36 Ophiuchi: Difference between revisions

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{{short description|Triple star system in the constellation Ophiuchus}}
{{short description|Triple star system in the constellation Ophiuchus}}
{{Sky|17|15|20.851|-|26|36|09.04|19.418}}
{{Sky|17|15|20.851|-|26|36|09.04|19.418}}
{{Starbox begin |
{{Starbox begin}}
  name=36 Ophiuchi
}}
{{Starbox image
{{Starbox image
|image={{Location map|100x100|AlternativeMap=Ophiuchus_constellation_map.svg
|image={{Location map|100x100|AlternativeMap=Ophiuchus_constellation_map.svg
Line 17: Line 15:
  | epoch=J2000  
  | epoch=J2000  
  | constell=[[Ophiuchus]]  
  | constell=[[Ophiuchus]]  
  | ra=A:&nbsp;{{RA|17|15|20.851}}<br/>B:&nbsp;{{RA|17|15|20.978}}<br/>C:&nbsp;{{RA|17|16|13.3624}}<ref name="SIMBAD">{{cite web
  | ra=A:&nbsp;{{RA|17|15|20.7836}}<ref name="GaiaDR3a"/><br/>B:&nbsp;{{RA|17|15|20.9838}}<ref name="GaiaDR3b"/><br/>C:&nbsp;{{RA|17|16|13.3624}}<ref name="GaiaDR3c"/>
| url=http://simbad.u-strasbg.fr/
| title=SIMBAD Astronomical Database
| publisher=[[Centre de Données astronomiques de Strasbourg]]
| access-date=2013-08-23
}}<br/>
* A: [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD%20155886 LHS 437 -- High proper-motion Star]
* B: [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD%20155885 LHS 438 -- High proper-motion Star ]
* C: [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD%20156026 V* V2215 Oph -- Variable of RS CVn type]</ref>
  |
  |
  dec=A:&nbsp;{{DEC| -26|36|09.04}}<br/>B:&nbsp;{{DEC| -26|36|10.18}}<br/>C:&nbsp;{{DEC| -26|32|46.129}}<ref name="SIMBAD"/>  
  dec=A:&nbsp;{{DEC|-26|36|06.117}}<ref name="GaiaDR3a"/><br/>B:&nbsp;{{DEC|-26|36|10.173}}<ref name="GaiaDR3b"/><br/>C:&nbsp;{{DEC|-26|32|46.137}}<ref name="GaiaDR3c"/>  
| appmag_v=5.08/5.03/6.34<ref name="SIMBAD"/>
| appmag_v=5.08/5.03/6.34<ref name="SIMBAD"/>
}}
}}
{{Starbox character  
{{Starbox character  
  |   class=K2&nbsp;V/K1&nbsp;V/K5&nbsp;V<ref name="SIMBAD"/>  
  | class=A: K2V<ref name=Gray2006/><br/>B: K1V<ref name=Gray2006/><br/>C: K5V<ref name=Gray2006/>
  | b-v=0.85(AB)/1.16
  | b-v=  
  | u-b=0.51(AB)/1.04
  | u-b=  
  | variable=C: [[RS Canum Venaticorum variable|RS CVn]] }}
  | variable=C: [[RS Canum Venaticorum variable|RS CVn]]
}}
{{Starbox astrometry
{{Starbox astrometry
  | component1 = 36 Oph A
  | component1 = 36 Oph A
  | radial_v=−0.6<ref name="SIMBAD"/>
  | radial_v={{val|+0.26|0.12}}<ref name="GaiaDR3a"/>
  | prop_mo_ra={{val|-498.600}}
  | prop_mo_ra={{val|-498.600}}
  | prop_mo_dec={{val|-1149.158|fmt=commas}}
  | prop_mo_dec={{val|-1149.158|fmt=commas}}
  | pm_footnote = <ref name="GaiaEDR3a"/>
  | pm_footnote = <ref name="GaiaDR3a"/>
  | parallax=168.0031
  | parallax=168.0031
  | p_error=0.1343
  | p_error=0.1343
  | parallax_footnote=<ref name="GaiaEDR3a">{{Cite Gaia EDR3|4109030160308320128}}</ref>
  | parallax_footnote=<ref name="GaiaDR3a">{{Cite Gaia DR3|4109030160308320128}}</ref>
  | absmag_v=
  | absmag_v=
  | component2 = 36 Oph B
  | component2 = 36 Oph B
  | radial_v2=0.0<ref name="SIMBAD"/>
  | radial_v2={{val|+0.10|0.13}}<ref name="SIMBAD"/>
  | prop_mo_ra2={{val|-465.861}}
  | prop_mo_ra2={{val|-465.861}}
  | prop_mo_dec2={{val|-1141.168|fmt=commas}}
  | prop_mo_dec2={{val|-1141.168|fmt=commas}}
  | pm_footnote2 = <ref name="GaiaEDR3b"/>
  | pm_footnote2 = <ref name="GaiaDR3b"/>
  | parallax2=168.1303
  | parallax2=168.1303
  | p_error2=0.1081
  | p_error2=0.1081
  | parallax_footnote2=<ref name="GaiaEDR3b">{{Cite Gaia EDR3|4109030160308317312}}</ref>
  | parallax_footnote2=<ref name="GaiaDR3b">{{Cite Gaia DR3|4109030160308317312}}</ref>
  | absmag_v2=
  | absmag_v2=
}}
}}
{{Starbox astrometry|no_heading=y
{{Starbox astrometry|no_heading=y
| component1 = 36 Oph C
| component1 = 36 Oph C
| radial_v={{val|-0.04|0.22}}<ref name="GaiaEDR3c"/>
| radial_v={{val|-0.07|0.12}}<ref name="GaiaDR3c"/>
| prop_mo_ra={{val|-479.573}}
| prop_mo_ra={{val|-479.573}}
| prop_mo_dec={{val|-1124.332|fmt=commas}}
| prop_mo_dec={{val|-1124.332|fmt=commas}}
| pm_footnote = <ref name="GaiaEDR3c"/>
| pm_footnote = <ref name="GaiaDR3c"/>
| parallax=167.9617
| parallax=167.9617
| p_error=0.0311
| p_error=0.0311
| parallax_footnote=<ref name="GaiaEDR3c">{{Cite Gaia EDR3|4109034455276324608}}</ref>
| parallax_footnote=<ref name="GaiaDR3c">{{Cite Gaia DR3|4109034455276324608}}</ref>
| absmag_v=
| absmag_v=
}}
}}
{{Starbox visbin
{{Starbox visbin
| reference = <ref name=Tokovinin2017/>
| reference = <ref name=Tokovinin2017/>
| name=36 Ophiuchi B
| primary=36 Oph A
| name=36 Oph B
| period= 470.9
| period= 470.9
| axis= 13
| axis= 13
Line 83: Line 75:
| temperature    = {{val|5103|29|fmt=commas}}<ref name=Luck2017/>
| temperature    = {{val|5103|29|fmt=commas}}<ref name=Luck2017/>
| metal_fe      = {{val|-0.23}}<ref name=Luck2017/>
| metal_fe      = {{val|-0.23}}<ref name=Luck2017/>
| age_gyr        = {{val|4.86|0.50|0.22}}<ref name=Luck2017/>
| rotation      = {{val|20.69|0.40}}<ref name=Otani2022/> days
| age_gyr        = 1.43<ref name=Otani2022/>
| component2    = 36 Oph B
| component2    = 36 Oph B
| mass2          = {{val|0.76|0.03|0.06}}<ref name=Luck2018/>
| mass2          = {{val|0.76|0.03|0.06}}<ref name=Luck2018/>
| radius2        = {{solar radius calculator|type=logLT|-0.49|5171|decimals=3}}<ref name=Luck2018/>{{Efn|name=radius2|1=Calculated, using the [[Stefan-Boltzmann law]] and the star's [[effective temperature]] and luminosity, with respect to the [[Sun|solar]] nominal effective temperature of 5,772&nbsp;[[Kelvin|K]]:<math display="block">\sqrt{\biggl(\frac{5,772}{5,171}\biggr)^4 \cdot 10^{-0.49}} = 0.709\ R_\odot.</math>}}
| radius2        = {{val|0.721|0.044}}<ref name=tic/>
| luminosity2    = 0.32<ref name=Luck2018/>
| luminosity2    = 0.32<ref name=Luck2018/>
| temperature2  = {{val|5171|71|fmt=commas}}<ref name=Luck2018/>
| temperature2  = {{val|5171|71|fmt=commas}}<ref name=Luck2018/>
| gravity2      = 4.61<ref name=Luck2018/>
| gravity2      = 4.61<ref name=Luck2018/>
| rotation2      = {{val|21.11|0.40}}<ref name=Otani2022/> days
| metal_fe2      = {{val|-0.22}}<ref name=Luck2018/>
| metal_fe2      = {{val|-0.22}}<ref name=Luck2018/>
| age_gyr2      = {{val|5.26|5.04|2.94}}<ref name=Luck2018/>
| age_gyr2       = 1.43<ref name=Otani2022/>
}}
{{Starbox detail|no_heading=y
| component1    = 36 Oph C
| mass          = {{Val|0.72|0.01}}<ref name=Luck2018/>
| radius        = {{Val|0.688|0.064}}<ref name=tic/>
| luminosity    = 0.14<ref name=Luck2018/>
| temperature    = {{Val|4474|22|fmt=commas}}<ref name=Luck2018/>
| gravity        = 4.70<ref name=Luck2018/>
| rotation       = {{Val|18.0|0.4}}<ref name=Otani2022/> days
| habitable_inner = 0.32<ref name=Painter2025/> [[astronomical unit|AU]]
| habitable_outer = 0.79<ref name=Painter2025/> AU
| metal_fe      = {{Val|-0.22}}<ref name=Luck2018/>
| age_myr        = {{Val|590|70}}<ref name=Otani2022/>
}}
}}
{{Starbox catalog  
{{Starbox catalog  
| names=36 Oph, [[Washington Double Star Catalog|WDS]]&nbsp;J17153-2636
| names={{odlist | F=36 Oph | WDS=J17153-2636}}
| component1 = AB
| component1 = AB
| names1=[[Gliese Catalogue of Nearby Stars|GJ]]&nbsp;663, [[Cordoba Durchmusterung|CD]]−26°12026, [[General Catalogue of Trigonometric Parallaxes|GCTP]]&nbsp;3908.00, [[Hipparcos catalogue|HIP]]&nbsp;84405
| names1={{odlist | CD=-26°12026 | GJ=663 | HIP=84405 | PLX=3908.00}}
| component2 = A
| component2 = A
| names2=Guniibuu, [[Bright Star Catalogue|HR]]&nbsp;6402, [[Henry Draper Catalogue|HD]]&nbsp;155886, [[Luyten Half-Second catalogue|LHS]]&nbsp;437, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]]&nbsp;185198
| names2={{odlist | name=Guniibuu | HD=155886 | HR=6402 | LHS=437 | SAO=185198}}
| component3 = B
| component3 = B
| names3=[[Bright Star Catalogue|HR]]&nbsp;6401, [[Henry Draper Catalogue|HD]]&nbsp;155885, [[Luyten Half-Second catalogue|LHS]]&nbsp;438, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]]&nbsp;185199
| names3={{odlist | HD=155885 | HR=6401 | LHS=438 | SAO=185199}}
| component4 = C
| component4 = C
| names4=[[Variable star designation|V2215]]&nbsp;Ophiuchi, [[Gliese Catalogue of Nearby Stars|GJ]]&nbsp;664, [[Cordoba Durchmusterung|CD]]−26°12036, [[Henry Draper Catalogue|HD]]&nbsp;156026, [[General Catalogue of Trigonometric Parallaxes|GCTP]]&nbsp;3913.00, [[Luyten Half-Second catalogue|LHS]]&nbsp;439, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]]&nbsp;185213, [[Hipparcos catalogue|HIP]]&nbsp;84478
| names4={{odlist | F=30 Sco | CD=-26°12036 | GJ=664 | HD=156026 | HIP=84478 | LHS=439 | PLX=3913.00 | SAO=185213 | V=V2215 Oph}}
 
}}
}}
{{Starbox reference
{{Starbox reference
Line 110: Line 116:
| Simbad3 = HD+155885|sn3=B
| Simbad3 = HD+155885|sn3=B
| Simbad4 = HD+156026|sn4=C
| Simbad4 = HD+156026|sn4=C
| NSTED = GJ+663A|nn=A
| NSTED = GJ 663B|nn=B
| NSTED2 = GJ+663B|nn2=B
| NSTED2 = GJ 664|nn2=C
| NSTED3 = GJ+664|nn3=C
| ARICNS = 01379|an=A
| ARICNS = 01379|an=A
| ARICNS2 = 01380|an2=B
| ARICNS2 = 01380|an2=B
Line 120: Line 125:


'''36 Ophiuchi''' (or '''Guniibuu''' for component A) is a triple [[star system]] 19.5 [[light-year]]s from [[Earth]] in the [[constellation]] [[Ophiuchus]].
'''36 Ophiuchi''' (or '''Guniibuu''' for component A) is a triple [[star system]] 19.5 [[light-year]]s from [[Earth]] in the [[constellation]] [[Ophiuchus]].
==Nomenclature==
''36 Ophiuchi'' is the system's [[Flamsteed designation]]. Component C (HD 156026) was also historically called ''30 Scorpii''.<ref name=Wagman1987/>
In the culture of the [[Kamilaroi]] and [[Euahlayi]] Aboriginal peoples in [[New South Wales]], Australia, the star is called ''Guniibuu'' and represents the robin red-breast bird ([[scarlet robin|''Petroica boodang'']]).<ref name=IAU-CSN/> In 2016, the [[IAU]] organized a [[Working Group on Star Names]] (WGSN)<ref name="WGSN">{{cite web | url=https://www.iau.org/science/scientific_bodies/working_groups/280/ | title=IAU Working Group on Star Names (WGSN)|access-date=17 September 2018}}</ref> to catalog and standardize proper names for stars. The WGSN approved the name ''Guniibuu'' for 36 Ophiuchi A on 10 August 2018 and it is now so included in the List of IAU-approved Star Names.<ref name=IAU-CSN/>


==Characteristics==
==Characteristics==
The primary and secondary stars (also known as HD 155886) are nearly identical orange [[main-sequence]] dwarfs of [[spectral type]] K2/K1. This binary is unusual because its eruptions do not seem to conform to the Waldmeier effect; that is, the strongest eruptions of HD 155886 are not the ones characterized by the fast eruption onset.<ref>{{citation|arxiv=1909.12148|year=2019|title=Waldmeier Effect in Stellar Cycles|doi=10.3847/1538-4357/ab4a17|last1=Garg|first1=Suyog|last2=Karak|first2=Bidya Binay|last3=Egeland|first3=Ricky|last4=Soon|first4=Willie|last5=Baliunas|first5=Sallie|journal=The Astrophysical Journal|volume=886|issue=2|page=132|bibcode=2019ApJ...886..132G|s2cid=202888617 |doi-access=free }}</ref> The tertiary star is an orange main-sequence dwarf of [[spectral type]] K5.
The primary and secondary stars (also known as HD 155886) are nearly identical orange [[main-sequence]] dwarfs of [[spectral type]] K2/K1. This binary is unusual because its eruptions do not seem to conform to the [[Waldmeier effect]]; that is, the strongest eruptions of HD 155886 are not the ones characterized by the fast eruption onset.<ref>{{cite journal|arxiv=1909.12148|year=2019|title=Waldmeier Effect in Stellar Cycles|doi=10.3847/1538-4357/ab4a17|last1=Garg|first1=Suyog|last2=Karak|first2=Bidya Binay|last3=Egeland|first3=Ricky|last4=Soon|first4=Willie|last5=Baliunas|first5=Sallie|journal=The Astrophysical Journal|volume=886|issue=2|page=132|bibcode=2019ApJ...886..132G|s2cid=202888617 |doi-access=free }}</ref>


[[Image:V2215OphLightCurve.png|300px|thumb|left|A [[Photometric system#Photometric letters|visual band]] [[light curve]] for 36 Ophiuchi C (V2215 Ophiuchi), plotted from ''[[All Sky Automated Survey for SuperNovae|ASAS-SN]]'' data<ref name="ASAS-SN"/>]]
[[Image:V2215OphLightCurve.png|300px|thumb|left|A [[Photometric system#Photometric letters|visual band]] [[light curve]] for 36 Ophiuchi C (V2215 Ophiuchi), plotted from ''[[All Sky Automated Survey for SuperNovae|ASAS-SN]]'' data<ref name="ASAS-SN"/>]]
The tertiary star is an orange main-sequence dwarf of [[spectral type]] K5. The age for this star derived using [[gyrochronology]] is about 600 million years, while the age derived for the AB pair is 1.43 billion years. This discrepancy suggest that the A/B stars interacted with each other and slowed down their rotation periods, providing a spuriously higher age.<ref name=Otani2022/>


Star C is separated from the A-B pair by 700 [[arcseconds]], compared to a minimum of 4.6 arcseconds for A-B, so its effect on the movements of the A-B pair is small. A and B have active [[chromosphere]]s.
Star C is separated from the A-B pair by 700 [[arcseconds]], compared to a minimum of 4.6 arcseconds for A-B, so its effect on the movements of the A-B pair is small. A and B have active [[chromosphere]]s.
At present the distance between the stars forming the AB-pair is 5.1 arcseconds and the position angle is 139 degrees, while star C is 731.6 arcseconds away from the A-component and situated at a position angle of 74 degrees.
At present the distance between the stars forming the AB-pair is 5.1 arcseconds and the position angle is 139 degrees, while star C is 731.6 arcseconds away from the A-component and situated at a position angle of 74 degrees.
==Nomenclature==
In the beliefs of the [[Kamilaroi]] and [[Euahlayi]] Aboriginal peoples in [[New South Wales]], Australia, the star is called ''Guniibuu'' that represents the robin red-breast bird ([[scarlet robin|''Petroica boodang'']]). In 2016, the [[IAU]] organized a [[Working Group on Star Names]] (WGSN)<ref name="WGSN">{{cite web | url=https://www.iau.org/science/scientific_bodies/working_groups/280/ | title=IAU Working Group on Star Names (WGSN)|access-date=17 September 2018}}</ref> to catalog and standardize proper names for stars. The WGSN approved the name ''Guniibuu'' for the star A on 10 August 2018 and it is now so included in the List of IAU-approved Star Names.<ref name="IAU-CSN">{{Cite web
|url=http://www.pas.rochester.edu/~emamajek/WGSN/IAU-CSN.txt
|title=IAU Catalog of Star Names
|publisher=[[International Astronomical Union]]
|access-date=2018-09-17}}</ref>


==Hunt for substellar objects==
==Hunt for substellar objects==
The [[McDonald Observatory]] team has set limits to the presence of one or more planets<ref name="search"/> around 36 Ophiuchi A with masses between 0.13 and 5.4 [[Jupiter mass]]es and average separations spanning between 0.05 and 5.2 [[astronomical unit]]s (AU), although beyond 1.5 AU orbits are inherently unstable around either 36 Ophiuchi A or 36 Ophiuchi B.<ref name="Irwin">Irwin ''et al.'' (1996).</ref>
The [[McDonald Observatory]] team has set limits to the presence of one or more planets<ref name=Wittenmyer2006/> around 36 Ophiuchi A with masses between 0.13 and 5.4 [[Jupiter mass]]es and average separations spanning between 0.05 and 5.2 [[astronomical unit]]s (AU), although beyond 1.5 AU orbits are inherently unstable around either 36 Ophiuchi A or 36 Ophiuchi B.<ref name=Irwin1996/>


The star C (or namely HD 156026) is among five nearby paradigms as [[K-type star]]s of a type in a 'sweet spot’ between Sun-analog stars and [[M-class star|M stars]] for the likelihood of evolved life, per analysis of Giada Arney from [[NASA]]'s [[Goddard Space Flight Center]].<ref name=Nasa2019-03-07/>
The star C (or namely HD 156026) is among five nearby paradigms as [[K-type star]]s of a type in a 'sweet spot’ between Sun-analog stars and [[M-class star|M stars]] for the likelihood of evolved life, per analysis of Giada Arney from [[NASA]]'s [[Goddard Space Flight Center]].<ref name=Nasa2019-03-07/> It presents a significant difference on [[proper motion]] measurements taken by the [[Hipparcos]] and [[Gaia (spacecraft)|Gaia]] spacecrafts, suggesting the presence of a giant planet.<ref name=Painter2025/>


==Observation==
==Observation==
On 26 October 2021, it was occulted by [[Venus]] as viewed from the [[Indian Ocean]].<ref name="Mus2002">{{cite book |date=2002 |first=Jan |last=Meeus |chapter=Mutual occultations of planets |pages=174–185 |title=More Mathematical Astronomy Morsels |publisher=Willmann-Bell |isbn=0943396743 |url=https://falakmu.id/khgt/dokumen/More%20mathematical%20astronomy%20morsels%20(Jean%20Meeus)%20(Z-Library).pdf}}</ref>{{rp|165}}


On 26 October 2021, it was occulted by [[Venus]] as viewed from the [[Indian Ocean]].<ref name="Mus2002">{{cite book |date=2002 |first=Jan |last=Meeus |chapter=Mutual occultations of planets |pages=174–185 |title=More Mathematical Astronomy Morsels |isbn=0943396743 |url=https://falakmu.id/khgt/dokumen/More%20mathematical%20astronomy%20morsels%20(Jean%20Meeus)%20(Z-Library).pdf}}</ref>{{rp|165}}
==See also==
 
* [[List of nearest stars by spectral type#List of nearest K-type stars|List of nearest K-type stars]]
==Notes==
{{Notelist}}


==References==
==References==


{{Reflist|refs=
{{Reflist|refs=
<ref name="SIMBAD">{{cite web
| url=http://simbad.u-strasbg.fr/
| title=SIMBAD Astronomical Database
| publisher=[[Centre de Données astronomiques de Strasbourg]]
| access-date=2013-08-23
}}<br/>
* A: [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD%20155886 LHS 437 -- High proper-motion Star]
* B: [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD%20155885 LHS 438 -- High proper-motion Star ]
* C: [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD%20156026 V* V2215 Oph -- Variable of RS CVn type]</ref>


<ref name=Nasa2019-03-07>
<ref name=Nasa2019-03-07>
Line 166: Line 179:


<ref name="ASAS-SN">{{cite web |url=https://asas-sn.osu.edu/variables/lookup |website=ASAS-SN Variable Stars Database|title=ASAS-SN Variable Stars Database|publisher=ASAS-SN |access-date=6 January 2022}}</ref>
<ref name="ASAS-SN">{{cite web |url=https://asas-sn.osu.edu/variables/lookup |website=ASAS-SN Variable Stars Database|title=ASAS-SN Variable Stars Database|publisher=ASAS-SN |access-date=6 January 2022}}</ref>
<ref name=Gray2006>{{cite journal | display-authors=1 | last1=Gray | first1=R. O. | last2=Corbally | first2=C. J. | last3=Garrison | first3=R. F. | last4=McFadden | first4=M. T. | last5=Bubar | first5=E. J. | last6=McGahee | first6=C. E. | last7=O'Donoghue | first7=A. A. | last8=Knox | first8=E. R. | title=Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample | journal=[[The Astronomical Journal]] | volume=132 | issue=1 | pages=161–170 |date=July 2006 | doi=10.1086/504637 | bibcode=2006AJ....132..161G | arxiv=astro-ph/0603770 | s2cid=119476992 }}</ref>


<ref name=Hardegree-Ullman2023>{{Cite journal |last1=Hardegree-Ullman |first1=Kevin K. |last2=Apai |first2=Dániel |last3=Bergsten |first3=Galen J. |last4=Pascucci |first4=Ilaria |last5=López-Morales |first5=Mercedes |date=2023-06-01 |title=Bioverse: A Comprehensive Assessment of the Capabilities of Extremely Large Telescopes to Probe Earth-like O2 Levels in Nearby Transiting Habitable-zone Exoplanets |bibcode=2023AJ....165..267H |journal=[[The Astronomical Journal]] |volume=165 |issue=6 |pages=267 |doi=10.3847/1538-3881/acd1ec |doi-access=free |arxiv=2304.12490 |issn=0004-6256}} [https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/AJ/165/267&Name=*%2036%20Oph%20A 36 Ophiuchi A's database entry] at [[VizieR]].</ref>
<ref name=Hardegree-Ullman2023>{{Cite journal |last1=Hardegree-Ullman |first1=Kevin K. |last2=Apai |first2=Dániel |last3=Bergsten |first3=Galen J. |last4=Pascucci |first4=Ilaria |last5=López-Morales |first5=Mercedes |date=2023-06-01 |title=Bioverse: A Comprehensive Assessment of the Capabilities of Extremely Large Telescopes to Probe Earth-like O2 Levels in Nearby Transiting Habitable-zone Exoplanets |bibcode=2023AJ....165..267H |journal=[[The Astronomical Journal]] |volume=165 |issue=6 |pages=267 |doi=10.3847/1538-3881/acd1ec |doi-access=free |arxiv=2304.12490 |issn=0004-6256}} [https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/AJ/165/267&Name=*%2036%20Oph%20A 36 Ophiuchi A's database entry] at [[VizieR]].</ref>
<ref name=Otani2022>{{Cite journal |last1=Otani |first1=Tomomi |last2=von Hippel |first2=Ted |last3=Buzasi |first3=Derek |last4=Oswalt |first4=T. D. |last5=Stone-Martinez |first5=Alexander |last6=Majewski |first6=Patrice |date=2022-05-01 |title=A Monte Carlo Method for Evaluating Empirical Gyrochronology Models and Its Application to Wide Binary Benchmarks |journal=[[The Astrophysical Journal]] |volume=930 |issue=1 |pages=36 |doi=10.3847/1538-4357/ac6035 |doi-access=free |arxiv=2105.07266 |bibcode=2022ApJ...930...36O |issn=0004-637X}}</ref>
<ref name=Painter2025>{{Cite journal |last1=Painter |first1=Katie E. |last2=Bowler |first2=Brendan P. |last3=Franson |first3=Kyle |last4=Becker |first4=Juliette C. |last5=Burt |first5=Jennifer A. |title=Astrometric Accelerations of Provisional Targets for the Habitable Worlds Observatory |date=2025-06-26 |arxiv=2506.21768 |journal=The Astronomical Journal |volume=170 |issue=3 |page=147 |doi=10.3847/1538-3881/ade442 |bibcode=2025AJ....170..147P |doi-access=free }}</ref>


<ref name=aaa505_1_205>{{cite journal
<ref name=aaa505_1_205>{{cite journal
Line 193: Line 212:
  }}</ref>
  }}</ref>


<ref name=tic>{{Cite journal |last1=Stassun |first1=Keivan G. |last2=Oelkers |first2=Ryan J. |last3=Paegert |first3=Martin |last4=Torres |first4=Guillermo |last5=Pepper |first5=Joshua |last6=De Lee |first6=Nathan |last7=Collins |first7=Kevin |last8=Latham |first8=David W. |last9=Muirhead |first9=Philip S. |last10=Chittidi |first10=Jay |last11=Rojas-Ayala |first11=Bárbara |last12=Fleming |first12=Scott W. |last13=Rose |first13=Mark E. |last14=Tenenbaum |first14=Peter |last15=Ting |first15=Eric B. |date=2019-10-01 |title=The Revised TESS Input Catalog and Candidate Target List |journal=The Astronomical Journal |volume=158 |issue=4 |pages=138 |doi=10.3847/1538-3881/ab3467 |doi-access=free |arxiv=1905.10694 |bibcode=2019AJ....158..138S |issn=0004-6256}} Database entries at [[VizieR]]:[https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=IV/38&TIC=1277142190 36 Oph B]<br>[https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=IV/38&TIC=79841001 36 Oph C]</ref>
<ref name="search">Wittenmeyer ''et al.'' (2006).</ref>
 
<ref name=Irwin1996>{{cite journal|last1=Irwin |first1=Alan W. |last2=Yang |first2=Stephenson L. S. |last3=Walker |first3=Gordon A. H. |name-list-style=amp |date=1996 |title=36 Ophiuchi AB: Incompatibility of the Orbit and Precise Radial Velocities |journal=Publications of the Astronomical Society of the Pacific |volume=108 |pages=580 |doi=10.1086/133768 |bibcode=1996PASP..108..580I|doi-access=free }}</ref>
 
<ref name=Wittenmyer2006>{{cite journal|last1=Wittenmyer |first1=R. A. |last2=Endl |first2=Michael |last3=Cochran |first3=William D. |last4=Hatzes |first4=Artie P. |last5=Walker |first5=G. A. H. |last6=Yang |first6=S. L. S. |last7=Paulson |first7=Diane B. |name-list-style=amp |date=2006 |title=Detection Limits from the McDonald Observatory Planet Search Program |journal=Astronomical Journal |volume=132 |issue=1 |pages=177–188 |doi=10.1086/504942 |bibcode=2006AJ....132..177W|arxiv = astro-ph/0604171 |s2cid=16755455 }}</ref>


<ref name=Tokovinin2017>{{Cite journal |last=Tokovinin |first=Andrei |date=July 2017 |title=Orbit Alignment in Triple Stars |journal=The Astrophysical Journal |language=en |volume=844 |issue=2 |pages=103 |doi=10.3847/1538-4357/aa7746 |doi-access=free |arxiv=1706.00748 |bibcode=2017ApJ...844..103T |issn=0004-637X}}</ref>
<ref name=Tokovinin2017>{{Cite journal |last=Tokovinin |first=Andrei |date=July 2017 |title=Orbit Alignment in Triple Stars |journal=The Astrophysical Journal |language=en |volume=844 |issue=2 |pages=103 |doi=10.3847/1538-4357/aa7746 |doi-access=free |arxiv=1706.00748 |bibcode=2017ApJ...844..103T |issn=0004-637X}}</ref>


<ref name=Luck2018>{{Cite journal |last=Luck |first=R. Earle |date=2018-03-01 |title=Abundances in the Local Region. III. Southern F, G, and K Dwarfs |bibcode=2018AJ....155..111L |journal=The Astronomical Journal |volume=155 |issue=3 |pages=111 |doi=10.3847/1538-3881/aaa9b5 |doi-access=free |issn=0004-6256}} [https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/AJ/155/111&ID=*%2036%20Oph%20B 36 Ophiuchi B's database entry] at [[VizieR]].</ref>
<ref name=Luck2018>{{Cite journal |last=Luck |first=R. Earle |date=2018-03-01 |title=Abundances in the Local Region. III. Southern F, G, and K Dwarfs |bibcode=2018AJ....155..111L |journal=The Astronomical Journal |volume=155 |issue=3 |pages=111 |doi=10.3847/1538-3881/aaa9b5 |doi-access=free |issn=0004-6256}} Database entries at [[VizieR]]:<br>[https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/AJ/155/111&ID=*%2036%20Oph%20B 36 Ophiuchi B]<br>[https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/AJ/155/111&ID=V*%20V2215%20Oph 36 Ophiuchi C]</ref>


<ref name=Luck2017>{{Cite journal |last=Luck |first=R. Earle |date=2017-01-01 |title=Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants |bibcode=2017AJ....153...21L |journal=The Astronomical Journal |volume=153 |issue=1 |pages=21 |doi=10.3847/1538-3881/153/1/21 |doi-access=free |issn=0004-6256|arxiv=1611.02897 }}[https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/AJ/153/21&Name=36%20Oph%20A 36 Ophiuchi A's database entry] at [[VizieR]].</ref>
<ref name=Luck2017>{{Cite journal |last=Luck |first=R. Earle |date=2017-01-01 |title=Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants |bibcode=2017AJ....153...21L |journal=The Astronomical Journal |volume=153 |issue=1 |pages=21 |doi=10.3847/1538-3881/153/1/21 |doi-access=free |issn=0004-6256|arxiv=1611.02897 }}[https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/AJ/153/21&Name=36%20Oph%20A 36 Ophiuchi A's database entry] at [[VizieR]].</ref>
<ref name=IAU-CSN>{{cite web |title=IAU Catalog of Star Names |url=https://exopla.net/star-names/modern-iau-star-names/ |access-date=20 November 2025}}</ref>
<ref name=Wagman1987>{{cite journal | last=Wagman | first=M. | title=Flamsteed's Missing Stars | journal=Journal for the History of Astronomy | volume=18 | issue=3 | page=211 |date=August 1987 | bibcode=1987JHA....18..209W | doi=10.1177/002182868701800305| s2cid=118445625 }}</ref>


}}
}}


==Further reading==
==Further reading==
*{{Citation |last1=Irwin |first1=Alan W. |last2=Yang |first2=Stephenson L. S. |last3=Walker |first3=Gordon A. H. |name-list-style=amp |date=1996 |title=36 Ophiuchi AB: Incompatibility of the Orbit and Precise Radial Velocities |journal=Publications of the Astronomical Society of the Pacific |volume=108 |pages=580 |doi=10.1086/133768 |bibcode=1996PASP..108..580I|doi-access=free }}
*{{cite journal|last1=Cayrel de Strobel |first1=G. |last2=Lebreton |first2=Y. |last3=Perrin |first3=M.-N. |last4=Cayrel |first4=R. |name-list-style=amp |date=1989 |title=A thorough spectroscopic study of the very nearby triple system - 36 Ophiuchi |journal=Astronomy and Astrophysics |volume=225 |issue=2 |pages=369–380 |bibcode = 1989A&A...225..369C }}
*{{Citation |last1=Cayrel de Strobel |first1=G. |last2=Lebreton |first2=Y. |last3=Perrin |first3=M.-N. |last4=Cayrel |first4=R. |name-list-style=amp |date=1989 |title=A thorough spectroscopic study of the very nearby triple system - 36 Ophiuchi |journal=Astronomy and Astrophysics |volume=225 |issue=2 |pages=369–380 |bibcode = 1989A&A...225..369C }}
*{{cite journal|last=Barnes |first=Sydney A. |date=2007 |title=Ages for Illustrative Field Stars Using Gyrochronology: Viability, Limitations, and Errors |journal=The Astrophysical Journal |volume=669 |issue=2 |pages=1167–1189 |doi=10.1086/519295 |bibcode=2007ApJ...669.1167B|arxiv = 0704.3068 |s2cid=14614725 }}
*{{Citation |last1=Wittenmeyer |first1=R. A. |last2=Endl |first2=Michael |last3=Cochran |first3=William D. |last4=Hatzes |first4=Artie P. |last5=Walker |first5=G. A. H. |last6=Yang |first6=S. L. S. |last7=Paulson |first7=Diane B. |name-list-style=amp |date=2006 |title=Detection Limits from the McDonald Observatory Planet Search Program |journal=Astronomical Journal |volume=132 |issue=1 |pages=177–188 |doi=10.1086/504942 |bibcode=2006AJ....132..177W|arxiv = astro-ph/0604171 |s2cid=16755455 }}
*{{Citation |last=Barnes |first=Sydney A. |date=2007 |title=Ages for Illustrative Field Stars Using Gyrochronology: Viability, Limitations, and Errors |journal=The Astrophysical Journal |volume=669 |issue=2 |pages=1167–1189 |doi=10.1086/519295 |bibcode=2007ApJ...669.1167B|arxiv = 0704.3068 |s2cid=14614725 }}


==External links==
==External links==
* {{cite web |
* {{cite web | title=36 Ophiuchi |  work=SolStation | url=http://www.solstation.com/stars/36ophiu3.htm | access-date=3 November 2005 }}
title=36 Ophiuchi |  
  work=SolStation |
url=http://www.solstation.com/stars/36ophiu3.htm |
access-date=3 November 2005 }}
* https://arxiv.org/abs/astro-ph/0604171
{{Nearest systems|3}}
{{Nearest systems|3}}
{{Stars of Ophiuchus}}
{{Stars of Ophiuchus}}

Latest revision as of 19:38, 9 December 2025

Template:Short description Template:Sky

36 Ophiuchi
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Observation data
Epoch J2000      Equinox J2000
Constellation Ophiuchus
Right ascension A: Template:RA[1]
B: Template:RA[2]
C: Template:RA[3]
Declination A: Template:DEC[1]
B: Template:DEC[2]
C: Template:DEC[3]
Apparent magnitude (V) 5.08/5.03/6.34[4]
Characteristics
Spectral type A: K2V[5]
B: K1V[5]
C: K5V[5]
Variable type C: RS CVn
Astrometry
36 Oph A
Radial velocity (Rv)Script error: No such module "val".[1] km/s
Proper motion (μ) RA: Script error: No such module "val". mas/yr[1]
Dec.: Script error: No such module "val". mas/yr[1]
Parallax (π)168.0031±0.1343 mas[1]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd pc)
36 Oph B
Radial velocity (Rv)Script error: No such module "val".[4] km/s
Proper motion (μ) RA: Script error: No such module "val". mas/yr[2]
Dec.: Script error: No such module "val". mas/yr[2]
Parallax (π)168.1303±0.1081 mas[2]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd pc)
36 Oph C
Radial velocity (Rv)Script error: No such module "val".[3] km/s
Proper motion (μ) RA: Script error: No such module "val". mas/yr[3]
Dec.: Script error: No such module "val". mas/yr[3]
Parallax (π)167.9617±0.0311 mas[3]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd pc)
Orbit[6]
Primary36 Oph A
Companion36 Oph B
Period (P)470.9 yr
Semi-major axis (a)13″
Eccentricity (e)0.916
Inclination (i)99.8°
Details
36 Oph A
MassScript error: No such module "val".[7] Template:Solar mass
RadiusScript error: No such module "val".[8] Template:Solar radius
LuminosityScript error: No such module "val".[9] Template:Solar luminosity
TemperatureScript error: No such module "val".[7] K
Metallicity [Fe/H]Script error: No such module "val".[7] dex
RotationScript error: No such module "val".[10] days
Age1.43[10] Gyr
36 Oph B
MassScript error: No such module "val".[11] Template:Solar mass
RadiusScript error: No such module "val".[12] Template:Solar radius
Luminosity0.32[11] Template:Solar luminosity
Surface gravity (log g)4.61[11] cgs
TemperatureScript error: No such module "val".[11] K
Metallicity [Fe/H]Script error: No such module "val".[11] dex
RotationScript error: No such module "val".[10] days
Age1.43[10] Gyr
36 Oph C
MassScript error: No such module "val".[11] Template:Solar mass
RadiusScript error: No such module "val".[12] Template:Solar radius
Luminosity0.14[11] Template:Solar luminosity
Habitable zone inner limit0.32[13] AU
Habitable zone outer limit0.79[13] AU
Surface gravity (log g)4.70[11] cgs
TemperatureScript error: No such module "val".[11] K
Metallicity [Fe/H]Script error: No such module "val".[11] dex
RotationScript error: No such module "val".[10] days
AgeScript error: No such module "val".[10] Myr
Metallicity [Fe/H]{{{metal_fe2}}} dex
Other designations
Template:Odlist
AB: Template:Odlist
A: Template:Odlist
B: Template:Odlist
C: Template:Odlist
Database references
SIMBADAB
A
B
C
Exoplanet ArchiveB
C
ARICNSA
B
C

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36 Ophiuchi (or Guniibuu for component A) is a triple star system 19.5 light-years from Earth in the constellation Ophiuchus.

Nomenclature

36 Ophiuchi is the system's Flamsteed designation. Component C (HD 156026) was also historically called 30 Scorpii.[14]

In the culture of the Kamilaroi and Euahlayi Aboriginal peoples in New South Wales, Australia, the star is called Guniibuu and represents the robin red-breast bird (Petroica boodang).[15] In 2016, the IAU organized a Working Group on Star Names (WGSN)[16] to catalog and standardize proper names for stars. The WGSN approved the name Guniibuu for 36 Ophiuchi A on 10 August 2018 and it is now so included in the List of IAU-approved Star Names.[15]

Characteristics

The primary and secondary stars (also known as HD 155886) are nearly identical orange main-sequence dwarfs of spectral type K2/K1. This binary is unusual because its eruptions do not seem to conform to the Waldmeier effect; that is, the strongest eruptions of HD 155886 are not the ones characterized by the fast eruption onset.[17]

File:V2215OphLightCurve.png
A visual band light curve for 36 Ophiuchi C (V2215 Ophiuchi), plotted from ASAS-SN data[18]

The tertiary star is an orange main-sequence dwarf of spectral type K5. The age for this star derived using gyrochronology is about 600 million years, while the age derived for the AB pair is 1.43 billion years. This discrepancy suggest that the A/B stars interacted with each other and slowed down their rotation periods, providing a spuriously higher age.[10]

Star C is separated from the A-B pair by 700 arcseconds, compared to a minimum of 4.6 arcseconds for A-B, so its effect on the movements of the A-B pair is small. A and B have active chromospheres. At present the distance between the stars forming the AB-pair is 5.1 arcseconds and the position angle is 139 degrees, while star C is 731.6 arcseconds away from the A-component and situated at a position angle of 74 degrees.

Hunt for substellar objects

The McDonald Observatory team has set limits to the presence of one or more planets[19] around 36 Ophiuchi A with masses between 0.13 and 5.4 Jupiter masses and average separations spanning between 0.05 and 5.2 astronomical units (AU), although beyond 1.5 AU orbits are inherently unstable around either 36 Ophiuchi A or 36 Ophiuchi B.[20]

The star C (or namely HD 156026) is among five nearby paradigms as K-type stars of a type in a 'sweet spot’ between Sun-analog stars and M stars for the likelihood of evolved life, per analysis of Giada Arney from NASA's Goddard Space Flight Center.[21] It presents a significant difference on proper motion measurements taken by the Hipparcos and Gaia spacecrafts, suggesting the presence of a giant planet.[13]

Observation

On 26 October 2021, it was occulted by Venus as viewed from the Indian Ocean.[22]Template:Rp

See also

References

<templatestyles src="Reflist/styles.css" />

  1. ↑ a b c d e Template:Cite Gaia DR3
  2. ↑ a b c d Template:Cite Gaia DR3
  3. ↑ a b c d e Template:Cite Gaia DR3
  4. ↑ a b Script error: No such module "citation/CS1".
  5. ↑ a b c Script error: No such module "Citation/CS1".
  6. ↑ Script error: No such module "Citation/CS1".
  7. ↑ a b c Script error: No such module "Citation/CS1".36 Ophiuchi A's database entry at VizieR.
  8. ↑ Script error: No such module "Citation/CS1".
  9. ↑ Script error: No such module "Citation/CS1". 36 Ophiuchi A's database entry at VizieR.
  10. ↑ a b c d e f g Script error: No such module "Citation/CS1".
  11. ↑ a b c d e f g h i j Script error: No such module "Citation/CS1". Database entries at VizieR:
    36 Ophiuchi B
    36 Ophiuchi C
  12. ↑ a b Script error: No such module "Citation/CS1". Database entries at VizieR:36 Oph B
    36 Oph C
  13. ↑ a b c Script error: No such module "Citation/CS1".
  14. ↑ Script error: No such module "Citation/CS1".
  15. ↑ a b Script error: No such module "citation/CS1".
  16. ↑ Script error: No such module "citation/CS1".
  17. ↑ Script error: No such module "Citation/CS1".
  18. ↑ Script error: No such module "citation/CS1".
  19. ↑ Script error: No such module "Citation/CS1".
  20. ↑ Script error: No such module "Citation/CS1".
  21. ↑ Script error: No such module "citation/CS1".
  22. ↑ Script error: No such module "citation/CS1".

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Further reading

  • Script error: No such module "Citation/CS1".
  • Script error: No such module "Citation/CS1".

External links

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Template:Nearest systems Template:Stars of Ophiuchus

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