SWEET-Cat update and FASMA

Andreasen, D. T.; Sousa, S. G.; Tsantaki, M.; Teixeira, G. D. C.; Mortier, A.; Santos, N. C.; Suárez-Andrés, L.; Delgado-Mena, E.; Ferreira, Andressa Coelho

doi:10.1051/0004-6361/201629967

Cited by 41 publications

(48 citation statements)

References 74 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…I cross match that sample on R.A. and decl. with the catalog of homogeneously derived exoplanet host star stellar parameters from SWEET-Cat (Santos et al 2013;Andreasen et al 2017). Though I did not explicitly restrict the sample to solar-type dwarf primaries, the requirements imposed above produce a sample of primary stars with 4500 K T eff 7000 K and log g 4.0.…”

Section: Sample Definitionmentioning

confidence: 99%

Evidence of an Upper Bound on the Masses of Planets and Its Implications for Giant Planet Formation

Schlaufman

2018

ApJ

149

128

View full text Add to dashboard Cite

Celestial bodies with a mass of M ≈ 10 M Jup have been found orbiting nearby stars. It is unknown whether these objects formed like gas-giant planets through core accretion or like stars through gravitational instability. I show that objects with M 4 M Jup orbit metal-rich solar-type dwarf stars, a property associated with core accretion. Objects with M 10 M Jup do not share this property. This transition is coincident with a minimum in the occurrence rate of such objects, suggesting that the maximum mass of a celestial body formed through core accretion like a planet is less than 10 M Jup . Consequently, objects with M 10 M Jup orbiting solar-type dwarf stars likely formed through gravitational instability and should not be thought of as planets. Theoretical models of giant planet formation in scaled minimum-mass solar nebula Shakura-Sunyaev disks with standard parameters tuned to produce giant planets predict a maximum mass nearly an order of magnitude larger. To prevent newly formed giant planets from growing larger than 10 M Jup , protoplanetary disks must therefore be significantly less viscous or of lower mass than typically assumed during the runaway gas accretion stage of giant planet formation. Either effect would act to slow the Type I/II migration of planetary embryos/giant planets and promote their survival. These inferences are insensitive to the host star mass, planet formation location, or characteristic disk dissipation time.

show abstract

Section: Sample Definitionmentioning

confidence: 99%

Evidence of an Upper Bound on the Masses of Planets and Its Implications for Giant Planet Formation

Schlaufman

2018

ApJ

149

128

View full text Add to dashboard Cite

show abstract

“…Equivalent width measurements were carried out with ARESv2 34 (Sousa et al 2015), while line analysis and spectrum synthesis was performed using MOOG 35 (Sneden 1973) jointly with the ATLAS9 grid of stellar model atmosphere from Castelli & Kurucz (2004), under the assumption of local thermodynamic equilibrium (LTE). We followed the prescription of Andreasen et al (2017) and applied the gravity correction from Mortier et al (2014). The analysis was performed on the resulting co-addition of individual spectra.…”

Section: Stellar Parametersmentioning

confidence: 99%

An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

et al. 2018

View full text Add to dashboard Cite

Ultra-short period (USP) planets are a class of low-mass planets with periods shorter than one day. Their origin is still unknown, with photo-evaporation of mini-Neptunes and in situ formation being the most credited hypotheses. Formation scenarios differ radically in the predicted composition of USP planets, and it is therefore extremely important to increase the still limited sample of USP planets with precise and accurate mass and density measurements. We report here the characterization of a USP planet with a period of 0.28 days around K2-141 (EPIC 246393474), and the validation of an outer planet with a period of 7.7 days in a grazing transit configuration. We derived the radii of the planets from the K2 light curve and used high-precision radial velocities gathered with the HARPS-N spectrograph for mass measurements. For K2-141b, we thus inferred a radius of 1.51±0.05R Å and a mass of 5.08±0.41M Å , consistent with a rocky composition and lack of a thick atmosphere. K2-141c is likely a Neptune-like planet, although due to the grazing transits and the non-detection in the RV data set, we were not able to put a strong constraint on its density. We also report the detection of secondary eclipses and phase curve variations for K2-141b. The phase variation can be modeled either by a planet with a geometric albedo of 0.30±0.06 in the Kepler bandpass, or by thermal emission from the surface of the planet at ∼3000 K. Only follow-up observations at longer wavelengths will allow us to distinguish between these two scenarios.

show abstract

“…[86][87][88]. The catalog is regularly updated [84,89] and after the last major update [90] it contains uniformly derived stellar parameters of ∼80% of bright stars (V <12 mag) hosting RV detected planets. Besides the main stellar parameters, SWEET-Cat will soon provide abundance of different chemical abundances of the host stars again derived in a homogeneous and uniform way [Sousa et al in prep.].…”

Section: Sweet-catmentioning

confidence: 99%

Heavy Metal Rules. I. Exoplanet Incidence and Metallicity

Adibekyan

2019

Geosciences

View full text Add to dashboard Cite

Discovery of only handful of exoplanets required to establish a correlation between giant planet occurrence and metallicity of their host stars. More than 20 years have already passed from that discovery, however, many questions are still under lively debate: What is the origin of that relation? what is the exact functional form of the giant planet -metallicity relation (in the metal-poor regime)?, does such a relation exist for terrestrial planets? All these question are very important for our understanding of the formation and evolution of (exo)planets of different types around different types of stars and are subject of the present manuscript. Besides making a comprehensive literature review about the role of metallicity on the formation of exoplanets, I also revisited most of the planet -metallicity related correlations reported in the literature using a large and homogeneous data provided by the SWEET-Cat catalog. This study lead to several new results and conclusions, two of which I believe deserve to be highlighted in the abstract: i) The hosts of sub-Jupiter mass planets (∼0.6 -0.9 M ) are systematically less metallic than the hosts of Jupiter-mass planets. This result might be related to the longer disk lifetime and higher amount of planet building materials available at high metallicities, which allow a formation of more massive Jupiter-like planets. ii) Contrary to the previous claims, our data and results do not support the existence of a breakpoint planetary mass at 4 M above and below which planet formation channels are different. However, the results also suggest that planets of the same (high) mass can be formed through different channels depending on the (disk) stellar mass i.e. environmental conditions.

show abstract

SWEET-Cat update and FASMA

Cited by 41 publications

References 74 publications

Evidence of an Upper Bound on the Masses of Planets and Its Implications for Giant Planet Formation

Evidence of an Upper Bound on the Masses of Planets and Its Implications for Giant Planet Formation

An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

Heavy Metal Rules. I. Exoplanet Incidence and Metallicity

Contact Info

Product

Resources

About