检索结果-内蒙古大学图书馆

Experimental brain research 2023年第7期241卷 1973页

作者： Otella Shoja Farzad Towhidkhah Hamidollah Hassanlouei Mindy F Levin Alireza Bahramian Sylvie Nadeau Lei Zhang Anatol G Feldman Department of Neuroscience University of Montreal Montreal QC Canada. Department of Biomedical Engineering Amirkabir University of Technology Tehran Iran. Department of Motor Behaviour Faculty of Sport Science and Health Shahid Beheshti University Tehran Iran. School of Physical and Occupational Therapy McGill University Montreal QC Canada. Center for Interdisciplinary Research in Rehabilitation of Greater Montreal (CRIR) Montreal QC Canada. Faculté de Médecine-École de Réadaptation Montreal QC Canada. Institute for Neural Computation Ruhr University Bochum Bochum Germany. Department of Neuroscience University of Montreal Montreal QC Canada. anatol.g.feldman@umontreal.ca. Center for Interdisciplinary Research in Rehabilitation of Greater Montreal (CRIR) Montreal QC Canada. anatol.g.feldman@umontreal.ca. Institut de réadaptation Gingras-Lindsay-de-Montréal (IRGLM) 6300 Darlington Montreal QC H3S 2J4 Canada. anatol.g.feldman@umontreal.ca.

Titelbild: Entropy-Mediated Stable Structural Evolution of Prussian White Cathodes for Long-Life Na-Ion Batteries (Angew. Chem. 7/2024)

学校读者我要写书评

暂无评论

Angewandte Chemie 2024年第7期136卷

作者： Yueyue He Sören L. Dreyer Yin-Ying Ting Prof. Yuan Ma Dr. Yang Hu Dr. Damian Goonetilleke Dr. Yushu Tang Dr. Thomas Diemant Bei Zhou Dr. Piotr M. Kowalski Prof. Maximilian Fichtner Prof. Horst Hahn Prof. Jasmin Aghassi-Hagmann Dr. Torsten Brezesinski Dr. Ben Breitung Prof. Yanjiao Ma Institute of Nanotechnology Karlsruhe Institute of Technology (KIT) Hermann-von-Helmholtz Platz 1 76344 Eggenstein-Leopoldshafen Germany Institute of Energy and Climate Research (IEK-13) Forschungszentrum Jülich GmbH Wilhelm-Johnen-Str. 52428 Jülich Germany Chair of Theory and Computation of Energy Materials Faculty of Georesources and Materials Engineering RWTH Aachen University 52062 Aachen Germany Helmholtz Institute Ulm (HIU) for Electrochemical Energy Storage Helmholtzstr. 11 89081 Ulm Germany Current address: Corporate Research and Development Umicore Watertorenstraat 33 2250 Olen Belgium Jülich Aachen Research Alliance JARA Energy & Center for Simulation and Data Science (CSD) 52425 Jülich Germany School of Chemical Biological and Materials Engineering The University of Oklahoma Norman OK 73019 USA Current address: School of Energy and Mechanical Engineering Jiangsu Key Laboratory of New Power Batteries Nanjing Normal University Nanjing 210023 China

Cover Picture: Entropy-Mediated Stable Structural Evolution of Prussian White Cathodes for Long-Life Na-Ion Batteries (Angew. Chem. Int. Ed. 7/2024)

学校读者我要写书评

暂无评论

Angewandte Chemie International Edition 2024年第7期63卷

Early Planet Formation in Embedded Disks (eDisk) XII: Accretion streamers, protoplanetary disk, and outflow in the Class I source Oph IRS63

学校读者我要写书评

暂无评论

arXiv 2023年

作者： Flores, Christian Ohashi, Nagayoshi Tobin, John J. Jørgensen, Jes K. Takakuwa, Shigehisa Li, Zhi-Yun Lin, Zhe-Yu Daniel van’t Hoff, Merel L.R. Plunkett, Adele L. Yamato, Yoshihide Sai, Jinshi Koch, Patrick M. Yen, Hsi-Wei Aikawa, Yuri Aso, Yusuke Gregorio-Monsalvo, Itziar de Kido, Miyu Kwon, Woojin Lee, Jeong-Eun Lee, Chang Won Looney, Leslie W. Santamaría-Miranda, Alejandro Sharma, Rajeeb Thieme, Travis J. Williams, Jonathan P. Han, Ilseung Narayanan, Suchitra Lai, Shih-Ping Academia Sinica Institute of Astronomy & Astrophysics 11F of Astronomy-Mathematics Building AS/NTU No.1 Sec. 4 Roosevelt Rd Taipei10617 Taiwan National Radio Astronomy Observatory 520 Edgemont Rd CharlottesvilleVA22903 United States Niels Bohr Institute University of Copenhagen Øster Voldgade 5-7 Copenhagen1350 Denmark Department of Physics and Astronomy Graduate School of Science and Engineering Kagoshima University 1-21-35 Korimoto Kagoshima Kagoshima890-0065 Japan University of Virginia 530 McCormick Rd. CharlottesvilleVA22904 United States Department of Astronomy University of Michigan 1085 S. University Ave. Ann ArborMI48109-1107 United States Department of Astronomy Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan Korea Astronomy and Space Science Institute 776 Daedeok-daero Yuseong-gu Daejeon34055 Korea Republic of European Southern Observatory Alonso de Cordova 3107 Casilla 19 Vitacura Santiago Chile Department of Earth Science Education Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of SNU Astronomy Research Center Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of Department of Physics and Astronomy Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of Division of Astronomy and Space Science University of Science and Technology 217 Gajeong-ro Yuseong-gu Daejeon34113 Korea Republic of Department of Astronomy University of Illinois 1002 West Green St UrbanaIL61801 United States Institute of Astronomy National Tsing Hua University No. 101 Section 2 Kuang-Fu Road Hsinchu30013 Taiwan Center for Informatics and Computation in Astronomy National Tsing Hua University No. 101 Section 2 Kuang-Fu Road Hsinchu30013 Taiwan Department of Physics National Tsing Hua University No. 101 Section 2 Kuang-Fu Road Hsinchu30013 Taiwan Institute for Astronomy University of Hawai‘i at Mānoa 2680 Woodl

We present ALMA observations of the Class I source Oph IRS63 in the context of the Early Planet Formation in Embedded Disks (eDisk) large program. Our ALMA observations of Oph IRS63 show a myriad of protostellar features, such as a shell-like bipolar outflow (in 12CO), an extended rotating envelope structure (in 13CO), a streamer connecting the envelope to the disk (in C18O), and several small-scale spiral structures seen towards the edge of the dust continuum (in SO). By analyzing the velocity pattern of 13CO and C18O, we measure a protostellar mass of M★ = 0.5±0.2 M☉ and confirm the presence of a disk rotating at almost Keplerian velocity that extends up to ∼ 260 au. These calculations also show that the gaseous disk is about four times larger than the dust disk, which could indicate dust evolution and radial drift. Furthermore, we model the C18O streamer and SO spiral structures as features originating from an infalling rotating structure that continuously feeds the young protostellar disk. We compute an envelope-to-disk mass infall rate of ∼ 10−6 M☉ yr−1 and compare it to the disk-to-star mass accretion rate of ∼ 10−8 M☉ yr−1, from which we infer that the protostellar disk is in a mass build-up phase. At the current mass infall rate, we speculate that soon the disk will become too massive to be gravitationally stable. © 2023, CC BY.

关键词： Dust

Quark masses using twisted mass fermion gauge ensembles

学校读者我要写书评

暂无评论

arXiv 2021年

作者： Alexandrou, C. Bacchio, S. Bergner, G. Constantinou, M. Di Carlo, M. Dimopoulos, P. Finkenrath, J. Fiorenza, E. Frezzotti, R. Garofalo, M. Hadjiyiannakou, K. Kostrzewa, B. Koutsou, G. Jansen, K. Lubicz, V. Mangin-Brinet, M. Manigrasso, F. Martinelli, G. Papadiofantous, E. Pittler, F. Rossi, G.C. Sanfilippo, F. Simula, Silvano Tarantino, C. Todaro, A. Urbach, C. Wenger, U. Department of Physics University of Cyprus Nicosia20537 Cyprus Computation-based Science and Technology Research Center The Cyprus Institute 20 Konstantinou Kavafi Street Nicosia2121 Cyprus University of Jena Institute for Theoretical Physics Max-Wien-Platz 1 JenaD-07743 Germany Department of Physics Temple University PhiladelphiaPA19122 - 1801 United States School of Physics and Astronomy The University of Edinburgh EdinburghEH9 3FD United Kingdom Istituto Nazionale di Fisica Nucleare Sezione di Roma La Sapienza Piazzale Aldo Moro 5 RomaI-00185 Italy Parma43124 Italy CP3-Origins University of Southern Denmark Campusvej 55 Odense5230 Denmark Dipartimento di Fisica INFN Università di Roma Tor Vergata Via della Ricerca Scientifica 1 RomaI-00133 Italy Rheinische Friedrich-Wilhelms-Universität Bonn Nussallee 14-16 Bonn53115 Germany High Performance Computing and Analytics Lab Rheinische Friedrich-Wilhelms-Universität Bonn Friedrich-Hirzebruch-Allee 8 Bonn53115 Germany NIC DESY Platanenallee 6 ZeuthenD-15738 Germany Dipartimento di Matematica e Fisica Università Roma Tre INFN Sezione di Roma Tre Via della Vasca Navale 84 RomeI-00146 Italy Theory Group Laboratoire de Physique Subatomique et de Cosmologie CNRS IN2P3 Grenoble38026 France Institut für Physik Humboldt-Universität zu Berlin Newtonstrasse 15 Berlin12489 Germany Dipartimento di Fisica INFN Università di Roma La Sapienza Piazzale Aldo Moro 5 RomaI-00185 Italy Centro Fermi Museo Storico della Fisica Centro Studi e Ricerche Enrico Fermi Piazza del Viminale 1 RomaI-00184 Italy Istituto Nazionale di Fisica Nucleare Sezione di Roma Tre Via della Vasca Navale 84 RomeI-00146 Italy Institute for Theoretical Physics Albert Einstein Center for Fundamental Physics University of Bern Sidlerstrasse 5 BernCH-3012 Switzerland

We present a calculation of the up, down, strange and charm quark masses performed within the lattice QCD framework. We use the twisted mass fermion action and carry out simulations that include in the sea two light mass-degenerate quarks, as well as the strange and charm quarks. In the analysis we use gauge ensembles simulated at three values of the lattice spacing and with light quarks that correspond to pion masses in the range from 350 MeV to the physical value, while the strange and charm quark masses are tuned approximately to their physical values. We use several quantities to set the scale in order to check for finite lattice spacing effects and in the continuum limit we get compatible results. The quark mass renormalization is carried out nonperturbatively using the RI'-MOM method converted into the MS scheme. For the determination of the quark masses we use physical observables from both the meson and the baryon sectors, obtaining mud = 3.636(66)(+60−57) MeV and ms = 98.7(2.4)(+4.0−3.2) MeV in the MS(2 GeV) scheme and mc = 1036(17)(+15−8 ) MeV in the MS(3 GeV) scheme, where the first errors are statistical and the second ones are combinations of systematic errors. For the quark mass ratios we get ms/mud = 27.17(32)(+56−38) and mc/ms = 11.48(12)(+25−19). Copyright © 2021, The Authors. All rights reserved.

关键词： Hadrons

Entropy-Mediated Stable Structural Evolution of Prussian White Cathodes for Long-Life Na-Ion Batteries

学校读者我要写书评

暂无评论

Angewandte Chemie 2023年第7期136卷

The high-entropy approach is applied to monoclinic Prussian White (PW) Na-ion cathodes to address the issue of unfavorable multilevel phase transitions upon electrochemical cycling, leading to poor stability and capacity decay. A series of Mn-based samples with up to six metal species sharing the N-coordinated positions was synthesized. The material of composition Na 1.65 Mn 0.4 Fe 0.12 Ni 0.12 Cu 0.12 Co 0.12 Cd 0.12 [Fe(CN) 6 ] 0.92 □ 0.08 ⋅ 1.09H 2 O was found to exhibit superior cyclability over medium/low-entropy and conventional single-metal PWs. We also report, to our knowledge for the first time, that a high-symmetry crystal structure may be advantageous for high-entropy PWs during battery operation. computational comparisons of the formation enthalpy demonstrate that the compositionally less complex materials are prone to phase transitions, which negatively affect cycling performance. Based on data from complementary characterization techniques, an intrinsic mechanism for the stability improvement of the disordered PW structure upon Na + insertion/extraction is proposed, namely the dual effect of suppression of phase transitions and mitigation of gas evolution.

关键词： High-Entropy Materials Outgassing Phase Transitions Prussian White Sodium-Ion Cathode

Testing Lyman Alpha Emitters and Lyman-Break Galaxies as Tracers of Large-Scale Structures at High Redshifts

学校读者我要写书评

暂无评论

arXiv 2024年

作者： Im, Sang Hyeok Hwang, Ho Seong Park, Jaehong Lee, Jaehyun Song, Hyunmi Appleby, Stephen Dubois, Yohan Few, C. Gareth Gibson, Brad K. Kim, Juhan Kim, Yonghwi Park, Changbom Pichon, Christophe Shin, Jihye Snaith, Owain N. Artale, Maria Celeste Gawiser, Eric Guaita, Lucia Jeong, Woong-Seob Lee, Kyoung-Soo Padilla, Nelson Ramakrishnan, Vandana Troncoso, Paulina Yang, Yujin Department of Physics and Astronomy Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of SNU Astronomy Research Center Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of Korea Institute for Advanced Study 85 Hoegi-ro Dongdaemun-gu Seoul02455 Korea Republic of 537 Haeansaneop-ro Sanam-myeon Gyeongsangnam-do Sacheon Korea Republic of Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon34055 Korea Republic of Department of Astronomy and Space Science Chungnam National University 99 Daehak-ro Yuseong-gu Daejeon34134 Korea Republic of Asia Pacific Center for Theoretical Physics Pohang37673 Korea Republic of Department of Physics POSTECH Pohang37673 Korea Republic of CNRS and Sorbonne Université UMR 7095 Institut d’Astrophysique de Paris 98 bis Boulevard Arago ParisF-75014 France E.A. Milne Centre for Astrophysics University of Hull HullHU6 7RX United Kingdom Woodmansey Primary School Woodmansey Hull Road HU17 0TH United Kingdom Center for Advanced Computation Korea Institute for Advanced Study 85 Hoegiro Dongdaemun-gu Seoul02455 Korea Republic of Korea Institute of Science and Technology Information 245 Daehak-ro Yuseong-gu Daejeon34141 Korea Republic of IPhT DRF-INP UMR 3680 CEA L’Orme des Merisiers Bât 774 Gif-sur-YvetteF-91191 France Department of Physics and Astronomy University of Exeter ExeterEX4 4QL United Kingdom Departamento de Ciencias Fisicas Universidad Andres Bello Fernandez Concha 700 Las Condes Santiago Chile Department of Physics and Astronomy Rutgers the State University of New Jersey PiscatawayNJ08854 United States Universidad Andres Bello Facultad de Ciencias Exactas Departamento de Fisica Instituto de Astrofisica Fernandez Concha 700 Las Condes RM Santiago Chile Department of Physics and Astronomy Purdue University 525 Northwestern Ave. West LafayetteIN47906 United States CONICET-UNC Laprida 854 CórdobaX

We test whether Lyman alpha emitters (LAEs) and Lyman-break galaxies (LBGs) can be good tracers of high-z large-scale structures, using the Horizon Run 5 cosmological hydrodynamical simulation. We identify LAEs using the Lyα emission line luminosity and its equivalent width, and LBGs using the broad-band magnitudes at z ∼ 2.4, 3.1, and 4.5. We first compare the spatial distributions of LAEs, LBGs, all galaxies, and dark matter around the filamentary structures defined by dark matter. The comparison shows that both LAEs and LBGs are more concentrated toward the dark matter filaments than dark matter. We also find an empirical fitting formula for the vertical density profile of filaments as a binomial power-law relation of the distance to the filaments. We then compare the spatial distributions of the samples around the filaments defined by themselves. LAEs and LBGs are again more concentrated toward their filaments than dark matter. We also find the overall consistency between filamentary structures defined by LAEs, LBGs, and dark matter, with the median spatial offsets that are smaller than the mean separation of the sample. These results support the idea that the LAEs and LBGs could be good tracers of large-scale structures of dark matter at high redshifts. © 2024, CC BY-NC-SA.

关键词： Dark Matter

VERTICO and IllustrisTNG: The spatially resolved effects of environment on galactic gas

学校读者我要写书评

暂无评论

arXiv 2023年

作者： Stevens, Adam R.H. Brown, Toby Diemer, Benedikt Pillepich, Annalisa Hernquist, Lars Nelson, Dylan Bahé, Yannick M. Boselli, Alessandro Davis, Timothy A. Elahi, Pascal J. Ellison, Sara L. Jiménez-Donaire, María J. Roberts, Ian D. Spekkens, Kristine Villanueva, Vicente Watts, Adam B. Wilson, Christine D. Zabel, Nikki International Centre for Radio Astronomy Research The University of Western Australia CrawleyWA6009 Australia Herzberg Astronomy and Astrophysics Research Centre National Research Council of Canada VictoriaBCV9E 2E7 Canada Department of Astronomy University of Maryland College ParkMD20742 United States Max-Planck-Institut für Astronomie Baden-Wúrttemburg HeidelbergD-69117 Germany Institute for Theory and Computation Harvard–Smithsonian Center for Astrophysics CambridgeMA02138 United States Institut für theoretische Astrophysik Zentrum für Astronomie Universität Heidelberg Baden-Wúrttemburg HeidelbergD-69120 Germany Observatoire de Sauverny Versoix1290 Switzerland Leiden Observatory Leiden University PO Box 9513 LeidenNL-2300 RA Netherlands Aix-Marseille Université CNRS CNES LAM Marseille France Cardiff Hub for Astrophysics Research & Technology School of Physics & Astronomy Cardiff University Queens Buildings CardiffCF24 3AA United Kingdom Pawsey Supercomputing Centre KensingtonWA6151 Australia Department of Physics & Astronomy University of Victoria Finnerty Road VictoriaBCV8P 1A1 Canada C/Alfonso XII 3 MadridE-28014 Spain Royal Military College of Canada PO Box 17000 Station Forces KingstonONK7K 7B4 Canada Department of Physics & Astronomy McMaster University 1280 Main Street W HamiltonONL8S 4M1 Canada Department of Astronomy University of Cape Town Private Bag X3 Rondebosch7701 South Africa

It has been shown in previous publications that the TNG100 simulation quantitatively reproduces the observed reduction in each of the total atomic and total molecular hydrogen gas for galaxies within massive halos, i.e. dense environments. In this Letter, we study how well TNG50 reproduces the resolved effects of a Virgo-like cluster environment on the gas surface densities of satellite galaxies with m∗ >109 M☉ and SFR > 0.05 M☉ yr−1. We select galaxies in the simulation that are analogous to those in the HERACLES and VERTICO surveys, and mock-observe them to the common specifications of the data. Although TNG50 does not quantitatively match the observed gas surface densities in the centers of galaxies, the simulation does qualitatively reproduce the trends of gas truncation and central density suppression seen in VERTICO in both H i and H2. This result promises that modern cosmological hydrodynamic simulations can be used to reliably model the post-infall histories of cluster satellite galaxies. Copyright © 2023, The Authors. All rights reserved.

关键词： Galaxies

Revealing the structure of light pseudoscalar mesons at the Electron-Ion Collider

学校读者我要写书评

暂无评论

arXiv 2021年

作者： Arrington, John Gayoso, Carlos Ayerbe Barry, Patrick C. Berdnikov, Vladimir Binosi, Daniele Chang, Lei Diefenthaler, Markus Ding, Minghui Ent, Rolf Frederico, Tobias Furletova, Yulia Hobbs, Tim J. Horn, Tanja Huber, Garth M. Kay, Stephen J.D. Keppel, Cynthia Lin, Huy-Wen Mezrag, Cedric Montgomery, Rachel Pegg, Ian L. Raya, Khepani Reimer, Paul Richards, David G. Roberts, Craig D. Rodríguez-Quintero, Jose Romanov, Dmitry Salmè, Giovanni Sato, Nobuo Segovia, Jorge Stepanov, Petr Tadepalli, Arun S. Trotta, Richard L. Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Mississippi State University StarkvilleMS United States Catholic University of America WashingtonDC United States I-38123 Italy School of Physics Nankai University Tianjin300071 China Thomas Jefferson National Accelerator Facility Newport NewsVA23606 United States Instituto Tecnológico de Aeronáutica São José dos Campos12.228-900 Brazil Southern Methodist University DallasTX75275-0175 United States University of Regina ReginaSKS4S 0A2 Canada Michigan State University East LansingMI48824 United States IRFU CEA Université Paris-Saclay Gif-sur-YvetteF-91191 France SUPA School of Physics and Astronomy University of Glasgow GlasgowG12 8QQ United Kingdom Instituto de Ciencias Nucleares Universidad Nacional Autónoma de México Apartado Postal 70-543 CDMXC.P. 04510 Mexico Argonne National Laboratory LemontIL60439 United States School of Physics Nanjing University Nanjing Jiangsu210093 China Institute for Nonperturbative Physics Nanjing University Nanjing Jiangsu210093 China Department of Integrated Sciences Center for Advanced Studies in Physics Mathematics and Computation University of Huelva HuelvaE-21071 Spain Istituto Nazionale di Fisica Nucleare Sezione di Roma P.le A. Moro 2 RomeI-00185 Italy Departamento de Sistemas Físicos Químicos y Naturales Universidad Pablo de Olavide SevillaE-41013 Spain Department of Physics Illinois Institute of Technology ChicagoIL60616 United States North Carolina State University RaleighNC27607 United States

How the bulk of the Universe’s visible mass emerges and how it is manifest in the existence and properties of hadrons are profound questions that probe into the heart of strongly interacting matter. Paradoxically, the lightest pseudoscalar mesons appear to be the key to the further understanding of the emergent mass and structure mechanisms. These mesons, namely the pion and kaon, are the Nambu-Goldstone boson modes of QCD. Unravelling their partonic structure and the interplay between emergent and Higgs-boson mass mechanisms is a common goal of three interdependent approaches – continuum QCD phenomenology, lattice-regularised QCD, and the global analysis of parton distributions – linked to experimental measurements of hadron structure. Experimentally, the foreseen electron-ion collider will enable a revolution in our ability to study pion and kaon structure, accessed by scattering from the "meson cloud" of the proton through the Sullivan process. With the goal of enabling a suite of measurements that can address these questions, we examine key reactions to identify the critical detector system requirements needed to map tagged pion and kaon cross sections over a wide range of kinematics. The excellent prospects for extracting pion structure function and form factor data are shown, and similar prospects for kaon structure are discussed in the context of a worldwide programme. Successful completion of the programme outlined herein will deliver deep, far-reaching insights into the emergence of pions and kaons, their properties, and their role as QCD’s Goldstone boson modes. Copyright © 2021, The Authors. All rights reserved.

关键词： Hadrons

Early Planet Formation in Embedded Disks (eDisk). IX. High-resolution ALMA Observations of the Class 0 Protostar R CrA IRS5N and Its Surroundings

学校读者我要写书评

暂无评论

Astrophysical Journal 2023年第1期954卷 69-69页

作者： Sharma, Rajeeb Jørgensen, Jes K. Gavino, Sacha Ohashi, Nagayoshi Tobin, John J. Lin, Zhe-Yu Daniel Li, Zhi-Yun Takakuwa, Shigehisa Lee, Chang Won Sai Kwon, Woojin De Gregorio-Monsalvo, Itziar Santamaria-Miranda, Alejandro Yen, Hsi-Wei Aikawa, Yuri Aso, Yusuke Lai, Shih-Ping Lee, Jeong-Eun Looney, Leslie W. Phuong, Nguyen Thi Thieme, Travis J. Williams, Jonathan P. Niels Bohr Institute University of Copenhagen Øster Voldgade 5-7 Copenhagen K DK-1350 Denmark Academia Sinica Institute of Astronomy& Astrophysics 11F of Astronomy-Mathematics Building AS/NTU No.1 Sec. 4 Roosevelt Rd Taipei 10617 Taiwan National Radio Astronomy Observatory 520 Edgemont Rd. Charlottesville 22903 VA United States University of Virginia 530 McCormick Rd. Charlottesville 22903 VA United States Department of Physics and Astronomy Graduate School of Science and Engineering Kagoshima University Kagoshima 1-21-35 Korimoto Kagoshima 890-0065 Japan Korea Astronomy and Space Science Institute 776 Daedeok-daero Yuseong-gu Daejeon 34055 South Korea University of Science and Technology 217 Gajeong-ro Yuseong-gu Daejeon 34113 South Korea Department of Earth Science Education Seoul National University 1 Gwanak-ro Gwanak-gu Seoul 08826 South Korea SNU Astronomy Research Center Seoul National University 1 Gwanak-ro Gwanak-gu Seoul 08826 South Korea European Southern Observatory Alonso de Cordova 3107 Casilla 19 Vitacura Santiago Chile Department of Astronomy Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo 113-0033 Japan Institute of Astronomy National Tsing Hua University No. 101 Sec. 2 Kuang-Fu Rd. Hsinchu 30013 Taiwan Center for Informatics and Computation in Astronomy National Tsing Hua University No. 101 Sec. 2 Kuang-Fu Rd. Hsinchu 30013 Taiwan Department of Physics National Tsing Hua University No. 101 Sec. 2 Kuang-Fu Rd. Hsinchu 30013 Taiwan Department of Physics and Astronomy Seoul National University 1 Gwanak-ro Gwanak-gu Seoul 08826 South Korea Department of Astronomy University of Illinois 1002 West Green St. Urbana 61801 IL United States Department of Astrophysics Vietnam National Space Center Vietnam Academy of Science and Techonology 18 Hoang Quoc Viet Cau Giay Hanoi Viet Nam Institute for Astronomy University of Hawai'i at Mānoa 2680 Woodlawn Dr. Honolulu 96822 HI

We present high-resolution high-sensitivity observations of the Class 0 protostar RCrA IRS5N as part of the Atacama Large Milimeter/submilimeter Array large program Early Planet Formation in Embedded Disks. The 1.3 mm continuum emission reveals a flattened continuum structure around IRS5N, consistent with a protostellar disk in the early phases of evolution. The continuum emission appears smooth and shows no substructures. However, a brightness asymmetry is observed along the minor axis of the disk, suggesting that the disk is optically and geometrically thick. We estimate the disk mass to be between 0.007 and 0.02 M ⊙. Furthermore, molecular emission has been detected from various species, including C18O (2-1), 12CO (2-1), 13CO (2-1), and H2CO (30,3 - 20,2, 32,1 - 22,0, and 32,2 - 22,1). By conducting a position-velocity analysis of the C18O (2-1) emission, we find that the disk of IRS5N exhibits characteristics consistent with Keplerian rotation around a central protostar with a mass of approximately 0.3 M ⊙. Additionally, we observe dust continuum emission from the nearby binary source IRS5a/b. The emission in 12CO toward IRS5a/b seems to emanate from IRS5b and flow into IRS5a, suggesting material transport between their mutual orbits. The lack of a detected outflow and large-scale negatives in 12CO observed toward IRS5N suggests that much of the flux from IRS5N is being resolved out. Using a 1D radiative transfer model, we infer the mass of the envelope surrounding IRS5N to be 1/41.2 M ⊙. Due to this substantial surrounding envelope, the central IRS5N protostar is expected to be significantly more massive in the future. © 2023. The Author(s). Published by the American Astronomical Society.

关键词：