Summary
HD 17092 is a star in the constellation of Perseus. It has an orange hue but is visible only with binoculars or better equipment, having an apparent visual magnitude of 7.73.[2] The distance to this star is approximately 750 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +5.5 km/s.[5]
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Perseus |
| Right ascension | 02h 46m 22.1179s[1] |
| Declination | +49° 39′ 11.0949″[1] |
| Apparent magnitude (V) | 7.73[2] |
| Characteristics | |
| Evolutionary stage | Giant[2] |
| Spectral type | K0III[3] |
| B−V color index | 1.247±0.014[4] |
| Astrometry | |
| Radial velocity (Rv) | 5.49±0.03[5] km/s |
| Proper motion (μ) | RA: 40.328±0.100[1] mas/yr Dec.: −10.312±0.099[1] mas/yr |
| Parallax (π) | 4.3499 ± 0.0516 mas[1] |
| Distance | 750 ± 9 ly (230 ± 3 pc) |
| Absolute magnitude (MV) | +1.76[4] |
| Details[6] | |
| Mass | 1.23±0.18 M☉ |
| Radius | 12.04+0.51 −0.35[1] R☉ |
| Luminosity | 57±1[1] L☉ |
| Surface gravity (log g) | 2.47±0.11 cgs |
| Temperature | 4,630±30 K |
| Metallicity [Fe/H] | 0.11±0.05 dex |
| Rotation | 505 days[4] |
| Rotational velocity (v sin i) | <1 km/s |
| Age | 5.82±2.75 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
This object is an aging giant star with a stellar classification of K0III,[3] which means it has exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence.[4] It is roughly six billion years old with 1.2[6] times the mass of the Sun and has expanded to 12 times the Sun's radius.[1] The star is radiating 57[1] times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,630 K.[6]
Planetary system edit
On 6 May 2007, a planet HD 17092 b was discovered with the Hobby-Eberly Telescope by Niedzielski who used the wobble method. This planet is a massive gas giant and orbits at 1.29 astronomical units from the star with a period of about 360 days.[4]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥4.6±0.3 MJ | 1.29±0.05 | 359.9±2.4 | 0.166±0.052 | — | — |
References edit
- ^ a b c d e f g h i 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 Maldonado, J.; et al. (April 2019), "Connecting substellar and stellar formation: the role of the host star's metallicity", Astronomy & Astrophysics, 624: 7, arXiv:1903.01141, Bibcode:2019A&A...624A..94M, doi:10.1051/0004-6361/201833827, S2CID 118934484, A94
- ^ a b Skiff, B. A. (October 2014), General Catalogue of Stellar Spectral Classifications, Bibcode:2014yCat....1.2023S
- ^ a b c d e f Niedzielski, A.; et al. (2007). "A Planetary‐Mass Companion to the K0 Giant HD 17092". The Astrophysical Journal. 669 (2): 1354–1358. arXiv:0705.0935. Bibcode:2007ApJ...669.1354N. doi:10.1086/521784. S2CID 14853462.
- ^ a b Deka-Szymankiewicz, B.; et al. (2018), "The Penn State - Toruń Centre for Astronomy Planet Search stars. IV. Dwarfs and the complete sample", Astronomy and Astrophysics, 615: A31, arXiv:1801.02899, Bibcode:2018A&A...615A..31D, doi:10.1051/0004-6361/201731696, S2CID 85526201
- ^ a b c Maldonado, J.; Villaver, E. (April 2016), "Evolved stars and the origin of abundance trends in planet hosts", Astronomy & Astrophysics, 588: 11, arXiv:1602.00835, Bibcode:2016A&A...588A..98M, doi:10.1051/0004-6361/201527883, S2CID 119212009, A98