Summary
Gamma Doradus, Latinized from γ Doradus, is the third-brightest star in the southern constellation of Dorado.[11] It is faintly visible to the naked eye with an apparent visual magnitude of approximately 4.25, and is a variable star, the prototype of the class of Gamma Doradus variables.[3] The star is located at a distance of 67 light years from the Sun based on parallax,[2] and is drifting further away with a radial velocity of +25 km/s.[6] Based on its motion through space, it appears to be a member of the IC 2391 supercluster.[12]
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Dorado |
| Right ascension | 04h 16m 01.58823s[2] |
| Declination | −51° 29′ 11.9191″[2] |
| Apparent magnitude (V) | 4.25[3] |
| Characteristics | |
| Evolutionary stage | Main sequence |
| Spectral type | F1V[4] |
| U−B color index | +0.03[5] |
| B−V color index | +0.30[5] |
| R−I color index | +0.16[5] |
| Variable type | γ Dor[3] |
| Astrometry | |
| Radial velocity (Rv) | +25.2±0.5[6] km/s |
| Proper motion (μ) | RA: +99.463[2] mas/yr Dec.: +183.353[2] mas/yr |
| Parallax (π) | 48.8984 ± 0.2817 mas[2] |
| Distance | 66.7 ± 0.4 ly (20.5 ± 0.1 pc) |
| Absolute magnitude (MV) | 2.72[3] |
| Details | |
| Mass | 1.56±0.06[7] M☉ |
| Radius | 1.85+0.25 −0.10[2] R☉ |
| Luminosity | 6.999+0.051 −0.052[2] L☉ |
| Luminosity (bolometric) | 7.0[3] L☉ |
| Surface gravity (log g) | 4.29±0.18[8] cgs |
| Temperature | 6,906+89 −423[2] K |
| Metallicity [Fe/H] | +0.05±0.14[8] dex |
| Rotational velocity (v sin i) | 56.6±0.5[9] km/s |
| Age | 0.535–1.207[7] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
This is an F-type main-sequence star with a stellar classification of F1V.[4] It is a pulsating variable that varies in brightness by less than a tenth of a magnitude owing to nonradial gravity wave oscillations.[3] Four pulsation frequencies have been identified with periods of 17.6, 12.8, 16.3, and 18.2 hours.[9][13] The star is around 0.5–1.2 billion years old and is spinning with a projected rotational velocity of 57 km/s.[9] It has 1.6[7] times the mass of the Sun and 1.9[2] times the Sun's radius. The star is radiating seven[2] times the luminosity of the Sun from its photosphere at an effective temperature of 6,906 K.[2]
An infrared excess has been detected at multiple frequencies,[14] indicating that the star is being orbited by a pair of debris disks.[15]
References edit
- ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
- ^ a b c d e f g h i j k l Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b c d e f Kaye, Anthony B.; et al. (July 1999). "Gamma Doradus Stars: Defining a New Class of Pulsating Variables". Publications of the Astronomical Society of the Pacific. 111 (761): 840–844. arXiv:astro-ph/9905042. Bibcode:1999PASP..111..840K. doi:10.1086/316399. S2CID 15583148.
- ^ a b Gray, R. O.; et al. (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. S2CID 119476992.
- ^ a b c Hoffleit, D.; Warren, Jr., W. H. HR 1338, database entry (5th Revised ed.).
{{cite book}}:|work=ignored (help) "V/50". CDS. Retrieved November 17, 2008. - ^ a b Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID 119231169.
- ^ a b c Esposito, Thomas M.; et al. (July 2020). "Debris Disk Results from the Gemini Planet Imager Exoplanet Survey's Polarimetric Imaging Campaign". The Astronomical Journal. 160 (1): 44. arXiv:2004.13722. Bibcode:2020AJ....160...24E. doi:10.3847/1538-3881/ab9199. S2CID 216641889. 24.
- ^ a b Bruntt, H.; et al. (February 2008). "A spectroscopic study of southern (candidate) γ Doradus stars. II. Detailed abundance analysis and fundamental parameters". Astronomy and Astrophysics. 478 (2): 487–496. arXiv:0711.3819. Bibcode:2008A&A...478..487B. doi:10.1051/0004-6361:20078523. S2CID 2713381.
- ^ a b c Brunsden, E.; et al. (April 2018). "Frequency and mode identification of γ Doradus from photometric and spectroscopic observations*". Monthly Notices of the Royal Astronomical Society. 475 (3): 3813–3822. arXiv:1803.06890. Bibcode:2018MNRAS.475.3813B. doi:10.1093/mnras/sty034.
- ^ "gam Dor". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-11-16.
- ^ Kaler, James B. "Gamma Dor". Stars. Retrieved 2020-11-16.
- ^ Eggen, Olin J. (December 1995). "Reality Tests of Superclusters in the Young Disk Population". Astronomical Journal. 110: 2862. Bibcode:1995AJ....110.2862E. doi:10.1086/117734.
- ^ Balona, L. A.; Krisciunas, K.; Cousins, A. W. J. (October 15, 1994). "γ Doradus: evidence for a new class of pulsating star". Monthly Notices of the Royal Astronomical Society. 270 (4): 905–913. Bibcode:1994MNRAS.270..905B. doi:10.1093/mnras/270.4.905.
- ^ Broekhoven-Fiene, Hannah; et al. (January 2013). "The Debris Disk around γ Doradus Resolved with Herschel". The Astrophysical Journal. 762 (1): 11. arXiv:1212.1450. Bibcode:2013ApJ...762...52B. doi:10.1088/0004-637X/762/1/52. S2CID 119276423. 52.
- ^ Greaves, J. S.; et al. (February 2014). "Alignment in star-debris disc systems seen by Herschel". Monthly Notices of the Royal Astronomical Society: Letters. 438 (1): L31–L35. arXiv:1310.6936. Bibcode:2014MNRAS.438L..31G. doi:10.1093/mnrasl/slt153.