Summary
HD 189245 is the Henry Draper catalogue designation for a solitary[10] star in the southern constellation of Sagittarius. It has an apparent visual magnitude of 5.66,[2] which means it is faintly visible to the naked eye. Parallax measurements from the Hipparcos satellite indicate a distance of 72 light years from the Sun.[1] It is drifting closer with a heliocentric radial velocity of −13 km/s.[5]
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Sagittarius |
| Right ascension | 20h 00m 20.249s[1] |
| Declination | −33° 42′ 12.42″[1] |
| Apparent magnitude (V) | 5.66[2] |
| Characteristics | |
| Spectral type | F8.5 V Fe−0.6 CH−0.5[3] |
| U−B color index | −0.04[2] |
| B−V color index | +0.498[4] |
| Astrometry | |
| Radial velocity (Rv) | −13.2[5] km/s |
| Proper motion (μ) | RA: +128.794 mas/yr[1] Dec.: −289.360 mas/yr[1] |
| Parallax (π) | 45.1537 ± 0.0551 mas[1] |
| Distance | 72.23 ± 0.09 ly (22.15 ± 0.03 pc) |
| Absolute magnitude (MV) | 4.06[6] |
| Details | |
| Surface gravity (log g) | 4.31[3] cgs |
| Temperature | 6,333[3] K |
| Metallicity [Fe/H] | −0.09[3] dex |
| Rotational velocity (v sin i) | 72.6[7] km/s |
| Age | 100 or 500[4] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
The stellar classification of this star is F8.5 V Fe−0.6 CH−0.5,[3] indicating that it is an F-type main sequence star with a spectrum that shows deficiencies in iron (Fe) and methylidyne (CH) in its outer atmosphere. It is a variable star with an active chromosphere and is a source of X-ray emission.[3][11] HD 189245 is spinning rapidly with a projected rotational velocity of 72.6[7] km/s. Gyrochronology indicates this is a young star with an estimated age of 500 million years. However, the amount of X-ray emission suggests an even younger star that is roughly 100 million years old.[4]
The velocity components of HD 189245 indicate that it is a likely member of the AB Doradus moving group of stars, which share a common motion through space. This group has an age of around 50 million years and is centered at a point 98 ly (30 pc) from the Sun.[12]
References edit
- ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b c Corben, P. M.; et al. (1972), "U, B, V photometry of 500 southern stars", Monthly Notes of the Astronomical Society of South Africa, 31: 7–22, Bibcode:1972MNSSA..31....8C.
- ^ a b c d e f 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, S2CID 119476992.
- ^ a b c Vican, Laura (June 2012), "Age Determination for 346 Nearby Stars in the Herschel DEBRIS Survey", The Astronomical Journal, 143 (6): 135, arXiv:1203.1966, Bibcode:2012AJ....143..135V, doi:10.1088/0004-6256/143/6/135, S2CID 118539505.
- ^ a b 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: 989–1019, arXiv:astro-ph/0405198, Bibcode:2004A&A...418..989N, doi:10.1051/0004-6361:20035959, S2CID 11027621.
- ^ Reiners, Ansgar (January 2006), "Rotation- and temperature-dependence of stellar latitudinal differential rotation", Astronomy and Astrophysics, 446 (1): 267–277, arXiv:astro-ph/0509399, Bibcode:2006A&A...446..267R, doi:10.1051/0004-6361:20053911, S2CID 8642707
- ^ a b Schröder, C.; et al. (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo" (PDF), Astronomy and Astrophysics, 493 (3): 1099–1107, Bibcode:2009A&A...493.1099S, doi:10.1051/0004-6361:200810377[permanent dead link]
- ^ Gould, Benjamin Apthorp (1879), Uranometria Argentina: brightness and position of every fixed star, down to the seventh magnitude, within one hundred degrees of the South Pole, Resultados, Universidad Nacional de Córdoba Observatorio Astronómico, vol. 1, Observatorio Nacional Argentino, p. 181". Coordinates are for the 1875 equinox."
{{citation}}: CS1 maint: postscript (link) - ^ "HD 189245". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-07-19.
- ^ 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, S2CID 14878976.
- ^ Jeffries, R. D.; Jewell, S. J. (September 1993), "The Kinematics of Active Late Type Stars Observed by the ROSAT Wide-Field Camera", Monthly Notices of the Royal Astronomical Society, 264 (1): 106, Bibcode:1993MNRAS.264..106J, doi:10.1093/mnras/264.1.106.
- ^ Nakajima, Tadashi; Morino, Jun-Ichi (January 2012), "Potential Members of Stellar Kinematic Groups within 30 pc of the Sun", The Astronomical Journal, 143 (1): 2, Bibcode:2012AJ....143....2N, doi:10.1088/0004-6256/143/1/2.