Matches in DBpedia 2016-04 for { ?s ?p "HD 30177 b is an extrasolar planet located approximately 178 light-years away in the constellation of Dorado, orbiting the star HD 30177. This is one of the most massive planets ever detected by the radial velocity method. In addition, the planet orbits far from the star, about 4 AU away, taking 2770 days (7.58 years) to orbit the star. Even though the massive planet is orbiting at 4 AU from the star, the radial velocity semi-amplitude is high, around 146.8±2.8 m/s. Since the inclination (and thus the true mass) is not known, this planet candidate may in fact be a brown dwarf.This planet was discovered on June 13, 2002 by Tinney, Butler, and Marcy et al. using the Doppler spectroscopy from the Anglo-Australian Telescope."@en }
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- HD_30177_b abstract "HD 30177 b is an extrasolar planet located approximately 178 light-years away in the constellation of Dorado, orbiting the star HD 30177. This is one of the most massive planets ever detected by the radial velocity method. In addition, the planet orbits far from the star, about 4 AU away, taking 2770 days (7.58 years) to orbit the star. Even though the massive planet is orbiting at 4 AU from the star, the radial velocity semi-amplitude is high, around 146.8±2.8 m/s. Since the inclination (and thus the true mass) is not known, this planet candidate may in fact be a brown dwarf.This planet was discovered on June 13, 2002 by Tinney, Butler, and Marcy et al. using the Doppler spectroscopy from the Anglo-Australian Telescope.".
- Q8408996 abstract "HD 30177 b is an extrasolar planet located approximately 178 light-years away in the constellation of Dorado, orbiting the star HD 30177. This is one of the most massive planets ever detected by the radial velocity method. In addition, the planet orbits far from the star, about 4 AU away, taking 2770 days (7.58 years) to orbit the star. Even though the massive planet is orbiting at 4 AU from the star, the radial velocity semi-amplitude is high, around 146.8±2.8 m/s. Since the inclination (and thus the true mass) is not known, this planet candidate may in fact be a brown dwarf.This planet was discovered on June 13, 2002 by Tinney, Butler, and Marcy et al. using the Doppler spectroscopy from the Anglo-Australian Telescope.".