36 Ophiuchi: Difference between revisions

From Wikipedia, the free encyclopedia
Browse history interactively
← Previous editNext edit →
Content deleted Content added
VisualWikitext
update and sorting
Citation bot (talk | contribs)
Bots
4,910,196 edits
Alter: title. Add: s2cid, bibcode, page, issue, volume, journal, doi, authors 1-5. Removed parameters. Some additions/deletions were parameter name changes. | Use this bot. Report bugs. | Suggested by Abductive | Category:Durchmusterung objects | #UCB_Category 197/3725
Line 86: Line 86:
'''36 Ophiuchi''' (or '''Guniibuu''' for A) is a [[triple star]] system 19.5 [[light year]]s from [[Earth]]. It is in the constellation [[Ophiuchus]].
'''36 Ophiuchi''' (or '''Guniibuu''' for A) is a [[triple star]] system 19.5 [[light year]]s from [[Earth]]. It is in the constellation [[Ophiuchus]].


The primary and secondary stars (also known ad HD 155886) are nearly identical orange [[main sequence]] dwarfs of [[spectral type]] K2/K1. This binary is unusual because its eruptions seems to do not conform to the Waldmeier Effect - i.e. 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}}</ref> The tertiary star is an orange [[main sequence]] dwarf of [[spectral type]] K5.
The primary and secondary stars (also known ad HD 155886) are nearly identical orange [[main sequence]] dwarfs of [[spectral type]] K2/K1. This binary is unusual because its eruptions seems to do not conform to the Waldmeier Effect - i.e. 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}}</ref> The tertiary star is an orange [[main sequence]] dwarf of [[spectral type]] K5.


Star C is separated from the A-B pair by 700 [[arc second]]s, compared to a minimum of 4.6 arcsec 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 [[arc second]]s, compared to a minimum of 4.6 arcsec for A-B, so its effect on the movements of the A-B pair is small. A and B have active [[chromosphere]]s.
Line 114: Line 114:
{{cite news
{{cite news
| url = https://www.nasa.gov/feature/goddard/2019/k-star-advantage
| url = https://www.nasa.gov/feature/goddard/2019/k-star-advantage
| title = “Goldilocks” Stars May Be “Just Right” for Finding Habitable Worlds
| title = "Goldilocks" Stars May Be "Just Right" for Finding Habitable Worlds
| work = [[NASA]]
| work = [[NASA]]
| author = Bill Steigerwald
| author = Bill Steigerwald
Line 123: Line 123:
</ref>
</ref>


<ref name=aaa505_1_205>{{citation | display-authors=1 | last1=Demory | first1=B.-O. | last2=Ségransan | first2=D. | last3=Forveille | first3=T. | last4=Queloz | first4=D. | last5=Beuzit | first5=J.-L. | last6=Delfosse | first6=X. | last7=di Folco | first7=E. | last8=Kervella | first8=P. | last9=Le Bouquin | first9=J.-B. |date=October 2009 | title=Mass-radius relation of low and very low-mass stars revisited with the VLTI | journal=Astronomy and Astrophysics | volume=505 | issue=1 | pages=205–215 | doi=10.1051/0004-6361/200911976 | bibcode=2009A&A...505..205D |arxiv = 0906.0602 }}</ref>
<ref name=aaa505_1_205>{{citation | display-authors=1 | last1=Demory | first1=B.-O. | last2=Ségransan | first2=D. | last3=Forveille | first3=T. | last4=Queloz | first4=D. | last5=Beuzit | first5=J.-L. | last6=Delfosse | first6=X. | last7=di Folco | first7=E. | last8=Kervella | first8=P. | last9=Le Bouquin | first9=J.-B. |date=October 2009 | title=Mass-radius relation of low and very low-mass stars revisited with the VLTI | journal=Astronomy and Astrophysics | volume=505 | issue=1 | pages=205–215 | doi=10.1051/0004-6361/200911976 | bibcode=2009A&A...505..205D |arxiv = 0906.0602 | s2cid=14786643 }}</ref>


<ref name=apjs161_2_444T>{{citation | last=Taylor | first=B. J. |date=December 2005 | title=Statistical Cataloging of Archival Data for Luminosity Class IV-V Stars. III. The Epoch 2004 [Fe/H] and Temperature Catalogs | journal=[[The Astrophysical Journal|The Astrophysical Journal Supplement Series]] | volume=161 | issue=2 | pages=444–455 | doi=10.1086/496885 | bibcode=2005ApJS..161..444T |postscript=. | doi-access=free }}[http://vizier.u-strasbg.fr/viz-bin/VizieR-5?-ref=VIZ52d212351f95&-out.add=.&-source=J/ApJS/161/444/catalog&recno=857 Vizier catalog entry]</ref>
<ref name=apjs161_2_444T>{{citation | last=Taylor | first=B. J. |date=December 2005 | title=Statistical Cataloging of Archival Data for Luminosity Class IV-V Stars. III. The Epoch 2004 [Fe/H] and Temperature Catalogs | journal=[[The Astrophysical Journal|The Astrophysical Journal Supplement Series]] | volume=161 | issue=2 | pages=444–455 | doi=10.1086/496885 | bibcode=2005ApJS..161..444T |postscript=. | doi-access=free }}[http://vizier.u-strasbg.fr/viz-bin/VizieR-5?-ref=VIZ52d212351f95&-out.add=.&-source=J/ApJS/161/444/catalog&recno=857 Vizier catalog entry]</ref>
Line 129: Line 129:
<ref name="search">Wittenmeyer ''et al.'' (2006).</ref>
<ref name="search">Wittenmeyer ''et al.'' (2006).</ref>


<ref name="MH08">{{Citation | last1=Mamajek | first1=Eric E. | last2=Hillenbrand | first2=Lynne A. | title=Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics | journal=The Astrophysical Journal | volume=687 | issue=2 | pages=1264–1293 | doi=10.1086/591785 | bibcode=2008ApJ...687.1264M |arxiv = 0807.1686 |date=November 2008}}</ref>
<ref name="MH08">{{Citation | last1=Mamajek | first1=Eric E. | last2=Hillenbrand | first2=Lynne A. | title=Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics | journal=The Astrophysical Journal | volume=687 | issue=2 | pages=1264–1293 | doi=10.1086/591785 | bibcode=2008ApJ...687.1264M |arxiv = 0807.1686 |date=November 2008| s2cid=27151456 }}</ref>


}}
}}


==Further reading==
==Further reading==
*{{Citation |last=Irwin |first=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 }}
*{{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 }}
*{{Citation |last=Cayrel de Strobel |first=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 }}
*{{Citation |last=Wittenmeyer |first=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 }}
*{{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 }}
*{{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==

Revision as of 22:46, 25 June 2021

36 Ophiuchi A/B/C
Observation data
Epoch J2000      Equinox J2000
Constellation Ophiuchus
Right ascension A: 17h 15m 20.851s
B: 17h 15m 20.978s
C: 17h 16m 13.3624s[1]
Declination A: −26° 36′ 09.04″
B: −26° 36′ 10.18″
C: −26° 32′ 46.129″[1]
Apparent magnitude (V) 5.08/5.03/6.34[1]
Characteristics
Spectral type K2 V/K1 V/K5 V[1]
U−B color index 0.51(AB)/1.04
B−V color index 0.85(AB)/1.16
Variable type C: RS CVn
Astrometry
Radial velocity (Rv)−0.6/0.0/−1.6[1] km/s
Proper motion (μ) RA: −488.2/−473/−480.06[1] mas/yr
Dec.: −1156.0/−1143/−1123.48[1] mas/yr
Parallax (π)167.1 ± 1.1 mas[1]
Distance19.5 ± 0.1 ly
(5.98 ± 0.04 pc)
Orbit
Companion36 Ophiuchi B
Period (P)568.9 yr
Semi-major axis (a)14.7″
Eccentricity (e)0.922
Inclination (i)99.6°
Longitude of the node (Ω)−83.6°
Periastron epoch (T)1763.39
Details
36 Oph A/B
Mass0.85/0.85 M☉
Radius0.817 ± 0.016[2]/0.81 R☉
Luminosity (bolometric)0.33/0.36[note 1] L☉
Luminosity (visual, LV)0.28/0.30 L☉
Temperature4,843 ± 134[2]/4,985 ± 20[3] K
MetallicityB: –0.31 ± 0.042[3] dex
Metallicity [Fe/H]A: –0.20[2] dex
Age0.6-1.8[4][5] Gyr
36 Oph C
Mass0.71 M☉
Radius0.72 R☉
Luminosity (bolometric)0.20[note 1] L☉
Luminosity (visual, LV)0.09 L☉
Temperature4,550 K
Metallicity46-100% Sun
Other designations
36 Oph, WDS J17153-2636
AB: GJ 663, CD−26°12026, GCTP 3908.00, HIP 84405
A: Guniibuu, HR 6402, HD 155886, LHS 437, SAO 185198
B: HR 6401, HD 155885, LHS 438, SAO 185199
C: V2215 Ophiuchi, GJ 664, CD−26°12036, HD 156026, GCTP 3913.00, LHS 439, SAO 185213, HIP 84478
Database references
SIMBADAB
A
B
C
Exoplanet ArchiveA
B
C
ARICNSA
B
C

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

The primary and secondary stars (also known ad HD 155886) are nearly identical orange main sequence dwarfs of spectral type K2/K1. This binary is unusual because its eruptions seems to do not conform to the Waldmeier Effect - i.e. strongest eruptions of HD 155886 are not the ones characterized by the fast eruption onset.[6] The tertiary star is an orange main sequence dwarf of spectral type K5.

Star C is separated from the A-B pair by 700 arc seconds, compared to a minimum of 4.6 arcsec for A-B, so its effect on the movements of the A-B pair is small. A and B have active chromospheres.

Nomenclature

In the Kamilaroi and Euahlayi Aboriginal peoples in modern-day New South Wales, Australia, the star A is called Guniibuu that represents the robin red-breast bird (Petroica boodang). In 2016, the IAU organized a Working Group on Star Names (WGSN)[7] 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.[8]

Hunt for substellar objects

The McDonald Observatory team has set limits to the presence of one or more planets[4] 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, although beyond 1.5 AU orbits are inherently unstable around either 36 Ophiuchi A or 36 Ophiuchi B.[9]

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.[10]

See also

Notes

  1. ^ a b From L=4πR2σTeff4, where L is the luminosity, R is the radius, Teff is the effective surface temperature and σ is the Stefan–Boltzmann constant.

References

  1. ^ a b c d e f g h "SIMBAD Astronomical Database". Centre de Données astronomiques de Strasbourg. Retrieved 2013-08-23.
  2. ^ a b c Demory, B.-O.; et al. (October 2009), "Mass-radius relation of low and very low-mass stars revisited with the VLTI", Astronomy and Astrophysics, 505 (1): 205–215, arXiv:0906.0602, Bibcode:2009A&A...505..205D, doi:10.1051/0004-6361/200911976, S2CID 14786643
  3. ^ a b Taylor, B. J. (December 2005), "Statistical Cataloging of Archival Data for Luminosity Class IV-V Stars. III. The Epoch 2004 [Fe/H] and Temperature Catalogs", The Astrophysical Journal Supplement Series, 161 (2): 444–455, Bibcode:2005ApJS..161..444T, doi:10.1086/496885.Vizier catalog entry
  4. ^ a b Wittenmeyer et al. (2006).
  5. ^ Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008), "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics", The Astrophysical Journal, 687 (2): 1264–1293, arXiv:0807.1686, Bibcode:2008ApJ...687.1264M, doi:10.1086/591785, S2CID 27151456
  6. ^ Garg, Suyog; Karak, Bidya Binay; Egeland, Ricky; Soon, Willie; Baliunas, Sallie (2019), "Waldmeier Effect in Stellar Cycles", The Astrophysical Journal, 886 (2): 132, arXiv:1909.12148, Bibcode:2019ApJ...886..132G, doi:10.3847/1538-4357/ab4a17, S2CID 202888617{{citation}}: CS1 maint: unflagged free DOI (link)
  7. ^ "IAU Working Group on Star Names (WGSN)". Retrieved 17 September 2018.
  8. ^ "IAU Catalog of Star Names". International Astronomical Union. Retrieved 2018-09-17.
  9. ^ Irwin et al. (1996).
  10. ^ Bill Steigerwald (2019-03-07). ""Goldilocks" Stars May Be "Just Right" for Finding Habitable Worlds". NASA. Retrieved 2020-05-12. 'I find that certain nearby K stars like 61 Cyg A/B, Epsilon Indi, Groombridge 1618, and HD 156026 may be particularly good targets for future biosignature searches,' said Arney.

Further reading

  • Irwin, Alan W.; Yang, Stephenson L. S. & Walker, Gordon A. H. (1996), "36 Ophiuchi AB: Incompatibility of the Orbit and Precise Radial Velocities", Publications of the Astronomical Society of the Pacific, 108: 580, Bibcode:1996PASP..108..580I, doi:10.1086/133768
  • Cayrel de Strobel, G.; Lebreton, Y.; Perrin, M.-N. & Cayrel, R. (1989), "A thorough spectroscopic study of the very nearby triple system - 36 Ophiuchi", Astronomy and Astrophysics, 225 (2): 369–380, Bibcode:1989A&A...225..369C
  • Wittenmeyer, R. A.; Endl, Michael; Cochran, William D.; Hatzes, Artie P.; Walker, G. A. H.; Yang, S. L. S. & Paulson, Diane B. (2006), "Detection Limits from the McDonald Observatory Planet Search Program", Astronomical Journal, 132 (1): 177–188, arXiv:astro-ph/0604171, Bibcode:2006AJ....132..177W, doi:10.1086/504942, S2CID 16755455
  • Barnes, Sydney A. (2007), "Ages for Illustrative Field Stars Using Gyrochronology: Viability, Limitations, and Errors", The Astrophysical Journal, 669 (2): 1167–1189, arXiv:0704.3068, Bibcode:2007ApJ...669.1167B, doi:10.1086/519295, S2CID 14614725

External links

Retrieved from "https://en.wikipedia.org/w/index.php?title=36_Ophiuchi&oldid=1030439429"