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HD 164509
Binary star in the constellation Ophiuchi From Wikipedia, the free encyclopedia
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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]
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Planetary system
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]
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References
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