47 Ophiuchi
{{Short description|Star in the constellation Ophiuchus}}
{{Starbox begin|name=47 Ophiuchi}}
{{Starbox image
| image = 250px
| caption = 47 Ophiuchi (right) with the globular cluster NGC 6366
}}
{{Starbox observe
|epoch=J2000
|constell=Ophiuchus{{cite web |url=http://djm.cc/constellation.html |title=Finding the constellation which contains given sky coordinates |date=2 August 2008 |website=djm.cc |access-date=23 May 2024 |archive-date=15 August 2019 |archive-url=https://web.archive.org/web/20190815143107/http://djm.cc/constellation.html |url-status=live }}
|appmag_v=4.54{{cite journal|bibcode=2002yCat.2237....0D|title=VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system|journal=CDS/ADC Collection of Electronic Catalogues|volume=2237|author1=Ducati, J. R.|year=2002}} (4.93 / 5.83)
}}
{{Starbox character
}}
{{Starbox astrometry
|prop_mo_ra=−93.066
|prop_mo_dec=−43.198
|parallax=30.9863
|p_error=0.1581
|absmag_v=
}}
{{Starbox orbit
|period_unitless={{nowrap|26.27565 ± 0.00004 d}}
|axis_unitless={{val|7.99|0.10|ul=mas}}
|inclination={{val|59.5|1.3}}
|node={{val|121.8|1.0}}
|periastron={{nowrap|JD 2448103.380{{±|0.026}}}}
|eccentricity={{val|0.481|0.002}}
|periarg={{val|27.04|0.54}}
|k1={{val|46.92|0.40}}
|k2={{val|52.80|0.39}}
}}
{{Starbox detail
|component1=A
|mass={{val|1.50|0.06}}
|radius={{val|2.06|0.07}}
|luminosity={{val|7.80|0.36}}
|component2=B
|mass2={{val|1.34|0.06}}
|radius2={{val|1.36|0.06}}
|luminosity2={{val|3.41|0.25}}
}}
{{Starbox detail|no_heading=y
|component1=C
|temperature={{val|1580|10|fmt=commas}}
}}
{{Starbox catalog
|names={{odlist|BD=−04°4275|FK5=647|HD=157950|HIP=85365|HR=6493|SAO=141665}}
}}
{{Starbox reference
|Simbad=47+Oph
}}
{{Starbox end}}
47 Ophiuchi (47 Oph) is a binary star in the constellation Ophiuchus. The combined apparent magnitude of the system is 4.54. The system is located about {{convert|105.3|ly|pc|lk=on|abbr=off}} away, based on its parallax as measured by Gaia.
47 Ophiuchi is a spectroscopic binary: that is, the two stars move fast enough that periodic Doppler shifts in the stars' spectra can be detected. In this case, the two stars have also been resolved using interferometry. The primary star is an F-type main-sequence star, that is 1.5 times the mass of the Sun and around twice as wide. Its companion star is 1.34 times the mass of the Sun, and 1.36 times the radius of the Sun. The two stars orbit each other every 26.3 days, and its orbital eccentricity is 0.481.
The designation 47 Ophiuchi was originally used for the star HR 6496.{{cite journal|last=Wagman|first=M.|title=Flamsteed's Missing Stars|journal=Journal for the History of Astronomy|number=3|volume=18|page=212|date=August 1987|bibcode=1987JHA....18..209W|doi=10.1177/002182868701800305|s2cid=118445625}} However, when constellation borders were redrawn, that star fell into the constellation Serpens, and the designation became used for this star, HR 6493, instead.{{cite journal|bibcode=1995yCat.5050....0H|title=VizieR Online Data Catalog: Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991)|journal=VizieR On-line Data Catalog: V/50. Originally Published in: 1964BS....C......0H|volume=5050|last1=Hoffleit|first1=D.|last2=Warren|first2=W. H.|year=1995}}
There is also a wider companion, a brown dwarf which has a projected separation of 8850 astronomical units from 47 Ophiuchi. It is a L-type brown dwarf with a spectral type of L5.5.{{Cite journal |last1=Deacon |first1=Niall R. |last2=Liu |first2=Michael C. |last3=Magnier |first3=Eugene A. |last4=Aller |first4=Kimberly M. |last5=Best |first5=William M. J. |last6=Dupuy |first6=Trent |last7=Bowler |first7=Brendan P. |last8=Mann |first8=Andrew W. |last9=Redstone |first9=Joshua A. |last10=Burgett |first10=William S. |last11=Chambers |first11=Kenneth C. |last12=Draper |first12=Peter W. |last13=Flewelling |first13=H. |last14=Hodapp |first14=Klaus W. |last15=Kaiser |first15=Nick |date=2014-09-01 |title=Wide Cool and Ultracool Companions to Nearby Stars from Pan-STARRS 1 |url=https://ui.adsabs.harvard.edu/abs/2014ApJ...792..119D |journal=The Astrophysical Journal |volume=792 |issue=2 |pages=119 |arxiv=1407.2938 |bibcode=2014ApJ...792..119D |doi=10.1088/0004-637X/792/2/119 |issn=0004-637X}} This object is 70 times more massive than Jupiter and is close to the hydrogen burning limit{{snd}}the dividing line between brown dwarfs and stars{{snd}}while its radius is only 0.93 times that of Jupiter.{{Cite journal |last1=Sanghi |first1=Aniket |last2=Liu |first2=Michael C. |last3=Best |first3=William M. J. |last4=Dupuy |first4=Trent J. |last5=Siverd |first5=Robert J. |last6=Zhang |first6=Zhoujian |last7=Hurt |first7=Spencer A. |last8=Magnier |first8=Eugene A. |last9=Aller |first9=Kimberly M. |last10=Deacon |first10=Niall R. |date=2023-11-08 |title=Table of Ultracool Fundamental Properties |url=https://zenodo.org/records/10086810 |journal=Zenodo |doi=10.5281/zenodo.10086810}}
References
{{reflist|refs=
{{Cite Gaia DR3|4362277714227206016}}
}}
{{Stars of Ophiuchus}}
{{DEFAULTSORT:47 Ophiuchi}}
Category:F-type main-sequence stars