HD 210277 b

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HD 210277 b is an exoplanet that orbits the star HD 210277. It was discovered on September 9, 1998, by the California and Carnegie Planet Search team using the radial velocity method. The planet is at least about 1.24 times as massive as Jupiter and orbits at roughly 1.14 astronomical units from the star. Its orbit is highly elongated (eccentricity about 0.476), so its distance from the star ranges from about 0.60 AU at closest approach to about 1.69 AU at farthest, with a period of about 442 days. The planet’s true mass depends on orbital inclination; early data suggested it could be a brown dwarf, but those results were not confirmed.