HIP 100963
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Vulpecula |
| Right ascension | 20h 28m 11.81471s[1] |
| Declination | +22° 07′ 44.3723″[1] |
| Apparent magnitude (V) | +7.088[2] |
| Characteristics | |
| Spectral type | G5[3] |
| B−V color index | +0.6[2] |
| V−R color index | +0.4[2] |
| R−I color index | +0.3[2] |
| Astrometry | |
| Radial velocity (Rv) | −1.6[4] km/s |
| Proper motion (μ) | RA: −23.90[1] mas/yr Dec.: −243.96[1] mas/yr |
| Parallax (π) | 35.42 ± 0.59[1] mas |
| Distance | 92 ± 2 ly (28.2 ± 0.5 pc) |
| Details | |
| Mass | 0.998 ± 0.006[5] M☉ |
| Luminosity | 0.968 ± 0.043[5] L☉ |
| Temperature | 5,779 ± 50[5] K |
| Metallicity [Fe/H] | −0.002[5] dex |
| Rotational velocity (v sin i) | 2.39[6] km/s |
| Age | 2.01–3.80[5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HIP 100963 is a star in the faint northern constellation of Vulpecula.[2] It has an apparent visual magnitude of approximately 7.1,[2] making it generally too faint to be seen with the naked eye in most circumstances. The distance to this star, as determined using parallax measurements from the Hipparcos mission, is around 92 light-years (28 parsecs).[1]
This star has a stellar classification of G5,[2] making it a G-type star with an undetermined luminosity class. It has similar mass, temperature and chemical abundance to the Sun and was called a solar twin in a 2009 study, although its lithium abundance is three to four times that of the Sun. This lithium excess suggests that the star has a younger age of between 2.01 and 3.80 billion years, compared to the previous estimate of 5.13+0.00
−2.99 Gyr from a 2007 study.[5]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (November 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
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 LTT 15980 -- High proper-motion Star, database entry, SIMBAD. Accessed on line February 8, 2011.
- ↑ White, Russel J.; Gabor, Jared M.; Hillenbrand, Lynne A. (June 2007), "High-Dispersion Optical Spectra of Nearby Stars Younger Than the Sun", The Astronomical Journal 133 (6): 2524–2536, arXiv:0706.0542, Bibcode:2007AJ....133.2524W, doi:10.1086/514336
- ↑ Nordström, B. et al. (May 2004). "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs". Astronomy and Astrophysics 418 (3): 989–1019. arXiv:astro-ph/0405198. Bibcode:2004A&A...418..989N. doi:10.1051/0004-6361:20035959.. See the Vizier entry for this star.
- ↑ 5.0 5.1 5.2 5.3 5.4 5.5 Do Nascimento, J. D., Jr. et al. (July 2009). "Age and mass of solar twins constrained by lithium abundance". Astronomy and Astrophysics 501 (2): 687–694. arXiv:0904.3580. Bibcode:2009A&A...501..687D. doi:10.1051/0004-6361/200911935.
- ↑ Takeda, Y. et al. (June 2010), "Behavior of Li abundances in solar-analog stars. II. Evidence of the connection with rotation and stellar activity", Astronomy and Astrophysics 515: A93, arXiv:1003.1564, Bibcode:2010A&A...515A..93T, doi:10.1051/0004-6361/200913897
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