Coordinated Space and Ground-Based Monitoring of Accretion Bursts in a Protoplanetary Disk: Establishing Mid-Infrared Hydrogen Lines as Accretion Diagnostics for JWST-MIRI
Benjamin M. Tofflemire, Carlo F. Manara, Andrea Banzatti, Klaus M. Pontoppidan, Joan Najita, Brunella Nisini, Emma T. Whelan, Justyn Campbell-White, Hala Alqube… 展开作者
Benjamin M. Tofflemire, Carlo F. Manara, Andrea Banzatti, Klaus M. Pontoppidan, Joan Najita, Brunella Nisini, Emma T. Whelan, Justyn Campbell-White, Hala Alqubelat, Adam L. Kraus, Christian Rab, Adrien Houge, Sebastiaan Krijt, James Muzerolle, Eleonora Fiorellino, Myriam Benisty, Lukasz Tychoniec, Colette Salyk, Guillaume Bourdarot, Jacob Hyden
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。
摘要：
在本文中，我们确立并校准了利用 JWST 观测到的中红外氢复合线，将其作为从星周盘吸积物质的前主序星的吸积示踪指标。这项工作是一项协调的多天文台观测计划的一部分，该计划对著名的双星系统 DQ Tau 进行了三个轨道周期的监测，捕捉到了其周期性的吸积爆发。在这第一篇论文中，我们展示了 9 个历元的 MIRI-MRS 光谱，以及近同时的 LCO 测光和 VLT X-Shooter 光谱。该计划捕捉到了异常的吸积变异性，在第一次近星点吸积爆发的峰值与随后的宁静阶段之间，吸积光度跨越了近两个数量级。MIRI 光谱显示的 H I 线光度与 LCO 和 X-Shooter 测得的吸积光度时间序列同步变化。与吸积的紧密相关性以及 MIRI 首次分辨出的较大线宽，支持中红外 H I 跃迁起源于吸积流。结合这三个出色的数据集，我们推导出了三种 H I 跃迁（10-7、7-6、8-7）的中红外线与吸积光度之间的精确关系，并改进了先前基于 Spitzer 光谱的关系。这些新关系为学界提供了一种利用 MIRI-MRS 光谱直接测量吸积光度的方法。由 MIRI 推导出的吸积光度对于时域化学研究以及目前光学波段无法观测的深埋/遥远源的吸积研究至关重要。利用这些新关系，我们为迄今已发表的 38 个原行星盘 MRS 光谱档案样本提供了吸积光度。
英文摘要：
In this paper, we establish and calibrate mid-infrared hydrogen recombination lines observed with JWST as accretion tracers for pre-main-sequence stars that accrete from circumstellar disks. This work is part of a coordinated, multi-observatory effort that monitored the well-known binary system DQ Tau over three orbital periods, capturing its periodic accretion bursts. In this first paper, we present 9 epochs of MIRI-MRS spectra with near-simultaneous LCO photometry and VLT X-Shooter spectroscopy. This program caught exceptional accretion variability, spanning almost two orders of magnitude between the peak of the first periastron accretion burst and the following quiescent phases. The MIRI spectra show H I line luminosities that vary in step with the accretion-luminosity time series measured with LCO and X-Shooter. The tight correlation with accretion and the large line widths, which MIRI resolves for the first time, support an accretion-flow origin for mid-infrared H I transitions. Combining these three exceptional datasets, we derive accurate relations between mid-infrared line and accretion luminosities for three H I transitions (10-7, 7-6, 8-7), and improve upon a previous relation based on Spitzer spectra. These new relations equip the community with a direct measurement of the accretion luminosity from MIRI-MRS spectra. A MIRI-derived accretion luminosity is fundamental for time-domain chemistry studies, as well as for studies of accretion in embedded/distant sources that are currently inaccessible in the optical. With these new relations, we provide accretion luminosities for an archival sample of 38 MRS spectra of protoplanetary disks published to date.
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）
Mass transfer from an evolved donor star to its binary companion is a standard feature of stellar evolution in binaries. In wide binaries, the companion star captures some of the mass ejected in a wind by the primary star. The captured material forms an accretion disk. Here, we study the evolution of wind-accretion disks, using a numerical approach which allows us to follow the long term evolution. For a broad range of initial conditions, we derive the radial density and temperature profiles of the disk. In most cases, wind-accretion leads to long-lived stable disks over the lifetime of the AG…
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…
(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。
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…
