2009
DOI: 10.1051/0004-6361/200911658
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A planet around the evolved intermediate-mass star HD 110014

Abstract: Context. We found evidence for a sub-stellar companion around the K giant star HD 110014. This cool evolved star, with a spectral type K2III and an estimated mass between 1.9 and 2.4 M , is slightly metal rich with [Fe/H] = 0.19 and a rotational velocity V sin i = 2.0 km s −1 . Aims. To search for extrasolar planets around intermediate-mass stars and to improve our knowledge of the nature of radial velocity variations shown by G and K giant stars. Methods. Based on radial velocity analysis, we found evidence f… Show more

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Cited by 24 publications
(17 citation statements)
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“…If confirmed, the determined orbit of the 1.8 M Jup mass planet is fairly eccentric, e = 0.25 ± 0.03, but, up to now, 6 out of 22 companions around K-giants show more than 0.2 eccentricity: e = 0.7 of ι Dra (Frink et al 2002), e = 0.2 of K1 III star HD 47536 (Setiawan et al 2003,b), e = 0.27 of K1 II-III star HD 13189 (Hatzes et al 2005), e = 0.43 of K1 III star 4 UMa (Döllinger et al 2007), e = 0.38 of K1.5 III star 42 Dra (Döllinger et al 2009), and e = 0.46 of K2 III star HD 110014 (de Medeiros et al 2009). The eccentricity for the planetary orbit of α Ari is therefore not unusual among K-giants, and such eccentric modulation is difficult to produce by surface variations or stellar oscillations.…”
Section: Discussionmentioning
confidence: 99%
“…If confirmed, the determined orbit of the 1.8 M Jup mass planet is fairly eccentric, e = 0.25 ± 0.03, but, up to now, 6 out of 22 companions around K-giants show more than 0.2 eccentricity: e = 0.7 of ι Dra (Frink et al 2002), e = 0.2 of K1 III star HD 47536 (Setiawan et al 2003,b), e = 0.27 of K1 II-III star HD 13189 (Hatzes et al 2005), e = 0.43 of K1 III star 4 UMa (Döllinger et al 2007), e = 0.38 of K1.5 III star 42 Dra (Döllinger et al 2009), and e = 0.46 of K2 III star HD 110014 (de Medeiros et al 2009). The eccentricity for the planetary orbit of α Ari is therefore not unusual among K-giants, and such eccentric modulation is difficult to produce by surface variations or stellar oscillations.…”
Section: Discussionmentioning
confidence: 99%
“…Different methods, such as radial velocity measurements (Butler et al 1996;de Medeiros et al 2009) and photometric light curves (Konacki et al 2003(Konacki et al , 2004, have been used to discover new planetary systems around other stars than the Sun. Aiming to make our sample homogeneous, we only use stars that had their planets discovered with radial velocity method.…”
Section: Stellar Working Sample and Datamentioning
confidence: 99%
“…This programme detected two giant exoplanets around HD 47536 (Setiawan et al 2003b), one around HD 11977 (Setiawan et al 2005), and more recently one around HD 110014 (de Medeiros et al 2009). We started a similar survey in February 2004 (Döllinger 2008) monitoring a sample of 62 K giant stars using higher RV accuracy at TLS.…”
Section: Introductionmentioning
confidence: 99%