Astronomy:HD 17092
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| 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[1] mas |
| 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 |
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]
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
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
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 Maldonado, J. et al. (April 2019), "Connecting substellar and stellar formation: the role of the host star's metallicity", Astronomy & Astrophysics 624: 7, doi:10.1051/0004-6361/201833827, A94, Bibcode: 2019A&A...624A..94M
- ↑ 3.0 3.1 Skiff, B. A. (October 2014), General Catalogue of Stellar Spectral Classifications, Bibcode: 2014yCat....1.2023S
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 Niedzielski, A. et al. (2007). "A Planetary‐Mass Companion to the K0 Giant HD 17092". The Astrophysical Journal 669 (2): 1354–1358. doi:10.1086/521784. Bibcode: 2007ApJ...669.1354N.
- ↑ 5.0 5.1 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, doi:10.1051/0004-6361/201731696, Bibcode: 2018A&A...615A..31D
- ↑ 6.0 6.1 6.2 Maldonado, J.; Villaver, E. (April 2016), "Evolved stars and the origin of abundance trends in planet hosts", Astronomy & Astrophysics 588: 11, doi:10.1051/0004-6361/201527883, A98, Bibcode: 2016A&A...588A..98M
Coordinates: 
02h 46m 22s, +49° 39′ 11″
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