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  • 21 Aug, 2019

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HD 222582

HD 222582 is a multiple star system in the equatorial constellation of Aquarius. It is invisible to the naked eye with an apparent visual magnitude of 7.7, but can be viewed with binoculars or a small telescope. The system is located at a distance of 137 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +12 km/s. It is located close enough to the ecliptic that it is subject to lunar occultations.

The primary member of this system, designated component A, is an ordinary G-type main-sequence star with a stellar classification of G5V. The physical properties of the star are similar enough to the Sun that it is considered a candidate solar twin. It is about 6.5 billion years old with an inactive chromosphere and is spinning with a low projected rotational velocity of 1.7 km/s. The mass and metallicity of this star are essentially the same as the Sun. It has a 14% larger radius and is radiating 1.3 times the luminosity of the Sun from its photosphere at an effective temperature of 5,790 K.

Component B of this system is a close binary system with the components designated HD 222582 Ba and Bb. The pair have a combined class of M4.5 V+ and about 20% the mass of the Sun.

Planetary system

In November 1999, a dense superjovian planet was announced orbiting the primary by the California and Carnegie Planet Search. Designated component 'b', it was discovered using the radial velocity method, using 24 observations over a period of 1.5 years. The exoplanet is orbiting with a period of 1.57 years and a very large eccentricity of 0.76, ranging in distance from 0.39 AU out to 2.31 AU away from the primary.

The HD 222582 planetary system
Companion
(in order from star)
Mass Semimajor axis
(AU)
Orbital period
(days)
Eccentricity Inclination Radius
b 8.37 MJ 1.35 572 0.76

See also

References

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  19. ^ "HD 222582 b". Exoplanet Catalogue. NASA Astrophysics Division. Retrieved 2020-12-31.