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Tau Cancri

From Wikipedia, the free encyclopedia
Star in the constellation Cancer
Tau Cancri
Observation data
EpochJ2000.0      EquinoxJ2000.0 (ICRS)
ConstellationCancer
Right ascension09h 08m 00.04963s[1]
Declination+29° 39′ 15.2428″[1]
Apparent magnitude (V)+5.42[2]
Characteristics
Spectral typeG8 III[3]
U−Bcolor index+0.57[2]
B−Vcolor index+0.89[2]
Astrometry
Radial velocity (Rv)−13.90±0.14[4] km/s
Proper motion (μ)RA: −32.51[1]mas/yr
Dec.: +2.79[1]mas/yr
Parallax (π)11.92±0.39 mas[1]
Distance274 ± 9 ly
(84 ± 3 pc)
Absolute magnitude (MV)+0.81[5]
Details[4]
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[6]
Database references
SIMBADdata

Tau Cancri (τ Cancri) is a solitary,[3] yellow-huedstar in thezodiacconstellation ofCancer. With anapparent visual magnitude of +5.42,[2] it is faintly visible to the naked eye. Based upon an annualparallax shift of 11.92 mas as seen from Earth,[1] it is located around 274 light-years from theSun.

With an age of about 620[4] million years and astellar classification of G8 III,[3] this is ared-clumpgiant star,[7] 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.[4]

References

[edit]
  1. ^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,S2CID 18759600.
  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. ^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.
  4. ^abcdJofré, 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.
  5. ^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.
  6. ^"tau Cnc".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2017-06-11.{{cite web}}: CS1 maint: postscript (link)
  7. ^Adelman, 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.
  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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