HD 4628
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Pisces |
| Right ascension | 00h 48m 22.98s[1] |
| Declination | +05° 16′ 50.2″[1] |
| Apparent magnitude (V) | 5.75 |
| Characteristics | |
| Spectral type | K2.5 V[2] |
| U−B color index | 0.59 |
| B−V color index | 0.89 |
| Variable type | None |
| Astrometry | |
| Radial velocity (Rv) | -12.6 km/s |
| Proper motion (μ) | RA: 757.11 ± 0.48[1] mas/yr Dec.: -1,141.33 ± 0.34[1] mas/yr |
| Parallax (π) | 134.14 ± 0.51[1] mas |
| Distance | 24.31 ± 0.09 ly (7.45 ± 0.03 pc) |
| Absolute magnitude (MV) | 5.88 |
| Details | |
| Mass | 0.70 ± 0.10[3] M☉ |
| Radius | 0.749 ± 0.051[4] R☉ |
| Luminosity | 0.28[3] L☉ |
| Surface gravity (log g) | 4.39 ± 0.16[3] cgs |
| Temperature | 5,829 ± 41[3] K |
| Metallicity [Fe/H] | –0.22[5] dex |
| Rotation | 38.0 days[5] |
| Age | 5.4[6] Gyr |
| Other designations | |
HD 4628 (96 G. Piscium) is a main sequence dwarf star in the constellation Pisces. It has a spectral classification of K2, giving it an orange-red hue and a slightly smaller mass and girth than our Sun. It lies at a distance of approximately 24 light years from us and has a relatively high proper motion.[1] The apparent magnitude is just sufficient for this star to be viewed with the unaided eye. The star appears to be slightly older than our Sun—approximately 5.4 billion years old.[6]
No definitive companion has yet been found in orbit around this star. In 1958 it was thought to have stellar companion that was also a flare star, but this was subsequently disproved.[8]
References
- 1 2 3 4 5 6 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. Vizier catalog entry
- ↑ Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637
- 1 2 3 4 Ghezzi, L.; et al. (September 2010), "Stellar Parameters and Metallicities of Stars Hosting Jovian and Neptunian Mass Planets: A Possible Dependence of Planetary Mass on Metallicity", The Astrophysical Journal 720 (2): 1290–1302, arXiv:1007.2681, Bibcode:2010ApJ...720.1290G, doi:10.1088/0004-637X/720/2/1290
- ↑ van Belle, Gerard T.; von Braun, Kaspar (2009). "Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars". The Astrophysical Journal 694 (2): 1085–1098. arXiv:0901.1206. Bibcode:2009ApJ...694.1085V. doi:10.1088/0004-637X/694/2/1085.
- 1 2 Maldonado, J.; et al. (October 2010), "A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups", Astronomy and Astrophysics 521: A12, arXiv:1007.1132, Bibcode:2010A&A...521A..12M, doi:10.1051/0004-6361/201014948
- 1 2 Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008), "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics", The Astrophysical Journal 687 (2): 1264–1293, arXiv:0807.1686, Bibcode:2008ApJ...687.1264M, doi:10.1086/591785
- ↑ Gould, B. A., Uranometria Argentina, Reprinted and updated by Pilcher, F, retrieved 2010-07-16
- ↑ Hartkopf & McAlister, 1984, "Binary stars unresolved by speckle interferometry", Astronomical Society of the Pacific, vol. 96.
External links
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