Intermediate-mass stars and the origin of the gas-giant planet-metallicity correlation
Context. Currently, the number of known planets around intermediate-mass stars (1.5 M⊙ < M⋆ < 3.5 M⊙) is rather low. As a consequence, models of planet formation derive their strongest observational evidence from the chemical signature of mostly low-mass (FGK) main-sequence (MS) stars with pla...
| Autores: | , , , , , |
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| Tipo de documento: | artigo |
| Estado: | Versão publicada |
| Data de publicação: | 2025 |
| País: | España |
| Recursos: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositório: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/411277 |
| Acesso em linha: | http://hdl.handle.net/10261/411277 |
| Access Level: | Acceso aberto |
| Palavra-chave: | Techniques: spectroscopic Planets and satellites: formation Stars: abundances Stars: early-type |
| Resumo: | Context. Currently, the number of known planets around intermediate-mass stars (1.5 M⊙ < M⋆ < 3.5 M⊙) is rather low. As a consequence, models of planet formation derive their strongest observational evidence from the chemical signature of mostly low-mass (FGK) main-sequence (MS) stars with planets. |
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