Compact Stellar X-Ray Sources Edited by Walter Lewin & Michiel Van Der Klis Frontmatter More Information
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2013 January/February AAS Newsletter 31 January, 2013
2013 January/February AAS Newsletter 31 January, 2013 President's Column David J. Helfand Quest University Canada As I noted in my opening remarks at the 221st meeting of the Society in Long Beach, the state of the AAS — unlike that of the nation — is strong. We ended the year with a small positive balance in the Society's account for the fourth year in a row. Our collection of journals — the highest impact journals in the world in our field — is in even stronger financial shape. Our semiannual conferences exceed expected attendance levels every time we meet, and we are exploiting the Executive Office's outstanding meeting organization resources to support more of our Division Meetings and to launch the Topical Conference Series with three smaller, focused meetings this summer. We will have an expanded public policy presence with the recruitment of Joel Parriott to the fulltime role of Director of Public Policy, and our education and public outreach activities continue to grow in size and impact. This enviable position of strength affords us the opportunity to examine many of the things we do for our members to see if we can do them even better. It also allows us to work on some of the issues in our discipline where we face notable challenges in the research funding trajectory, in facilities access, and with employment/demographic issues. In the months ahead, you will see initiatives in several of these areas. The Employment Committee, chaired by Kelle Cruz, has a new Strategic Plan which promises future benefits for our members. -
Curriculum Vitae Ralph A.M.J. Wijers
Curriculum Vitae Ralph A.M.J. Wijers August 2018 Biographical sketch Ralph Wijers has been professor of high-energy astrophysics at the Uni- versity of Amsterdam since 2002. He specialises in energetic explosions from extreme objects such as black holes and neutron stars and is PI of the AARTFAAC all-sky radio telescope. He got his MSc from Leiden Observatory and his PhD from the University of Amsterdam. He went on to Princeton on a NASA Compton Fellowship and Cambridge on a Royal Society Fellowship, after which he became assistant professor at Stony- brook University. He is a VICI and ERC Advanced Investigator laureate and winner of the 2002 EU Descartes Prize for his discoveries in gamma- ray bursts, with an international team. He teaches enthusiastically from the broad undergraduate level to highly specialised graduate courses, and is actively involved in outreach. Astrid and he have two daughters. He is a member of several national and international scientific governing and advisory councils. Since 2011, he is director of the Anton Pannekoek Institute for Astronomy. Address: Anton Pannekoek Institute for Astronomy Faculty of Science, University of Amsterdam Science Park 904, 1098 XH Amsterdam, The Netherlands. Tel: +31-20-5257488 (self) or 7491 (secr.) Fax: +31-20-5257484 Email: [email protected] Website: www.uva.nl/en/profile/w/i/r.a.m.j.wijers/r.a.m.j.wijers.html ORCID: orcid.org/0000-0002-3101-1808 2 CONTENTS Contents Curriculum Vitae — Major and Summary Facts 3 1 Summary information 3 2 Key papers 7 3 History of key ideas 8 4 Invited talks and colloquia 9 Curriculum Vitae — Complete Listings 11 5 PhD students and postdocs supervised 11 5.1 PhDstudents.................................... -
Livio Scarsi: 40 Years of Astrophysics from Space
Livio Scarsi: 60 years of scientific activity dedicated to Physics, Cosmic Rays and High Energy Astrophysics from Space. (B. Sacco, 6th Intnl Workshop of the “Data Analysis in Astronomy, Livio Scarsi, 15-22 April 2007, Erice, Italy ) The reach scientific career of Livio Scarsi starts at Genoa University, as physics student in the Institute of Augusto Occhialini father of Beppo Occhialini. On 1950’ Livio took the degree in physics discussing a thesis on “ Cosmic Radiation Soft Electromagnetic Component at Pic du Midi : Investigation with nuclear emulsions “ . Tutor : Giuseppe (Beppo) Occhialini . “ During the studies in Genoa he had, also, the opportunity to know Bruno Rossi. Beppo Occhialini and Bruno Rossi are the reference points in the scientific life of Livio. From memories of Livio: Bruno Rossi and Beppo Occhialini Artistic photo composition by A. Spizzichino, “The Active X-ray Sky”, 21-24 October, 1997, Roma A. Watson, Intl. Workshop “ The UHE Universe”, Villa Mondragone, Frascati,19-21 June,2006 In 1952 Livio follows Beppo Occhialini in Milan and in 1955 Beppo send Livio in France, at the Centre d’Etudes Nucleaires de Saclay where he remains for 3 years: researches for “New Particles” in the Cosmic Radiation with the tecnique of Nuclear Emulsions flown in the Upper Atmosphere with Stratospheric Balloons. Relevant results are : First classification of Decay modes for K-mesons and Hyperons In 1957 he comes back in Milan but ….. From memories of Livio: “A. Watson, UHE Workshop , Villa Mondragone, Frascati, June 21, 2006.” Volcano Ranch , “ The desert Quinn” In Volcano Ranch, New Mexico desert, Jonh Linsley and Livio Scarsi installed 19 plastic scintillators (3.3 m2 area each-one) in an exagone of about 2,430,000 m2 area. -
Arxiv:2009.10347V3 [Astro-Ph.IM] 24 Feb 2021
Draft version February 25, 2021 Typeset using LATEX twocolumn style in AASTeX63 Timing Calibration of the NuSTAR X-ray Telescope Matteo Bachetti,1, 2, ∗ Craig B. Markwardt,3 Brian W. Grefenstette,2 Eric V. Gotthelf,4 Lucien Kuiper,5 Didier Barret,6 W. Rick Cook,2 Andrew Davis,2 Felix Furst¨ ,7 Karl Forster,2 Fiona A. Harrison,2 Kristin K. Madsen,2, 3 Hiromasa Miyasaka,2 Bryce Roberts,8 John A. Tomsick,8 and Dominic J. walton9 1INAF-Osservatorio Astronomico di Cagliari, via della Scienza 5, I-09047 Selargius, Italy 2Space Radiation Laboratory, Caltech, 1200 E California Blvd, Pasadena, CA 91125 3Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 4Columbia Astrophysics Laboratory, Columbia University, 550 West 120th Street, New York, NY 10027-6601, USA 5SRON Netherlands Institute for Space Research, Sorbonnelaan 2, NL-3584 CA Utrecht, the Netherlands 6IRAP, Universit´ede Toulouse, CNRS, UPS, CNES, 9, Avenue du Colonel Roche, BP 44346, F-31028 Toulouse Cedex 4, France 7European Space Astronomy Centre (ESA/ESAC), Operations Department, Villanueva de la Ca~nada(Madrid), Spain 8Space Sciences Laboratory, 7 Gauss Way, University of California, Berkeley, CA 94720-7450, USA 9Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK (Received January 1, 2018; Revised January 7, 2018; Accepted February 25, 2021) Submitted to ApJ ABSTRACT The Nuclear Spectroscopic Telescope Array (NuSTAR) mission is the first focusing X-ray telescope in the hard X-ray (3-79 keV) band. Among the phenomena that can be studied in this energy band, some require high time resolution and stability: rotation-powered and accreting millisecond pulsars, fast variability from black holes and neutron stars, X-ray bursts, and more. -
Pos(MQW7)004 Ce
Hard (State) Problems PoS(MQW7)004 John A. Tomsick Space Science Laboratory, 7 Gauss Way, University of California, Berkeley, CA 94720-7450, USA E-mail: [email protected] For microquasars, the one time when these systems exhibit steady and powerful jets is when they are in the hard state. Thus, our understanding of this state is key to learning about the disk/jet connection. Recent observational and theoretical results have led to questions about whether we really understand the physical properties of this state, and even our basic picture of this state is uncertain. Here, I discuss some of the recent developmentsand possible problems with our under- standing of this state. Overall, it appears that the strongest challenge to the standard truncated disk picture is the detection of broad iron features in the X-ray spectra, and it seems that either there is a problem with the truncated disk picture or there is a problem with the relativistic reflection models used to explain the broad iron features. VII Microquasar Workshop: Microquasars and Beyond September 1-5 2008 Foca, Izmir, Turkey ¡ Speaker. ¢c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. http://pos.sissa.it/ Hard (State) Problems John A. Tomsick 1. Overview This work is devoted to a discussion of our current understanding of accreting black hole sys- tems when they are in the hard state. In this work, I start by describing the defining properties of the hard state and the questions that we would like to answer concerning the hard state. -
On the Disappearance of Kilohertz Quasi-Periodic Oscillations at a High Mass Accretion Rate in Low-Mass X-Ray Binaries
The Astrophysical Journal Letters: 534, L31, 2000 May 1 On the Disappearance of Kilohertz Quasi-Periodic Oscillations at a High Mass Accretion Rate in Low-Mass X-ray Binaries Wei Cui Center for Space Research, Massachusetts Institute of Technology, Room 37-571, Cambridge, MA 02139; [email protected] ABSTRACT For all sources in which the phenomenon of kilo-Hertz quasi-periodic oscillation (kHz QPO) is observed, the QPOs disappear abruptly when the inferred mass accretion rate exceeds a certain threshold. Although the threshold cannot at present be accurately determined (or even quantified) observationally, it is clearly higher for bright Z sources than for faint atoll sources. Here we propose that the observational manifestation of kHz QPOs requires direct interaction between the neutron star magnetosphere and the Keplerian accretion disk and that the cessation of kHz QPOs at high accretion rate is due to the lack of such an interact when the Keplerian disk terminates at the last stable orbit and yet the magnetosphere is pushed farther inward. The threshold is therefore dependent of the magnetic field strength — the stronger the magnetic field the higher the threshold. This is certainly in agreement with the atoll/Z paradigm, but we argue that it is also generally true, even for individual sources within each (atoll or Z) category. For atoll sources, the kHz QPOs also seem to vanish at low accretion rate. Perhaps the “disengagement” between the magnetosphere and the Keplerian disk also takes place under such circumstances, because of, for instance, the presence of quasi-spherical advection-dominated accretion flow (ADAF) close to the arXiv:astro-ph/0003243v2 5 Jun 2000 neutron star. -
Optical Studies of Massive X-Ray Binaries" Door E.J
C 7A OPTICAL STUDIES OF SIVE m EJ. ZUIDERWIJK optical studies of massive X- ray binaries ACADEMISCH PROEFSCHRIFT TER VERKRIJGING VAN DE GRAAD VAN DOCTOR IN DE WISKUNDE EN NATUURWETENSCHAPPEN AAN DE UNIVERSITEIT VAN AMSTERDAM, OP GEZAG VAN DE RECTOR MAGNIFICUS, DR. J. BRUYN, HOOGLERAAR IN DE FACULTEIT DER LETTEREN, IN HET OPENBAAR TE VERDEDIGEN IN DE AULA DER UNIVERSITEIT (TIJDELIJK IN DE LUTHERSE KERK, INGANG SINGEL 411, HOEK SPUI) OP WOENSDAG 20 JUN11979 DES NAMIDDAGS TE 15.00 UUR PRECIES DOOR EDUARDUSJOSEPHUSZUIDERWIJK GEBOREN TE HAARLEM PROMOTOR : Prof. Dr. E.P.J. van den Heave 1 COREFERENT : Dr. H.G L.M. Lamers The work described in this thesis was supported by the "Netherlands Organi- sation for the advancement of Pure Re- search" (ZWO) and by the University of of Amsterdam. -\ Voor mijn Iet en onze Ouders i Na het voltooien van mijn proefschrift wil ik graag allen bedanken die aan het tot stand komen ervan hebben bijgedragen. Allereerst dank ik mijn ouders, die mij de gelegenheid gaven een aca- demische opleiding te volgen. Bijzonder erkentelijk ben ik mijn Promotor Prof. Dr. E.P.J. van den Heuvel, die het voor mij mogelijk maakte het onderzoek uit te voeren. Hij is daarbij altijd een steun geweest door de interesse getoond in mijn werk, die onder andere tot uiting kwam in langdurige en diepgaande gedach- tenwisselingen. De coreferent Dr. H.J.G.L.M. Lamers dank ik voor het kritisch lezen van het proefschrift. Het grootste deel van de in mijn proefschrift verwerkte publicaties zijn tot stand gekomen in nauwe samenwerking met mijn collega's van het Sterrenkundig Instituut van de universiteit van Amsterdam en van het As- trophysisch Instituut van de Vrije Universiteit van Brussel. -
Uva-DARE (Digital Academic Repository)
UvA-DARE (Digital Academic Repository) A comparison between the rapid burster and GRO J1744-28 Lewin, W.H.G.; Rutledge, R.E.; Kommers, J.M.; van Paradijs, J.A.; Kouveliotou, C. DOI 10.1086/310022 Publication date 1996 Published in Astrophysical Journal Link to publication Citation for published version (APA): Lewin, W. H. G., Rutledge, R. E., Kommers, J. M., van Paradijs, J. A., & Kouveliotou, C. (1996). A comparison between the rapid burster and GRO J1744-28. Astrophysical Journal, 462, L39-L42. https://doi.org/10.1086/310022 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:30 Sep 2021 THE ASTROPHYSICAL JOURNAL, 462 : L39–L42, 1996 May 1 q 1996. The American Astronomical Society. All rights reserved. -
Relativistic Jets in Active Galactic Nuclei and Microquasars
SSRv manuscript No. (will be inserted by the editor) Relativistic Jets in Active Galactic Nuclei and Microquasars Gustavo E. Romero · M. Boettcher · S. Markoff · F. Tavecchio Received: date / Accepted: date Abstract Collimated outflows (jets) appear to be a ubiquitous phenomenon associated with the accretion of material onto a compact object. Despite this ubiquity, many fundamental physics aspects of jets are still poorly un- derstood and constrained. These include the mechanism of launching and accelerating jets, the connection between these processes and the nature of the accretion flow, and the role of magnetic fields; the physics responsible for the collimation of jets over tens of thousands to even millions of gravi- tational radii of the central accreting object; the matter content of jets; the location of the region(s) accelerating particles to TeV (possibly even PeV and EeV) energies (as evidenced by γ-ray emission observed from many jet sources) and the physical processes responsible for this particle accelera- tion; the radiative processes giving rise to the observed multi-wavelength emission; and the topology of magnetic fields and their role in the jet colli- mation and particle acceleration processes. This chapter reviews the main knowns and unknowns in our current understanding of relativistic jets, in the context of the main model ingredients for Galactic and extragalactic jet sources. It discusses aspects specific to active Galactic nuclei (especially Gustavo E. Romero Instituto Argentino de Radioastronoma (IAR), C.C. No. 5, 1894, Buenos Aires, Argentina E-mail: [email protected] M. Boettcher Centre for Space Research, Private Bag X6001, North-West University, Potchef- stroom, 2520, South Africa E-mail: [email protected] S. -
European X-Ray Astronomy –From a Faltering Start to World Leadership
European X-ray Astronomy –from a faltering start to world leadership Ken Pounds University of Leicester 60 years ago….. • early ‘pioneers’ from cosmic ray physics (eg JT) • or solar astronomy (eg me) • Sun the only known x-ray source in 1956 when I joined UCL Rocket Group - as yet with no rocket • expectations higher for UV and Gamma-ray sources - one reason why ESRO was slow to respond Wider context: Sputnik (1957): NASA (1958): CERN (1959) 1964 ESRO formed – with UK as largest funder 1968 ESRO-2, ESRO-1, HEOS-1 launched, but no x-ray mission planned although …. 1962/3 first cosmic x-ray sources detected by Giacconi and Friedman and Skylark observations from Woomera in 1967 ---------------- 1967 X-ray proposal to ESRO (COS-A) rejected due to impact on COS-B gamma-ray observatory ------------- 1969 Astro group recommends lunar occultation mission – with similar (source i.d.) objectives to COS A 1971 LPAC approval of HELOS for ESTEC study for start in 1975, and launch in 1979. -------------- • Financial crisis led to further delay – with ESRO + ELDO >> ESA in 1975 • 1983 launch with modified payload but deep space orbit retained EXOSAT (1983-86) • first X-ray satellite in deep space orbit – real-time operations and continuous monitoring – first dedicated guest observer facility • Over 1800 successful observations of galactic and extragalactic x-ray sources • Strong user support form ESA with “science quality” data products and software tools available online • A model later transferred to GSFC to become the foundation of NASA’s HEASARC • Combination of MEDA and CMA detectors provided unique broad-spectrum X-ray spectra • ‘Long looks’ in final months a great success 19 February 1987 EXOSAT Legacies • EXOSAT Results Database: online data archive from 1989 • Strong user support and provided a model for future x-ray missions • Deep space orbit adopted for Chandra and XMM-Newton but perhaps even more important for the longer term…. -
The X-Ray Timing Behavior of the X-Ray Burst Source SLX 1735-269
A&A manuscript no. ASTRONOMY (will be inserted by hand later) AND Your thesaurus codes are: 06 (02.01.2; 08.09.2; 08.14.1; 13.25.5) ASTROPHYSICS The X-ray Timing Behavior of the X-ray Burst Source SLX 1735–269 Rudy Wijnands & Michiel van der Klis Astronomical Institute “Anton Pannekoek” and Center for High Energy Astrophysics, University of Amsterdam, Kruislaan 403, NL-1098 SJ Amsterdam, The Netherlands; [email protected], [email protected] Received; accepted Abstract. We report for the first time on the rapid X-ray little is known about this source. Goldwurm et al. 1996 variability of the galactic bulge source and X-ray burster detected the source up to about 150 keV with a spectral SLX 1735–269. The power spectrum as observed with the index above 30 keV of ∼−3. This is steeper than usually Rossi X-ray Timing Explorer is characterized by a strong observed for black-hole candidates and therefore they ten- band-limited noise component which is approximately flat tatively suggested that the compact object in the system below a 0.1–2.3 Hz break frequency; above this frequency is a neutron star. ASCA observations of this source below the power spectrum declines as a power law of index 0.9. 10 keV also could not uniquely identify the nature of the At the highest observed count rate a broad bump is super- compact object (David et al. 1997) but they were consis- imposed on this band-limited noise. The power spectrum tent with the neutron star hypothesis. -
Faint Gamma-Ray Bursts and Other High-Energy Transients Detected
Faint Gamma-Ray Bursts and Other High-Energy Transients Detected with BATSE by Jefferson Michael Kommers Submitted to the Department of Physics in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Physics at the MASSACHUSETTS INSTITUTE OF TECHNOLOGY February 1999 © Massachusetts Institute of Technology 1999. All rights reserved. C Author........V .V ....... .. .. ...........- ... -- - ..... ...........----.- - Department of Physics December 15, 1998 d4 Certified byV Walter H. G. Lewin Professor of Physics Thesis Supervisor Accepted by ............... /Thomas, .Greytak Professor of Physics Associate Department Head for Education MCH SETTS INSTI TUTE LIBRARIES Faint Gamma-Ray Bursts and Other High-Energy Transients Detected with BATSE by Jefferson Michael Kommers Submitted to the Department of Physics on December 15, 1998, in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Physics ABSTRACT The Burst and Transient Source Experiment (BATSE) onboard the Compton Gamma Ray Observatory detects gamma-ray bursts (GRBs) and other high-energy astronomi- cal transients using a real-time burst detection system running onboard the spacecraft. This thesis describes a search of the archival BATSE data for GRBs, emission from soft gamma-ray repeaters (SGRs), bursts and flares from X-ray binaries, and other transients that were not detected by the onboard system. The search covers six years of the mission, from 1992 December 9.0 to 1997 December 17.0. The search reveals 873 GRB candidates that did not activate the onboard burst detection because they were too faint, because they occurred while the onboard system was disabled for technical reasons, or because their time profile artificially raised the onboard detection threshold.