Measuring Elemental Abundances of JWST Target Stars for Exoplanet Characterization I. FGK Stars

Kolecki, Jared R.; Wang, Ji

doi:10.48550/arxiv.2112.02031

Cited by 8 publications

(19 citation statements)

References 45 publications

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“…There is some tension between our parameters and those reported by Kolecki & Wang (2021) that we attribute to their neglect of extinction and their use of Two Micron All Sky Survey (2MASS) and Wide-field Infrared Survey Explorer (WISE) photometry for WASP-77 A that were contaminated by its binary companion WASP-77 B. The excellent agreement between our photospheric and fundamental stellar parameters for WASP-77 A and those inferred by other groups suggests that any systematic uncertainties present must be small.…”

Section: (2021)contrasting

confidence: 90%

Section: Elemental Abundancessupporting

confidence: 89%

“…Our abundance inferences for carbon, sodium, magnesium, and silicon are consistent with those presented in Kolecki & Wang (2021), though our oxygen and potassium abundances are significantly higher than those presented in that paper. We are able to reproduce the oxygen abundance reported in Kolecki & Wang (2021) using their photospheric stellar parameters, our equivalent width measurements, and 3D non-LTE abundance corrections from Amarsi et al (2019). We are therefore confident that the tension between our oxygen abundances results from the photospheric stellar parameters Kolecki & Wang (2021) derived for WASP-77 A that are hotter and more metal-poor than those derived by us, Maxted et al (2013), andMortier et al (2013) as updated by Sousa et al (2021).…”

Section: Elemental Abundancessupporting

confidence: 89%

“…In that way, all of the parameters necessary to characterize an exoplanet system can be made self-consistent to eliminate the small but possibly important systematic uncertainties that can effect an exoplanet atmosphere abundance inference. If the photospheric stellar parameters that produce carbon and oxygen abundances are not used to self consistently infer (1) stellar masses and radii and (2) planet parameters using observables, then those photospheric abundances are not suitable for exoplanet atmospheric characterization (e.g., Kolecki & Wang 2021).…”

Section: Updated Planetary Parametersmentioning

confidence: 99%

“…in the paper announcing the discovery of WASP-77 A b. Photospheric and/or fundamental parameters for the star based on highresolution spectroscopy have since been published byMortier et al (2013) (updated in Sousa et al 2021 andKolecki & Wang (2021) Maxted et al (2013). found T eff = 5500 ± 80 K, log g = 4.33 ± 0.08, [Fe/H] = 0.00 ± 0.11, M * = 1.00 ± 0.07 M , τ iso = 8 Gyr, and P rot = 15.4 ± 0.4 days Mortier et al (2013).…”

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confidence: 99%

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Evidence that the Hot Jupiter WASP-77 A b Formed Beyond Its Parent Protoplanetary Disk's H2O Ice Line

Reggiani,

Schlaufman,

Healy

et al. 2022

Preprint

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Idealized protoplanetary disk and giant planet formation models have been interpreted to suggest that a giant planet's atmospheric abundances can be used to infer its formation location in its parent protoplanetary disk. It has recently been reported that the hot Jupiter WASP-77 A b has sub-solar atmospheric carbon and oxygen abundances with a solar C/O abundance ratio. Assuming solar carbon and oxygen abundances for its host star WASP-77 A, WASP-77 A b's atmospheric carbon and oxygen abundances possibly indicate that it accreted its envelope interior to its parent protoplanetary disk's H 2 O ice line from carbon-depleted gas with little subsequent planetesimal accretion or core erosion. We comprehensively model WASP-77 A and use our results to better characterize WASP-77 A b. We show that the photospheric abundances of carbon and oxygen in WASP-77 A are super-solar with a sub-solar C/O abundance ratio, implying that WASP-77 A b's atmosphere has significantly sub-stellar carbon and oxygen abundances with a super-stellar C/O ratio. Our result possibly indicates that WASP-77 A b's envelope was accreted by the planet beyond its parent protoplanetary disk's H 2 O ice line. While numerous theoretical complications to these idealized models have now been identified, the possibility of non-solar protoplanetary disk abundance ratios confound even the most sophisticated protoplanetary disk and giant planet formation models. We therefore argue that giant planet atmospheric abundance ratios can only be meaningfully interpreted relative to the possibly non-solar mean compositions of their parent protoplanetary disks as recorded in the photospheric abundances of their solar-type dwarf host stars.

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Section: (2021)contrasting

confidence: 90%

Section: Elemental Abundancessupporting

confidence: 89%

Section: Elemental Abundancessupporting

confidence: 89%

Section: Updated Planetary Parametersmentioning

confidence: 99%

mentioning

confidence: 99%

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Evidence that the Hot Jupiter WASP-77 A b Formed Beyond Its Parent Protoplanetary Disk's H2O Ice Line

Reggiani,

Schlaufman,

Healy

et al. 2022

Preprint

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How drifting and evaporating pebbles shape giant planets

Bitsch

Kreidberg

2022

A&A

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Atmospheric abundances of exoplanets are thought to constrain the planet formation pathway, because different species evaporate at different temperatures and thus radii in the protoplanetary disc, leaving distinct signatures inside the accreted planetary atmosphere. In particular the planetary C/O ratio is thought to constrain the planet formation pathway, because of the condensation sequence of H 2 O, CO 2 , CH 4 , and CO, resulting in an increase of the gas phase C/O ratio with increasing distance to the host star. Here we use a disc evolution model including pebble growth, drift and evaporation coupled with a planet formation model that includes pebble and gas accretion as well as planet migration to compute the atmospheric compositions of giant planets. We compare our results to the recent observational constraints of the hot Jupiters WASP-77A b and τ Boötis b. WASP-77A b's atmosphere features sub-solar C/H, O/H, H 2 O/H with slightly super-solar C/O, while τ Boötis b's atmosphere features super-solar C/H, O/H and C/O with sub-solar H 2 O/H. Our simulations qualitatively reproduce these measurements and show that giants like WASP-77A b should start to form beyond the CO 2 evaporation front, while giants like τ Boötis b should originate from beyond the water ice line. Our model allows the formation of sub-and super-solar atmospheric compositions within the same framework. On the other hand, simulations without pebble evaporation, as used in classical models, can not reproduce the super-solar C/H and O/H ratios of τ Boötis b's atmosphere without the additional accretion of solids. Furthermore, we identify the α viscosity parameter of the disc as a key ingredient regarding planetary composition, because the viscosity drives the inward motion of volatile enriched vapor, responsible for the accretion of gaseous carbon and oxygen. Depending on the planet's migration history through the disc across different evaporation fronts, orderof-magnitude differences in atmospheric carbon and oxygen abundance should be expected. Our simulations additionally predict super-solar N/H for τ Boötis b and solar N/H for WASP-77A b. We conclude thus that pebble evaporation is a key ingredient to explain the variety of exoplanet atmospheres, because it can explain both, sub-and super-solar atmospheric abundances.

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The GAPS Programme at TNG

Biazzo

D’Orazi

Desidera

et al. 2022

A&A

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Context. Exoplanetary properties strongly depend on stellar properties: to know the planet with accuracy and precision it is necessary to know the star as accurately and precisely as possible. Aims. Our immediate aim is to characterize in a homogeneous and accurate way a sample of 27 transiting planet-hosting stars observed within the Global Architecture of Planetary System program. For the wide visual binary XO-2, we considered both components (N: hosting a transiting planet; S: without a known transiting planet). Our final goal is to widely analyze the sample by deriving several stellar properties, abundances of many elements, kinematic parameters, and discuss them in the context of planetary formation. Methods. We determined the stellar parameters (effective temperature, surface gravity, rotational velocity) and abundances of 26 elements (Li, C,

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Measuring Elemental Abundances of JWST Target Stars for Exoplanet Characterization I. FGK Stars

Cited by 8 publications

References 45 publications

Evidence that the Hot Jupiter WASP-77 A b Formed Beyond Its Parent Protoplanetary Disk's H2O Ice Line

Evidence that the Hot Jupiter WASP-77 A b Formed Beyond Its Parent Protoplanetary Disk's H2O Ice Line

How drifting and evaporating pebbles shape giant planets

The GAPS Programme at TNG

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