Star in the constellation Cancer
For other stars with this Bayer designation, see
σ Cancri .
Sigma3 Cancri Observation dataEpoch J2000.0 Equinox J2000.0 (ICRS ) Constellation Cancer Right ascension 08h 59m 32.655s [ 1] Declination +32° 25′ 06.81″[ 1] Apparent magnitude (V)+5.24[ 2] Characteristics Evolutionary stage red clump [ 3] Spectral type G9 III[ 4] U−Bcolor index +0.64[ 2] B−Vcolor index +0.91[ 2] Astrometry Radial velocity (Rv )± 0.21[ 5] km/s Proper motion (μ)RA: −43.741mas /yr [ 1] Dec.: −34.754mas /yr [ 1] Parallax (π)10.7481± 0.0965 mas [ 6] Distance 303 ± 3 ly pc ) Absolute magnitude (MV )0.45[ 7] Details[ 5] Mass ± 0.11M ☉ Radius 10.32 R ☉ Luminosity 72 L ☉ Surface gravity (log g )3.18 cgs Temperature ± 21K Metallicity [Fe/H] ± 0.06dex Rotational velocity (v sin i )± 0.47Age ± 40Myr Other designations σ3 Cnc ,64 Cancri ,BD +32°1821FK5 1232GC 12417HD 76813HIP 44154HR 3575SAO 61177WDS J08595+3225A[ 8] Database references SIMBAD data
Sigma3 Cancri is a solitary,[ 9] star in thezodiac constellation ofCancer . Its name is aBayer designation that isLatinized from σ3 Cancri, and abbreviated Sigma3 Cnc or σ3 Cnc. With anapparent visual magnitude of +5.24,[ 2] parallax shift ofmas [ 6] light-years (93 pc ) from theSun . The star'sproper motion makes it a candidate for membership in theIC 2391 supercluster.[ 10]
This is anevolved ,G-type giant star with astellar classification of G9 III.[ 4] [ 5] red clump star on thehorizontal branch , which indicates it is generating energy throughhelium fusion at itscore .[ 3] 3 Cancri has 2.8 times themass of the Sun and has expanded to 10.3 times theSun's radius . It is radiating 72 times thesolar luminosity from itsphotosphere at aneffective temperature of 5,170 K.[ 5]
^a b c Vallenari, A.; et al. (Gaia collaboration) (2023),"Gaia Data Release 3. Summary of the content and survey properties" ,Astronomy and Astrophysics ,674 : A1,arXiv :2208.00211 Bibcode :2023A&A...674A...1G ,doi :10.1051/0004-6361/202243940 S2CID 244398875 . Gaia DR3 record for this source atVizieR .^a b c d Guetter, H. H.; Hewitt, A. V. (1984), "Photoelectric UBV photometry for 317 PZT and VZT stars",Astronomical Society of the Pacific ,96 :441– 443,Bibcode :1984PASP...96..441G ,doi :10.1086/131362 ^a b Mishenina, T. V.; et al. (September 2006), "Elemental abundances in the atmosphere of clump giants",Astronomy and Astrophysics ,456 (3):1109– 1120,arXiv :astro-ph/0605615 Bibcode :2006A&A...456.1109M ,doi :10.1051/0004-6361:20065141 ,S2CID 18764566 . ^a b Sato, K.; Kuji, S. (1990), "MK classification and photometry of stars used for time and latitude observations at Mizusawa and Washington",Astronomy and Astrophysics Supplement Series ,85 : 1069,Bibcode :1990A&AS...85.1069S . ^a b c d Jofré, E.; et al. (2015), "Stellar parameters and chemical abundances of 223 evolved stars with and without planets",Astronomy & Astrophysics ,574 : A50,arXiv :1410.6422 Bibcode :2015A&A...574A..50J ,doi :10.1051/0004-6361/201424474 ,S2CID 53666931 . ^a b van 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 ,S2CID 18759600 . ^ Da Silva, Ronaldo; et al. (2015), "Homogeneous abundance analysis of FGK dwarf, subgiant, and giant stars with and without giant planets",Astronomy & Astrophysics ,580 : A24,arXiv :1505.01726 Bibcode :2015A&A...580A..24D ,doi :10.1051/0004-6361/201525770 ,S2CID 119216425 . ^ "sig03 Cnc" ,SIMBAD Centre de données astronomiques de Strasbourg , retrieved2017-06-11 .^ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems",Monthly Notices of the Royal Astronomical Society 389 (2):869– 879,arXiv :0806.2878 Bibcode :2008MNRAS.389..869E ,doi :10.1111/j.1365-2966.2008.13596.x S2CID 14878976 . ^ Eggen, Olin J. (December 1995), "Reality Tests of Superclusters in the Young Disk Population",Astronomical Journal ,110 : 2862,Bibcode :1995AJ....110.2862E ,doi :10.1086/117734 .
