Binary star in the constellation Ophiuchi
HD 164509 is a binary star system in the constellation of Ophiuchus .[ 1] The primary component has an orbiting exoplanet companion.[ 6] This system is located at a distance of 175 light years based on parallax measurements,[ 2] and is drifting further away with a radial velocity of 13.7 km/s.[ 5] It has an absolute magnitude of 4.64,[ 6] but at that distance the system has an apparent visual magnitude of 8.10,[ 1] which is too faint to be seen with the naked eye.
The primary component is a Sun-like G-type main-sequence star [ 6] with a stellar classification of G2V.[ 3] It is young and metal rich , having heavy elements abundance 160% of solar.[ 9] The star has a modest level of magnetic activity in its chromosphere .[ 6] It has 1.10 times the mass of the Sun and 1.04 times the Sun's radius.[ 8] This star is radiating 1.15[ 8] times the luminosity of the Sun from its photosphere at an effective temperature of 5,865 K.[ 8]
Initially it was thought the system consisted of a single star, but in 2016 it was discovered the primary is accompanied by the M-class red dwarf star at a projected separation of 36.5± 1.9 AU .[ 7] The evidence for this stellar companion being on a bound orbit was further fortified in 2017.[ 11] [ 4]
Planetary system
Artistic illustration of the planet
In 2011, a gas giant , HD 164509 Ab, was discovered orbiting the primary of HD 164509 using Doppler spectroscopy .[ 6] Given the binary nature of this system, the planet HD 164509 Ab could not have formed on the current orbit, which is unstable in long term.[ 12] Instead, it may be a captured body formed elsewhere.[ 13]
References
^ a b c d Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters . 38 (5): 331. arXiv :1108.4971 . Bibcode :2012AstL...38..331A . doi :10.1134/S1063773712050015 . S2CID 119257644 .
^ a b c d e f g h Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties" . Astronomy and Astrophysics . 674 : A1. arXiv :2208.00211 . Bibcode :2023A&A...674A...1G . doi :10.1051/0004-6361/202243940 . S2CID 244398875 .
Gaia DR3 record for this source at VizieR .
^ a b Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey . 5 . Bibcode :1999MSS...C05....0H .
^ a b c d Gonzales, Erica J.; et al. (April 2020), "The TRENDS High-contrast Imaging Survey. VIII. Compendium of Benchmark Objects", The Astrophysical Journal , 893 (1): 27, arXiv :2010.11866 , Bibcode :2020ApJ...893...27G , doi :10.3847/1538-4357/ab71fb , S2CID 216296289 , 27
^ a b Soubiran, C.; et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics . 616 : A7. arXiv :1804.09370 . Bibcode :2018A&A...616A...7S . doi :10.1051/0004-6361/201832795 . S2CID 52952408 .
^ a b c d e f g h Giguere, Matthew J.; et al. (2012). "A High-Eccentricity Component in the Double-Planet System Around Hd 163607 and a Planet Around Hd 164509". The Astrophysical Journal . 744 (1): 4. arXiv :1109.2955 . Bibcode :2012ApJ...744....4G . doi :10.1088/0004-637X/744/1/4 . S2CID 119207947 .
^ a b Wittrock, Justin M.; et al. (2016). "Stellar Companions to the Exoplanet Host Stars HD 2638 and HD 164509" . The Astronomical Journal . 152 (5): 149. arXiv :1609.00016 . Bibcode :2016AJ....152..149W . doi :10.3847/0004-6256/152/5/149 . S2CID 45942803 .
^ a b c d e f g h i Bonfanti, A.; Ortolani, S.; Piotto, G.; Nascimbeni, V. (2015). "Revising the ages of planet-hosting stars". Astronomy & Astrophysics . 575 : A18. arXiv :1411.4302 . Bibcode :2015A&A...575A..18B . doi :10.1051/0004-6361/201424951 . S2CID 54555839 .
^ a b Bryan, Marta L.; et al. (April 2016). "Statistics of Long Period Gas Giant Planets in Known Planetary Systems" . The Astrophysical Journal . 821 (2): 89. arXiv :1601.07595 . Bibcode :2016ApJ...821...89B . doi :10.3847/0004-637X/821/2/89 . 89.
^ "HD 164509" . SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2023-12-27 .
^ Ngo, Henry; et al. (2017). "No Difference in Orbital Parameters of RV-detected Giant Planets between 0.1 and 5 au in Single versus Multi-stellar Systems" . The Astronomical Journal . 153 (6): 242. arXiv :1704.02326 . Bibcode :2017AJ....153..242N . doi :10.3847/1538-3881/aa6cac . S2CID 119106164 .
^ Quarles, Billy; Li, Gongjie; Kostov, Veselin; Haghighipour, Nader (2020). "Orbital Stability of Circumstellar Planets in Binary Systems" . The Astronomical Journal . 159 (3): 80. arXiv :1912.11019 . Bibcode :2020AJ....159...80Q . doi :10.3847/1538-3881/ab64fa . S2CID 209444271 .
^ Fragione, Giacomo (2018). "Dynamical origin of S-type planets in close binary stars" . Monthly Notices of the Royal Astronomical Society . 483 (3): 3465–3471. arXiv :1812.02754 . Bibcode :2019MNRAS.483.3465F . doi :10.1093/mnras/sty3367 . S2CID 119457949 .