The homogeneous characterisation of Ariel host stars
C. Danielski, A. Brucalassi, S. Benatti, T. Campante, E. Delgado-Mena, M. Rainer, G. Sacco, V. Adibekyan, K. Biazzo, D. Bossini, G. Bruno, G. Casali, P. Kabath,… 展开作者
C. Danielski, A. Brucalassi, S. Benatti, T. Campante, E. Delgado-Mena, M. Rainer, G. Sacco, V. Adibekyan, K. Biazzo, D. Bossini, G. Bruno, G. Casali, P. Kabath, L. Magrini, G. Micela, G. Morello, P. Palladino, N. Sanna, S. Sarkar, S. Sousa, M. Tsantaki, D. Turrini, M. Van der Swaelmen
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24 pages, 9 figures, 3 tables. Published in Experimental Astronomy
The Ariel mission will characterise the chemical and thermal properties of the atmospheres of about a thousand exoplanets transiting their host star(s). The observation of such a large sample of planets will allow to deepen our understanding of planetary and atmospheric formation at the early stages, providing a truly representative picture of the chemical nature of exoplanets, and relating this directly to the type and chemical environment of the host star. Hence, the accurate and precise determination of the host star fundamental properties is essential to Ariel for drawing a comprehensive picture of the underlying essence of these planetary systems. We present here a structured approach for the characterisation of Ariel stars that accounts for the concepts of homogeneity and coherence among a large set of stellar parameters. We present here the studies and benchmark analyses we have been performing to determine robust stellar fundamental parameters, elemental abundances, activity indices, and stellar ages. In particular, we present results for the homogeneous estimation of the activity indices S and log(R'HK), and preliminary results for elemental abundances of Na, Al, Mg, Si, C, N. In addition, we analyse the variation of a planetary spectrum, obtained with Ariel, as a function of the uncertainty on the stellar effective temperature. Finally, we present our observational campaign for precisely and homogeneously characterising all Ariel stars in order to perform a meaningful choice of final targets before the mission launch.
Ariel stellar characterisation IV. Fundamental parameters of 18 hot stars in the Ariel mission candidate sample
Space Research Institute, Austrian Academy of Sciences（奥地利科学院空间研究所）；Institute for Theoretical and Computation Physics, Graz University of Technology（格拉茨工业大学理论与计算物理研究所）；Department of Physics and Astronomy G. Galilei, University of Padova（帕多瓦大学伽利略物理学与天文学系）；INAF – Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Departament d’Astronomia i Astrofísica, Universitat de València（瓦伦西亚大学天文与天体物理系）；INAF – Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；INAF – Osservatorio Astrofisico di Torino（意大利国家天体物理研究所都灵天文台）；Instituto de Astrofísica de Canarias（加那利群岛天体物理研究所）；Universidad de La Laguna（拉古纳大学）；Institute for Space Astrophysics and Planetology INAF-IAPS（意大利国家天体物理研究所空间天体物理与行星学研究所）；Department of Physics and Astronomy, University College London（伦敦大学学院物理学与天文学系）
Stellar flares with Ariel: detection prospects and impacts on exoplanet spectroscopy
Konkoly Observatory（孔科利天文台）；HUN-REN Research Centre for Astronomy and Earth Sciences（匈牙利研究网络地球与天文学研究中心）；HUN-REN CSFK MTA Centre of Excellence（匈牙利研究网络 CSFK 马塔科学院卓越中心）；SRON Space Research Organisation Netherlands（荷兰空间研究组织 SRON）
Spectropolarimetric characterisation of exoplanet host stars in preparation of the $Ariel$ mission II. The magnetised wind environment of TOI-1860, DS Tuc A, and HD 63433
Ariel Tier 3 Observations: An Opportunity to Explore both Stellar and Planetary Variability through Broad Wavelength Time-domain Spectroscopy
INAF-Osservatorio Astronomico di Palermo（意大利国家天体物理研究所巴勒莫天文台）；ESA/ESTEC Science Engagement and Oversight Office (SCI-E) Directorate of Science (SCI)（欧洲空间局/欧洲空间研究与技术中心科学参与和监督办公室（SCI-E）科学司（SCI））
Coralie radial-velocity search for companions around evolved stars (CASCADES) III. A new Jupiter host-star: in-depth analysis of HD 29399 using TESS data
HATS-9b and HATS-10b: Two Compact Hot Jupiters in Field 7 of the K2 Mission
我们报告的发现两个凌日系外行星的HAT南调查。HATS-9 b围绕一颗老的（10.8 $\pm$ 1.5 Gyr）V=13.3 G的矮星运行，周期P = 1.9153 d。主恒星质量为1.03 M $_{\odot}$，半径为1.503 R $_\odot$，有效温度为5366 $\pm$ 70 K。行星伴星的质量为0.837 M $_J$，半径为1.065 R $_J$，平均密度为0.85 g cm $^{-3}$。HATS-10 b围绕一颗V=13.1 G的矮星运行，周期P = 3.3128 d。主恒星质量为1.1 M $_\odot$，半径为1.11 R $_\odot$，有效温度为5880 $\pm$ 120 K。行星伴星的质量为0.53 M $_J$，半径为0.97 R $_J$，平均密度为0.7 g cm $^{-3}$。这两颗行星都是紧凑的，与接受类似辐射的行星相比，它们都位于K2的场7的名义坐标上，但只有HATS-9 b落在工作硅上。HATS-9 b的未来特性与开普勒望远镜的精密光度精度可能会提供其反射光特征的测量。
Asteroseismic modelling of main-sequence solar-like stars and Kepler exoplanet host stars with the FICO procedure I. Catalogue of fundamental stellar properties
Uppsala University（乌普萨拉大学）；Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CY Cergy Paris Université, CNRS（巴黎天文台，巴黎文理研究大学，索邦大学，巴黎西岱大学，CY塞吉-蓬图瓦兹大学，法国国家科学研究中心）；STAR Institute, Université de Liège（列日大学天体物理、恒星和系外行星研究所）；Istituto Nazionale di Astrofisica – Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP（波尔图大学空间科学与天体物理研究所）
Bridging stellar evolution and planet formation: from birth, to survivors of the fittest, to the second generation of planets
European Southern Observatory（欧洲南方天文台）；KU Leuven（荷语鲁汶大学）；Chalmers University of Technology（查尔姆斯理工大学）；Macquarie University（麦考瑞大学）；Georgia State University（佐治亚州立大学）；University of Exeter（埃克塞特大学）；Konkoly Observatory（孔科利天文台）；Côte d’Azur Observatory（蔚蓝海岸天文台）；Universidad de Chile（智利大学）
