Tau Cancri
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Cancer |
| Right ascension | 09h 08m 00.04963s[1] |
| Declination | +29° 39′ 15.2428″[1] |
| Apparent magnitude (V) | +5.42[2] |
| Characteristics | |
| Spectral type | G8 III[3] |
| U−B color index | +0.57[2] |
| B−V color 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] |
| Distance | 274 ± 9 ly (84 ± 3 pc) |
| Absolute magnitude (MV) | +0.81[5] |
| Details[4] | |
| Mass | 2.42±0.09 M☉ |
| Radius | 7.76±0.51 R☉ |
| Luminosity | 40 L☉ |
| Surface gravity (log g) | 3.21 cgs |
| Temperature | 5,153 K |
| Metallicity [Fe/H] | −0.06 dex |
| Rotational velocity (v sin i) | 1.95±0.45 km/s |
| Age | 620±60 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Tau Cancri (τ Cancri) is a solitary,[3] yellow-hued star in the zodiac constellation of Cancer. With an apparent visual magnitude of +5.42,[2] it is faintly visible to the naked eye. Based upon an annual parallax shift of 11.92 mas as seen from Earth,[1] it is located around 274 light years from the Sun.
With an age of about 620[4] million years and a stellar classification of G8 III,[3] this is a red clump giant star,[7] which indicates that it has evolved onto the horizontal branch and is generating energy through helium fusion at its core. It is a microvariable, showing a luminosity variation of 0.04 in magnitude.[8] Tau Cancri has an estimated 2.4 times the mass of the Sun and 7.8 times the Sun's radius. The star radiates 40 times the solar luminosity from its photosphere at an effective temperature of 5,153 K.[4]
References
- ^ a b c d e f 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.
- ^ a b c d Argue, A. N. (1963), "UBV photometry of 300 G and K type stars", Monthly Notices of the Royal Astronomical Society, 125 (6): 557, Bibcode:1963MNRAS.125..557A, doi:10.1093/mnras/125.6.557
- ^ a b c 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.
{{citation}}: CS1 maint: unflagged free DOI (link) - ^ 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.
- ^ 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.
- ^ "tau Cnc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-06-11.
{{cite web}}: CS1 maint: postscript (link) - ^ Adelman, Saul J. (2001), "On the Photometric Variability of Red Clump Giants", Baltic Astronomy, 10: 593–597, Bibcode:2001BaltA..10..593A.
- ^ 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.
