Tau1 Gruis
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Grus |
| Right ascension | 22h 53m 37.9324s[1] |
| Declination | –48° 35′ 53.824″[1] |
| Apparent magnitude (V) | +6.02[2] |
| Characteristics | |
| Spectral type | G0 V[3] |
| U−B color index | 0.17[2] |
| B−V color index | 0.62[2] |
| Variable type | None |
| Astrometry | |
| Radial velocity (Rv) | –1.1[4] km/s |
| Proper motion (μ) | RA: 217.943(18) mas/yr[1] Dec.: −81.013(26) mas/yr[1] |
| Parallax (π) | 30.1918 ± 0.0298 mas[1] |
| Distance | 108.0 ± 0.1 ly (33.12 ± 0.03 pc) |
| Absolute magnitude (MV) | +3.46[5] |
| Details | |
| Mass | 1.28±0.04[6] M☉ |
| Radius | 1.71±0.04[6] R☉ |
| Luminosity | 3.39±0.02[6] L☉ |
| Surface gravity (log g) | 4.07±0.03[6] cgs |
| Temperature | 5,996±56[6] K |
| Metallicity [Fe/H] | 0.27±0.02[7] dex |
| Rotational velocity (v sin i) | 5.13[8] km/s |
| Age | 4.2±0.6[6] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| ARICNS | data |
Tau1 Gruis, Latinized from τ1 Gruis, and catalogued as HD 216435 and HR 8700, is a yellow-hued star approximately 108 light-years away[1] in the constellation of Grus (the Crane). The star is visible to the naked eye for some people, placing it in the Bright Star Catalogue. In 2002, one extrasolar planet was confirmed to orbit the star.
Characteristics
[edit]Tau1 Gruis is a G-type main-sequence star of spectral type G0 V. It is estimated that the star has about 1.28 times the mass of the Sun, 1.71 times the Sun's radius, and about 3.6 times the luminosity. Due to its unusual brightness, at least one source suspects that the star may be a highly evolved subgiant star.[9] It is thought that Tau1 Gruis is about 1.4 times more enriched with elements heavier than hydrogen, making a high abundance of iron likely. The Ca-II H line of the star suggests that it is chromospherically inactive, making it significantly older than previously predicted.
Planetary system
[edit]On September 17, 2002, a team of astronomers led by Geoffrey Marcy announced the discovery of a giant planet around Tau1 Gruis.[9] The radial velocity measurements suggest that the star has a companion with at least 1.23 times the mass of Jupiter. The planet's orbit stays inside the system's habitable zone for most of its revolution around the star, though at apoapsis, the planet falls outside of this zone.[citation needed]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >1.26 ± 0.13 MJ | 2.56 ± 0.17 | 1311 ± 49 | 0.070 ± 0.078 | — | — |
See also
[edit]References
[edit]- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 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.
- ^ 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.
- ^ Nordström, B.; et al. (May 2014), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ~14000 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, S2CID 11027621.
- ^ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
- ^ a b c d e f Bonfanti, A.; et al. (2015). "Revising the ages of planet-hosting stars". Astronomy and Astrophysics. 575: A18. arXiv:1411.4302. Bibcode:2015A&A...575A..18B. doi:10.1051/0004-6361/201424951. S2CID 54555839.
- ^ Tsantaki, M.; et al. (July 2013), "Deriving precise parameters for cool solar-type stars. Optimizing the iron line list", Astronomy & Astrophysics, 555: A150, arXiv:1304.6639, Bibcode:2013A&A...555A.150T, doi:10.1051/0004-6361/201321103, S2CID 118388752.
- ^ Delgado Mena, E.; et al. (April 2015), "Li abundances in F stars: planets, rotation, and Galactic evolution", Astronomy & Astrophysics, 576: 24, arXiv:1412.4618, Bibcode:2015A&A...576A..69D, doi:10.1051/0004-6361/201425433, S2CID 56051637, A69.
- ^ a b Jones, R. Paul; et al. (2003). "An exoplanet in orbit around τ1 Gruis". Monthly Notices of the Royal Astronomical Society. 341 (3): 948–952. arXiv:astro-ph/0209302. Bibcode:2003MNRAS.341..948J. doi:10.1046/j.1365-8711.2003.06481.x. S2CID 1575040.
- ^ Butler, R. P.; et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv:astro-ph/0607493. Bibcode:2006ApJ...646..505B. doi:10.1086/504701. S2CID 119067572.
External links
[edit]- "Notes for star HD 216435". Extrasolar Planets Encyclopaedia. Archived from the original on September 26, 2007. Retrieved 2008-06-22.
- "Tau1 Gruis". Solstation. Retrieved 2008-06-22.
