A substellar companion around the intermediate-mass  giant star HD 11977

Setiawan, J.; Rodmann, J.; Silva, L. da; Hatzes, A. P.; Pasquini, L.; Lühe, O. von der; Medeiros, J. R. De; Döllinger, M. P.; Girardi, L.

doi:10.1051/0004-6361:200500133

Cited by 74 publications

(63 citation statements)

References 17 publications

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“…235.4 ± 10.6 f (m) [M ] ( 4 .79 ± 0.57) × 10 −7 a [AU] 2.36 ± 0.02 survey carried out with the Fiber-fed Extended Range Optical Spectrograph (FEROS) by Setiawan et al (2004aSetiawan et al ( , 2005. The FEROS and TLS giants have radii on average about 10 times larger than solar stars (da Silva et al 2006;Döllinger et al 2008b).…”

Section: Discussionmentioning

confidence: 99%

Planetary companion candidates around the K giant stars 42 Draconis and HD 139 357

Döllinger¹,

Hatzes

Pasquini³

et al. 2009

A&A

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Context. For the past 3 years we have been monitoring 62 K giant stars using precise stellar radial velocity (RV) measurements with the 2 m Alfred Jensch Telescope of the Thüringer Landessternwarte Tautenburg (TLS). Aims. To probe the dependence of planet formation on stellar mass by finding planets around intermediate-mass giant stars. Methods. We present high accuracy RV measurements of the K1.5 III star 42 Dra and the K4 III star HD 139357. The wavelength reference for the RV measurements was provided by an iodine absorption cell placed in the optical path of the spectrograph. Results. Our measurements reveal that the time series of the radial velocity of 42 Dra shows a periodic variation of 479.1 days with a semiamplitude of K = 112.5 m s −1 . An orbital solution yields a mass function of f (m) = (5.29 ± 0.62) × 10 −8 solar masses (M ) and an eccentricity of e = 0.38 ± 0.06. From our template spectra, taken without the iodine cell, we determine a metallicity of −0.46 ± 0.04 dex and a stellar mass of 0.98 ± 0.06 M for this star. HD 139 357 shows periodic RV variations of 1125.7 days with a semiamplitude K = 159.9 m s −1 . An orbital solution yields an eccentricity, e = 0.10 ± 0.02 and mass function, f (m) = (4.79 ± 0.57) × 10 −7 M . An iron abundance of −0.13 ± 0.04 dex is obtained, and a stellar mass of 1.31 ± 0.24 M for the parent star is derived. An analysis of the HIPPARCOS photometry as well as our Hα core flux measurements reveal no variability with the radial velocity period. Keplerian motion is the most likely explanation for the observed radial velocity variations for these stars. Conclusions. The K giant stars 42 Dra and HD 139 357 host extrasolar planets with "minimum masses" of 3.88 ± 0.85 Jupiter masses M Jup and 9.76 ± 2.15 M Jup , respectively.

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Section: Discussionmentioning

confidence: 99%

Planetary companion candidates around the K giant stars 42 Draconis and HD 139 357

Döllinger¹,

Hatzes

Pasquini³

et al. 2009

A&A

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“…At the other end of the mass scale, the problems inherent to massive, early-type stars can be overcome by observing targets at a later stage of their evolution (Hatzes et al 2003;Setiawan et al 2005;Sato et al 2005;Reffert et al 2006;Johnson et al 2007b;Niedzielski et al 2007;Liu et al 2008;Döllinger et al 2009). Once stars exhaust their core hydrogen fuel sources, they move off of the main sequence, become cooler, and shed a large fraction of their primordial angular momentum (Gray & Nagar 1985;do Nascimento et al 2000).…”

Section: Introductionmentioning

confidence: 99%

Giant Planet Occurrence in the Stellar Mass-Metallicity Plane

Johnson¹,

Aller²,

Howard³

et al. 2010

PUBL ASTRON SOC PAC

746

824

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ABSTRACT. Correlations between stellar properties and the occurrence rate of exoplanets can be used to inform the target selection of future planet-search efforts and provide valuable clues about the planet-formation process. We analyze a sample of 1266 stars drawn from the California Planet Survey targets to determine the empirical functional form describing the likelihood of a star harboring a giant planet as a function of its mass and metallicity. Our stellar sample ranges from M dwarfs with masses as low as 0:2 M ⊙ to intermediate-mass subgiants with masses as high as 1:9 M ⊙ . In agreement with previous studies, our sample exhibits a planet-metallicity correlation at all stellar masses; the fraction of stars that harbor giant planets scales as f ∝ 10 1:2½Fe=H . We can rule out a flat metallicity relationship among our evolved stars (at 98% confidence), which argues that the high metallicities of stars with planets is not likely due to convective envelope "pollution." Our data also rule out a constant planet occurrence rate for ½Fe=H < 0, indicating that giant planets continue to become rarer at sub-Solar metallicities. We also find that planet occurrence increases with stellar mass (f ∝ M ⋆ ), characterized by a rise from 3% around M dwarfs (0:5 M ⊙ ) to 14% around A stars (2 M ⊙ ), at Solar metallicity. We argue that the correlation between stellar properties and giant planet occurrence is strong supporting evidence of the core-accretion model of planet formation.

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“…Therefore, G and K giant stars are suitable targets for detecting exoplanets with the RV technique. There are several ongoing exoplanet survey projects around giant stars (Setiawan et al 2005;Hatzes et al 2005;Sato et al 2007;Johnson et al 2007;Lovis & Mayor 2007;Niedzielski et al 2007;Liu et al 2008). Now, more Based on observations made with the BOES spectrograph at the 1.8 m telescope of BOAO, KASI RV data (Table 3) is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/509/A24 than 20 exoplanets have been detected around giant stars and from this sample some statistical studies on the planetary systems around giants have been made (Pasquini et al 2007;Hekker et al 2008;Sato et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Detection of a planetary companion around the giant star γ¹Leonis

Han¹,

Lee

Kim³

et al. 2010

A&A

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Aims. Our primary goal is to search for planets around intermediate mass stars. We are also interested in studying the nature of radial velocity (RV) variations of K giant stars. Methods. We selected about 55 early K giant (K0−K4) stars brighter than fifth magnitude that were observed using BOES, a high resolution spectrograph attached to the 1.8 m telescope at BOAO (Bohyunsan Optical Astronomy Observatory). BOES is equipped with I 2 absorption cell for high precision RV measurements. Results. We detected a periodic radial velocity variations in the K0 III star γ 1 Leonis with a period of P = 429 days. An orbital fit of the observed RVs yields a period of P = 429 days, a semi-amplitude of K = 208 m s −1 , and an eccentricity of e = 0.14. To investigate the nature of the RV variations, we analyzed the photometric, Ca II λ 8662 equivalent width, and line-bisector variations of γ 1 Leonis . We conclude that the detected RV variations can be best explained by a planetary companion with an estimated mass of m sin i = 8.78 M Jupiter and a semi-major axis of a = 1.19 AU, assuming a stellar mass of 1.23 M .

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A substellar companion around the intermediate-mass giant star HD 11977

Cited by 74 publications

References 17 publications

Planetary companion candidates around the K giant stars 42 Draconis and HD 139 357

Planetary companion candidates around the K giant stars 42 Draconis and HD 139 357

Giant Planet Occurrence in the Stellar Mass-Metallicity Plane

Detection of a planetary companion around the giant star γ¹Leonis

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A substellar companion around the intermediate-mass giant star HD 11977

Cited by 74 publications

References 17 publications

Planetary companion candidates around the K giant stars 42 Draconis and HD 139 357

Planetary companion candidates around the K giant stars 42 Draconis and HD 139 357

Giant Planet Occurrence in the Stellar Mass-Metallicity Plane

Detection of a planetary companion around the giant star γ1Leonis

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Product

Resources

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Detection of a planetary companion around the giant star γ¹Leonis