HD 17092

HD 17092
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]
Distance750 ± 9 ly
(230 ± 3 pc)
Absolute magnitude (MV)+1.76[4]
Details[6]
Mass1.23±0.18 M☉
Radius12.04+0.51
−0.35[1] R☉
Luminosity57±1[1] L☉
Surface gravity (log g)2.47±0.11 cgs
Temperature4,630±30 K
Metallicity [Fe/H]0.11±0.05 dex
Rotation505 days[4]
Rotational velocity (v sin i)<1 km/s
Age5.82±2.75 Gyr
Other designations
BD+49° 767, HD 17092, SAO 38313, PPM 45466
Database references
SIMBADdata

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]

The HD 17092 planetary system[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. ^ 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.
  2. ^ 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
  3. ^ a b Skiff, B. A. (October 2014), General Catalogue of Stellar Spectral Classifications, Bibcode:2014yCat....1.2023S
  4. ^ 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.
  5. ^ 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
  6. ^ 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