Year: 2021
Type: article
Abstract: Dynamical histories of planetary systems, as well as the atmospheric evolution of highly irradiated planets, can be studied by characterizing the ultra-short-period planet population, which the TESS mission is particularly well suited to discover. Here, we report on the follow-up of a transit signal detected in the TESS sector 19 photometric time series of the M3.0 V star TOI-1685 (2MASS J04342248+4302148). We confirm the planetary nature of the transit signal, which has a period ofPb= 0.6691403−0.0000021+0.0000023d, using precise radial velocity measurements taken with the CARMENES spectrograph. From the joint photometry and radial velocity analysis, we estimate the following parameters for TOI-1685 b: a mass ofMb= 3.78−0.63+0.63M⊕, a radius ofRb= 1.70−0.07+0.07R⊕, which together result in a bulk density ofρb= 4.21−0.82+0.95g cm−3, and an equilibrium temperature ofTeq= 1069−16+16K. TOI-1685 b is the least dense ultra-short-period planet around an M dwarf known to date. TOI-1685 b is also one of the hottest transiting super-Earth planets with accurate dynamical mass measurements, which makes it a particularly attractive target for thermal emission spectroscopy. Additionally, we report with moderate evidence an additional non-transiting planet candidate in the system, TOI-1685 [c], which has an orbital period ofPc= 9.02−0.12+0.10d.
Source: Astronomy and Astrophysics
Authors: P. Bluhm, E. Pallé, K. Molaverdikhani, J. Kemmer, A. P. Hatzes, D. Kossakowski, S. Stock, J. A. Caballero, J. Lillo-Box, V. J. S. Béjar, M. G. Soto, P. J. Amado, P. Brown, C. Cadieux, R. Cloutier, K. A. Collins, K. I. Collins, M. Cortés-Contreras, R. Doyon, S. Dreizler, N. Espinoza, A. Fukui, E. González-Álvarez, Th. Henning, K. Horne, S. V. Jeffers, J. M. Jenkins, E. L. N. Jensen, A. Kaminski, J. F. Kielkopf, N. Kusakabe, M. Kürster, D. Lafrenière, R. Luque, F. Murgas, D. Montes, J. C. Morales, N. Narita, V. M. Passegger, A. Quirrenbach, P. Schöfer, S. Reffert, A. Reiners, I. Ribas, G. R. Ricker, S. Seager, A. Schweitzer, R. P. Schwarz, M. Tamura, T. Trifonov, R. Vanderspek, J. Winn, M. Zechmeister, M. R. Zapatero Osorio
Institutions: Heidelberg University, Universidad de La Laguna, Instituto de Astrofísica de Canarias, Max Planck Institute for Astronomy, Thüringer Landessternwarte Tautenburg, Centro de Astrobiología, Queen Mary University of London, Instituto de Astrofísica de Andalucía, Vanderbilt University, Université de Montréal, Center for Astrophysics Harvard & Smithsonian, George Mason University, University of Göttingen, Space Telescope Science Institute, The University of Tokyo, University of St Andrews, Max Planck Institute for Solar System Research, Ames Research Center, Swarthmore College, University of Louisville, National Astronomical Observatory of Japan, Universidad Complutense de Madrid, Institute of Space Sciences, Institut d'Estudis Espacials de Catalunya, Japan Science and Technology Agency, Astrobiology Center, Komaba Institute for Science, The University of Tokyo, Universität Hamburg, University of Oklahoma, Massachusetts Institute of Technology, Princeton University
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: bronze
Funders: National Science Foundation, National Aeronautics and Space Administration, California Institute of Technology, Université Laval, Ministerio de Ciencia, Innovación y Universidades, Centres de Recerca de Catalunya, European Commission, Deutsche Forschungsgemeinschaft, Generalitat de Catalunya, Universidad Complutense de Madrid, Fonds Québécois de la Recherche sur la Nature et les Technologies, Ministerio de Economía y Competitividad, Max-Planck-Gesellschaft, Université de Montréal, National Astronomical Observatory of Japan, Klaus Tschira Stiftung, Junta de Andalucía, Fundación Bancaria Caixa d'Estalvis i Pensions de Barcelona, Instituto de Astrofísica de Andalucía, Max-Planck-Institut für Astronomie, Instituto de Astrofísica de Canarias, Science Mission Directorate, Science and Technology Facilities Council, Japan Society for the Promotion of Science, Consejo Superior de Investigaciones Científicas, European Regional Development Fund, Agencia Estatal de Investigación, Precursory Research for Embryonic Science and Technology
Awards: G100543663, G1092424111, G1105844351, Search for Nearby, Small-sized Transiting Exoplanets and Study of Their Atmospheres, G1175115578, G1255325603, Development of Exoplanet Researches with New IR Technologies, G1348953298, G1361227261, G1459069146, G1515373893, G1735320636, Junior Leader la Caixa Postdoctoral Fellowship Programme: Shaping the new generation of leaders in research, G1877798660, G2064873908, G2153927466, G2262748287, G2350454921, G2421061772, G2462415295, G2601397997, G2627485041, G2633884080, G2673512141, G3005324705, G300979063, G3180925806, G3181696191, G3452655474, G3480869486, G3522231704, G3546882995, G3681454997, G3803561910, Uncovering the nature of small exoplanets via collaborations between observational and theoretical studies, G3975875632, G4042783231, G410571670, G4190160184, G4211331249, G425668148, G434337789, THE CHEMICAL COMPOSITION OF STARS IS AN IMPORTANT INGREDIENT IN OUR UNDERSTANDING OF THE FORMATION STRUCTURE AND EVOLUTION OF BOTH THE GALAXY AND THE SOLAR SYSTEM. THE COMPOSITION OF THE SUN ITSELF IS AN ESSENTIAL REFERENCE STANDARD AGAINST WHICH THE ELEMENTAL CONTENTS OF OTHER ASTRONOMICAL OBJECTS ARE COMPARED. RECENTLY REDETERMINATION OF THE ELEMENTAL ABUNDANCES USING THREE DIMENSIONAL TIME DEPENDENT HYDRODYNAMICAL MODELS OF THE SOLAR ATMOSPHERE HAS LED TO A REDUCTION IN THE INFERRED METAL ABUNDANCES PARTICULARLY C N O AND NE. HOWEVER THIS REDUCTION IN METALS REDUCES THE OPACITY SUCH THAT MODELS OF THE SUN NO LONGER AGREE WITH THE OBSERVED RESULTS OBTAINED USING HELIOSEISMOLOGY.THREE DIMENSIONAL 3 D RADIATIVE TRANSFER IS AN IMPORTANT PROBLEM IN PHYSICS ASTROPHYSICS AND METEOROLOGY. RADIATIVE TRANSFER IS EXTREMELY COMPUTATIONALLY COMPLEX AND IT IS A NATURAL PROBLEM THAT REQUIRES COMPUTATION ONTHE EXASCALE. WE INTEND TO CALCULATE THE DETAILED COMPOSITIONAL STRUCTURE OF THE SUN AND OTHER STARS AT HIGH RESOLUTION WITH FULL NLTE TREATING THE TURBULENT VELOCITY FLOWS IN FULL DETAIL IN ORDER TO COMPARE RESULTS FROM HYDRODYNAMICS AND HELIOSEISMOLOGY AND UNDERSTAND THE NATURE OF THE DISCREPANCIES FOUND BETWEEN THE TWO APPROACHES.WE PROPOSE TO PERFORM 3 D HIGH RESOLUTION RADIATIVE TRANSFER CALCULATIONS WITH THE PHOENIX 3D SUITE OF SOLAR AND OTHER STARS USING 3 D HYDRODYNAMIC MODELS FROM DIFFERENT GROUPS. WHILE NLTE RADIATIVE TRANSFER HAS BEEN TREATED BY THE GROUPS DOING HYDRODYNAMICS THEY ARE NECESSARILY LIMITED IN THEIR RESOLUTION TO THE CONSIDERATION OF ONLY A FEW 4 20 FREQUENCY BINS WHEREAS WE CAN CALCULATE FULL NLTE INCLUDING THOUSANDS OF WAVELENGTH POINTS RESOLVING THE LINE PROFILES AND SOLVING THE SCATTERING PROBLEM WITH EXTREMELY HIGH ANGULAR RESOLUTION. THE CODE HAS BEEN USED FOR THE ANALYSIS OF SUPERNOVA SPECTRA STELLAR AND PLANETARY SPECTRA AND FOR TIME DEPENDENT MODELING OF TRANSIENT OBJECTS. PHOENIX 3D RUNS AND SCALES VERY WELL ON CRAY XC 30 AND XC 40 MACHINES TESTED UP TO 100 800 CPU CORES AND SHOULDSCALE UP TO SEVERAL MILLION CORES FOR LARGE SIMULATIONS. NON LOCAL PROBLEMS PARTICULARLY RADIATION HYDRODYNAMICS PROBLEMS ARE AT THE FOREFRONT OF COMPUTATIONAL ASTROPHYSICS AND WE WILL SHARE OUR WORK WITH THE COMMUNITY.OUR RESEARCH PROGRAM BRINGS A UNIFIED MODELING STRATEGY TO THE RESULTS OF SEVERAL DISPARATE GROUPS AND THUS WILLPROVIDE A UNIFYING FRAMEWORK WITH WHICH TO ASSESS THE METAL ABUNDANCE OF THE STARS AND THE CHEMICAL EVOLUTION OF THE GALAXY. WE WILL BRING TOGETHER 3 D HYDRODYNAMICAL MODELS DETAILED RADIATIVE TRANSFER AND ASTRONOMICAL ABUNDANCE STUDIES. WE WILL ALSO PROVIDE RESULTS OF INTEREST TO THE ATOMIC PHYSICS AND PLASMA PHYSICS COMMUNITIES. OUR WORK WILL USE DATA FROM NASA TELESCOPES INCLUDING THE HUBBLE SPACE TELESCOPE AND THE JAMES WEBB SPACE TELESCOPE. THE ABILITY TO WORK WITH DATA FROM THE UV TO THE FAR IR IS CRUCIAL FROM VALIDATING OUR RESULTS. OUR WORK WILL ALSO EXTEND THE EXASCALE COMPUTATIONAL CAPABILITIES WHICH IS A NATIONAL GOAL., G4502305455, G451917667, G454991031, G4730695835, G491712853, G5080475149, G5099673792, G5145896149, G5178665745, G5195188938, G5505639174, G5505857039, G5539308778, G5555131222, G5601225551, G5635532810, G5654724244, G5913267992, G5955501538, G5965985481, G5967599077, Astronomy at St Andrews 2018-2021, G6080697404, G6326031618, G6359581693, G6379254292, G6471706487, G6656126374, G6728930308, G6731467812, G6777050707, G6877102632, G6880300208, G6890900265, G7047877648, G7084143925, G7184498898, G7394739467, G7425137858, G7471327171, 古代説話における諸寺縁起の研究, G7685134749, G7805626310, G7863371703, Earth-like Planet Search on the Subaru Telescope, G7915813472, G793471318, G8020484511, G8028352098, G8355605048, G8413134427, G8430294048, G8497050386, G8524849061, G855041801, G8662767329, G8684520763, G869884560, G8739736297, G8864104891, G8886077057, G936025562, G939699906
OpenAlex ID: W3134765539