The star is young and very active and is a member of theAB Doradus Moving Group.[8] The star has also been studied and monitored bySuperWASP group and found to coincide with theROSAT source 1RXS J072343.6+202500.[1] The planet candidate was announced in December 2009.[5]
The Keplerian fit of theradial velocity data suggested an orbital solution for a close-in massiveplanet with an orbital period of 7.7834 days. Moreover, the presence of a close-in massivejovian 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 aroundTW Hydrae, which was also found to be due to stellar activity rather than orbital motion.[10]
^abSamus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)".VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S.1.Bibcode:2009yCat....102025S.
^Torres, C. A. O.; Quast, G. R.; Melo, C. H. F.; Sterzik, M. F. (2008). "Young Nearby Loose Associations".Handbook of Star Forming Regions, Volume II: The Southern Sky. ASP Monograph Publications. Vol. 5. pp. 1–757.arXiv:0808.3362.Bibcode:2008hsf2.book..757T.
^Figueira; Marmier; Bonfils; di Folco; Udry; Santos; Lovis; Megevand; Melo; Pepe, F.; Queloz, D.; Segransan, D.; Triaud, A. H. M. J.; Viana Almeida, P.; et al. (2010). "Evidence against the young hot-Jupiter around BD +20 1790".Astronomy and Astrophysics.513: L8.arXiv:1003.3678.Bibcode:2010A&A...513L...8F.doi:10.1051/0004-6361/201014323.S2CID119199263.
