| 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 |
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
- ^ 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
| Stars |
| ||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| |||||||||||||
|
Star clusters |
| ||||||||||||
| Nebulae |
| ||||||||||||
| Galaxies |
| ||||||||||||
| |||||||||||||
| |||||||||||||
| 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 |
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
- ^ 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
| Stars |
| ||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| |||||||||||||
|
Star clusters |
| ||||||||||||
| Nebulae |
| ||||||||||||
| Galaxies |
| ||||||||||||
| |||||||||||||
| |||||||||||||