A Comprehensive Characterization of the 70 Virginis Planetary System
Stephen R. Kane, Tabetha S. Boyajian, Gregory W. Henry, Y. Katherina Feng, Natalie R. Hinkel, Debra A. Fischer, Kaspar von Braun, Andrew W. Howard, Jason T. Wright
An on-going effort in the characterization of exoplanetary systems is the accurate determination of host star properties. This effort extends to the relatively bright host stars of planets discovered with the radial velocity method. The Transit Ephemeris Refinement and Monitoring Survey (TERMS) is aiding in these efforts as part of its observational campaign for exoplanet host stars. One of the first known systems is that of 70 Virginis, which harbors a jovian planet in an eccentric orbit. Here we present a complete characterization of this system with a compilation of TERMS photometry, spectroscopy, and interferometry. We provide fundamental properties of the host star through direct interferometric measurements of the radius (1.5\% uncertainty) and through spectroscopic analysis. We combined 59 new Keck HIRES radial velocity measurements with the 169 previously published from the ELODIE, Hamilton, and HIRES spectrographs, to calculate a refined orbital solution and construct a transit ephemeris for the planet. These newly determined system characteristics are used to describe the Habitable Zone of the system with a discussion of possible additional planets and related stability simulations. Finally, we present 19 years of precision robotic photometry that constrain stellar activity and rule out central planetary transits for a Jupiter-radius planet at the 5$σ$ level, with reduced significance down to an impact parameter of $b = 0.95$.
Er et al. (2021) recently proposed a two-planet solution to account for eclipse timing variations (ETVs) observed from the sdB binary NY Virginis. We tested the proposed planetary system for orbit stability using both numerical simulations and chaotic behavior analysis. The best-fit orbits, as well as those with parameters varying by the published uncertainty range in each parameter, were unstable on a timescale much less than the presumed lifetime of the PCEB phase ($\sim$100 Myr). suggesting that the proposed circumbinary companions fail to provide a complete explanation for the observed ETV…
Towards a Comprehensive Understanding of Planetary Systems through Population-Level, Large-Scale Surveys
Instituto de Astrofísica de Andalucía, CSIC（安达卢西亚天体物理研究所）；Centro Astronómico Hispano en Andalucía, Observatorio de Calar Alto（西班牙-安达卢西亚天文中心，卡拉阿托天文台）；Astrophotonics (innoFSPEC), Leibniz-Institut für Astrophysik Potsdam (AIP)（莱布尼茨波茨坦天体物理研究所）；Institut für Physik und Astronomie, Universität Potsdam（波茨坦大学物理与天文学研究所）；Sydney Institute for Astronomy, The University of Sydney（悉尼大学悉尼天体物理研究所）
A comprehensive study of the relations between the properties of planetary systems and the chemical compositions of their host stars
Universidade Federal do Rio de Janeiro（里约热内卢联邦大学）；Observatório Nacional（国家天文台）；Universidade Federal de Sergipe（塞尔希培联邦大学）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）
We present the results of a uniform search for additional planets around all stars with confirmed hot Jupiters observed by the Transiting Exoplanet Survey Satellite (TESS) in its Cycle 1 survey of the southern ecliptic hemisphere. Our search comprises 184 total planetary systems with confirmed hot Jupiters with $R_{p}$ > 8$R_\oplus$ and orbital period < 10 days. The Transit Least Squares (TLS) algorithm was utilized to search for periodic signals that may have been missed by other planet search pipelines. While we recovered 169 of these confirmed hot Jupiters, our search yielded no new statist…
Recent studies have shown that the radii and masses of adjacent planets within a planetary system are correlated. It is unknown how this 'peas-in-a-pod' phenomenon originates, whether it is in place at birth or requires evolution, and whether it (initially) applies only to neighboring planets or to all planets within a system. Here we address these questions by making use of the recent discovery that planetary system architectures strongly depend on ambient stellar clustering. Based on Gaia's second data release, we divide the sample of planetary systems hosting multiple planets into those res…
Synthesizing Exoplanet Demographics: A Single Population of Long-Period Planetary Companions to M Dwarfs Consistent with Microlensing, Radial Velocity, and Direct Imaging Surveys
We present the first study to synthesize results from five different exoplanet surveys using three independent detection methods: microlensing, radial velocity, and direct imaging. The constraints derived herein represent the most comprehensive picture of the demographics of large-separation (>~ 2 AU) planets orbiting the most common stars in our Galaxy that has been constructed to date. We assume a simple, joint power-law planet distribution function of the form d^2 N_{pl} /[dlog(m_p)dlog(a)] = A(m_p/ M_{Sat} )^{alpha}(a/2.5 AU)^{beta} with an outer cutoff radius of the separation distributio…
S-Type and P-Type Habitability in Stellar Binary Systems: A Comprehensive Approach III. Results for Mars, Earth, and super-Earth Planets
在论文I和II中，采用了一种综合方法，计算了双星系统中的S-型和P-型可居住区，包括双星组成部分的圆形和椭圆形轨道。它考虑了一个联合约束，包括轨道稳定性和通过恒星辐射能量通量（“辐射宜居带“; RHZ）的可能系统行星的适居区。具体地说，恒星S型和P型RHZ的计算基于四阶多项式的解决方案。然而，在同时的发展中，主要是在2013年和2014年，基于R. K. Kopparapu和合作者。这些模型需要对恒星宜居带的内部和外部界限进行相当大的改变。此外，关于失控的温室效应造成的可居住性极限，由于大气模型的差异，地球、火星和超级地球行星之间存在显著差异，从而影响了它们的可居住性潜力。本研究的目的是根据更新的行星模型计算双星的S型和P型适居区。此外，我们的研究还将考虑改善低光度恒星的有效温度，半径和质量之间的关系。
KELT-9b is an ultra-hot Jupiter observed to be undergoing extreme mass loss. Its A0-type host star has a radiative envelope, which makes its surface layers prone to retaining recently accreted material. To search for potential signs of planetary material polluting the stellar surface, we carry out the most comprehensive chemical characterisation of KELT-9 to-date. New element detections include Na and Y, which had previously been detected in the ultra-hot Jupiter but not studied in the star; these detections complete the set of nine elements measured in both star and planet. In comparing KELT-…
Rapid and Predictive Planet Population Synthesis Model (RAPPS) I. Upgraded model and resulting synthetic populations
Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）；UTokyo Organization for Planetary Space Science (UTOPS), University of Tokyo（东京大学地球行星科学宇宙科学研究机构（UTOPS））；Division of Science, National Astronomical Observatory of Japan（日本国立天文台理学院）；Astrobiology Center (ABC)（天体生物学中心）；Graduate Institute for Advanced Studies, SOKENDAI（SOKENDAI高等研究院）；Department of Earth and Planetary Science, University of Tokyo（东京大学地球行星科学系）
Beyond the mass-radius plane: Integrated radiative-convective and interior structure simulations of the exoplanet continuum
Institute of Astronomy, University of Cambridge（剑桥大学天文研究所）；Atmospheric Oceanic and Planetary Physics, University of Oxford（牛津大学大气海洋与行星物理系）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）
We want to understand global observable consequences of different physical processes and initial properties on the demographics of the planetary population. We use the Generation III Bern model to perform planetary population synthesis. We synthesise five populations with each a different initial number of Moon-mass embryos per disc: 1, 10, 20, 50, and 100. The last is our nominal population around 1 Sun-mass stars. The properties of giant planets do not change much as long as there are at least 10 embryos in each system. The study of giants can thus be done with simulations requiring less com…
High-precision transit photometry supplies ideal opportunities for detecting new exoplanets and characterizing their physical properties, which usually encode valuable information for unveiling the planetary structure, atmosphere and dynamical history. We present revised properties of three transiting systems (i.e., HAT-P-13, HAT-P-16 and WASP-32) through analyzing TESS photometry and ground-based transit observations, which were obtained at the 1m and 2.4m telescopes of Yunnan Observatories, China, and the 1.2m telescope of Hamburg Observatory, Germany, as well as the data in the literature. …
The international planetary science community met in London in January 2020, united in the goal of realising the first dedicated robotic mission to the distant Ice Giants, Uranus and Neptune, as the only major class of Solar System planet yet to be comprehensively explored. Ice-Giant-sized worlds appear to be a common outcome of the planet formation process, and pose unique and extreme tests of our understanding of planetary origins, exotic water-rich planetary interiors, dynamic seasonal atmospheres, complex magnetospheric configurations, geologically-rich icy satellites (both natural and cap…
Planets orbiting low-mass stars such as M dwarfs are now considered a cornerstone in the search for life-harbouring planets. GJ273 is a planetary system orbiting an M dwarf only 3.75 pc away, composed of two confirmed planets, GJ273b and GJ273c, and two promising candidates, GJ273d and GJ273e. Planet GJ273b resides in the habitable zone. Currently, due to a lack of observed planetary transits, only the minimum masses of the planets are known.Despite being an interesting system, the GJ273 planetary system is still poorly studied. We aim at precisely determine the physical parameters of the indi…
CORALIE radial-velocity search for companions around evolved stars (CASCADES) V. Three planetary companions and achievable precision
Instituto de Astrofísica de Andalucía-CSIC（安达卢西亚天体物理研究所）；Observatoire Astronomique de l’Université de Genève（日内瓦大学天文台）；Instituut voor Sterrenkunde, KU Leuven（荷语鲁汶大学天文研究所）；Space sciences, Technologies and Astrophysics Research（空间科学、技术与天体物理研究）
A comprehensive spectroscopic reference of the solar system and its application to exoplanet direct imaging
NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Southeastern Universities Research Association (SURA)（东南大学研究协会）；Centre for Planetary Habitability, Department of Geosciences, University of Oslo（奥斯陆大学地球科学系行星宜居性中心）；American University（美国大学）；Oak Ridge Associated Universities (ORAU), NPP Program（橡树岭联合大学国家博士后培养项目）
Minimizing the bias in exoplanet detection - application to radial velocities of LHS 1140
一颗围绕LHS 1140运行的周期为24.7d的岩石行星已经被发现，这是基于在其光和高精度径向速度数据中发现的凌日现象（Dittmann et al. 2017）。通过两种独立的方法得到的这一发现是一种观察性的尝试，然而，我们发现对数据的保守分析给出了不同的解决方案。根据我们对恒星活动的诊断，在径向速度数据中，一个三行星系统是显而易见的。我们鼓励进一步进行有针对性的光度和径向速度观测，以限制显然造成3.8天和90天径向速度信号的小型海王星和超级地球质量物体。我们使用我们的软件包Agatha（https：//phillippro.shinyapps.io/Agatha/）提供一个全面的策略，从径向速度数据中的恒星活动中解开行星信号。
Revisiting TOI-4438 and TOI-442 planetary systems with new observations from SPIRou and TESS
Instituto de Ciencias Físicas (ICIFI-CONICET), ECyT-UNSAM（物理科学研究所（ICIFI-CONICET），萨米森理工学院）；Instituto Tecnológico de Buenos Aires (ITBA)（布宜诺斯艾利斯理工大学）；Institut d’astrophysique de Paris, CNRS, UMR 7095, Sorbonne Université（巴黎天体物理学研究所，法国国家科学研究中心，索邦大学）；Observatoire de Haute-Provence（上普罗旺斯天文台）；Laboratório Nacional de Astrofisica（国家天体物理学实验室）；SOAR Telescope/NSF’s NOIRLab（南方自动望远镜/美国国家光学红外天文研究实验室）；Institute for Particle Physics and Astrophysics, ETH Zurich（苏黎世联邦理工学院粒子物理与天体物理研究所）；Canada France Hawaii Telescope (CFHT) Corporation（加拿大-法国-夏威夷望远镜公司）；Trottier Institute for Research on Exoplanets and Department of Physics, Université de Montréal（蒙特利尔大学系外行星研究特罗蒂耶研究所和物理系）；Aix Marseille Univ, CNRS, CNES, LAM（艾克斯-马赛大学，法国国家科学研究中心，法国国家太空研究中心）；Univ. Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学，法国国家科学研究中心）；Université de Toulouse, CNRS, IRAP（图卢兹大学，法国国家科学研究中心）；Department of Physics, McGill University（麦吉尔大学物理系）
