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TESS Asteroseismology of α Mensae: Benchmark Ages for a G7 Dwarf and Its M Dwarf Companion

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  • Ashley Chontos, University of Hawaii at Manoa
  • ,
  • Daniel Huber, University of Hawaii at Manoa
  • ,
  • Travis A. Berger, University of Hawaii at Manoa
  • ,
  • Hans Kjeldsen
  • Aldo M. Serenelli, CSIC, Institute of Space Studies of Catalonia
  • ,
  • Victor Silva Aguirre
  • Warrick H. Ball, University of Birmingham
  • ,
  • Sarbani Basu, Yale University
  • ,
  • Timothy R. Bedding, University of Sydney
  • ,
  • William J. Chaplin, University of Birmingham
  • ,
  • Zachary R. Claytor, University of Hawaii at Manoa
  • ,
  • Enrico Corsaro, Osservatorio Astrofisico di Catania
  • ,
  • Rafael A. Garcia, Universite Paris-Saclay
  • ,
  • Steve B. Howell, NASA Ames Research Center
  • ,
  • Mia S. Lundkvist
  • Savita Mathur, Instituto Astrofisico de Canarias, University of La Laguna
  • ,
  • Travis S. Metcalfe
  • Martin B. Nielsen, University of Birmingham, New York University Abu Dhabi
  • ,
  • Jia Mian Joel Ong, Yale University
  • ,
  • Zeynep Celik Orhan, Ege University
  • ,
  • Sibel Ortel, Ege University
  • ,
  • Maissa Salama, University of Hawaii at Manoa
  • ,
  • Keivan G. Stassun, Vanderbilt University
  • ,
  • R. H.D. Townsend, University of Wisconsin-Madison, University of California at Santa Barbara
  • ,
  • Jennifer L. Van Saders, University of Hawaii at Manoa
  • ,
  • Mark Winther
  • Mutlu Yildiz, Ege University
  • ,
  • R. Paul Butler, Carnegie Institution of Washington
  • ,
  • C. G. Tinney, University of New South Wales
  • ,
  • Robert A. Wittenmyer, University of Southern Queensland

Asteroseismology of bright stars has become increasingly important as a method to determine the fundamental properties (in particular ages) of stars. The Kepler Space Telescope initiated a revolution by detecting oscillations in more than 500 main-sequence and subgiant stars. However, most Kepler stars are faint and therefore have limited constraints from independent methods such as long-baseline interferometry. Here we present the discovery of solar-like oscillations in α Men A, a naked-eye (V = 5.1) G7 dwarf in TESS's southern continuous viewing zone. Using a combination of astrometry, spectroscopy, and asteroseismology, we precisely characterize the solar analog α Men A (T eff = 5569 62 K, R ∗ = 0.960 0.016 R o˙, M ∗ = 0.964 0.045 M o˙). To characterize the fully convective M dwarf companion, we derive empirical relations to estimate mass, radius, and temperature given the absolute Gaia magnitude and metallicity, yielding M ∗ = 0.169 0.006 M o˙, R ∗ = 0.19 0.01 R o˙, and T eff = 3054 44 K. Our asteroseismic age of 6.2 1.4 (stat) 0.6 (sys) Gyr for the primary places α Men B within a small population of M dwarfs with precisely measured ages. We combined multiple ground-based spectroscopy surveys to reveal an activity cycle of P = 13.1 1.1 yr for α Men A, a period similar to that observed in the Sun. We used different gyrochronology models with the asteroseismic age to estimate a rotation period of ∼30 days for the primary. Alpha Men A is now the closest (d = 10 pc) solar analog with a precise asteroseismic age from space-based photometry, making it a prime target for next-generation direct-imaging missions searching for true Earth analogs.

OriginalsprogEngelsk
Artikelnummer229
TidsskriftAstrophysical Journal
Vol/bind922
Nummer2
ISSN0004-637X
DOI
StatusUdgivet - dec. 2021

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