Theoretical Physics Research
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Optimizing Tracking Software for a Time Projection Chamber Wilson H
Journal of the Arkansas Academy of Science Volume 49 Article 18 1995 Optimizing Tracking Software for a Time Projection Chamber Wilson H. Howe University of Arkansas at Little Rock Christine A. Byrd University of Arkansas at Little Rock Amber D. Climer University of Arkansas at Little Rock Wilfred J. Braithwaite University of Arkansas at Little Rock Jeffrey T. Mitchell Brookhaven National Laboratory Follow this and additional works at: http://scholarworks.uark.edu/jaas Part of the Nuclear Commons Recommended Citation Howe, Wilson H.; Byrd, Christine A.; Climer, Amber D.; Braithwaite, Wilfred J.; and Mitchell, Jeffrey T. (1995) "Optimizing Tracking Software for a Time Projection Chamber," Journal of the Arkansas Academy of Science: Vol. 49 , Article 18. Available at: http://scholarworks.uark.edu/jaas/vol49/iss1/18 This article is available for use under the Creative Commons license: Attribution-NoDerivatives 4.0 International (CC BY-ND 4.0). Users are able to read, download, copy, print, distribute, search, link to the full texts of these articles, or use them for any other lawful purpose, without asking prior permission from the publisher or the author. This Article is brought to you for free and open access by ScholarWorks@UARK. It has been accepted for inclusion in Journal of the Arkansas Academy of Science by an authorized editor of ScholarWorks@UARK. For more information, please contact [email protected], [email protected]. Journal of the Arkansas Academy of Science, Vol. 49 [1995], Art. 18 a Time Projection Chamber Wilson H. Howe, Christine A.Byrd, Amber D. Climer, W.J. Braithwaite Department of Physics and Astronomy University of Arkansas at Little Rock LittleRock, Ar 72204 Jeffrey T.Mitchell Brookhaven National Laboratory Upton, NY11973 Abstract International research collaborations willbe using accelerators in the U.S. -
Development of a Liquid Xenon Time Projection Chamber for the XENON Dark Matter Search
Development of a Liquid Xenon Time Projection Chamber for the XENON Dark Matter Search Kaixuan Ni Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Graduate School of Arts and Sciences COLUMBIA UNIVERSITY 2006 c 2006 Kaixuan Ni All rights reserved Development of a Liquid Xenon Time Projection Chamber for the XENON Dark Matter Search Kaixuan Ni Advisor: Professor Elena Aprile Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Graduate School of Arts and Sciences COLUMBIA UNIVERSITY 2006 c 2006 Kaixuan Ni All rights reserved ABSTRACT Development of a Liquid Xenon Time Projection Chamber for the XENON Dark Matter Search Kaixuan Ni This thesis describes the research conducted for the XENON dark matter direct detection experiment. The tiny energy and small cross-section, from the interaction of dark matter particle on the target, requires a low threshold and sufficient background rejection capability of the detector. The XENON experiment uses dual phase technology to detect scintillation and ionization simultaneously from an event in liquid xenon (LXe). The distinct ratio, be- tween scintillation and ionization, for nuclear recoil and electron recoil events provides excellent background rejection potential. The XENON detector is designed to have 3D position sensitivity down to mm scale, which provides additional event information for background rejection. Started in 2002, the XENON project made steady progress in the R&D phase during the past few years. Those include developing sensitive photon detectors in LXe, improving the energy resolution and LXe purity for detect- ing very low energy events. -
Using a Two-Phase Xenon Time Projection Chamber for Improved Background Rejection in Searches for Neutrinoless Double-Beta Decay
Using a two-phase xenon time projection chamber for improved background rejection in searches for neutrinoless double-beta decay by Callan Jessiman A thesis submitted to the Faculty of Graduate and Postdoctoral Affairs in partial fulfilment of the requirements for the degree of Master of Science in Physics Department of Physics Carleton University Ottawa, Ontario January 2020 c 2020 Callan⃝ Jessiman Abstract The nature of the neutrino masses is an important open question in particle physics; neutrinos were conceived and implemented into the Standard Model as massless, and their masses, now known to be nonzero, represent an area of new physics. Essential to the investigation of this area are mechanisms by which one might measure these masses, including the hypothetical neutrinoless double-beta decay, which has a lifetime related to the neutrino masses. Experiments searching for this rare decay, such as EXO, are impacted heavily by sources of background radiation. Here, a prototype two-phase time projection chamber is described, having superior temporal resolution to the existing EXO architecture. A machine- learning analysis of data from this prototype is used for pulse-shape discrimination, which has the potential to significantly increase EXO's sensitivity; the preliminary efforts described here are able to reduce backgrounds by 94%, while rejecting only 21% of the signal. ii Acknowledgements First, and foremost, I express my gratitude towards my supervisor, David Sinclair, and my colleague Braeden Veenstra. The entire project was of David's devising, as was the leadership that saw it through. Meanwhile, getting the thing to actually work, and extracting results from it, was Braeden's task as much as it was mine. -
Open Batalha-Dissertation.Pdf
The Pennsylvania State University The Graduate School Eberly College of Science A SYNERGISTIC APPROACH TO INTERPRETING PLANETARY ATMOSPHERES A Dissertation in Astronomy and Astrophysics by Natasha E. Batalha © 2017 Natasha E. Batalha Submitted in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy August 2017 The dissertation of Natasha E. Batalha was reviewed and approved∗ by the following: Steinn Sigurdsson Professor of Astronomy and Astrophysics Dissertation Co-Advisor, Co-Chair of Committee James Kasting Professor of Geosciences Dissertation Co-Advisor, Co-Chair of Committee Jason Wright Professor of Astronomy and Astrophysics Eric Ford Professor of Astronomy and Astrophysics Chris Forest Professor of Meteorology Avi Mandell NASA Goddard Space Flight Center, Research Scientist Special Signatory Michael Eracleous Professor of Astronomy and Astrophysics Graduate Program Chair ∗Signatures are on file in the Graduate School. ii Abstract We will soon have the technological capability to measure the atmospheric compo- sition of temperate Earth-sized planets orbiting nearby stars. Interpreting these atmospheric signals poses a new challenge to planetary science. In contrast to jovian-like atmospheres, whose bulk compositions consist of hydrogen and helium, terrestrial planet atmospheres are likely comprised of high mean molecular weight secondary atmospheres, which have gone through a high degree of evolution. For example, present-day Mars has a frozen surface with a thin tenuous atmosphere, but 4 billion years ago it may have been warmed by a thick greenhouse atmosphere. Several processes contribute to a planet’s atmospheric evolution: stellar evolution, geological processes, atmospheric escape, biology, etc. Each of these individual processes affects the planetary system as a whole and therefore they all must be considered in the modeling of terrestrial planets. -
SAS-2019 the Symposium on Telescope Science
Proceedings for the 38th Annual Conference of the Society for Astronomical Sciences SAS-2019 The Symposium on Telescope Science Joint Meeting with the Center for Backyard Astrophysics Editors: Robert K. Buchheim Robert M. Gill Wayne Green John C. Martin John Menke Robert Stephens May, 2019 Ontario, CA i Disclaimer The acceptance of a paper for the SAS Proceedings does not imply nor should it be inferred as an endorsement by the Society for Astronomical Sciences of any product, service, method, or results mentioned in the paper. The opinions expressed are those of the authors and may not reflect those of the Society for Astronomical Sciences, its members, or symposium Sponsors Published by the Society for Astronomical Sciences, Inc. Rancho Cucamonga, CA First printing: May 2019 Photo Credits: Front Cover: NGC 2024 (Flame Nebula) and B33 (Horsehead Nebula) Alson Wong, Center for Solar System Studies Back Cover: SA-200 Grism spectrum of Wolf-Rayet star HD214419 Forrest Sims, Desert Celestial Observatory ii TABLE OF CONTENTS PREFACE v SYMPOSIUM SPONSORS vi SYMPOSIUM SCHEDULE viii PRESENTATION PAPERS Robert D. Stephens, Brian D. Warner THE SEARCH FOR VERY WIDE BINARY ASTEROIDS 1 Tom Polakis LESSONS LEARNED DURING THREE YEARS OF ASTEROID PHOTOMETRY 7 David Boyd SUDDEN CHANGE IN THE ORBITAL PERIOD OF HS 2325+8205 15 Tom Kaye EXOPLANET DETECTION USING BRUTE FORCE TECHNIQUES 21 Joe Patterson, et al FORTY YEARS OF AM CANUM VENATICORIUM 25 Robert Denny ASCOM – NOT JUST FOR WINDOWS ANY MORE 31 Kalee Tock HIGH ALTITUDE BALLOONING 33 William Rust MINIMIZING DISTORTION IN TIME EXPOSED CELESTIAL IMAGES 43 James Synge PROJECT PANOPTES 49 Steve Conard, et al THE USE OF FIXED OBSERVATORIES FOR FAINT HIGH VALUE OCCULTATIONS 51 John Martin, Logan Kimball UPDATE ON THE M31 AND M33 LUMINOUS STARS SURVEY 53 John Morris CURRENT STATUS OF “VISUAL” COMET PHOTOMETRY 55 Joe Patterson, et al ASASSN-18EY = MAXIJ1820+070 = “MAXIE”: KING OF THE BLACK HOLE 61 SUPERHUMPS Richard Berry IMAGING THE MOON AT THERMAL INFRARED WAVELENGTHS 67 iii Jerrold L. -
SCIENCE and SUSTAINABILITY Impacts of Scientific Knowledge and Technology on Human Society and Its Environment
EM AD IA C S A C I A E PONTIFICIAE ACADEMIAE SCIENTIARVM ACTA 24 I N C T I I F A I R T V N Edited by Werner Arber M O P Joachim von Braun Marcelo Sánchez Sorondo SCIENCE and SUSTAINABILITY Impacts of Scientific Knowledge and Technology on Human Society and Its Environment Plenary Session | 25-29 November 2016 Casina Pio IV | Vatican City LIBRERIA EDITRICE VATICANA VATICAN CITY 2020 Science and Sustainability. Impacts of Scientific Knowledge and Technology on Human Society and its Environment Pontificiae Academiae Scientiarvm Acta 24 The Proceedings of the Plenary Session on Science and Sustainability. Impacts of Scientific Knowledge and Technology on Human Society and its Environment 25-29 November 2016 Edited by Werner Arber Joachim von Braun Marcelo Sánchez Sorondo EX AEDIBVS ACADEMICIS IN CIVITATE VATICANA • MMXX The Pontifical Academy of Sciences Casina Pio IV, 00120 Vatican City Tel: +39 0669883195 • Fax: +39 0669885218 Email: [email protected] • Website: www.pas.va The opinions expressed with absolute freedom during the presentation of the papers of this meeting, although published by the Academy, represent only the points of view of the participants and not those of the Academy. ISBN 978-88-7761-113-0 © Copyright 2020 All rights reserved. No part of this publication may be reproduced, stored in a retrieval system, or transmitted in any form, or by any means, electronic, mechanical, recording, pho- tocopying or otherwise without the expressed written permission of the publisher. PONTIFICIA ACADEMIA SCIENTIARVM LIBRERIA EDITRICE VATICANA VATICAN CITY The climate is a common good, belonging to all and meant for all. -
Parity Non-Conservation in Atoms L.M
INIJ. •®'82 Dl OF THE INTERNATIONAL CONFERENCE '82 14-19 JUNE, 1982 BALATONFURED, HUNGARY EDITORS A. FRENKEL LJENIK BUDAPEST, 1982 III. CONTENTS Volume I ! -4- OPENING ADDRESS NEUTRINO OSCILLATION SEARCH FOR NEUTRINO OSCILLATIONS - A PROGRESS REPORT R. L. Mös sbauer 1 SEARCH FOR NEUTRINO OSCILLATION F. Reines Suppl NEUTRINO OSCILLATION EXPERIMENTS ON AMERICAN ACCELERATORS C. Baltay , Suppl PAST AND FUTURE OSCILLATION EXPERIMENTS IN CERN NEUTRINO BEAMS H. Wachsmuth 13 DETECTION OF MATTER EFFECTS ON NEUTRINO OSCILLATIONS BY DUMAND R.J. Oakes 23 LARGE AMPLITUDE NEUTRINO OSCILLATIONS WITH MAJORANA MASS EIGENSTATES? B. Pontecorvo 35 TRULY NEUTRAL MICROOBJECTS AND OSCILLATIONS IN PARTICLE PHYSICS S.M. Bilenky 42 A POSSIBLE TEST OF CP INVARIANCE IN NEUTRINO OSCILLATIONS S.M. Bilenky 46 *Papers labelled "Suppl" are to be found in the Supplement to this Proceedings. Their titles as given here are provisional. IV. NEUTRINO MASS AN EXPERIMENT TO STUDV THE 3-DECAY OF FREE ATOMIC AND MOLECULAR TRITIUM R.G.H. Robertson 51 MEASUREMENT OF THE MASS OF THE ELECTRON NEUTRINO USING THE ELECTRON CAPTURE DECAY PROCESS OF THE NUCLEUS S. Yasumi 59 AN EXPERIMENT TO DETERMINE THE MASS OF THE ELECTRON ANTINEUTRINO R.N. Boyd 67 DETERMINATION OF AN UPPER LIMIT OF THE MASS OF THE MUONIC NEUTRINO FROM THE PION DECAY IN FLIGHT P. Le Coultre , 75 RADIATIVE DECAYS OF DIRAC AND MAJORANA NEUTRINOS (RECENT RESULTS) S.T. Petcov 82 BEAM DUMP PROMPT NEUTRINO OSCILLATION BY 4OO GeV PROTON INTERACTIONS R. J. Loveless 89 A STUDY OF THE FORWARD PRODUCTION OF CHARM STATES AND PROMPT MUONS IN 350 GeV p-Fe AND 278 GeV n~-Fe INTERACTIONS A. -
Design and Construction of the Spirit Tpc
DESIGN AND CONSTRUCTION OF THE SPIRIT TPC By Suwat Tangwancharoen A DISSERTATION Submitted to Michigan State University in partial fulfillment of the requirements for the degree of Physics-Doctor of Philosophy 2016 ABSTRACT DESIGN AND CONSTRUCTION OF THE SPIRIT TPC By Suwat Tangwancharoen The nuclear symmetry energy, the density dependent term of the nuclear equation of state (EOS), governs important properties of neutron stars and dense nuclear matter. At present, it is largely unconstrained in the supra-saturation density region. This dissertation concerns the design and construction of the SπRIT Time Projection Chamber (SπRIT TPC) at Michigan State University as part of an international collaborations to constrain the symmetry energy at supra-saturation density. The SπRIT TPC has been constructed during the dissertation and transported to Radioactive Isotope Beam Factory (RIBF) at RIKEN, Japan where it will be used in conjunction with the SAMURAI Spectrometer. The detector will measure yield ratios for pions and other light charged particles produced in central collisions of neutron-rich heavy ions such as 132Sn + 124Sn. The dissertation describes the design and solutions to the problem presented by the measurement. This also compares some of the initial fast measurement of the TPC to calculation of the performance characteristics. ACKNOWLEDGMENTS The design and construction of the SAMURAI Pion-Reconstruction and Ion Tracker Time Projection Chamber (SπRIT TPC) involved an international collaboration to study and constrain the symmetry energy term in the nuclear equation of state (EOS) at twice supra- saturation density. The TPC design and construction as well as many additional aspects of the project were supported financially by the U.S. -
Astrophysics New Galactic Wolf-Rayet Stars, and Candidates
UvA-DARE (Digital Academic Repository) New Galactic Wolf-Rayet stars, and candidates (Research note) An annex to The VIIth Catalogue of Galactic Wolf-Rayet Stars van der Hucht, K.A. DOI 10.1051/0004-6361:20065819 Publication date 2006 Document Version Final published version Published in Astronomy & Astrophysics Link to publication Citation for published version (APA): van der Hucht, K. A. (2006). New Galactic Wolf-Rayet stars, and candidates (Research note): An annex to The VIIth Catalogue of Galactic Wolf-Rayet Stars. Astronomy & Astrophysics, 458(2), 453-459. https://doi.org/10.1051/0004-6361:20065819 General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:03 Oct 2021 A&A 458, 453–459 (2006) Astronomy DOI: 10.1051/0004-6361:20065819 & c ESO 2006 Astrophysics New Galactic Wolf-Rayet stars, and candidates (Research Note) An annex to The VIIth Catalogue of Galactic Wolf-Rayet Stars K. -
The Electric Sun Hypothesis
Basics of astrophysics revisited. II. Mass- luminosity- rotation relation for F, A, B, O and WR class stars Edgars Alksnis [email protected] Small volume statistics show, that luminosity of bright stars is proportional to their angular momentums of rotation when certain relation between stellar mass and stellar rotation speed is reached. Cause should be outside of standard stellar model. Concept allows strengthen hypotheses of 1) fast rotation of Wolf-Rayet stars and 2) low mass central black hole of the Milky Way. Keywords: mass-luminosity relation, stellar rotation, Wolf-Rayet stars, stellar angular momentum, Sagittarius A* mass, Sagittarius A* luminosity. In previous work (Alksnis, 2017) we have shown, that in slow rotating stars stellar luminosity is proportional to spin angular momentum of the star. This allows us to see, that there in fact are no stars outside of “main sequence” within stellar classes G, K and M. METHOD We have analyzed possible connection between stellar luminosity and stellar angular momentum in samples of most known F, A, B, O and WR class stars (tables 1-5). Stellar equatorial rotation speed (vsini) was used as main parameter of stellar rotation when possible. Several diverse data for one star were averaged. Zero stellar rotation speed was considered as an error and corresponding star has been not included in sample. RESULTS 2 F class star Relative Relative Luminosity, Relative M*R *eq mass, M radius, L rotation, L R eq HATP-6 1.29 1.46 3.55 2.950 2.28 α UMi B 1.39 1.38 3.90 38.573 26.18 Alpha Fornacis 1.33 -
3 Detector Gas 25 3.1 Gas Properties
DISSERTATION Titel der Dissertation A GEM based Time Projection Chamber prototype for the PANDA¯ experiment - Gas system development and forward tracking studies Verfasser Mag. rer. nat. Philipp Müllner angestrebter akademischer Grad Doktor der Naturwissenschaften (Dr. rer. nat.) Wien, 2012 Studienkennzahl lt. Studienblatt: A 091 411 Dissertationsgebiet lt. Studienblatt: Physik Betreuer: Doz. Dr. Johann Zmeskal 2 Abstract The PANDA¯ collaboration is building a state-of-the-art universal detector for strong interaction studies at the High Energy Storage Ring (HESR) at the new Facility for Antiproton and Ion Research (FAIR) at Darmstadt, Germany. The facility will provide a high intensity, cooled antiproton beam. Together with the advanced particle identification system of the PANDA¯ detector a wide experimental program ranging from QCD studies to funda- mental symmetry tests will be accessible. One of two options for the PANDA¯ central tracker was a Gas Electron Multiplier (GEM) based Time Projection Chamber (TPC). The low ma- terial budget GEM based TPC is an ideal device for 3-dimensional space tracking, which features fulfill the PANDA¯ tracking system requirements, e.g. high rate capability, continuous operation, high momentum resolution, high spatial resolution and full solid coverage. In the course of the detector developments for PANDA,¯ a large GEM- TPC prototype was build and tested at GSI (Darmstadt, Germany) by the GEM-TPC collaboration. Within the framework of this work, an overview of the prototype general design will be given. The main task of my thesis was the development of a closed gas supply system for the large GEM-TPC prototype. The detector requirements made it necessary to build it as closed circulation system with infrastructures for O2 and H2O measurement and purification as well as for precise pressure controlling inside the gas system. -
The Galactic WC and WO Stars the Impact of Revised Distances from Gaia DR2 and Their Role As Massive Black Hole Progenitors
A&A 621, A92 (2019) Astronomy https://doi.org/10.1051/0004-6361/201833712 & c ESO 2019 Astrophysics The Galactic WC and WO stars The impact of revised distances from Gaia DR2 and their role as massive black hole progenitors A. A. C. Sander1,2, W.-R. Hamann1, H. Todt1, R. Hainich1, T. Shenar1,3, V. Ramachandran1, and L. M. Oskinova1 1 Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Str. 24/25, 14476 Potsdam, Germany e-mail: [email protected] 2 Armagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, UK 3 Institute of Astrophysics, KU Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium Received 25 June 2018 / Accepted 26 November 2018 ABSTRACT Wolf-Rayet stars of the carbon sequence (WC stars) are an important cornerstone in the late evolution of massive stars before their core collapse. As core-helium burning, hydrogen-free objects with huge mass-loss, they are likely the last observable stage before collapse and thus promising progenitor candidates for type Ib/c supernovae. Their strong mass-loss furthermore provides challenges and constraints to the theory of radiatively driven winds. Thus, the determination of the WC star parameters is of major importance for several astrophysical fields. With Gaia DR2, for the first time parallaxes for a large sample of Galactic WC stars are available, removing major uncertainties inherent to earlier studies. In this work, we re-examine a previously studied sample of WC stars to derive key properties of the Galactic WC population. All quantities depending on the distance are updated, while the underlying spectral analyzes remain untouched.