Plasma Physics of the Local Cosmos
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Dermining the Photon Budget of Galaxies During Reionization with Numerical Simulations, and Studying the Impact of Dust Joseph Lewis
Who reionized the Universe ? : dermining the photon budget of galaxies during reionization with numerical simulations, and studying the impact of dust Joseph Lewis To cite this version: Joseph Lewis. Who reionized the Universe ? : dermining the photon budget of galaxies during reioniza- tion with numerical simulations, and studying the impact of dust. Astrophysics [astro-ph]. Université de Strasbourg, 2020. English. NNT : 2020STRAE041. tel-03199136 HAL Id: tel-03199136 https://tel.archives-ouvertes.fr/tel-03199136 Submitted on 15 Apr 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. UNIVERSITÉ DE STRASBOURG ÉCOLE DOCTORALE 182 UMR 7550, Observatoire astronomique de Strasbourg THÈSE présentée par : Joseph Lewis soutenue le : 25 septembre 2020 pour obtenir le grade de : Docteur de l’université de Strasbourg Discipline/ Spécialité : Astrophysique Qui a réionisé l’Univers ? Détermination par la simulation numérique du budget de photons des galaxies pendant l’époque de la Réionisation, et étude de l’impact des poussières THÈSE dirigée par : M. AUBERT Dominique Professeur des universités, Université de Strasbourg RAPPORTEURS : M. GONZALES Mathias Maître de conférences, Université de Paris M. LANGER Mathieu Professeur des universités, Université Paris-Saclay AUTRES MEMBRES DU JURY : M. -
Executive Summary
The Boston University Astronomy Department Annual Report 2010 Chair: James Jackson Administrator: Laura Wipf 1 2 TABLE OF CONTENTS Executive Summary 5 Faculty and Staff 5 Teaching 6 Undergraduate Programs 6 Observatory and Facilities 8 Graduate Program 9 Colloquium Series 10 Alumni Affairs/Public Outreach 10 Research 11 Funding 12 Future Plans/Departmental Needs 13 APPENDIX A: Faculty, Staff, and Graduate Students 16 APPENDIX B: 2009/2010 Astronomy Graduates 18 APPENDIX C: Seminar Series 19 APPENDIX D: Sponsored Project Funding 21 APPENDIX E: Accounts Income Expenditures 25 APPENDIX F: Publications 27 Cover photo: An ultraviolet image of Saturn taken by Prof. John Clarke and his group using the Hubble Space Telescope. The oval ribbons toward the top and bottom of the image shows the location of auroral activity near Saturn’s poles. This activity is analogous to Earth’s aurora borealis and aurora australis, the so-called “northern” and “southern lights,” and is caused by energetic particles from the sun trapped in Saturn’s magnetic field. 3 4 EXECUTIVE SUMMARY associates authored or co-authored a total of 204 refereed, scholarly papers in the disciplines’ most The Department of Astronomy teaches science to prestigious journals. hundreds of non-science majors from throughout the university, and runs one of the largest astronomy degree The funding of the Astronomy Department, the Center programs in the country. Research within the for Space Physics, and the Institute for Astrophysical Astronomy Department is thriving, and we retain our Research was changed this past year. In previous years, strong commitment to teaching and service. only the research centers received research funding, but last year the Department received a portion of this The Department graduated a class of twelve research funding based on grant activity by its faculty. -
Space Weather — History and Current Status
Space Weather — History and Current Status Ji Wu National Space Science Center, CAS Oct. 3, 2017 1 Contents 1. Beginning of Space Age and Dangerous Environment 2. The Dynamic Space Environment so far We Know 3. The Space Weather Concept and Current Programs 4. Looking at the Future Space Weather Programs 2 1.Beginning of Space Age and Dangerous Environment 3 Space Age Kai'erdishi Korolev Oct. 4, 1957, humanity‘s first artificial satellite, Sputnik-1, has launched, ushering in the Space Age. 4 Space Age Explorer 1 was the first satellite of the United States, launched on Jan 31, 1958, with scientific object to explore the radiation environment of geospace. 5 Unknown Space Environment Sputnik-2 (Nov 3, 1957) detected the Earth's outer radiation belt in the far northern latitudes, but researchers did not immediately realize the significance of the elevated radiation because Sputnik 2 passed through the Van Allen belt too far out of range of the Soviet tracking stations. Explorer-1 detected fewer cosmic rays in its orbit (which ranged from 220 miles from Earth to 1,563 miles) than Van Allen expected. 6 Space Age - unknown and dangerous space environment 7 Satellite failures due to the unknown and Particle dangerous space environment Radiation! Statistics show that the space radiation environment is one of the main causes of satellite failure. The space radiation environment caused about 2,300 satellite failures of all the 5000 failure events during the 1966-1994 period collected by the National Geophysical Data Center. Statistics of the United States in 1996 indicate that the space environment caused more than 40% of satellite failures in 1958-1986, and 36% in 1986-1996. -
PANDORA a New Facility for Interdisciplinary In-Plasma Physics
EPJ manuscript No. (will be inserted by the editor) PANDORA a New Facility for Interdisciplinary In-Plasma Physics D. Mascali1, A. Musumarra1,2a, F. Leone1,2,4, F.P. Romano1,3, A. Galat´a5, S. Gammino1, and C. Massimi6,7 1 INFN-Laboratori Nazionali del Sud, I-95123 Catania, Italy 2 Department of Physics and Astronomy University of Catania, I-95123 Catania, Italy 3 CNR-IBAM, I-95124 Catania, Italy 4 INAF-OACT, I-95123 Catania, Italy 5 INFN-Laboratori Nazionali di Legnaro, Legnaro I-35020, Italy 6 Department of Physics and Astronomy University of Bologna, I-40126 Bologna, Italy 7 INFN-Bologna, I-40126 Bologna, Italy Received: date / Revised version: date Abstract. PANDORA, Plasmas for Astrophysics, Nuclear Decays Observation and Radiation for Ar- chaeometry, is planned as a groundbreaking new facility based on a state-of-the-art plasma trap confining extremely energetic plasma for performing interdisciplinary research in thefields of Nuclear Astrophysics, Astrophysics, Plasma Physics and Applications in Material Science and Archaeometry: the plasmas become the environment for measuring, for thefirst time, nuclear decays rates in stellar-like condition (such as 7Be decay and beta-decay involved in s-process nucleosynthesis), especially as a function of the ionization state of the plasma ions. These studies are of paramount importance for addressing several astrophysical issues in both stellar and primordial nucleosynthesis environment (e.g. determination of solar neutrino flux and 7Li Cosmological Problem), moreover the confined energetic plasma will be a unique light source for high performance stellar spectroscopy measurements in the visible, UV and X-ray domains, offering advancements in observational astronomy. -
A Case for Electron-Astrophysics
1. Core Proposing Team A Case for Electron-Astrophysics WHITE PAPER FOR THE VOYAGE 2050 LONG-TERM PLAN IN THE ESA SCIENCE PROGRAMME Contact Scientist: Daniel Verscharen Mullard Space Science Laboratory Department of Space and Climate Physics University College London Holmbury St Mary Dorking RH5 6NT United Kingdom E-Mail: [email protected] Telephone: +44 1483 20-4951 Voyage 2050 White Paper: A Case for Electron-Astrophysics 1 Core Proposing Team Contact Scientist: Daniel Verscharen (University College London, United Kingdom) Deputy: Robert T. Wicks (University College London, United Kingdom) Olga Alexandrova (Observatoire de Paris, France) Roberto Bruno (INAF, Italy) David Burgess (Queen Mary University of London, United Kingdom) Christopher H. K. Chen (Queen Mary University of London, United Kingdom) Raffaella D’Amicis (INAF, Italy) Johan De Keyser (BIRA-IASB, Belgium) Thierry Dudok de Wit (LPC2E, France) Luca Franci (Queen Mary University of London, United Kingdom) Jiansen He (Peking University, China) Pierre Henri (LPC2E, CNRS, France) Satoshi Kasahara (University of Tokyo, Japan) Yuri Khotyaintsev (Institutet för Rymdfysik, Sweden) Kristopher G. Klein (University of Arizona, United States) Benoit Lavraud (Institut de Recherche en Astrophysique et Planétologie, France) Bennett A. Maruca (University of Delaware, United States) Milan Maksimovic (Observatoire de Paris, France) Ferdinand Plaschke (Institute for Space Research, Austria) Stefaan Poedts (KU Leuven, Belgium) Christopher S. Reynolds (University of Cambridge, United Kingdom) Owen Roberts (Institute for Space Research, Austria) Fouad Sahraoui (Laboratoire de Physique des Plasmas, France) Shinji Saito (Nagoya University, Japan) Chadi S. Salem (Space Sciences Laboratory, UC Berkeley, United States) Joachim Saur (University of Cologne, Germany) Sergio Servidio (University of Calabria, Italy) Julia E. -
Supernova Remnant N103B, Radio Pulsar B1951+32, and the Rabbit
On Understanding the Lives of Dead Stars: Supernova Remnant N103B, Radio Pulsar B1951+32, and the Rabbit by Joshua Marc Migliazzo Bachelor of Science, Physics (2001) University of Texas at Austin Submitted to the Department of Physics in partial fulfillment of the requirements for the degree of Master of Science in Physics at the MASSACHUSETTS INSTITUTE OF TECHNOLOGY February 2003 c Joshua Marc Migliazzo, MMIII. All rights reserved. The author hereby grants to MIT permission to reproduce and distribute publicly paper and electronic copies of this thesis document in whole or in part. Author.............................................................. Department of Physics January 17, 2003 Certifiedby.......................................................... Claude R. Canizares Associate Provost and Bruno Rossi Professor of Physics Thesis Supervisor Accepted by . ..................................................... Thomas J. Greytak Chairman, Department Committee on Graduate Students 2 On Understanding the Lives of Dead Stars: Supernova Remnant N103B, Radio Pulsar B1951+32, and the Rabbit by Joshua Marc Migliazzo Submitted to the Department of Physics on January 17, 2003, in partial fulfillment of the requirements for the degree of Master of Science in Physics Abstract Using the Chandra High Energy Transmission Grating Spectrometer, we observed the young Supernova Remnant N103B in the Large Magellanic Cloud as part of the Guaranteed Time Observation program. N103B has a small overall extent and shows substructure on arcsecond spatial scales. The spectrum, based on 116 ks of data, reveals unambiguous Mg, Ne, and O emission lines. Due to the elemental abundances, we are able to tentatively reject suggestions that N103B arose from a Type Ia supernova, in favor of the massive progenitor, core-collapse hypothesis indicated by earlier radio and optical studies, and by some recent X-ray results. -
Turbulence and Magnetic Fields in Astrophysical Plasmas
Magnetohydrodynamics — Historical Evolution and Trends S. Molokov, R. Moreau and H. K. Moffatt, Eds. (Berlin: Springer 2007) pp. 85–115 [E-print: astro-ph/0507686] Turbulence and Magnetic Fields in Astrophysical Plasmas Alexander A Schekochihin1 and Steven C Cowley2 1 DAMTP, University of Cambridge, Cambridge CB3 0WA and Department of Physics, Imperial College, London SW7 2BW, United Kingdom ([email protected]) 2 Department of Physics and Astronomy, UCLA, Los Angeles, CA 90095-1547, USA and Department of Physics, Imperial College, London SW7 2BW, United Kingdom ([email protected]) 1 Introduction Magnetic fields permeate the Universe. They are found in planets, stars, accre- tion discs, galaxies, clusters of galaxies, and the intergalactic medium. While there is often a component of the field that is spatially coherent at the scale of the astrophysical object, the field lines are tangled chaotically and there are magnetic fluctuations at scales that range over orders of magnitude. The cause of this disorder is the turbulent state of the plasma in these systems. This plasma is, as a rule, highly conducting, so the magnetic field lines are en- trained by (frozen into) the fluid motion. As the fields are stretched and bent by the turbulence, they can resist deformation by exerting the Lorentz force on the plasma. The turbulent advection of the magnetic field and the field’s back reaction together give rise to the statistically steady state of fully devel- oped MHD turbulence. In this state, energy and momentum injected at large (object-size) scales are transfered to smaller scales and eventually dissipated. -
Astrophysical Plasma Modeling of the Hot Universe : Advances and Challenges in High-Resolution X-Ray Spectroscopy Date: 2018-06-07 Summary
Cover Page The handle http://hdl.handle.net/1887/62735 holds various files of this Leiden University dissertation Author: Mao, Junjie Title: Astrophysical plasma modeling of the hot Universe : advances and challenges in high-resolution X-ray spectroscopy Date: 2018-06-07 Summary Hot astrophysical plasma is ubiquitous in the Universe, from comets in our Solar system to the largest scale structures – the cosmic web filaments. These hot plas- mas, with temperatures of a few million of degrees, are often observed in the X-ray wavelength range. Spectroscopic diagnostics enable us to probe physical prop- erties like temperature, density, abundance, microscopic turbulence, line of sight velocity, etc. High spectral resolving power is essential to overcome the confu- sion caused by unresolved spectral features. Thanks to the grating spectrometers aboard XMM-Newton and Chandra, our knowledge of the hot and energetic Uni- verse is advanced. On the other hand, high quality spectra from current and future generations of X-ray spectrometers also challenge plasma models that are widely used in the community. Plasma model To interpret the spectra in a self-consistent way, we need plasma models built on an extensive atomic database. Different plasma models suitable for different astro- physical scenarios are required. For instance, plasmas exposed to a strong external radiation field (e.g. circumnuclear media of active galactic nuclei) require a plasma model in photoionization equilibrium, while low-density high-temperature thermal plasmas (e.g. intracluster media of relaxed galaxy clusters) require a plasma model in collisional ionization equilibrium. In this thesis, we use the SPEX package. SPEX is a software package optimized for the analysis and interpretation of high-resolution cosmic X-ray spectra. -
Space Weather ± Physics and Effects Volker Bothmer and Ioannis A
Space Weather ± Physics and Effects Volker Bothmer and Ioannis A. Daglis Space Weather ± Physics and Effects Published in association with Praxis Publishing Chichester, UK Dr Volker Bothmer Dr Ioannis A. Daglis Institute for Astrophysics National Observatory of Athens University of GoÈttingen Athens GoÈ ttingen Greece Germany SPRINGER±PRAXIS BOOKS IN ENVIRONMENTAL SCIENCES SUBJECT ADVISORY EDITOR: John Mason B.Sc., M.Sc., Ph.D. ISBN 10: 3-540-23907-3 Springer-Verlag Berlin Heidelberg New York ISBN 13: 978-3-540-23907-9 Springer-Verlag Berlin Heidelberg New York Springer is part of Springer-Science + Business Media (springer.com) Bibliographic information published by Die Deutsche Bibliothek Die Deutsche Bibliothek lists this publication in the Deutsche Nationalbibliogra®e; detailed bibliographic data are available from the Internet at http://dnb.ddb.de Library of Congress Control Number: 2006921904 Apart from any fair dealing for the purposes of research or private study, or criticism or review, as permitted under the Copyright, Designs and Patents Act 1988, this publication may only be reproduced, stored or transmitted, in any form or by any means, with the prior permission in writing of the publishers, or in the case of reprographic reproduction in accordance with the terms of licences issued by the Copyright Licensing Agency. Enquiries concerning reproduction outside those terms should be sent to the publishers. # Praxis Publishing Ltd, Chichester, UK, 2007 Printed in Germany The use of general descriptive names, registered names, trademarks, etc. in this publication does not imply, even in the absence of a speci®c statement, that such names are exempt from the relevant protective laws and regulations and therefore free for general use. -
NASA Living with a Star TR&T Town Hall Renaissance Washington, DC
NASA Living With a Star TR&T Town Hall Renaissance Washington, DC Downtown 13 December, 2018 LWS Town Hall Agenda Item Time Agenda Item Presenter 1 6:30 PM Welcome Nicky Fox 2 6:35 PM LPAG Status Anthea Coster / Mark Linton 3 6:55 PM LWS Program Status Jeff Morrill / Simon Plunkett 4 7:15 PM Multi-Agency Collaborations & Space Janet Kozyra Weather Activities 5 7:30 PM GDC STDT Status Jared Leisner 6 7:45 PM LWS Infrastructure & New Initiatives Lika Guhathakurtha 7 8:00 PM ADJOURN 2 LWS Town Hall Agenda Item Time Agenda Item Presenter 1 6:30 PM Welcome Nicky Fox 2 6:35 PM LPAG Status Anthea Coster / Mark Linton 3 6:55 PM LWS Program Status Jeff Morrill / Simon Plunkett 4 7:15 PM Multi-Agency Collaborations & Space Janet Kozyra Weather Activities 5 7:30 PM GDC STDT Status Jared Leisner 6 7:45 PM LWS Infrastructure & New Initiatives Lika Guhathakurtha 7 8:00 PM ADJOURN 3 NASA Living with a Star Program Analysis Group (LPAG) Executive Committee (EC) Co-Chairs: • Anthea Coster (MIT Haystack Observatory) • Mark Linton (Naval Research Laboratory, NRL) EC Members: • Joe Borovsky (Space Science Institute) • Richard Collins (University of Alaska) • Seebany Datta-Barua (Illinois Institute of Technology) • Matina Gkioulidou (JHU / APL) • Fan Guo (Los Alamos National Laboratory) • Jorg-Micha Jahn (Southwest Research Institute) • Enrico Landi (University of Michigan) • John Leibacher (National Solar Observatory) • Sabrina Savage (NASA / MSFC) • Brian Walsh (Boston University) See website at https://lwstrt.gsfc.nasa.gov/lpag 4 Living with a Star LPAG, continued Liaison Members: Charles N. -
NASA's Office of Space Science and Applications: Process, Priorities and Goals
NASA's Office of Space Science and Applications: Process, Priorities and Goals January 1992 NTIS order #PB92-152503 Office of Technology Assessment Congressional Board of the 102d Congress GEORGE E. BROWN, JR., California, Chairman TED STEVENS, Alaska, Vice Chairman Senate House EDWARD M. KENNEDY JOHN 0. DINGELL Massachusetts Michigan ERNEST F. HOLLINGS CLARENCE E. MILLER South Carolina Ohio CLAIBORNE PELL DON SUNDQUIST Rhode Island Tennessee ORRIN G. HATCH AMO HOUGHTON Utah New York CHARLES E. GRASSLEY (Vacancy) Iowa JOHN H. GIBB0NS (Nonvoting) Advisory Council CHASE N. PETERSON, Chairman MICHEL T. HALBOUTY MAX LENNON University of Utah Chairman of the Board & President Salt Lake City, Utah Chief Executive Officer Clemson University Michel T Halbouty Energy Co. Clemson, South Carolina Houston, Texas JOSHUA LEDERBERG, Vice Chairman - NEIL E. HARL JOSEPH E. ROSS Professor Professor Director Rockefeller University Department of Economics Congressional Research Service New York, New York Iowa State University The Library of Congress Ames,. Iowa Washington, D.C. CHARLES A. BOWSHER JAMES C. HUNT JOHN F.M. SIMS Comptroller General of Chancellor Vice President Marketing the United States Health Sciences Center Usibelli Coal Mine, Inc. Washington, D.C. University of Tennessee Fairbanks, Alaska Memphis, Tennessee LEWIS M. BRANSCOMB HENRY KOFFLER MARINA v.N. WHITMAN Director of Science, Technology & President Emeritus Vice President & Group Executive Public Policy Program University of Arizona Public Affairs Staffs Group Albert Pratt Public Service -
Outstanding Problems in Astrophysical Plasmas and Magnetic Fields on All Scales
Outstanding Problems in Astrophysical Plasmas and Magnetic Fields on all Scales 21#September#2015# Plasma#Fest# The baryonic universe consists almost entirely of plasmas ! ! stellar (solar) atmospheres ! supernova remnants ! stellar interiors ! intergalactic medium ! pre-recombination universe ! pulsar wind nebulae (< 380,000 years ABB) ! ! post-reionization universe astrophysical jets ! ! HII regions cosmic rays ! ! stellar (solar) winds coronal gas ! ! accretion disks around synchrotron nebulae compact objects ! relativistic shocks The baryonic universe consists almost entirely of plasmas ! ! stellar (solar) atmospheres ! supernova remnants ! stellar interiors ! intergalactic medium ! pre-recombination universe ! pulsar wind nebulae (< 380,000 years ABB) ! astrophysical jets ! post-reionization universe ! cosmic rays ! HII regions ! coronal gas ! stellar (solar) winds ! synchrotron nebulae ! accretion disks around compact objects ! relativistic shocks " Even neutral gas clouds have a plasma description because of residual ionization and the coupling between ions and neutrals Research on astrophysical plasmas very closely coupled to research on magnetic felds • jets, fares, loops, flaments " all organized or generated by magnetic felds • magnetosphere-wind and magnetosphere-accretion- fow interactions • disk evolution " magnetic feld fosters angular momentum transport via magnetic tension and MHD instabilities that generate turbulent viscosity. • modern star formation theories all include magnetic braking mechanisms to facilitate accretion.