Parent Stars of Extrasolar Planets. VII. New Abundance Analyses of 30 Systems

Laws, Chris; González, Guillermo; Walker, Kyle M.; Tyagi, S.; Dodsworth, Jeremy A.; Snider, Keely; Suntzeff, Nicholas B.

doi:10.1086/374626

Cited by 131 publications

(179 citation statements)

References 48 publications

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“…( Table 1). LTE analysis of our HIRES spectra shows that ½Fe=H ¼ À0:42 , in good agreement with the value found by Santos et al (2004) of À0:38 AE 0:04 and by Laws et al (2003) of À0:37 AE 0:03. The Ca ii H and K emission cores show that log R 0 HK ¼ À4:90, implying an expected jitter of 3.2 m s À1 .…”

Section: Hd 50499supporting

confidence: 90%

“…The Ca ii H and K emission cores show that log R 0 HK ¼ À4:90, implying an expected jitter of 3.2 m s À1 . From its B À V of 0.67, M V , metallicity, and the models of Girardi et al (2002), the stellar mass is M ¼ 0:78 AE 0:1 M , in good agreement with the mass found by Santos et al (2004) of 0.75 M and by Laws et al (2003) of 0.77 M . But see Fernandes & Santos (2004), who find M ¼ 0:94 M .…”

Section: Hd 50499supporting

confidence: 78%

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Five New Multicomponent Planetary Systems

Vogt

Butler

Marcy

et al. 2005

ApJ

233

274

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We report Doppler measurements for six nearby G-and K-type main-sequence stars that show multiple low-mass companions, at least one of which has planetary mass. One system has three planets, the fourth triple-planet system known around a normal star, and another has an extremely low minimum mass of 18 M È . HD 128311 ( K0 V ) has two planets (one previously known) with minimum masses (M sin i) of 2.18M J and 3.21M J and orbital periods of 1.26 and 2.54 yr, suggesting a possible 2:1 resonance. For HD 108874 (G5 V ), the velocities reveal two planets (one previously known) having minimum masses and periods of (M sin i b ¼ 1:36M J , P b ¼ 1:08 yr) and (M sin i c ¼ 1:02M J , P c ¼ 4:4 yr). HD 50499 (G1 V ) has a planet with P ¼ 6:8 yr and M sin i ¼ 1:7M J , and the velocity residuals exhibit a trend of À4.8 m s À1 yr À1 , indicating a more distant companion with P > 10 yr and minimum mass of 2M J . HD 37124 (G4 IV-V ) has three planets, one having M sin i ¼ 0:61M J and P ¼ 154:5 days, as previously known. We find two plausible triple-planet models that fit the data, both having a second planet near P ¼ 840 days, with the more likely model having its third planet in a 6 yr orbit and the other one in a 29 day orbit. For HD 190360, we confirm the planet having P ¼ 7:9 yr and M sin i ¼ 1:5M J as found by the Geneva team, but we find a distinctly noncircular orbit with e ¼ 0:36 AE 0:03, rendering this not an analog of Jupiter as had been reported. Our velocities also reveal a second planet with P ¼ 17:1 days and M sin i ¼ 18:1 M È . HD 217107 (G8 IV) has a previously known ''hot Jupiter'' with M sin i ¼ 1:4M J and P ¼ 7:13 days, and we confirm its high eccentricity, e ¼ 0:13. The velocity residuals reveal an outer companion in an eccentric orbit, having minimum mass of M sin i > 2M J , eccentricity e $ 0:5, and a period P > 8 yr, implying a semimajor axis a > 4 AU and providing an opportunity for direct detection. We have obtained high-precision photometry of five of the six planetary host stars with three of the automated telescopes at Fairborn Observatory. We can rule out significant brightness variations in phase with the radial velocities in most cases, thus supporting planetary reflex motion as the cause of the velocity variations. Transits are ruled out to very shallow limits for HD 217107 and are also shown to be unlikely for the prospective inner planets of the HD 37124 and HD 108874 systems. HD 128311 is photometrically variable with an amplitude of 0.03 mag and a period of 11.53 days, which is much shorter than the orbital periods of its two planetary companions. This rotation period explains the origin of periodic velocity residuals to the two-planet model of this star. All of the planetary systems here would be further constrained with astrometry by the Space Interferometry Mission.

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Section: Hd 50499supporting

confidence: 90%

Section: Hd 50499supporting

confidence: 78%

Five New Multicomponent Planetary Systems

Vogt

Butler

Marcy

et al. 2005

ApJ

233

274

View full text Add to dashboard Cite

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“…A well-established direct dependence exists between the occurrence rate of giant planets and the metal content of their main-sequence hosts (Gonzalez 1997;Butler et al 2000;Laws et al 2003;Santos et al 2004;Fischer & Valenti 2005;Udry & Santos 2007;Sozzetti et al 2009;Mortier et al 2012). …”

Section: Introductionmentioning

confidence: 99%

The GAPS programme with HARPS-N at TNG

Biazzo

Gratton

Desidera

et al. 2015

A&A

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Binary stars hosting exoplanets are a unique laboratory where chemical tagging can be performed to measure the elemental abundances of both stellar components with high accuracy, with the aim to investigate the formation of planets and their subsequent evolution. Here, we present a high-precision differential abundance analysis of the XO-2 wide stellar binary based on high-resolution HARPS-N at TNG spectra. Both components are very similar K-dwarfs and host planets. Since they formed presumably within the same molecular cloud, we expect that they possess the same initial elemental abundances. We investigated whether planets can cause some chemical imprints in the stellar atmospheric abundances. We measure abundances of 25 elements for both stars with a range of condensation temperature T C = 40−1741 K, achieving typical precisions of ∼0.07 dex. The northern component shows abundances in all elements higher by +0.067 ± 0.032 dex on average, with a mean difference of +0.078 dex for elements with T C > 800 K. The significance of the XO-2N abundance difference relative to XO-2S is at the 2σ level for almost all elements. We discuss that this result might be interpreted as the signature of the ingestion of material by XO-2N or depletion in XO-2S that is due to locking of heavy elements by the planetary companions. We estimate a mass of several tens of M ⊕ in heavy elements. The difference in abundances between XO-2N and XO-2S shows a positive correlation with the condensation temperatures of the elements, with a slope of (4.7 ± 0.9) × 10 −5 dex K −1 , which could mean that both components have not formed terrestrial planets, but first experienced the accretion of rocky core interior to the subsequent giant planets.

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“…Numerous studies have reached the conclusion that giant planets are detected more often around metal-rich stars [115,119,120]. The origin of the trend has 2) Stellar photospheric chemical abundances are typically given as the logarithm of the fractional abundance relative to the hydrogen abundance and on a scale relative to the solar value.…”

Section: Planet-stellar Composition Correlationmentioning

confidence: 99%

Exoplanet Observations

Bean

2010

Formation and Evolution of Exoplanets

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Parent Stars of Extrasolar Planets. VII. New Abundance Analyses of 30 Systems

Cited by 131 publications

References 48 publications

Five New Multicomponent Planetary Systems

Five New Multicomponent Planetary Systems

The GAPS programme with HARPS-N at TNG

Exoplanet Observations

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