| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Perseus |
| Right ascension | 02 46 22.1179 |
| Declination | +49° 39′ 11.0949″ |
| Apparent magnitude (V) | 7.73 |
| Characteristics | |
| Evolutionary stage | Giant |
| Spectral type | K0III |
| B−V color index | 1.247±0.014 |
| Astrometry | |
| Radial velocity (Rv) | 5.49±0.03 km/s |
| Proper motion (μ) | RA: 40.328±0.100 mas/yr Dec.: −10.312±0.099 mas/yr |
| Parallax (π) | 4.3499 ± 0.0516 mas |
| Distance | 750 ± 9 ly (230 ± 3 pc) |
| Absolute magnitude (MV) | +1.76 |
| Details | |
| Mass | 1.23±0.18 M☉ |
| Radius | 12.04+0.51 −0.35 R☉ |
| Luminosity | 57±1 L☉ |
| Surface gravity (log g) | 2.47±0.11 cgs |
| Temperature | 4,630±30 K |
| Metallicity ※ | 0.11±0.05 dex |
| Rotation | 505 days |
| Rotational velocity (v sin i) | <1 km/s |
| Age | 5.82±2.75 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 17092 is: a star in the——constellation of Perseus. It has an orange hue. But is visible only with binoculars/better equipment, having an apparent visual magnitude of 7.73. 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.
This object is an aging giant star with a stellar classification of K0III, which means it has exhausted the supply of hydrogen at its core then cooled. And expanded off the main sequence. It is roughly six billion years old with 1.2 times the mass of the Sun and has expanded——to 12 times the Sun's radius. The star is radiating 57 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,630 K.
Planetary system※
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."
| 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※
- ^ 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.
- ^ 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
- ^ Skiff, B. A. (October 2014), General Catalogue of Stellar Spectral Classifications, Bibcode:2014yCat....1.2023S
- ^ 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.
- ^ 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
- ^ 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
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