The stellar metallicity--giant planet connection

González, Guillermo

doi:10.1093/mnras/285.2.403

Cited by 609 publications

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“…The enrichment of refractory elements in XO-2N when compared with XO-2S could be due to accretion of material onto the star and subsequent ingestion of rocky material coming from already formed planets or from the inner part of the disk and pushed into XO-2N by its hot Jupiter as it migrated inward to the current position, most likely as a result of planet-planet scattering (Gonzalez 1997;Ida & Lin 2008;Raymond et al 2011). We discussed in Paper II that migration to the current close orbit of XO-2Nb cannot be due to Kozai interaction for the current orbit configuration, supporting a phase of dynamical instability in the planetary system.…”

Section: Excess Of Heavy Elements In Xo-2n?mentioning

confidence: 99%

“…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%

“…Two different versions of this second scenario have been proposed. In the first one, disk-planet or planet-planet interactions may cause the infall of metal-rich (rocky) material onto the star (Gonzalez 1997). In this case, the presence of planets is expected to positively correlate with metallicity.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Excess Of Heavy Elements In Xo-2n?mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The GAPS programme with HARPS-N at TNG

Biazzo

Gratton

Desidera

et al. 2015

A&A

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“…However, before interpreting these results physically, it is important to check for metallicity bias in the subsample of stars around which Neptune mass planets could have been found. Santos, Israelian, & Mayor (2004) and performed analogous tests for giant planets after Gonzalez (1997) noted that published planet hosts were all metal rich. In this case, Neptunes might only be detectable around stars with low intrinsic velocity variations, which might imply low activity, old age, and hence low metallicity.…”

Section: Frequency Of Neptune Mass Planetsmentioning

confidence: 99%

“…Nonetheless, the dependence of planet formation on disk abundances can be observationally constrained by studying the frequency of observed planets as a function of photospheric abundance. Gonzalez (1997) noted that the first four stars known to host an exoplanet were all metal rich compared to the Sun. As more planet hosts were discovered, Gonzalez and others showed that known planet hosts tended to be metal rich compared to the Sun.…”

Section: Introductionmentioning

confidence: 99%

Metallicity and Planet Formation – Observations

Valenti¹

2009

Proc. IAU

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Abstract. Early abundance measurements established that stars known to host giant planets are metal rich compared to the Sun. More extensive abundance measurements then showed that giant planet hosts are metal rich compared to the parent sample in planet searches. Stars spanning a range of convection zone depths all show the same metallicity effect, ruling out significant abundance enhancements due to selective accretion. Most known planets migrated inwards from the snow line, but subsamples closer to and further from the star have similar iron abundances, so the stopping point of migration does not depend on metallicity. Stars recently discovered to host Neptune mass planets may be metal poor compared to the Sun, particularly if one focusses on stars that do not also host higher mass planets. This would be consistent with core-accretion models of planet formation. Before drawing physical conclusions, it will be necessary to check for metallicity bias in the subsample of stars around which Neptune mass planets could have been found. M dwarf abundances are currently too uncertain to relate planet frequency and host star metallicity, due mainly to missing or incorrect molecular line data.

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Exoplanet Observations

Bean

2010

Formation and Evolution of Exoplanets

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The stellar metallicity--giant planet connection

Cited by 609 publications

References 0 publications

The GAPS programme with HARPS-N at TNG

The GAPS programme with HARPS-N at TNG

Metallicity and Planet Formation – Observations

Exoplanet Observations

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