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V429 Geminorum
V429 Geminorum (BD+20°1790) is a young orange dwarf star in the constellation Gemini, located 90 light years away from the Sun. It is a BY Draconis variable, a cool dwarf which varies rapidly in brightness as it rotates. DescriptionThe star is young and very active and is a member of the AB Doradus Moving Group.[8] The star has also been studied and monitored by SuperWASP group and found to coincide with the ROSAT source 1RXS J072343.6+202500.[1] The planet candidate was announced in December 2009.[5] Disproven planetThe Keplerian fit of the radial velocity data suggested an orbital solution for a close-in massive planet with an orbital period of 7.7834 days. Moreover, the presence of a close-in massive jovian planet could explain the high level of stellar activity detected.[5] However, further study suggests that this planet does not exist because the radial velocity variations are strongly correlated to stellar activity, suggesting this activity is the cause of the variations.[9][6] This echoes the similar case of the disproven planet detection around TW Hydrae, which was also found to be due to stellar activity rather than orbital motion.[10] References
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