MINDS. The detection of $^{13}$CO$_{2}$ with JWST-MIRI indicates abundant CO$_{2}$ in a protoplanetary disk
Sierra L. Grant, Ewine F. van Dishoeck, Benoît Tabone, Danny Gasman, Thomas Henning, Inga Kamp, Manuel Güdel, Pierre-Olivier Lagage, Giulio Bettoni, Giulia Pero… 展开作者
Sierra L. Grant, Ewine F. van Dishoeck, Benoît Tabone, Danny Gasman, Thomas Henning, Inga Kamp, Manuel Güdel, Pierre-Olivier Lagage, Giulio Bettoni, Giulia Perotti, Valentin Christiaens, Matthias Samland, Aditya M. Arabhavi, Ioannis Argyriou, Alain Abergel, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alessio Caratti o Garatti, Vincent Geers, Adrian M. Glauser, Rodrigo Guadarrama, Hyerin Jang, Jayatee Kanwar, Fred Lahuis, Maria Morales-Calderón, Michael Mueller, Cyrine Nehmé, Göran Olofsson, Eric Pantin, Nicole Pawellek, Tom P. Ray, Donna Rodgers-Lee, Silvia Scheithauer, Jürgen Schreiber, Kamber Schwarz, Milou Temmink, Bart Vandenbussche, Marissa Vlasblom, L. B. F. M. Waters, Gillian Wright, Luis Colina, Thomas R. Greve, Kay Justannont, Göran Östlin
We present JWST-MIRI MRS spectra of the protoplanetary disk around the low-mass T Tauri star GW Lup from the MIRI mid-INfrared Disk Survey (MINDS) GTO program. Emission from $^{12}$CO$_{2}$, $^{13}$CO$_{2}$, H$_{2}$O, HCN, C$_{2}$H$_{2}$, and OH is identified with $^{13}$CO$_{2}$ being detected for the first time in a protoplanetary disk. We characterize the chemical and physical conditions in the inner few au of the GW Lup disk using these molecules as probes. The spectral resolution of JWST-MIRI MRS paired with high signal-to-noise data is essential to identify these species and determine their column densities and temperatures. The $Q$-branches of these molecules, including those of hot-bands, are particularly sensitive to temperature and column density. We find that the $^{12}$CO$_{2}$ emission in the GW Lup disk is coming from optically thick emission at a temperature of $\sim$400 K. $^{13}$CO$_{2}$ is optically thinner and based on a lower temperature of $\sim$325 K, may be tracing deeper into the disk and/or a larger emitting radius than $^{12}$CO$_{2}$. The derived $N_{\rm{CO_{2}}}$/$N_{\rm{H_{2}O}}$ ratio is orders of magnitude higher than previously derived for GW Lup and other targets based on \textit{Spitzer}-IRS data. This high column density ratio may be due to an inner cavity with a radius in between the H$_{2}$O and CO$_{2}$ snowlines and/or an overall lower disk temperature. This paper demonstrates the unique ability of JWST to probe inner disk structures and chemistry through weak, previously unseen molecular features.
Coordinated Space and Ground-Based Monitoring of Accretion Bursts in a Protoplanetary Disk: Establishing Mid-Infrared Hydrogen Lines as Accretion Diagnostics for JWST-MIRI
本文利用 JWST-MIRI 对 DQ Tau 双星系统三个轨道周期的协调监测，首次确立并校准了中红外氢复合线作为原行星盘吸积光度诊断指标，并据此为 38 个已发表的原行星盘 MRS 光谱档案样本提供了吸积光度。
MINDS. Young binary systems with JWST/MIRI: Variable water-rich primaries and extended emission
Carnegie Institution for Science（卡内基科学机构）；Leiden University（莱顿大学）；Max-Planck-Institut für Astronomie (MPIA)（马克斯·普朗克天文学研究所）；Rijksuniversiteit Groningen（格罗宁根大学）；KU Leuven（荷语鲁汶大学）；Université de Liège（列日大学）；Texas State University（德克萨斯州立大学）；University of Exeter（埃克塞特大学）
MINDS survey of silicates in T Tauri disks: Correlation between dust and gas
Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Sciences（孔科利天文台，匈牙利研究与创新学院天文学与地球科学研究中心）；Max-Planck-Institut für Astronomie (MPIA)（马克斯·普朗克天文学研究所）；Department of Astrophysics/IMAPP, Radboud University（拉德堡德大学天体物理学系/IMAPP部门）；SRON Netherlands Institute for Space Research（荷兰空间研究所）；Kapteyn Astronomical Institute, Rijksuniversiteit Groningen（格罗宁根大学卡普坦天文研究所）；Institute of Physics and Astronomy, ELTE Eötvös Loránd University（罗兰大学物理与天文学研究所）；Dept. of Astrophysics, University of Vienna（维也纳大学天体物理学系）
JWST-MIRI's multi-dimensional view of mass loss in the irradiated disks of NGC 1977
Center for Astrophysics | Harvard & Smithsonian（哈佛-史密森天体物理中心）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Division of Geological and Planetary Sciences, California Institute of Technology（加州理工学院地质与行星科学系）；Astronomy Unit, Department of Physics and Astronomy, Queen Mary University of London（伦敦玛丽女王大学物理与天文学系天文学组）；Lunar and Planetary Laboratory, The University of Arizona（亚利桑那大学月球与行星实验室）；National Radio Astronomy Observatory（国家射电天文台）
JWST Imaging of Edge-on Protoplanetary Disks. V. Flux Ratio Reversal and Disk-edge Structure in the Flying Saucer
Univ. Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Department of Astronomy, University of California, Berkeley（加州大学伯克利分校天文学系）；Department of Earth Science and Astronomy, The University of Tokyo（东京大学地球系统行星科学科）
The Effect of X-Ray and Accretion Variability on Mid-Infrared Lines in the Young Disk-Bearing Binary DQ Tau
The Pennsylvania State University（宾夕法尼亚州立大学）；Center for Exoplanets and Habitable Worlds, Penn State University（系外行星与宜居世界中心，宾夕法尼亚州立大学）；Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Sciences（孔科利天文台，匈牙利研究网络天文学与地球科学研究中心）；Zentrum für Astronomie der Universität Heidelberg（海德堡大学天文学中心）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Institute of Astronomy, Russian Academy of Sciences（俄罗斯科学院天文学研究所）；Institute of Physics and Astronomy, ELTE Eötvös Loránd University（罗兰大学物理与天文学研究所）；Centre for Astrophysics Research, University of Hertfordshire（赫特福德大学天体物理学研究中心）
The efficiency of radial transport of icy solid material from outer disk to the inner disk is currently unconstrained. Efficient radial transport of icy dust grains could significantly alter the composition of the gas in the inner disk. Our aim is to model the gaseous CO$_2$ abundance in the inner disk and use this to probe the efficiency of icy dust transport in a viscous disk. Features in the simulated CO$_2$ spectra are investigated for their dust flux tracing potential. We have developed a 1D viscous disk model that includes gas and grain motions as well as dust growth, sublimation and fre…
H$_2^{18}$O in the terrestrial planet-forming regions of protoplanetary disks
Vassar College（瓦萨学院）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Division of Geological and Planetary Sciences, California Institute of Technology（加州理工学院地质与行星科学系）；Department of Astronomy, University of Wisconsin-Madison（威斯康星大学麦迪逊分校天文学系）；Center for Astrophysics, Harvard & Smithsonian（哈佛-史密森尼天体物理中心）；Department of Physics, Texas State University（德克萨斯州立大学物理系）；Weber State University（韦伯州立大学）；Department of Astronomy, University of Michigan（密歇根大学天文学系）；Astrophysics & Space Institute, Schmidt Sciences（施密特科学天体物理学与空间研究所）；Department of Physics and Astronomy, University of Exeter（埃克塞特大学物理与天文系）；Department of Astronomy, University of Maryland（马里兰大学天文学系）
(Abridged) Organic molecules are important constituents of protoplanetary disks. Their ro-vibrational lines observed in the near- and mid-infrared are commonly detected toward T Tauri disks. These lines are the only way to probe the chemistry in the inner few au where terrestrial planets form. To understand this chemistry, accurate molecular abundances have to be determined. This is complicated by excitation effects. Most analyses so far have made the assumption of local thermal equilibrium (LTE). Starting from estimates for the collisional rate coefficients of HCN, non-LTE slab models of the …
JWST/MIRI Detection of Molecular H$_2$ Winds from an Edge-on Class II Source HV Tau C
Tata Institute of Fundamental Research（塔塔基础研究所）；Max-Planck-Institut für Astronomie (MPIA)（马克斯·普朗克天文学研究所）；Kapteyn Astronomical Institute, Rijksuniversiteit Groningen（格罗宁根大学卡佩因天文研究所）；INAF – Osservatorio Astronomico di Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）
研究利用JWST/MIRI-MRS数据分析近边缘取向的II类盘HV Tau C分子氢发射特性，探测到广角双锥分子风，估计其质量损失率等，发现分子H₂风对盘演化等仍重要，吸积率或因边缘取向被低估。
Protoplanetary Disk Evolution in a Low-Metallicity Environment: JWST's First Mid-Infrared Census of Low-Mass Stars
National Astronomical Observatory of Japan（日本国立天文台）；SOKENDAI (The Graduate University for Advanced Studies)（综合研究大学院大学）；Graduate School of Science, Nagoya University（名古屋大学理学研究科）；Institute of Astronomy, School of Science, University of Tokyo（东京大学理学部天体物理系）；Kiso Observatory, Institute of Astronomy, School of Science, University of Tokyo（东京大学理学部天文科学系木曾观测站）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）
Impact of accretion variability on the CO emission of a disk around a very-low-mass star with JWST
Université Paris-Saclay, CNRS, Institut d’Astrophysique Spatiale（巴黎萨克雷大学，法国国家科学研究中心，空间天体物理研究所）；School of Physics and Astronomy, Sun Yat-sen University（中山大学物理与天文学院）；Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学科维理天文与天体物理研究所）；Department of Astronomy, Peking University（北京大学天文系）；INAF – Osservatorio Astronomico di Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Max-Planck-Institut für Extraterrestrische Physik（马克斯·普朗克地外物理学研究所）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Earth and Planets Laboratory, Carnegie Institution for Science（卡内基科学学会地球与行星实验室）；Dept. of Astrophysics, University of Vienna（维也纳大学天体物理系）；ETH Zürich, Institute for Particle Physics and Astrophysics（苏黎世联邦理工学院粒子物理与天体物理研究所）；Kapteyn Astronomical Institute, Rijksuniversiteit Groningen（格罗宁根大学卡普坦天文研究所）；Department of Astronomy, University of Michigan（密歇根大学天文系）
We introduce a new modelling framework called FLiTs to simulate infrared line emission spectra from protoplanetary discs. This paper focuses on the mid-IR spectral region between 9.7 um to 40 um for T Tauri stars. The generated spectra contain several tens of thousands of molecular emission lines of H2O, OH, CO, CO2, HCN, C2H2, H2 and a few other molecules, as well as the forbidden atomic emission lines of SI, SII, SIII, SiII, FeII, NeII, NeIII, ArII and ArIII. In contrast to previously published works, we do not treat the abundances of the molecules nor the temperature in the disc as free par…
[Abridged] The infrared ro-vibrational emission lines from organic molecules in the inner regions of protoplanetary disks are unique probes of the physical and chemical structure of planet forming regions and the processes that shape them. The non-LTE excitation effects of carbon dioxide (CO2) are studied in a full disk model to evaluate: (i) what the emitting regions of the different CO2 ro-vibrational bands are; (ii) how the CO2 abundance can be best traced using CO2 ro-vibrational lines using future JWST data and; (iii) what the excitation and abundances tell us about the inner disk physics…
The mid-IR detection rate of water lines in disks around Herbig stars disks is about 5\%, while it is around 50\% for disks around TTauri stars. The reason for this is still unclear. In this study, we want to find an explanation for the different detection rates between low mass and high mass pre-main-sequence stars (PMSs) in the mid-IR regime. We run disk models with stellar parameters adjusted to spectral types B9 through M2, using the radiation thermo-chemical disk modeling code ProDiMo. We produce convolved spectra at the resolution of Spitzer IRS, JWST MIRI and VLT VISIR spectrographs. We…
