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Kepler / TESS (And Gaia): 6 Little Information on Their Detailed Properties 0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 Jmag-Kmag ASJ-Kteros ASTERO CHRONOMETRY CHRONOMETRY

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Kepler / TESS (And Gaia): 6 Little Information on Their Detailed Properties 0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 Jmag-Kmag ASJ-Kteros ASTERO CHRONOMETRY CHRONOMETRY ASTEROSEISMOLOGY MODEL CALIBRATION A. Miglio, J. Montalban, B. Mosser, P. Ventura WP127: seismic constraints from ageing stars ASTERO ASTERO CHRONOMETRY CHRONOMETRY Logo on white background Logo on dark background aim TESS S-CVZ -6 what which stars are we referring to -4 -2 s K 0 2 kmag+5*log10(parallax)-10 4 6 0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 jmag-kmag ASJ-KTEROs ASTERO CHRONOMETRY CHRONOMETRY Logo on white background Logo on dark background aim TESS S-CVZ -6 what which stars are we referring to -4 -2 are they relevant for s why PLATO’s core science K 0 2 kmag+5*log10(parallax)-10 4 6 0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 jmag-kmag ASJ-KTEROs ASTERO CHRONOMETRY CHRONOMETRY Logo on white background Logo on dark background aim TESS S-CVZ -6 what which stars are we referring to -4 -2 are they relevant for s why PLATO’s core science K 0 2 scientific return kmag+5*log10(parallax)-10 how can we maximise 4 number of targets 6 0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 jmag-kmag ASJ-KTEROs ASTERO CHRONOMETRY CHRONOMETRY Logo on white background Logo on dark background what TESS S-CVZ G-K giants -6 radii up to 10 Rsun -4 -2 M ~ 0.8 - 4 Msun s K 0 all metallicities [-2, 0.5] 2 kmag+5*log10(parallax)-10 4 prior to CoRoT / Kepler / TESS (and Gaia): 6 little information on their detailed properties 0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 jmag-kmag ASJ-KTEROs ASTERO CHRONOMETRY CHRONOMETRY Logo on white background Logo on dark background what TESS S-CVZ G-K giants -6 radii up to 10 Rsun -4 -2 M ~ 0.8 - 4 Msun s K 0 all metallicities [-2, 0.5] 2 kmag+5*log10(parallax)-10 4 prior to CoRoT / Kepler / TESS (and Gaia): 6 little information on their detailed properties 0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 jmag-kmag ASJ-KTEROs ASTERO CHRONOMETRY CHRONOMETRY Logo on white background Logo on dark background what + asteroseismology gravity acoustic mode mode νi Hz] 30 μ / 2 He core 15 120 140 160 200 H-burning shell [ppm PSD Frequency [μHz] H-rich radiative transport of angular momentum core talk by Charlotte Gehan later today constraints on internal mixing precise and accurate global parameters ASTERO ASTERO CHRONOMETRY CHRONOMETRY Logo on white background Logo on dark background 2 whyCampante et al. (Received January 1, 2018; Revised January 7, 2018; Accepted September 16, 2019) Submitted to ApJ planets around G-K giants ABSTRACT The Transiting Exoplanet Survey Satellite (TESS) is performing a near all-sky survey for planets thatimproved transit bright stellar stars. properties In addition, its excellent improved photometric planetary precision parameters enables asteroseismology of solar-type and red-giant stars, which exhibit convection-driven, solar-like oscillations. Simulations Draftpredict version that September TESS will 16, detect 2019 solar-like oscillations in nearly 100 stars already known to host planets. A TypesetIn this using paper, L TEX wetwocolumn presentstyle ane.g. asteroseismic in AASTeX62Campante analysis et ofal. the 2019, known in red-giant press 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 TESSthe mission’s ASTEROSEISMOLOGY potential to conduct OF THE asteroseismology KNOWN RED-GIANT of red-giant HOST stars. STARS We HD estimate 212771 the AND fundamental HD 203949 propertiesTiago L. of Campante both stars,1, 2, through 3 Enrico a Corsaro grid-based,4 Mikkel modeling N. Lund approach,5, 3 Beno thatˆıt uses Mosser global,6 Aldo asteroseismic Serenelli,7, param- 8, 3 9, 10, 3, 1 11 12, 5 13 eters asDimitri input. Veras We discuss, ⇤ theVardan evolutionary Adibekyan state, H. of M. HD Antia 203949, Warrick in depth Ball and, noteSarbani the large Basu discrepancy, Timothybetween R.its Bedding asteroseismic,14, 5, 3 Diego mass ( BossiniM =1,1.23Guy0 R..15 Davies M if,12, on 5 Elisa the red-giant Delgado branch Mena,1 orRafaelM =1 A..00 Garc0´.ıa16,15, M 16 Rasmus Handberg,5 Marc Hon,17 ⇤Stephen± R. Kane,18 Steven D. Kawaler,19, 3 James S.⇤ Kuszlewicz± ,20, 5 if in the clump)19 and the mass21, 22 quoted in the discovery23 paper (M =2.112, 5,0 24.1M ), implying a change25, 3 Miles Lucas, Savita Mathur, Nicolas Nardetto, Martin B. Nielsen⇤ , ± Marc H. Pinsonneault, >Sabine30 % Reffert in the, planet’s26 V´ıctor mass. Silva Aguirre Assuming,5 Keivan HD 203949 G. Stassun to be,27, in 28 Dennis the clump, Stello we,17, investigate 14, 5, 3 Stephan the Stock planet’s,26 past orbitalMathieu evolution Vrard,1 Mutlu and discuss Yıldız, how29 William it could J. Chaplin have avoided,12, 5, 3 Daniel engulfment Huber at,30, 3 theJacob tip L. of Bean the red-giant,31 29 1, 2 5, 3 5, 32 branch.Zeynep Finally, C¸elik Orhan HD 212771, Margarida was observed S. Cunha by, K2Jørgen during Christensen-Dalsgaard its Campaign 3, thus allowing, Hans for Kjeldsen a preliminary, Travis S. Metcalfe,33, 20 Andrea Miglio,12, 5 Mario´ J. P. F. G. Monteiro,1, 2 Benard Nsamba,1 Sibel Ortel¨ ,29 comparisonFilipe of the Pereira asteroseismic,1 Sergio´ performances G. Sousa,1, 2 Maria of TESS Tsantaki and, K2.1 and We Margaret estimate C. the Turnbull ratio of34 the observed oscillation amplitudes for this star to be ATESS/AK2 =0.75 0.14, consistent with the expected ratio 1Instituto de Astrof´ısica e Ciˆencias do Espa¸co, Universidademax max do Porto,± Rua das Estrelas, 4150-762 Porto, Portugal 2 of 0.85 due to the redder bandpass of TESS. ASTERO Departamento de F´ısica e Astronomia, Faculdade de Ciˆencias da Universidade do Porto, Rua doAS Campo Alegre, s/n,TERO 4169-007 Porto, ⇠ Portugal Keywords:3Kavliasteroseismology Institute for Theoretical — planet-star Physics, University interactions of California, — stars: Santa Barbara, fundamental CACHRONOMETRY 93106-4030, parameters USA — stars: CHRONOMETRY 4 individualINAF (HD — Osservatorio 212771, HD Astrofisico 203949) di Catania, — techniques: via S. Sofia photometric 78, 95123 Catania, Italy 5Stellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, 8000 Aarhus C, Denmark 6LESIA, Observatoire1. INTRODUCTION de Paris, Universit´ePSL, CNRS, Sorbonne Universit´e,ing Universit´ede (e.g., Serenelli Paris, et 5 al.place2017 Jules; Janssen,Silva Aguirre 92195 Meudon, et al. 2017; France Nsamba et al. 2018) strategies, as well as on state-of-the- Major advances7 in stellar interiors physics and evolu- Institute of Space Sciences (ICE, CSIC) Campus UAB, Carrerart de optimization Can Magrans, s/n, procedures E-08193, Bellaterra, that make Spain use of individual tion have recently8 beenInstitut made d’Estudis possible Espacials by de asteroseismol- Catalunya (IEEC), C/Gran Capit`a, 2-4, E-08034, Barcelona, Spain ogy. This has largely9 beenCentre due for Exoplanets to the exquisite and Habitability, space- Universityoscillation of Warwick, frequencies Coventry CV4 (e.g., 7AL,Metcalfe UK et al. 2010; Mathur based data made available10 byDepartment CNES/ESA’s of Physics, CoRoT University of Warwick,et al. 2012 Coventry; Silva CV4 Aguirre 7AL, UK et al. 2015; Rendle et al. 2019). 11 (Baglin et al. 2009) and NASA’s KeplerTata Institute/K2 (Borucki of Fundamental Research,These Mumbai, techniques India make it possible to estimate precise 12School of Physics and Astronomy, University of Birmingham,properties Edgbaston, of large Birmingham numbers B15 of 2TT, field UK stars, for which such et al. 2010; Koch et13 al. 2010; Howell et al. 2014) missions. Department of Astronomy, Yale University, P.O. Boxinformation 208101, New Haven, is sparse. CT 06520-8101, As a result, USA asteroseismology is In particular, asteroseismology14Sydney Institute for has Astronomy vastly benefited (SIfA), School the of Physics, University of Sydney, NSW 2006, Australia having a profound impact on modern astrophysics, no- study of solar-type and red-giant15IRFU, stars, CEA, Universit´eParis-Saclay, which exhibit F-91191 Gif-sur-Yvette, France convection-driven,16AIM, CEA, CNRS,solar-like Universit´eParis-Saclay, oscillations (for Universit´eParis a review, Diderot,tably Sorbonne on the Paris field Cit´e, of F-91191 exoplanetary Gif-sur-Yvette, science France (Campante 17 see Chaplin & Miglio 2013School). The of Physics, revolution The University triggered of by New Southet Wales, al. 2018 Sydney). Characterization NSW 2052, Australia of exoplanet-host stars via 18Department of Earth and Planetary Sciences, Universityasteroseismology of California, Riverside, allows CA for 92521, unmatched USA precision in the CoRoT and Kepler/K219 is set to continue over the com- Department of Physics and Astronomy, Iowa Stateabsolute University, properties Ames, IA of 50011, their USA planets (Huber et al. 2013a; ing decade, with20 NASA’s TESS (Ricker et al. 2015) and Max-Planck-Institut f¨urSonnensystemforschung, Justus-von-Liebig-WegBallard et al. 3,2014 37077; Campante G¨ottingen, Germany et al. 2015; Silva Aguirre ESA’s PLATO (Rauer et21 al.Instituto2014) de missions Astrof´ısica expected de Canarias to (IAC), E-38205 La Laguna, Tenerife, Spain raise the number22 ofUniversidad known solar-like de La Laguna oscillators (ULL), Departamento by up to de Astrof´ısica,et al. 2015 E-38206; Lundkvist La Laguna, et Tenerife, al. 2016 Spain). Furthermore, aster- two orders of magnitude23Universit´eCˆote (Huber 2018 d’Azur,). Observatoire de la Cˆote d’Azur,oseismology CNRS, Laboratoire enables Lagrange, constraints France on the spin-orbit align- 24 Logo on white background Logo on dark background Fueled by theCenter wealth for Space of high-quality Science, NYUAD seismic Institute, data, New the York Universityment Abu of Dhabi, exoplanet PO Box systems 129188, ( AbuChaplin Dhabi, et UAE al.
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