A close-in giant planet escapes engulfment by its star.

Autor: Hon M; Institute for Astronomy, University of Hawaii, Honolulu, HI, USA. mtyhon@hawaii.edu., Huber D; Institute for Astronomy, University of Hawaii, Honolulu, HI, USA.; Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Camperdown, New South Wales, Australia., Rui NZ; TAPIR, California Institute of Technology, Pasadena, CA, USA., Fuller J; TAPIR, California Institute of Technology, Pasadena, CA, USA., Veras D; Centre for Exoplanets and Habitability, University of Warwick, Coventry, UK.; Centre for Space Domain Awareness, University of Warwick, Coventry, UK.; Department of Physics, University of Warwick, Coventry, UK., Kuszlewicz JS; Center for Astronomy (Landessternwarte), Heidelberg University, Heidelberg, Germany.; Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Aarhus, Denmark., Kochukhov O; Department of Physics and Astronomy, Uppsala University, Uppsala, Sweden., Stokholm A; Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Aarhus, Denmark.; Dipartimento di Fisica e Astronomia, Università degli Studi di Bologna, Bologna, Italy.; INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Bologna, Italy., Rørsted JL; Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Aarhus, Denmark., Yıldız M; Department of Astronomy and Space Sciences, Science Faculty, Ege University, İzmir, Turkey., Orhan ZÇ; Department of Astronomy and Space Sciences, Science Faculty, Ege University, İzmir, Turkey., Örtel S; Department of Astronomy and Space Sciences, Science Faculty, Ege University, İzmir, Turkey., Jiang C; Max-Planck-Institut für Sonnensystemforschung, Göttingen, Germany., Hey DR; Institute for Astronomy, University of Hawaii, Honolulu, HI, USA., Isaacson H; Department of Astronomy, University of California Berkeley, Berkeley, CA, USA., Zhang J; Institute for Astronomy, University of Hawaii, Honolulu, HI, USA., Vrard M; Department of Astronomy, The Ohio State University, Columbus, OH, USA., Stassun KG; Department of Physics and Astronomy, Vanderbilt University, Nashville, TN, USA., Shappee BJ; Institute for Astronomy, University of Hawaii, Honolulu, HI, USA., Tayar J; Institute for Astronomy, University of Hawaii, Honolulu, HI, USA.; Department of Astronomy, Bryant Space Science Center, University of Florida, Gainesville, FL, USA., Claytor ZR; Institute for Astronomy, University of Hawaii, Honolulu, HI, USA.; Department of Astronomy, Bryant Space Science Center, University of Florida, Gainesville, FL, USA., Beard C; Department of Physics and Astronomy, University of California, Irvine, Irvine, CA, USA., Bedding TR; Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Camperdown, New South Wales, Australia., Brinkman C; Institute for Astronomy, University of Hawaii, Honolulu, HI, USA., Campante TL; Instituto de Astrofísica e Ciências do Espaço, CAUP, Universidade do Porto, Porto, Portugal.; Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Porto, Portugal., Chaplin WJ; School of Physics and Astronomy, University of Birmingham, Birmingham, UK., Chontos A; Institute for Astronomy, University of Hawaii, Honolulu, HI, USA.; Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA., Giacalone S; Max-Planck-Institut für Sonnensystemforschung, Göttingen, Germany., Holcomb R; Department of Astronomy, Bryant Space Science Center, University of Florida, Gainesville, FL, USA., Howard AW; Department of Astronomy, California Institute of Technology, Pasadena, CA, USA., Lubin J; Department of Astronomy, Bryant Space Science Center, University of Florida, Gainesville, FL, USA., MacDougall M; Department of Physics and Astronomy, University of California, Los Angeles, Los Angeles, CA, USA., Montet BT; School of Physics, University of New South Wales, Sydney, New South Wales, Australia.; UNSW Data Science Hub, University of New South Wales, Sydney, New South Wales, Australia.; Australian Centre for Astrobiology, University of New South Wales, Sydney, New South Wales, Australia., Murphy JMA; Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA., Ong J; Institute for Astronomy, University of Hawaii, Honolulu, HI, USA.; Department of Astronomy, Yale University, New Haven, CT, USA., Pidhorodetska D; Department of Earth and Planetary Sciences, University of California, Riverside, Riverside, CA, USA., Polanski AS; Department of Physics and Astronomy, University of Kansas, Lawrence, KS, USA., Rice M; Department of Astronomy, Yale University, New Haven, CT, USA.; Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA., Stello D; Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Camperdown, New South Wales, Australia.; School of Physics, University of New South Wales, Sydney, New South Wales, Australia.; ARC Centre of Excellence for All Sky Astrophysics in Three Dimensions (ASTRO-3D), Sydney, New South Wales, Australia., Tyler D; Department of Physics and Astronomy, University of California, Los Angeles, Los Angeles, CA, USA., Van Zandt J; Department of Physics and Astronomy, University of California, Los Angeles, Los Angeles, CA, USA., Weiss LM; Department of Physics and Astronomy, University of Notre Dame, Notre Dame, IN, USA.
Jazyk: angličtina
Zdroj: Nature [Nature] 2023 Jun; Vol. 618 (7967), pp. 917-920. Date of Electronic Publication: 2023 Jun 28.
DOI: 10.1038/s41586-023-06029-0
Abstrakt: When main-sequence stars expand into red giants, they are expected to engulf close-in planets 1-5 . Until now, the absence of planets with short orbital periods around post-expansion, core-helium-burning red giants 6-8 has been interpreted as evidence that short-period planets around Sun-like stars do not survive the giant expansion phase of their host stars 9 . Here we present the discovery that the giant planet 8 Ursae Minoris b 10 orbits a core-helium-burning red giant. At a distance of only 0.5 AU from its host star, the planet would have been engulfed by its host star, which is predicted by standard single-star evolution to have previously expanded to a radius of 0.7 AU. Given the brief lifetime of helium-burning giants, the nearly circular orbit of the planet is challenging to reconcile with scenarios in which the planet survives by having a distant orbit initially. Instead, the planet may have avoided engulfment through a stellar merger that either altered the evolution of the host star or produced 8 Ursae Minoris b as a second-generation planet 11 . This system shows that core-helium-burning red giants can harbour close planets and provides evidence for the role of non-canonical stellar evolution in the extended survival of late-stage exoplanetary systems.
(© 2023. The Author(s), under exclusive licence to Springer Nature Limited.)
Databáze: MEDLINE
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