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

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dc.authoridButler, Robert Paul/0000-0003-1305-3761
dc.authoridTinney, C.G./0000-0002-7595-0970
dc.authoridLundkvist, Mia Sloth/0000-0002-8661-2571
dc.authoridCelik Orhan, Zeynep/0000-0002-9424-2339
dc.authoridChontos, Ashley/0000-0003-1125-2564
dc.authorscopusid6506726179
dc.authorscopusid57217238775
dc.authorscopusid57201273904
dc.authorscopusid57204345527
dc.authorscopusid6603474740
dc.authorscopusid57202249292
dc.authorscopusid56018513900
dc.authorwosidButler, Robert Paul/B-1125-2009
dc.authorwosidChontos, Ashley/Z-1191-2018
dc.contributor.authorChontos, Ashley
dc.contributor.authorHuber, Daniel
dc.contributor.authorBerger, Travis A.
dc.contributor.authorKjeldsen, Hans
dc.contributor.authorSerenelli, Aldo M.
dc.contributor.authorAguirre, Victor Silva
dc.contributor.authorBall, Warrick H.
dc.date.accessioned2023-01-12T20:15:58Z
dc.date.available2023-01-12T20:15:58Z
dc.date.issued2021
dc.departmentN/A/Departmenten_US
dc.description.abstractAsteroseismology 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 alpha 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 alpha Men A (T-eff = 5569 +/- 62 K, R-star = 0.960 +/- 0.016 R-circle dot, M-star = 0.964 +/- 0.045 M-circle dot). 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-star = 0.169 +/- 0.006 M (circle dot), R-star = 0.19 +/- 0.01 R-circle dot, and T-eff = 3054 +/- 44 K. Our asteroseismic age of 6.2 +/- 1.4 (stat) +/- 0.6 (sys) Gyr for the primary places alpha 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 alpha 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 similar to 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.en_US
dc.description.sponsorshipNational Science Foundation under the Graduate Research Fellowship Program [DGE 1842402]; Alfred P. Sloan Foundation; National Aeronautics and Space Administration [80NSSC18K1585, 80NSSC19K0379]; National Science Foundation [AST-1717000]; NASA FINESST award [80NSSC19K1424]; MICINN project [PRPPID2019-108709GBI00]; Independent Research Fund Denmark [7027-00096B]; Carlsberg Foundation [CF19-0649, CF17-0760]; Australian Research Council [DP210103119]; UK Science and Technology Facilities Council (STFC) [ST/R0023297/1]; PLATO CNES grant; GOLF CNES grant; Danish National Research Foundation [DNRF106]; Spanish Ministry of Science and Innovation; Ramon y Cajal fellowship [RYC-201517697]; NASA [80NSSC20K0458, 80NSSC20K0515]; XSEDE [TG-AST090107]; NSF [ACI-1663696, AST1716436, PHY-1748958]; NASA Exoplanet Exploration Program; [PID2019-107187GB-I00]en_US
dc.description.sponsorshipWe acknowledge the traditional owners of the land on which the Anglo-Australian Telescope stands, the Gamilaraay people, and pay our respects to elders past, present, and emerging. The authors would like to thank the staff at the Gemini South Observatory for follow-up observations. A.C. acknowledges support from the National Science Foundation under the Graduate Research Fellowship Program (DGE 1842402). D.H. acknowledges support from the Alfred P. Sloan Foundation, the National Aeronautics and Space Administration (80NSSC18K1585, 80NSSC19K0379), and the National Science Foundation (AST-1717000). T.A.B. acknowledges support from a NASA FINESST award (80NSSC19K1424). A.S. is partially supported by MICINN project PRPPID2019-108709GBI00. V.S.A. acknowledges support from the Independent Research Fund Denmark (research grant 7027-00096B) and the Carlsberg Foundation (grant agreement CF19-0649). T.R.B. acknowledges support from the Australian Research Council (DP210103119). W.H.B., W.J.C., and M.B.N. thank the UK Science and Technology Facilities Council (STFC) for support under grant ST/R0023297/1. R.A.G. acknowledges the support of the PLATO and GOLF CNES grants. M.S.L. is supported by the Carlsberg Foundation (grant agreement No. CF17-0760). Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation (grant DNRF106). S.M. acknowledges support from the Spanish Ministry of Science and Innovation with Ramon y Cajal fellowship No. RYC-201517697 and from grant No. PID2019-107187GB-I00. T.S.M. acknowledges support from NASA grant 80NSSC20K0458. Computational time at the Texas Advanced Computing Center was provided through XSEDE allocation TG-AST090107. R.H. D.T. acknowledges support from NSF grants ACI-1663696, AST1716436, and PHY-1748958 and NASA grant 80NSSC20K0515. Some of the observations in the paper made use of the highresolution imaging instrument Zorro obtained under Gemini LLP proposal No. GN/S-2021A-LP-105. Zorro was funded by the NASA Exoplanet Exploration Program and built at the NASA AMES Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.en_US
dc.identifier.doi10.3847/1538-4357/ac1269
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.issn0004-637Xen_US
dc.identifier.issn1538-4357en_US
dc.identifier.issue2en_US
dc.identifier.scopus2-s2.0-85121813311en_US
dc.identifier.scopusqualityQ1en_US
dc.identifier.urihttps://doi.org/10.3847/1538-4357/ac1269
dc.identifier.urihttps://hdl.handle.net/11454/78619
dc.identifier.volume922en_US
dc.identifier.wosWOS:000724866500001en_US
dc.identifier.wosqualityQ1en_US
dc.indekslendigikaynakWeb of Scienceen_US
dc.indekslendigikaynakScopusen_US
dc.language.isoenen_US
dc.publisherIop Publishing Ltden_US
dc.relation.ispartofAstrophysical Journalen_US
dc.relation.publicationcategoryMakale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanıen_US
dc.rightsinfo:eu-repo/semantics/openAccessen_US
dc.subjectSolar-Like Oscillationsen_US
dc.subjectStellar Evolution Codeen_US
dc.subjectP-Mode Oscillationsen_US
dc.subjectLower Main-Sequenceen_US
dc.subjectCa-Ii Emissionen_US
dc.subjectMagnetic Activityen_US
dc.subjectNearby Starsen_US
dc.subjectChromospheric Variationsen_US
dc.subjectFundamental Parametersen_US
dc.subjectMultisite Campaignen_US
dc.titleTESS Asteroseismology of alpha Mensae: Benchmark Ages for a G7 Dwarf and Its M Dwarf Companionen_US
dc.typeArticleen_US

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