Gliese 146
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Horologium |
| Right ascension | 03h 35m 00.93987s[1] |
| Declination | −48° 25′ 08.9085″[1] |
| Apparent magnitude (V) | 8.64[2] |
| Characteristics | |
| Evolutionary stage | Main Sequence[3] |
| Spectral type | K6.5V[3] |
| U−B color index | +1.24[2] |
| B−V color index | +1.30[2] |
| Variable type | suspected, range 8.57 to 8.7 mag, NSV 1203[4][5] |
| Astrometry | |
| Radial velocity (Rv) | +21.38±0.13[1] km/s |
| Proper motion (μ) | RA: 404.441 mas/yr[1] Dec.: 307.498 mas/yr[1] |
| Parallax (π) | 73.5199 ± 0.0164 mas[1] |
| Distance | 44.363 ± 0.010 ly (13.602 ± 0.003 pc) |
| Details[6] | |
| Mass | 0.684±0.013 M☉ |
| Radius | 0.674±0.020 R☉ |
| Luminosity | 0.121[7] L☉ |
| Surface gravity (log g) | 4.69±0.05 cgs |
| Temperature | 4385±21 K |
| Metallicity [Fe/H] | -0.08±0.02 dex |
| Rotation | 34.99+0.58 −0.53 |
| Age | 970[8] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| ARICNS | data |
Gliese 146 is a star with an orbiting exoplanet in the constellation Horologium. Gliese 146 is also catalogued as HD 22496, HIP 16711, SAO-216392, and LHS 1563.[9] With an apparent visual magnitude of 8.64,[2] it is too faint to be visible to the naked eye. Gliese 146 is located at a distance of 44.4 light years based on parallax measurements, and is drifting further away with a heliocentric radial velocity of +21 km/s.[1]
This is an ordinary K-type main-sequence star with a stellar classification of K6.5V.[3] It has 68% of the mass of the Sun and 67% of the Sun's girth. Gliese 146 is radiating 12% of the luminosity of the Sun from its photosphere at an effective temperature of 4,385 K.[6] Classified as a suspected variable star,[4][5] Gliese 146 was found to be a flare star, with average flare frequency 0.23 flares per day.[10]
Its velocity relative to the Sun is 38.1 km/second, and its galactic orbit ranges between 20,800 and 25,400 light years from the center of the Galaxy, placing it within a thin disk.[6] It belongs to the Hyades supercluster of stars,[11] and is one of 155 K-type stars within 50 light years.[9]
Planetary system[edit]
It is one of 500 stars selected in 2009 for the SCUBA-2 All Sky Survey for stars with debris disks.[12] The debris disk was not detected by any survey as in 2015 though.[7]
In 2021, a Sub-Neptune planet HD 22496b was discovered utilizing a Doppler spectroscopy method. It is orbiting very close to the host star at a separation of 0.0510 AU (7.63 Gm) and an orbital period of five days. The planet is not known to be transiting. As the inclination of the orbital plane is unknown, only a rough lower bound on the mass of this planet can be established: it has at least ~5.6 times the mass of the Earth.[6]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >5.57+0.73 −0.68, <16 M🜨 |
0.0510+0.0024 −0.0026 |
5.09071 ± 0.00026 | 0 | — | — |
See also[edit]
References[edit]
- ^ a b c d e f 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 d Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data. SIMBAD, Bibcode:1986EgUBV........0M.
- ^ a b c 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 "HD 22496 -- High proper-motion Star", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2016-06-21
- ^ a b VizieR Detailed Page for NSV=1203
- ^ a b c d e Lillo-Box, J.; et al. (2021), "HD 22496 b: The first ESPRESSO stand-alone planet discovery", Astronomy & Astrophysics, 654: A60, arXiv:2109.00226, doi:10.1051/0004-6361/202141714, S2CID 237371680
- ^ a b Moro-Martín, A.; Marshall, J. P.; Kennedy, G.; Sibthorpe, B.; Matthews, B. C.; Eiroa, C.; Wyatt, M. C.; Lestrade, J.-F.; Maldonado, J.; Rodriguez, D.; Greaves, J. S.; Montesinos, B.; Mora, A.; Booth, M.; Duchêne, G.; Wilner, D.; Horner, J. (2015), "Does the Presence of Planets Affect the Frequency and Properties of Extrasolar Kuiper Belts? Results from Theherscheldebris and Dunes Surveys", The Astrophysical Journal, 801 (2): 143, arXiv:1501.03813, doi:10.1088/0004-637X/801/2/143, S2CID 55170390
- ^ 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 K stars within 100 light-years - SolStation.com
- ^ Lammer, H.; Kővári, Zs; Hanslmeier, A.; Koller, F.; Korhonen, H.; Guenther, E. W.; Kriskovics, L.; Vida, K.; Greimel, R.; Odert, P.; Leitzinger, M. (2020), "A census of coronal mass ejections on solar-like stars", Monthly Notices of the Royal Astronomical Society, 493 (3): 4570–4589, arXiv:2002.04430, doi:10.1093/mnras/staa504
- ^ siblings of HD 22496 (SIMBAD)
- ^ Phillips, N. M.; Greaves, J. S.; Dent, W. R. F.; Matthews, B. C.; Holland, W. S.; Wyatt, M. C.; Sibthorpe, B. (April 2010). "Target selection for the SUNS and DEBRIS surveys for debris discs in the solar neighbourhood". Monthly Notices of the Royal Astronomical Society. 403 (3): 1089–1101. arXiv:0911.3426. Bibcode:2010MNRAS.403.1089P. doi:10.1111/j.1365-2966.2009.15641.x.
External links[edit]
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