juno rotates in a [[direct motion|prograde]] direction with an [[axial tilt]] of approximately 50°.<ref name="kaasalainen2002">The north pole points towards [[ecliptic coordinate system|ecliptic coordinates]] (β, λ) = (27°, 103°) within a 5° uncertainty.  
Juno rotates in a [[direct motion|prograde]] direction with an [[axial tilt]] of approximately 50°.<ref name="kaasalainen2002">The north pole points towards [[Ecliptic coordinate system|ecliptic coordinates]] (β, λ) = (27°, 103°) within a 5° uncertainty.
{{cite journal | last= Kaasalainen | first= M. | author2= Torppa, J. | author3= Piironen, J. | title= Models of Twenty Asteroids from Photometric Data | journal= Icarus | volume= 159 | issue= 2 | pages= 369–395 | date= 2002 | url= http://www.rni.helsinki.fi/~mjk/IcarPIII.pdf | doi= 10.1006/icar.2002.6907 | bibcode= 2002Icar..159..369K | access-date= 30 November 2005 | archive-date= 16 February 2008 | archive-url= https://web.archive.org/web/20080216072340/http://www.rni.helsinki.fi/~mjk/IcarPIII.pdf | url-status= dead }}</ref> The maximum temperature on the surface, directly facing the Sun, was measured at about 293 [[Kelvin|K]] on 2 October 2001. Taking into account the [[heliocentric]] distance at the time, this gives an estimated maximum temperature of 301 K (+28&nbsp;°C) at perihelion.<ref name="lim2005"/>


[[File:Juno orbit 2018.png|thumb|The orbit of Juno is significantly elliptical with a small inclination, moving between Mars and Jupiter|center|400x400px]]Spectroscopic studies of the Junonian surface permit the conclusion that Juno could be the progenitor of [[chondrite]]s, a common type of stony [[meteorite]] composed of iron-bearing [[silicate]]s such as [[olivine]] and [[pyroxene]].<ref name="gaffey1993">
{{cite journal |last=Kaasalainen |first=M. |author2=Torppa, J. |author3=Piironen, J. |date=2002 |title=Models of Twenty Asteroids from Photometric Data |url=http://www.rni.helsinki.fi/~mjk/IcarPIII.pdf |url-status=dead |journal=Icarus |volume=159 |issue=2 |pages=369–395 |bibcode=2002Icar..159..369K |doi=10.1006/icar.2002.6907 |archive-url=https://web.archive.org/web/20080216072340/http://www.rni.helsinki.fi/~mjk/IcarPIII.pdf |archive-date=16 February 2008 |access-date=30 November 2005}}</ref> The maximum temperature on the surface, directly facing the Sun, was measured at about 293&nbsp;[[Kelvin|K]] on 2 October 2001. Taking into account the [[Heliocentric orbit|heliocentric]] distance at the time, this gives an estimated maximum temperature of 301&nbsp;K (+28&nbsp;°C) at perihelion.<ref name="lim2005" />
 
[[File:Juno orbit 2018.png|thumb|The orbit of Juno is significantly elliptical with a small inclination, moving between Mars and Jupiter|center|400x400px]]
[[Spectroscopic]] studies of the Junonian surface permit the conclusion that Juno could be the progenitor of [[chondrite]]s, a common type of stony [[meteorite]] composed of iron-bearing [[silicate]]s such as [[olivine]] and [[pyroxene]].<ref name="gaffey1993">
{{cite journal
{{cite journal
  | last= Gaffey
  | last= Gaffey
Line 194: Line 194:
  | journal= Icarus | date= 1993 | volume= 106 | issue= 2 | page= 573
  | journal= Icarus | date= 1993 | volume= 106 | issue= 2 | page= 573
  | bibcode= 1993Icar..106..573G | doi= 10.1006/icar.1993.1194}}
  | bibcode= 1993Icar..106..573G | doi= 10.1006/icar.1993.1194}}
</ref> [[Infrared]] images reveal that Juno possesses an approximately 100&nbsp;km-wide crater or ejecta feature, the result of a geologically young impact.<ref name="harvard-pr0318">
</ref> [[Infrared]] images reveal that Juno possesses an approximately 100&nbsp;km-wide [[Impact crater|crater]] or [[ejecta]] feature, the result of a geologically young impact.<ref name="harvard-pr0318">
  {{cite web
  {{cite web
  |title=Asteroid Juno Has A Bite Out Of It  
  |title=Asteroid Juno Has A Bite Out Of It  
Line 228: Line 228:
  }}</ref>
  }}</ref>


Based on MIDAS infrared data using the [[Hale Telescope]], an average radius of 135.7 ± 11 km was reported in 2004.<ref name="mit.edu">{{cite journal|doi=10.1016/j.icarus.2004.08.005|url=https://www.mit.edu/people/lucylim/2005_Icarus_LimMcConnochie_Thermal_infrared_8-13_micron_spectra.pdf|title=Thermal infrared (8?13 ?m) spectra of 29 asteroids: The Cornell Mid-Infrared Asteroid Spectroscopy (MIDAS) Survey|journal=Icarus|volume=173|issue=2|pages=385|year=2005|last1=Lim|first1=L|last2=McConnochie|first2=T|last3=Belliii|first3=J|last4=Hayward|first4=T|bibcode=2005Icar..173..385L|access-date=26 August 2019|archive-url=https://web.archive.org/web/20160303232808/http://www.mit.edu/people/lucylim/2005_Icarus_LimMcConnochie_Thermal_infrared_8-13_micron_spectra.pdf|archive-date=3 March 2016|url-status=dead}}</ref>
Based on Mid-Infrared Asteroid Spectroscopy (MIDAS) data using the [[Hale Telescope]], an average radius of 135.7&nbsp;±&nbsp;11 km was reported in 2004.<ref name="mit.edu">{{cite journal|doi=10.1016/j.icarus.2004.08.005|url=https://www.mit.edu/people/lucylim/2005_Icarus_LimMcConnochie_Thermal_infrared_8-13_micron_spectra.pdf|title=Thermal infrared (8?13 ?m) spectra of 29 asteroids: The Cornell Mid-Infrared Asteroid Spectroscopy (MIDAS) Survey|journal=Icarus|volume=173|issue=2|pages=385|year=2005|last1=Lim|first1=L|last2=McConnochie|first2=T|last3=Belliii|first3=J|last4=Hayward|first4=T|bibcode=2005Icar..173..385L|access-date=26 August 2019|archive-url=https://web.archive.org/web/20160303232808/http://www.mit.edu/people/lucylim/2005_Icarus_LimMcConnochie_Thermal_infrared_8-13_micron_spectra.pdf|archive-date=3 March 2016|url-status=dead}}</ref>


== Observations ==
== Observations ==
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  | archive-url= https://web.archive.org/web/20231214154823/https://library2.smu.ca:443/bitstream/handle/01/26050/Dupuy_David_L_article_1981.pdf;jsessionid=FA53E7FF3F1BCDB4CC3B578960F38AB8?sequence=1
  | archive-url= https://web.archive.org/web/20231214154823/https://library2.smu.ca:443/bitstream/handle/01/26050/Dupuy_David_L_article_1981.pdf;jsessionid=FA53E7FF3F1BCDB4CC3B578960F38AB8?sequence=1
  | url-status= live
  | url-status= live
  }}</ref>
  }}</ref> It occulted the magnitude 11.3 star [[PPMX 9823370]] on 29 July 2013,<ref>[https://archive.today/20130729233004/http://www.asteroidoccultation.com/2013_07/0729_3_30531.htm Asteroid Occultation Updates – 29 Jul 2013]</ref> and [[2UCAC 30446947]] on 30 July 2013.<ref>[https://archive.today/20130729232944/http://www.asteroidoccultation.com/2013_07/0730_3_29995.htm Asteroid Occultation Updates – 30 Jul 2013].</ref>
Juno occulted the magnitude 11.3 star [[PPMX 9823370]] on 29 July 2013,<ref>[https://archive.today/20130729233004/http://www.asteroidoccultation.com/2013_07/0729_3_30531.htm Asteroid Occultation Updates – 29 Jul 2013]</ref> and [[2UCAC 30446947]] on 30 July 2013.<ref>[https://archive.today/20130729232944/http://www.asteroidoccultation.com/2013_07/0730_3_29995.htm Asteroid Occultation Updates – 30 Jul 2013].</ref>


Radio signals from spacecraft in orbit around [[Mars]] and on its surface have been used to estimate the mass of Juno from the tiny perturbations induced by it onto the motion of Mars.<ref name="Pitjeva04">
Radio signals from spacecraft in orbit around [[Mars]] and on its surface have been used to estimate the mass of Juno from the tiny perturbations induced by it onto the motion of Mars.<ref name="Pitjeva04">
Line 269: Line 268:
  | bibcode= 2004cosp...35.2014P}}</ref> Juno's [[orbit]] appears to have changed slightly around 1839, very likely due to perturbations from a passing asteroid, whose identity has not been determined.<ref name="usno1999">{{cite journal |last=Hilton |first=James L. |title=US Naval Observatory Ephemerides of the Largest Asteroids |journal=Astronomical Journal |volume=117 |issue=2 |pages=1077–1086 |date=February 1999 |doi=10.1086/300728 |bibcode=1999AJ....117.1077H |doi-access=free }}</ref>
  | bibcode= 2004cosp...35.2014P}}</ref> Juno's [[orbit]] appears to have changed slightly around 1839, very likely due to perturbations from a passing asteroid, whose identity has not been determined.<ref name="usno1999">{{cite journal |last=Hilton |first=James L. |title=US Naval Observatory Ephemerides of the Largest Asteroids |journal=Astronomical Journal |volume=117 |issue=2 |pages=1077–1086 |date=February 1999 |doi=10.1086/300728 |bibcode=1999AJ....117.1077H |doi-access=free }}</ref>


In 1996, Juno was imaged by the [[Hooker Telescope]] at [[Mount Wilson Observatory]] at visible and near-IR wavelengths, using [[adaptive optics]]. The images spanned a whole rotation period and revealed an irregular shape and a dark albedo feature, interpreted as a fresh impact site.<ref name="baliunas2003"/>
In 1996, Juno was imaged by the [[Hooker Telescope]] at [[Mount Wilson Observatory]] at visible and [[near-IR]] wavelengths, using [[adaptive optics]]. The images spanned a whole rotation period and revealed an irregular shape and a dark albedo feature, interpreted as a fresh impact site.<ref name="baliunas2003" />
<gallery mode="packed" heights="200px">
<gallery mode="packed" heights="200px">
File:Juno 4 wavelengths.jpg|Juno seen at four wavelengths with a large [[Impact crater|crater]] in the dark ([[Hooker telescope]], 2003
File:Juno 4 wavelengths.jpg|Juno seen at four wavelengths with a large [[Impact crater|crater]] in the dark ([[Hooker telescope]], 2003)
File:Juno mpl anim.gif|Juno moving across background stars
File:Juno mpl anim.gif|Juno moving across background stars
File:3Juno-LB1-apmag.jpg|Juno during opposition in 2009
File:3Juno-LB1-apmag.jpg|Juno during opposition in 2009
File:Animation of the asteroid Juno as imaged by ALMA.webm|Video of Juno taken as part of ALMA's Long Baseline Campaign
File:Animation of the asteroid Juno as imaged by ALMA.webm|Video of Juno taken as part of [[Atacama Large Millimeter Array|ALMA]]'s Long Baseline Campaign
</gallery>
</gallery>


== Oppositions ==
== Oppositions ==
Juno reaches [[Opposition (astronomy)|opposition]] from the Sun every 15.5 months or so, with its minimum distance varying greatly depending on whether it is near perihelion or aphelion. Sequences of favorable oppositions occur every 10th opposition, i.e. just over every 13 years. The last favorable oppositions were on 1 December 2005, at a distance of 1.063 AU, magnitude 7.55, and on 17 November 2018, at a minimum distance of 1.036 AU, magnitude 7.45.<ref>The Astronomical Almanac for the year 2018, G14</ref><ref>[https://in-the-sky.org/news.php?id=20181116_14_100 Asteroid 3 Juno at opposition] {{Webarchive|url=https://web.archive.org/web/20171201031802/https://in-the-sky.org/news.php?id=20181116_14_100 |date=1 December 2017 }} 16 Nov 2018 at 11:31 UTC</ref> The next favorable opposition will be 30 October 2031, at a distance of 1.044 AU, magnitude 7.42.
Juno reaches [[Opposition (astronomy)|opposition]] from the Sun every 15.5 months or so, with its minimum distance varying greatly depending on whether it is near perihelion or aphelion. Sequences of favorable oppositions occur every 10th opposition, i.e. just over every 13 years. The last favorable oppositions were on 1 December 2005, at a distance of 1.063&nbsp;[[Astronomical unit|AU]], magnitude 7.55, and on 17 November 2018, at a minimum distance of 1.036&nbsp;AU, magnitude 7.45.<ref>The Astronomical Almanac for the year 2018, G14</ref><ref>[https://in-the-sky.org/news.php?id=20181116_14_100 Asteroid 3 Juno at opposition] {{Webarchive|url=https://web.archive.org/web/20171201031802/https://in-the-sky.org/news.php?id=20181116_14_100 |date=1 December 2017 }} 16 Nov 2018 at 11:31 UTC</ref> The next favorable opposition will be 30 October 2031, at a distance of 1.044&nbsp;AU, magnitude 7.42.


==See also==
==See also==
Line 305: Line 304:
{{Commons}}
{{Commons}}
* [http://ssd.jpl.nasa.gov/horizons.cgi?find_body=1&body_group=sb&sstr=3 JPL Ephemeris]
* [http://ssd.jpl.nasa.gov/horizons.cgi?find_body=1&body_group=sb&sstr=3 JPL Ephemeris]
* [https://web.archive.org/web/20060627152558/http://www.cfa.harvard.edu/press/pr0318image.html Well resolved images from four angles] taken at [[Mount Wilson observatory]]
* [https://web.archive.org/web/20060627152558/http://www.cfa.harvard.edu/press/pr0318image.html Well resolved images from four angles] taken at Mount Wilson observatory
* [http://www.rni.helsinki.fi/~mjk/IcarPIII.pdf Shape model deduced from light curve]
* [http://www.rni.helsinki.fi/~mjk/IcarPIII.pdf Shape model deduced from light curve]
* [http://www.jpl.nasa.gov/news/features.cfm?feature=2314 Asteroid Juno Grabs the Spotlight]
* [http://www.jpl.nasa.gov/news/features.cfm?feature=2314 NASA JPL: Asteroid Juno Grabs the Spotlight]
* {{cite web|title=Elements and Ephemeris for (3) Juno |publisher=Minor Planet Center |url=http://scully.cfa.harvard.edu/cgi-bin/returnprepeph.cgi?d=b2011&o=00003 |url-status=dead |archive-url=https://web.archive.org/web/20150904083927/http://scully.cfa.harvard.edu/cgi-bin/returnprepeph.cgi?d=b2011&o=00003 |archive-date=2015-09-04 }} (displays [[Elongation (astronomy)|Elong]] from Sun and [[apparent magnitude|V mag]] for 2011)
* {{cite web|title=Elements and Ephemeris for (3) Juno |publisher=Minor Planet Center |url=http://scully.cfa.harvard.edu/cgi-bin/returnprepeph.cgi?d=b2011&o=00003 |url-status=dead |archive-url=https://web.archive.org/web/20150904083927/http://scully.cfa.harvard.edu/cgi-bin/returnprepeph.cgi?d=b2011&o=00003 |archive-date=2015-09-04 }} (displays elongation from Sun and apparent magnitude for 2011)
* {{AstDys|3}}
* {{AstDys|3}}
* {{JPL small body}}
* {{JPL small body}}


{{Use dmy dates|date=October 2019}}
{{Large asteroids}}
{{Large asteroids}}
{{Solar System table}}
{{Solar System table}}

Latest revision as of 02:52, 13 November 2025

Template:Short description Script error: No such module "other uses". Template:Use dmy dates Script error: No such module "infobox".Script error: No such module "Check for unknown parameters".

Juno (minor-planet designation: 3 Juno) is a large asteroid in the asteroid belt. Juno was the third asteroid discovered, in 1804, by German astronomer Karl Harding.[1] It is tied with three other asteroids as the thirteenth largest asteroid, and it is one of the two largest stony (S-type) asteroids, along with 15 Eunomia. It is estimated to contain 1% of the total mass of the asteroid belt.[2]

History

Discovery

Juno was discovered on 1 September 1804, by Karl Ludwig Harding.[3] It was the third asteroid found, but was initially considered to be a planet; it was reclassified as an asteroid and minor planet during the 1850s.[4]

Name and symbol

Juno is named after the mythological Juno, the highest Roman goddess. The adjectival form is Junonian (from Template:Langx), with the historical final n of the name (still seen in the French form, Script error: No such module "Lang".) reappearing, analogous to Pluto: Plutonian.[5] Juno is the international name for the asteroid, subject to local variations, such as Italian Script error: No such module "Lang"., French Script error: No such module "Lang"., and Russian Script error: No such module "Lang". (Script error: No such module "Lang".).[lower-alpha 1]

The old astronomical symbol of Juno, still used in astrology, is a scepter topped by a star: ⚵. There are many graphic variants with more elaborate scepters, such as orbed symbol of Juno, sometimes tilted at an angle to provide more room for decoration. The generic asteroid symbol of a disk with its discovery number (③ for Juno) was introduced in 1852 and quickly became the norm.[6][7] The scepter symbol was resurrected for astrological use in 1973.[8]

Characteristics

Juno is one of the larger asteroids, perhaps tenth by size and containing approximately 1% the mass of the entire asteroid belt.[9] It is the second-most-massive S-type asteroid after 15 Eunomia.[10] Even so, Juno has only 3% the mass of the largest asteroid, Ceres.[10] The orbital period of Juno is 4.36578 years.[11]

Amongst S-type asteroids, Juno is unusually reflective, which may be indicative of distinct surface properties. This high albedo explains its relatively high apparent magnitude for a small object not near the inner edge of the asteroid belt. Juno can reach +7.5 at a favourable opposition, which is brighter than Neptune or Titan, and is the reason for it being discovered before the larger asteroids Hygiea, Europa, Davida, and Interamnia. At most oppositions, however, Juno only reaches a magnitude of around +8.7[12]—only just visible with binoculars—and at smaller elongations a Template:Convert telescope is required to resolve it.[13] It is the main body in the Juno family.

Juno was originally considered a planet, along with 1 Ceres, 2 Pallas, and 4 Vesta.[4] In 1811, Johann Schröter estimated Juno to be as large as 2290 km in diameter.[4] All four were reclassified as asteroids as additional asteroids were discovered. Juno's small size and irregular shape preclude it from being designated a dwarf planet.

File:Moon and Asteroids 1 to 10.svg
Size comparison: the first 10 asteroids discovered, profiled against Earth's Moon. Juno is third from the left.

Juno orbits at a slightly closer mean distance to the Sun than Ceres or Pallas. Its orbit is moderately inclined at around 12° to the ecliptic, but has an extreme eccentricity, greater than that of Pluto. This high eccentricity brings Juno closer to the Sun at perihelion than Vesta and further out at aphelion than Ceres. It had the most eccentric orbit of any known body until 33 Polyhymnia was discovered in 1854, and of asteroids over 200 km in diameter only 324 Bamberga has a more eccentric orbit.[14]

Juno rotates in a prograde direction with an axial tilt of approximately 50°.[15] The maximum temperature on the surface, directly facing the Sun, was measured at about 293 K on 2 October 2001. Taking into account the heliocentric distance at the time, this gives an estimated maximum temperature of 301 K (+28 °C) at perihelion.[16]

File:Juno orbit 2018.png
The orbit of Juno is significantly elliptical with a small inclination, moving between Mars and Jupiter

Spectroscopic studies of the Junonian surface permit the conclusion that Juno could be the progenitor of chondrites, a common type of stony meteorite composed of iron-bearing silicates such as olivine and pyroxene.[17] Infrared images reveal that Juno possesses an approximately 100 km-wide crater or ejecta feature, the result of a geologically young impact.[18][19]

Based on Mid-Infrared Asteroid Spectroscopy (MIDAS) data using the Hale Telescope, an average radius of 135.7 ± 11 km was reported in 2004.[20]

Observations

Juno was the first asteroid for which an occultation was observed. It passed in front of a dim star (SAO 112328) on 19 February 1958. Since then, several occultations by Juno have been observed, the most fruitful being the occultation of SAO 115946 on 11 December 1979, which was registered by 18 observers.[21] It occulted the magnitude 11.3 star PPMX 9823370 on 29 July 2013,[22] and 2UCAC 30446947 on 30 July 2013.[23]

Radio signals from spacecraft in orbit around Mars and on its surface have been used to estimate the mass of Juno from the tiny perturbations induced by it onto the motion of Mars.[24] Juno's orbit appears to have changed slightly around 1839, very likely due to perturbations from a passing asteroid, whose identity has not been determined.[25]

In 1996, Juno was imaged by the Hooker Telescope at Mount Wilson Observatory at visible and near-IR wavelengths, using adaptive optics. The images spanned a whole rotation period and revealed an irregular shape and a dark albedo feature, interpreted as a fresh impact site.[19]

Oppositions

Juno reaches opposition from the Sun every 15.5 months or so, with its minimum distance varying greatly depending on whether it is near perihelion or aphelion. Sequences of favorable oppositions occur every 10th opposition, i.e. just over every 13 years. The last favorable oppositions were on 1 December 2005, at a distance of 1.063 AU, magnitude 7.55, and on 17 November 2018, at a minimum distance of 1.036 AU, magnitude 7.45.[26][27] The next favorable opposition will be 30 October 2031, at a distance of 1.044 AU, magnitude 7.42.

See also

Notes

Template:Notelist

References

Template:Reflist

External links

Template:Sister project

Template:Large asteroids Script error: No such module "Navbox". Template:Navbox with columns Script error: No such module "Navbox". Template:Portal bar Template:Authority control

  1. ↑ Script error: No such module "citation/CS1".
  2. ↑ Script error: No such module "Citation/CS1".
  3. ↑ Script error: No such module "citation/CS1".
  4. ↑ a b c Script error: No such module "citation/CS1".
  5. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named OED
  6. ↑ Script error: No such module "Citation/CS1".
  7. ↑ Script error: No such module "Citation/CS1".
  8. ↑ Eleanor Bach (1973). Ephemerides of the asteroids: Ceres, Pallas, Juno, Vesta, 1900–2000. Celestial Communications.
  9. ↑ Pitjeva, E. V.; Precise determination of the motion of planets and some astronomical constants from modern observations Template:Webarchive, in Kurtz, D. W. (Ed.), Proceedings of IAU Colloquium No. 196: Transits of Venus: New Views of the Solar System and Galaxy, 2004
  10. ↑ a b Cite error: Invalid <ref> tag; no text was provided for refs named Baer
  11. ↑ Script error: No such module "citation/CS1".
  12. ↑ Script error: No such module "citation/CS1".
  13. ↑ Script error: No such module "citation/CS1". (archived)
  14. ↑ Script error: No such module "citation/CS1".
  15. ↑ The north pole points towards ecliptic coordinates (β, λ) = (27°, 103°) within a 5° uncertainty. Script error: No such module "Citation/CS1".
  16. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named lim2005
  17. ↑ Script error: No such module "Citation/CS1".
  18. ↑ Script error: No such module "citation/CS1".
  19. ↑ a b Script error: No such module "Citation/CS1".
  20. ↑ Script error: No such module "Citation/CS1".
  21. ↑ Script error: No such module "Citation/CS1".
  22. ↑ Asteroid Occultation Updates – 29 Jul 2013
  23. ↑ Asteroid Occultation Updates – 30 Jul 2013.
  24. ↑ Script error: No such module "citation/CS1".
  25. ↑ Script error: No such module "Citation/CS1".
  26. ↑ The Astronomical Almanac for the year 2018, G14
  27. ↑ Asteroid 3 Juno at opposition Template:Webarchive 16 Nov 2018 at 11:31 UTC


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