Xi Cancri
  | |
| Observation data EpochJ2000.0EquinoxJ2000.0(ICRS) | |
|---|---|
| Constellation | Cancer |
| Right ascension | 09h09m21.53325s[1] |
| Declination | +22° 02′ 43.6053″[1] |
| Apparent magnitude(V) | +5.15[2](5.70 + 6.20)[3] |
| Characteristics | |
| Spectral type | G9 III Fe-1 CH-0.5[4] |
| U−Bcolor index | +0.75[2] |
| B−Vcolor index | +0.96[2] |
| Astrometry | |
| Radial velocity(Rv) | +7.7±0.3[5]km/s |
| Proper motion(μ) | RA:−1.00[1]mas/yr Dec.:−0.52[1]mas/yr |
| Parallax(π) | 8.74 ± 0.49mas[1] |
| Distance | 370 ± 20ly (114 ± 6pc) |
| Absolute magnitude(MV) | −0.12[4] |
| Orbit[6][7] | |
| Period(P) | 1,700.76 d |
| Semi-major axis(a) | 0.0105±0.0017[3]″ |
| Eccentricity(e) | 0.06 |
| Periastronepoch(T) | 2,428,876.86 ± 10.0JD |
| Argument of periastron(ω) (secondary) | 301.1° |
| Semi-amplitude(K1) (primary) | 4.4 km/s |
| Details | |
| Luminosity | 118[8]L☉ |
| Temperature | 5,101[8]K |
| Other designations | |
| Database references | |
| SIMBAD | data |
Xi Cancri(ξ Cancri,abbreviatedXi Cnc,ξ Cnc) is aspectroscopic binarystar systemin thezodiacconstellationofCancer.It is visible to the naked eye with anapparent visual magnitudeof +5.15.[2]Based uponparallaxmeasurements obtained during theHipparcosmission,[1]it is roughly 370light-yearsdistant from theSun.
The two components are designated Xi Cancri A (formally namedNahn/ˈnɑːn/)[10]and B.
Nomenclature
[edit]ξ Cancri(LatinisedtoXi Cancri) is the system'sBayer designation.The designations of the two components asXi Cancri AandBderive from the convention used by the Washington Multiplicity Catalog (WMC) for multiplestar systems,and adopted by theInternational Astronomical Union(IAU).[11]
Xi Cancri together withLambda Leonis(Alterf) were the PersianNahn,"the Nose", and theCopticPiautos,"the Eye", both lunarasterisms.[12]Nahnwas also the name given to Xi Cancri in a 1971NASAtechnical memorandum.[13]In 2016, the IAU organized aWorking Group on Star Names(WGSN)[14]to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entiremultiple systems.[15]It approved the nameNahnfor the component Xi Cancri A on 1 June 2018 and it is now so included in the List of IAU-approved Star Names.[10]
Properties
[edit]At its present distance, the visual magnitude is diminished by anextinction factorof 0.135 due tointerstellar dust.[3]
Xi Cancri is a single-linedspectroscopic binarystar system with anorbital periodof 4.66 years, aneccentricityof 0.06, and asemimajor axisof 0.01arcsecond.The primary, Xi Cancri A, is a yellowG-typegiantwith anapparent magnitudeof +5.70. Its companion, Xi Cancri B, is of magnitude 6.20.[3]
References
[edit]- ^abcdefvan Leeuwen, F. (2007), "Validation of the new Hipparcos reduction",Astronomy and Astrophysics,474(2): 653–664,arXiv:0708.1752,Bibcode:2007A&A...474..653V,doi:10.1051/0004-6361:20078357,S2CID18759600.
- ^abcdSturch, C. R.; Helfer, H. L. (November 1972), "UBVRI photometry of north galactic pole K giants. II",Astronomical Journal,77:726,Bibcode:1972AJ.....77..726S,doi:10.1086/111344.
- ^abcdMalkov, O. Yu.; et al. (2012), "Dynamical masses of a selected sample of orbital binaries",Astronomy & Astrophysics,546:A69,Bibcode:2012A&A...546A..69M,doi:10.1051/0004-6361/201219774.
- ^abAnderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation",Astronomy Letters,38(5): 331,arXiv:1108.4971,Bibcode:2012AstL...38..331A,doi:10.1134/S1063773712050015,S2CID119257644.
- ^de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project",Astronomy & Astrophysics,546:14,arXiv:1208.3048,Bibcode:2012A&A...546A..61D,doi:10.1051/0004-6361/201219219,S2CID59451347,A61.
- ^Pourbaix, D.; et al. (2004), "SB9:The ninth catalogue of spectroscopic binary orbits ",Astronomy & Astrophysics,424(2): 727–732,arXiv:astro-ph/0406573,Bibcode:2004A&A...424..727P,doi:10.1051/0004-6361:20041213,S2CID119387088.
- ^Jackson, E. S.; et al. (May 1957), "The Orbits of the Spectroscopic Binaries Omicron Tauri, Xi Cancri, and Mu Ursae Majories",Astrophysical Journal,125:712,Bibcode:1957ApJ...125..712J,doi:10.1086/146345.
- ^abMcDonald, I.; et al. (2012), "Fundamental Parameters and Infrared Excesses of Hipparcos Stars",Monthly Notices of the Royal Astronomical Society,427(1): 343–57,arXiv:1208.2037,Bibcode:2012MNRAS.427..343M,doi:10.1111/j.1365-2966.2012.21873.x,S2CID118665352.
- ^"ksi Cnc".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved2017-06-15.
- ^ab"Naming Stars".IAU.org.Retrieved18 June2018.
- ^Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets".arXiv:1012.0707[astro-ph.SR].
- ^Allen, R. H.(1963),Star Names: Their Lore and Meaning(Reprint ed.), New York, NY: Dover Publications Inc., p.114,ISBN0-486-21079-0,retrieved2010-12-12.
- ^Rhoads, Jack W. (November 15, 1971),Technical Memorandum 33-507-A Reduced Star Catalog Containing 537 Named Stars(PDF),Jet Propulsion Laboratory, California Institute of Technology.
- ^"IAU Working Group on Star Names (WGSN)".Retrieved22 May2016.
- ^"WG Triennial Report (2015–2018) – Star Names"(PDF).p. 5.Retrieved2018-07-14.
