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Tau Cancri

From Wikipedia, the free encyclopedia
Star in the constellation Cancer
τ Cancri
Observation data
EpochJ2000.0      EquinoxJ2000.0 (ICRS)
ConstellationCancer
Right ascension09h 08m 00.050s[1]
Declination+29° 39′ 15.24″[1]
Apparent magnitude (V)+5.42[2]
Characteristics
Evolutionary stagered clump[3]
Spectral typeG8 III[4]
U−Bcolor index+0.57[2]
B−Vcolor index+0.89[2]
Astrometry
Radial velocity (Rv)−13.90±0.14[5] km/s
Proper motion (μ)RA: −32.199mas/yr[1]
Dec.: +2.640mas/yr[1]
Parallax (π)12.0346±0.1007 mas[1]
Distance271 ± 2 ly
(83.1 ± 0.7 pc)
Absolute magnitude (MV)+0.81[6]
Details[5]
Mass2.42±0.09 M
Radius7.76±0.51 R
Luminosity40 L
Surface gravity (log g)3.21 cgs
Temperature5,153 K
Metallicity[Fe/H]−0.06 dex
Rotational velocity (v sin i)1.95±0.45 km/s
Age620±60 Myr
Other designations
τ Cnc,72 Cancri,BD+30°1817,FK5 2719,HD 78235,HIP 44818,HR 3621,SAO 80650[7]
Database references
SIMBADdata

Tau Cancri is a solitary,[4] yellow-huedstar in thezodiacconstellation ofCancer. Its name is aBayer designation that isLatinized from τ Cancri, and abbreviated Tau Cnc or τ Cnc. With anapparent visual magnitude of +5.42,[2] it is faintly visible to thenaked eye. Based upon an annualparallax shift of12.03 mas as seen from Earth,[1] it is located around 272light-years (83 pc) from theEarth. The star is drifting closer to the Sun with a line of sight velocity of −14 km/s.[5]

With an age of about 620[5] million years and astellar classification of G8 III,[4] this is ared-clumpgiant star,[3] which indicates that it hasevolved onto thehorizontal branch and is generating energy throughhelium fusion at its core. It is amicrovariable, showing aluminosity variation of 0.04 inmagnitude.[8] Tau Cancri has an estimated 2.4 times themass of the Sun and 7.8 times theSun's radius. The star radiates 40 times thesolar luminosity from itsphotosphere at aneffective temperature of5,153 K.[5] It is spinning slowly with aprojected rotational velocity of 2 km/s.[5]

References

[edit]
  1. ^abcdeVallenari, 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.
  2. ^abcdArgue, A. N. (1963), "UBV photometry of 300 G and K type stars",Monthly Notices of the Royal Astronomical Society,125 (6):557–570,Bibcode:1963MNRAS.125..557A,doi:10.1093/mnras/125.6.557
  3. ^abAdelman, Saul J. (2001), "On the Photometric Variability of Red Clump Giants",Baltic Astronomy,10 (4):593–597,Bibcode:2001BaltA..10..593A,doi:10.1515/astro-2001-0404,S2CID 118317147.
  4. ^abcEggleton, 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.
  5. ^abcdefJofré, 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.
  6. ^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.
  7. ^"tau Cnc",SIMBAD,Centre de données astronomiques de Strasbourg, retrieved2017-06-11.
  8. ^Adelman, S. J.; et al. (December 2000), "On the Variability of G0-G9 Stars",Information Bulletin on Variable Stars,4993: 1,Bibcode:2000IBVS.4993....1A.
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