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Mikkel Nørup Lund

TESS Asteroseismology of the Known Red-giant Host Stars HD 212771 and HD 203949

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DOI

  • Tiago L. Campante, Instituto de Astrofísica e Ciência Do Espaço, University of Porto, Departamento de Física e Astronomia, University of California at Santa Barbara
  • ,
  • Enrico Corsaro, Osservatorio Astrofisico di Catania
  • ,
  • Mikkel N. Lund
  • Benoît Mosser, Observatoire de Paris
  • ,
  • Aldo Serenelli, University of California at Santa Barbara, Autonomous University of Barcelona, Institute of Space Studies of Catalonia
  • ,
  • Dimitri Veras, University of California at Santa Barbara, University of Warwick
  • ,
  • Vardan Adibekyan, University of Porto
  • ,
  • H. M. Antia, Tata Institute of Fundamental Research
  • ,
  • Warrick Ball, School of Physics and Astronomy, University of Birmingham, UK, Birmingham University
  • ,
  • Sarbani Basu, Yale University
  • ,
  • Timothy R. Bedding, University of California at Santa Barbara, University of Sydney
  • ,
  • Diego Bossini, Instituto de Astrofísica e Ciência Do Espaço, University of Porto
  • ,
  • Guy R. Davies, Birmingham University
  • ,
  • Elisa Delgado Mena, University of Porto
  • ,
  • Rafael A. García, Universite Paris-Saclay
  • ,
  • Rasmus Handberg
  • Marc Hon, University of New South Wales (UNSW) Australia
  • ,
  • Stephen R. Kane, University of California, Riverside
  • ,
  • Steven D. Kawaler, University of California at Santa Barbara, Iowa State University
  • ,
  • James S. Kuszlewicz, Max-Planck-Institut für Sonnensystemforschung
  • ,
  • Miles Lucas, Iowa State University
  • ,
  • Savita Mathur, Instituto de Astrofísica de Canarias, La Laguna University
  • ,
  • Nicolas Nardetto, Observatoire de la Cote d'Azur
  • ,
  • Martin B. Nielsen, Birmingham University
  • ,
  • Marc H. Pinsonneault, University of California at Santa Barbara, The Ohio State University
  • ,
  • Sabine Reffert, Landessternwarte Heidelberg
  • ,
  • Víctor Silva Aguirre
  • Keivan G. Stassun, Vanderbilt University
  • ,
  • Dennis Stello
  • Stephan Stock, Landessternwarte Heidelberg
  • ,
  • Mathieu Vrard, University of Porto
  • ,
  • Mutlu Yildiz, Ege University
  • ,
  • William J. Chaplin, University of California at Santa Barbara, Birmingham University
  • ,
  • Daniel Huber, University of California at Santa Barbara, Institute for Astronomy, University of Hawaii at Manoa
  • ,
  • Jacob L. Bean, University of Chicago, Chicago, Illinois.
  • ,
  • Zeynep Çelik Orhan, Ege University
  • ,
  • Margarida S. Cunha, University of Porto
  • ,
  • Jørgen Christensen-Dalsgaard
  • Hans Kjeldsen
  • Travis S. Metcalfe
  • Andrea Miglio, Birmingham University
  • ,
  • Mário J.P.F.G. Monteiro, University of Porto
  • ,
  • Benard Nsamba, University of Porto
  • ,
  • Sibel Örtel, Ege University
  • ,
  • Filipe Pereira, University of Porto
  • ,
  • Sérgio G. Sousa, University of Porto
  • ,
  • Maria Tsantaki, University of Porto
  • ,
  • Margaret C. Turnbull, Carl Sagan Center for the Study of Life in the Universe

The Transiting Exoplanet Survey Satellite (TESS) is performing a near all-sky survey for planets that transit bright stars. In addition, its excellent photometric precision enables asteroseismology of solar-type and red-giant stars, which exhibit convection-driven, solar-like oscillations. Simulations predict that TESS will detect solar-like oscillations in nearly 100 stars already known to host planets. In this paper, we present an asteroseismic analysis of the known red-giant host stars HD 212771 and HD 203949, both systems having a long-period planet detected through radial velocities. These are the first detections of oscillations in previously known exoplanet-host stars by TESS, further showcasing the mission's potential to conduct asteroseismology of red-giant stars. We estimate the fundamental properties of both stars through a grid-based modeling approach that uses global asteroseismic parameters as input. We discuss the evolutionary state of HD 203949 in depth and note the large discrepancy between its asteroseismic mass (M = 1.23 ± 0.15 M o if on the red-giant branch or M = 1.00 ± 0.16 M o if in the clump) and the mass quoted in the discovery paper (M = 2.1 ± 0.1 M o), implying a change >30% in the planet's mass. Assuming HD 203949 to be in the clump, we investigate the planet's past orbital evolution and discuss how it could have avoided engulfment at the tip of the red-giant branch. Finally, HD 212771 was observed by K2 during its Campaign 3, thus allowing for a preliminary comparison of the asteroseismic performances of TESS and K2. We estimate the ratio of the observed oscillation amplitudes for this star to be, consistent with the expected ratio of ∼0.85 due to the redder bandpass of TESS.

OriginalsprogEngelsk
Artikelnummer31
TidsskriftAstrophysical Journal
Vol/bind885
Nummer1
Antal sider12
ISSN0004-637X
DOI
StatusUdgivet - 2019

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