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A giant exoplanet orbiting a very-low-mass star challenges planet formation models.

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Title: A giant exoplanet orbiting a very-low-mass star challenges planet formation models.
Authors: Morales, J. C., Mustill, A. J., Ribas, I., Davies, M. B., Reiners, A., Bauer, F. F., Kossakowski, D., Herrero, E., Rodríguez, E., López-González, M. J., Rodríguez-López, C., Béjar, V. J. S., González-Cuesta, L., Luque, R., Pallé, E., Perger, M., Baroch, D., Johansen, A., Klahr, H., Mordasini, C.
Source: Science (pre-March 2025). 9/27/2019, Vol. 365 Issue 6460, p1441-1445. 5p. 3 Diagrams.
Subjects: Extrasolar planets, Stars, Origin of planets, Super-Earths, Accretion (Astrophysics)
Abstract: Surveys have shown that super-Earth and Neptune-mass exoplanets are more frequent than gas giants around low-mass stars, as predicted by the core accretion theory of planet formation. We report the discovery of a giant planet around the very-low-mass star GJ 3512, as determined by optical and near-infrared radial-velocity observations. The planet has a minimum mass of 0.46 Jupiter masses, very high for such a small host star, and an eccentric 204-dayorbit. Dynamical models show that the high eccentricity is most likely due to planet-planet interactions. We use simulations to demonstrate that the GJ 3512 planetary system challenges generally accepted formation theories, and that it puts constraints on the planet accretion and migration rates. Disk instabilities may be more efficient in forming planets than previously thought. [ABSTRACT FROM AUTHOR]
Copyright of Science (pre-March 2025) is the property of American Association for the Advancement of Science and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
Database: Psychology and Behavioral Sciences Collection
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  Data: A giant exoplanet orbiting a very-low-mass star challenges planet formation models.
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  Data: <searchLink fieldCode="AR" term="%22Morales%2C+J%2E+C%2E%22">Morales, J. C.</searchLink><br /><searchLink fieldCode="AR" term="%22Mustill%2C+A%2E+J%2E%22">Mustill, A. J.</searchLink><br /><searchLink fieldCode="AR" term="%22Ribas%2C+I%2E%22">Ribas, I.</searchLink><br /><searchLink fieldCode="AR" term="%22Davies%2C+M%2E+B%2E%22">Davies, M. B.</searchLink><br /><searchLink fieldCode="AR" term="%22Reiners%2C+A%2E%22">Reiners, A.</searchLink><br /><searchLink fieldCode="AR" term="%22Bauer%2C+F%2E+F%2E%22">Bauer, F. F.</searchLink><br /><searchLink fieldCode="AR" term="%22Kossakowski%2C+D%2E%22">Kossakowski, D.</searchLink><br /><searchLink fieldCode="AR" term="%22Herrero%2C+E%2E%22">Herrero, E.</searchLink><br /><searchLink fieldCode="AR" term="%22Rodríguez%2C+E%2E%22">Rodríguez, E.</searchLink><br /><searchLink fieldCode="AR" term="%22López-González%2C+M%2E+J%2E%22">López-González, M. J.</searchLink><br /><searchLink fieldCode="AR" term="%22Rodríguez-López%2C+C%2E%22">Rodríguez-López, C.</searchLink><br /><searchLink fieldCode="AR" term="%22Béjar%2C+V%2E+J%2E+S%2E%22">Béjar, V. J. S.</searchLink><br /><searchLink fieldCode="AR" term="%22González-Cuesta%2C+L%2E%22">González-Cuesta, L.</searchLink><br /><searchLink fieldCode="AR" term="%22Luque%2C+R%2E%22">Luque, R.</searchLink><br /><searchLink fieldCode="AR" term="%22Pallé%2C+E%2E%22">Pallé, E.</searchLink><br /><searchLink fieldCode="AR" term="%22Perger%2C+M%2E%22">Perger, M.</searchLink><br /><searchLink fieldCode="AR" term="%22Baroch%2C+D%2E%22">Baroch, D.</searchLink><br /><searchLink fieldCode="AR" term="%22Johansen%2C+A%2E%22">Johansen, A.</searchLink><br /><searchLink fieldCode="AR" term="%22Klahr%2C+H%2E%22">Klahr, H.</searchLink><br /><searchLink fieldCode="AR" term="%22Mordasini%2C+C%2E%22">Mordasini, C.</searchLink>
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  Data: <searchLink fieldCode="JN" term="%22Science+%28pre-March+2025%29%22">Science (pre-March 2025)</searchLink>. 9/27/2019, Vol. 365 Issue 6460, p1441-1445. 5p. 3 Diagrams.
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  Data: <searchLink fieldCode="DE" term="%22Extrasolar+planets%22">Extrasolar planets</searchLink><br /><searchLink fieldCode="DE" term="%22Stars%22">Stars</searchLink><br /><searchLink fieldCode="DE" term="%22Origin+of+planets%22">Origin of planets</searchLink><br /><searchLink fieldCode="DE" term="%22Super-Earths%22">Super-Earths</searchLink><br /><searchLink fieldCode="DE" term="%22Accretion+%28Astrophysics%29%22">Accretion (Astrophysics)</searchLink>
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  Data: Surveys have shown that super-Earth and Neptune-mass exoplanets are more frequent than gas giants around low-mass stars, as predicted by the core accretion theory of planet formation. We report the discovery of a giant planet around the very-low-mass star GJ 3512, as determined by optical and near-infrared radial-velocity observations. The planet has a minimum mass of 0.46 Jupiter masses, very high for such a small host star, and an eccentric 204-dayorbit. Dynamical models show that the high eccentricity is most likely due to planet-planet interactions. We use simulations to demonstrate that the GJ 3512 planetary system challenges generally accepted formation theories, and that it puts constraints on the planet accretion and migration rates. Disk instabilities may be more efficient in forming planets than previously thought. [ABSTRACT FROM AUTHOR]
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  Data: <i>Copyright of Science (pre-March 2025) is the property of American Association for the Advancement of Science and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
PLink https://search.ebscohost.com/login.aspx?direct=true&site=eds-live&db=pbh&AN=138908339
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