Astronomy:Gamma Pavonis
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Pavo |
| Right ascension | 21h 26m 26.60498s[1] |
| Declination | −65° 21′ 58.3131″[1] |
| Apparent magnitude (V) | 4.22[2] |
| Characteristics | |
| Spectral type | F9 V Fe-1.4 CH-0.7[3] |
| U−B color index | −0.13[4] |
| B−V color index | +0.48[4] |
| Variable type | Suspected |
| Astrometry | |
| Radial velocity (Rv) | −29.78±0.12[1] km/s |
| Proper motion (μ) | RA: +80.815[1] mas/yr Dec.: +800.573[1] mas/yr |
| Parallax (π) | 108.0102 ± 0.1061[1] mas |
| Distance | 30.20 ± 0.03 ly (9.258 ± 0.009 pc) |
| Absolute magnitude (MV) | 4.40[5] |
| Details | |
| Mass | 0.934±0.033[6] M☉ |
| Radius | 1.057±0.012[6] R☉ |
| Luminosity | 1.461±0.049[6] L☉ |
| Surface gravity (log g) | 4.359±0.008[6] cgs |
| Temperature | 6,168±130[6] K |
| Metallicity [Fe/H] | −0.66±0.09[6] dex |
| Rotational velocity (v sin i) | 1.0±0.6[7] km/s |
| Age | 5.9±1.2[6] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Gamma Pavonis, Latinized from γ Pavonis, is a star in the southern circumpolar constellation of Pavo. With an apparent visual magnitude of 4.22,[2] it is a fourth-magnitude star and thereby visible to the naked eye. From parallax observations with the Gaia satellite, the distance to this star has been measured at 30.20 light-years (9.26 parsecs). It is drifting closer to the Sun with a radial velocity of −30 km/s.[1]
The stellar classification of F9 V[3] puts it in the class of F-type main sequence stars that generate energy through the nuclear fusion of hydrogen at the core. It is a metal-poor star, which means it has a low abundance of elements heavier than helium. This star has about 93% of the Sun's mass, and about 106% its radius. It is a brighter star with 146% of the Sun's luminosity, which is it radiating from the outer envelope at an effective temperature of 6,168 K. Its age is estimated at 5.9 billion years.[6]
This star had rank 14 on TPF-C's top 100 target stars to search for a rocky planet in the Habitable Zone, approximately 1.2 AU, or a little beyond an Earth-like orbit.[8]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 Jehin, E. et al. (January 1999). "Abundance correlations in mildly metal-poor stars". Astronomy and Astrophysics 341: 241–255. Bibcode: 1999A&A...341..241J.
- ↑ 3.0 3.1 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. doi:10.1086/504637. Bibcode: 2006AJ....132..161G.
- ↑ 4.0 4.1 Johnson, H. L. et al. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory 4 (99): 99. Bibcode: 1966CoLPL...4...99J.
- ↑ Holmberg, J.; Nordstrom, B.; Andersen, J. (July 2009). "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics". Astronomy and Astrophysics 501 (3): 941–947. doi:10.1051/0004-6361/200811191. Bibcode: 2009A&A...501..941H.
- ↑ 6.0 6.1 6.2 6.3 6.4 6.5 6.6 6.7 Huber, Daniel et al. (2022-02-01). "A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of π Men c". The Astronomical Journal 163 (2): 79. doi:10.3847/1538-3881/ac3000. ISSN 0004-6256. Bibcode: 2022AJ....163...79H.
- ↑ Bruntt, H. et al. (July 2010). "Accurate fundamental parameters for 23 bright solar-type stars". Monthly Notices of the Royal Astronomical Society 405 (3): 1907–1923. doi:10.1111/j.1365-2966.2010.16575.x. Bibcode: 2010MNRAS.405.1907B.
- ↑ "TPF-C Top 100". http://sco.stsci.edu/tpf_top100/index.php.
External links
- Gamma Pavonis SolStation entry.
- ARICNS
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