DOCSLIB.ORG

Diapositiva 1

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Diapositiva 1 MARCO FEROCI INAF, ROME ANNA WATTS UNIV. OF AMSTERDAM MICHIEL VAN DER KLIS UNIV. OF AMSTERDAM ON BEHALF OF THE LOFT CONSORTIUM LOFT LARGE OBSERVATORY ESA COSMIC VISION M3 FOR X-RAY TIMING CANDIDATE MISSIONS PRESENTATION EVENT LOFT SCIENCE LOFT ADDRESSES THE COSMIC VISION THEME “Matter Under Extreme Conditions” Probe the state of matter at supra nuclear densities in Neutron Stars (“Dense Matter”) Probe gravity theory in the very strong field environment of Black Holes (“Strong Gravity”) Probe physics of hundreds of galactic and bright extragalactic cosmic sources (“Observatory Science”) PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS THE LOFT APPROACH WHAT LOFT MUST HAVE Exploit the Diagnostics of X-ray Variability on Dynamical Timescales: Large Collecting Area Exploit the Diagnostics of Spectral Variability on Dynamical Timescales: Good Energy Resolution (XMM-class) PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS THE LOFT APPROACH WHATWHATLOFTLOFT MUST HASHAVE! Large Collecting Area 200 eV Good Energy Resolution (XMM-class) PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS THE LOFT APPROACH WHATWHATLOFTLOFT MUST HASHAVE! Large Collecting Area LHC SDD Detectors Heritage 200 eV Good Energy Resolution (XMM-class) Microchannel Plate Collimators PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS LOFT’S CHANGING THE GAME LOFT UNITES SPECTROSCOPY & TIMING, AT ENORMOUS AREA RXTE LOFT 2 1100 eV, 0.65 m2 200 eV, 10 m XMM 130 eV, 0.085 m2 No pile-up pile-up-limited not part of any planned X-ray mission PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS LOFT - LARGE AREA DETECTOR 125x 2000x 16 µm 83 µm 4 m2 @ 2 keV EFFECTIVE AREA 10 m2 @ 8 keV 1 m2 @ 30 keV 2-30 keV ENERGY RANGE (30-80 keV ext.) ENERGY 200 eV @ 6 keV RESOLUTION FWHM COLLIMATED FOV 1 deg FWHM ABSOLUTE TIME 1 s ACCURACY PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS LOFT - LARGE AREA DETECTOR PERFORMANCE LAD INSTANTANEOUS SKY VISIBILITY 180 eV 240 eV 300 eV 340 eV 75% of the sky accessibile to LAD at any time. Combination of Sky Visibility and Mission Duration ensures required number of transients PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS LOFT - WIDE FIELD MONITOR 5 Units 10 Cameras FIELD OF VIEW 5.5 steradian POSITION ACCURACY (10) 1 arcmin ENERGY RANGE 2-50 keV ENERGY RESOLUTION 300 eV @ 6 keV COLLECTING AREA 1820 cm2 10 s (trigger) TIME RESOLUTION minutes (images) SENSITIVITY (5σ, 270 mCrab (3s) GALACTIC CENTER) 2.1 mCrab (1day) GROUND TRANSMISSION OF < 30s GRB COORDINATES PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS LOFT - WIDE FIELD MONITOR PERFORMANCE FIELD OF VIEW cm2 EXPOSURE MAP Ms PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS MISSION CONFIGURATION FEASIBLE MISSION IN SEVERAL CONFIGURATIONS, WITH STANDARD EQUIPMENT South atlantic anomaly Item Value Orbit Equatorial, 550 km Launcher Soyuz (6,000 kg launch capability) Mass 4,000 kg Power 4 kW Telemetry 6.7 Gbit/orbit Ground Stations Kourou, Malindi Pointing 3-axis stabilized Mission Duration 3+2 years PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS MISSION FEASIBILITY FEASIBLE MISSION IN SEVERAL CONFIGURATIONS, WITH STANDARD EQUIPMENT ESA Review: South atlantic anomaly “mission feasible and of low technical risk and medium schedule risk for a 2022 launch date; a launch in 2023Item is seen as realisticValue ” Orbit Equatorial, 550 km “The overall instrument as wellLauncher as the ScienceSoyuz Ground Segment concept is considered to be mature and well documented. The level of detail with which theMass instrument design4,000 kg is described significantly exceedsPower general expectations4 kW at the end ofTelemetry a Phase A study10 Gbit.” /orbit Ground Stations Kourou, Malindi Pointing 3-axis stabilized Mission Duration 3+2 years PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS THE ESA PREFERRED LOFT CONCEPT PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS PROGRAMMATICS AND SCIENCE MANAGEMENT Payload and Science Data Center provided by Institutes in ESA Member States. LOFT Science Team even wider in Europe and worldwide LOFT IS AN OPEN OBSERVATORY All LAD data open to the Community through peer-reviewed proposals. All WFM data public after validation. PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS LOFT IN THE MULTI-FREQUENCY CONTEXT LOFT in the Multi-wavelength and Multi-messenger Context of Time Domain Astronomy PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS LOFT IN THE MULTI-FREQUENCY CONTEXT LOFT in the Multi-wavelength and Multi-messenger Context of Time Domain Astronomy PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS DENSE MATTER Dense matter Strong field gravity Observatory science PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS LOFT DENSE MATTER THEME The strong force determines the state of nuclear matter - from atomic nuclei to neutron stars. It is a major problem within modern physics. PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS LOFT DENSE MATTER THEME The strong force determines the state of nuclear matter - from atomic nuclei to neutron stars. It is a major problem within modern physics. PROGRESS IS DRIVEN BY LABORATORY EXPERIMENT AND ASTROPHYSICAL OBSERVATION. PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS DENSE MATTER AND NEUTRON STARS – A UNIQUE REGIME Neutron LOFT Stars PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS DENSE MATTER AND NEUTRON STARS – A UNIQUE REGIME Neutron stars contain the densest and most neutron-rich matter in the Universe. Neutron LOFT Stars LOFT WILL STUDY NUCLEONIC MATTER IN A UNIQUE REGIME, AND EXOTIC STATES OF MATTER THAT COULD NEVER EXIST IN THE LABORATORY. PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS STRONG FORCE, EQUATION OF STATE, AND MASS-RADIUS RELATION Equation of state (EOS) The strong force determines the ‘stiffness’ of neutron star matter. This is encoded in the EQUATION OF STATE. PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS STRONG FORCE, EQUATION OF STATE, AND MASS-RADIUS RELATION Equation Nucleonic of state (EOS) The strong force determines the ‘stiffness’ of neutron star matter. This is encoded in the EQUATION OF STATE. PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS STRONG FORCE, EQUATION OF STATE, AND MASS-RADIUS RELATION Equation Nucleonic of state (EOS) The strong force determines the ‘stiffness’ of neutron star matter. This is encoded in the EQUATION OF STATE. Quark stars PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS STRONG FORCE, EQUATION OF STATE, AND MASS-RADIUS RELATION Equation Nucleonic of state (EOS) The strong force determines the Strange ‘stiffness’ of neutron cores star matter. This is encoded in the EQUATION OF STATE. Quark stars PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS STRONG FORCE, EQUATION OF STATE, AND MASS-RADIUS RELATION Equation Nucleonic of state (EOS) The strong force determines the Strange ‘stiffness’ of neutron cores Chiral EFT star matter. models This is encoded in the EQUATION OF STATE. Quark stars PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS STRONG FORCE, EQUATION OF STATE, AND MASS-RADIUS RELATION EOS PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS STRONG FORCE, EQUATION OF STATE, AND MASS-RADIUS RELATION EOS PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS STRONG FORCE, EQUATION OF STATE, AND MASS-RADIUS RELATION Stellar structure equations EOS Mass-Radius (M-R) LOFT MUST MEASURE BOTH M AND R TO HIGH PRECISION (LOW STATISTICAL AND SYSTEMATIC ERRORS) FOR A RANGE OF M. PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS PULSE PROFILE MODELLING (1) General Relativity Hotspots on accreting neutron stars generate pulsations. Relativistic effects (light-bending, redshifts, aberration) encode information about M and R. Hotspot in thermonuclear burst LOFT WILL RECOVER M AND R FROM THE (Spitkovsky et al. 2002) PHOTON ENERGY-DEPENDENT PULSE PROFILE. PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS PULSE PROFILE MODELLING (2) 3.0 TE RX 2.5 Detailed simulations carried out to evaluate fitting General Relativity 2.0 LOFT procedure and accuracies ) ) ) • • • (Lo et al. 2013, ApJ). O O O M M M ( ( ( s s s 1.5 s s s Few % accuracy needs a a a 6 2 M M M ~10 photons: 10m area 1.0 crucial. 0.5 Multiple same-source cross- checks. 0.0 8 10 12 14 16 Radius (km) USING ONLY KNOWN SOURCES, LOFT’S PULSE PROFILE MODELLING MEASUREMENTS WILL MAP THE M-R RELATION AND HENCE THE EOS. PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS SPIN MEASUREMENTS For most accreting NS spin is not yet Spin rates constrain EOS via known. Pulsations (especially for high mass-shedding limit. accretion rate sources) are weak or intermittent. LOFT’S EXQUISITE SENSITIVITY WILL ALLOW FULL CHARACTERIZATION OF THE SPIN DISTRIBUTION OF ACCRETING NEUTRON STARS. PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS ASTEROSEISMOLOGY Starquakes on magnetars trigger Magneto-elastic seismic global seismic vibrations. Current vibration models constrain M-R data come from the rarest, most and hence the EOS. energetic events. LOFT WILL BE SENSITIVE TO SEISMIC VIBRATIONS FROM SMALLER STARQUAKES, DRIVING THE EMERGING FIELD OF NEUTRON STAR ASTEROSEISMOLOGY. PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS LOFT AND DENSE MATTER - SUMMARY LOFT • measures both M and R. • minimises statistical error with its large effective area. • minimises systematic error with complementary methods and same source cross-checks. • relies only on known sources to deliver the required number of data points. No other facility does this. LOFT WILL MEASURE THE EOS OF DENSE MATTER, THE KEY TO UNDERSTANDING THE STRONG
Load more

Recommended publications
  • First Circular
    First Circular With great pleasure we announce the first circular for the international confer- ence The Structure and Signals of Neutron Stars, from Birth to Death, to be held in Florence, Italy from March 24-28, 2014. The conference is affili- ated with a six week workshop of the same title to be held at the Galileo Galilei Institute, also in Florence, from March 10-April 18, 2014. The study of neutron stars represents an active field of both observational and theoretical research, requiring the expertise of scientists across a range of disciplines, including astrophysics, nuclear and particle physics and Gravitational Wave (GW) physics. A conference dedicated to all facets of neutron stars is particularly relevant at this moment, given recent advances such as • The discovery of massive neutron stars, which has placed new constraints on the equation of state (EoS) of dense matter. • Observations of cooling of the young NS in Cas A, hinting at a transition to neutron superfluidity. • Gravitational wave interferometers LIGO and Virgo being upgraded to ad- vanced sensitivity, and starting to take data as soon as 2015. • New observations challenging models for Gamma Ray Bursts and their cen- tral engines. New observations of core collapse supernovae, showing an un- expected diversity in their explosion mechanisms. • New lab experiments testing matter at high density and temperature that will start taking data in 2015 (NICA - Dubna). • The discovery of a magnetar near the Galactic center. This conference aims to bring together astronomers from across the electro- magnetic and GW spectrum who are interested in observations that can constrain the neutron star EoS, as well as nuclear physicists interested in the behavior of matter at high densities.
    [Show full text]
  • Dense Matter with Extp Arxiv
    UvA-DARE (Digital Academic Repository) Dense matter with eXTP Watts, A.L.; Riley, T.E.; Degenaar, N.; Di Salvo, T.; Homan, J.; Stappers, B.; eXTP Mission DOI 10.1007/s11433-017-9188-4 Publication date 2019 Document Version Submitted manuscript Published in Science China: Physics, Mechanics and Astronomy Link to publication Citation for published version (APA): Watts, A. L., Riley, T. E., Degenaar, N., Di Salvo, T., Homan, J., Stappers, B., & eXTP Mission (2019). Dense matter with eXTP. Science China: Physics, Mechanics and Astronomy, 62(2), [29503]. https://doi.org/10.1007/s11433-017-9188-4 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:05 Oct 2021 Watts A L, Yu W, Poutanen J, Zhang S, etSCIENCE al Sci.
    [Show full text]
  • Dr Anna Watts
    Dr Anna Watts School of Mathematics - Assistant Professor, University of Amsterdam Beyond star gazing. Anna’s career in astrophysics Winning a place on a space science summer school was a life-changing experience for astrophysicist Anna Watts. “Although I always liked solving problems, my interest in Physics only really started with my A levels,” she admits. “But this two week course at Brunel University convinced me that I wanted to make science my career.” Anna was advised to get a good degree in Physics first, then specialise in astrophysics. She went to Merton College, Oxford and enjoyed her time there: “It was a small, friendly college and I had fantastic tutors. I come from the north of England and wondered what Oxford would be like but I loved it.” After graduation, not sure an academic career was for her, Anna decided to get a job and signed up for the Ministry of Defence civil service fast track science stream: “I stayed there for five years and learned a lot. We worked in a wide range of areas and they moved us around to several sites. But eventually, I realised I missed the science too much to stay.” During her work with the MoD, Anna met her future husband, fellow scientist Jason Farquhar. Both decided to resign at the same time and study for PhDs, coincidentally both at Southampton. “This was a big decision and I knew I had to go to the right place and find the right supervisor. I asked my former tutors at Oxford for advice and they reckoned I’d enjoy working with Professor Nils Andersson at Southampton.” Anna’s doctorate involved investigating neutron stars, some of the most compact objects in the universe, and the gravitational and electromagnetic radiation they emit.
    [Show full text]
  • X-Ray Timing & Spectroscopy on Dynamical Timescales From
    X-ray Timing & Spectroscopy on Dynamical Timescales from Microseconds to Years Paul Ray (U.S. Naval Research Laboratory) Steering Committee: Colleen Wilson-Hodge (MSFC) Tom Maccarone (Texas Tech) Zaven Arzoumanian, Keith Gendreau (GSFC) Deepto Chakrabarty, Ron Remillard (MIT) Peter Jenke (UAH), Marco Feroci (INAF), Silvia Zane (UCL), Soren Brandt (DTU) , Alessandra DeRosa (INAF), Margarita Hernanz (IEEC), Anna Watts (Amsterdam), Kent Wood (NRL), John Tomsick (Berkeley), Laura Brenneman (CfA), David Ballantyne (GA Tech), Mike McDonald (MIT), Adam Goldstein (MSFC), Abbie Stevens (MSU), Enrico Bozzo (Geneva), Dieter Hartmann (Clemson), Bernard Phlips (NRL), Marc Christophersen (NRL) + > 150 members of SWG The STROBE-X study is funded by NASA Why a Flexible, High-Throughput Observatory? • The high-energy sky is highly dynamic – requires catching the right source at the right time – Necessitates both wide field monitoring and the ability to repoint quickly (as RXTE and Swift have demonstrated) • Critical capability in the era of time domain and multi-messenger astronomy • Large areas with low dead time access the shortest timescales • Both soft and hard X-ray bands are needed to accurately measure the continuum spectral shape, constrain absorption, and understand the relationship between thermal and non-thermal components Figure from Ron Remillard HEA Time Domain Desirati 2020 Courtesy Daryl Haggard Discovery & Monitoring Rapid Response High Time Resolution • All Sky Monitor •Rapid slew (< hr) • Sub-ms timing • Science drivers: •Science drivers:
    [Show full text]
  • 2 December 2020, 14:57 • From: Anna Watts • To: Division D High Energy
    • Date sent: 2 December 2020, 14:57 • From: Anna Watts • To: Division D High Energy Phenomena and Fundamental Physics • Subject: IAU Div D (High energy phenomena and fundamental physics) Bulletin - December 2020 ***IAU Division D Bulletin, December 2020*** INDEX *AHEAD2020 Announcement of Opportunity Cycle 1 *Survey on research culture in Astronomy *Upcoming Conferences, Meetings, Workshops and Schools ======================================= *AHEAD2020 Announcement of Opportunity Cycle 1 The AHEAD2020 (Integrated Activities for High Energy Astrophysics*) will call for a program of transnational visits to be started around Spring 2021. The main objectives are: 1) fostering new or strengthening existing collaborations in the fields of technology and data analysis (visitor program); 2) providing training and/or mentoring on high energy data analysis, use of advanced tools and computational astrophysics; 3) providing free access to some of the best European ground test and calibration facilities relevant for high-energy astrophysics. Visitor grants include full reimbursement of travel and subsistence expenses. To face possible restrictions to travel as an effect of the current pandemic, the possibility of remote access for a number of services in the area of data analysis, tools and computational astrophysics will be provided. AO-1 Calls opening: 11 January 2021 Submission Deadline: 22 February 2021 For further information and links to the AO-1 calls: http://ahead.iaps.inaf.it/ * AHEAD2020 is a Research Infrastructure program funded by EU Horizon 2020. Its main goal is to integrate and open research infrastructures for high energy Astrophysics. For general information on AHEAD2020: http://ahead.iaps.inaf.it/ ======================================= *Survey on research culture in astronomy Julia Heuritsch, a PhD Candidate at Humboldt Universität zu Berlin, is undertaking a survey to study the research culture in astronomy, and would like to solicit input from IAU members and their colleagues, particularly early career researchers.
    [Show full text]
  • Annalesai637salmi.Pdf (1.102Mb)
    ANNALES UNIVERSITATIS TURKUENSIS UNIVERSITATIS ANNALES AI 637 AI Tuomo Salmi Tuomo MASS AND RADIUS CONSTRAINTS FOR NEUTRON STARS USING X-RAY TIMING, SPECTRAL, AND POLARIZATION OBSERVATIONS Tuomo Salmi Painosalama Oy, Turku, Finland 2020 Finland Turku, Oy, Painosalama ISBN 978-951-29-8277-6 (PRINT) – ISBN 978-951-29-8278-3 (PDF) TURUN YLIOPISTON JULKAISUJA ANNALES UNIVERSITATIS TURKUENSIS ISSN 0082-7002 (Print) SARJA – SER. AI OSA – TOM. 637 | ASTRONOMICA – CHEMICA – PHYSICA – MATHEMATICA | TURKU 2020 ISSN 2343-3175 (Online) MASS AND RADIUS CONSTRAINTS FOR NEUTRON STARS USING X-RAY TIMING, SPECTRAL, AND POLARIZATION OBSERVATIONS Tuomo Salmi TURUN YLIOPISTON JULKAISUJA – ANNALES UNIVERSITATIS TURKUENSIS SARJA – SER. AI OSA – TOM. 637 | ASTRONOMICA – CHEMICA – PHYSICA – MATHEMATICA | TURKU 2020 University of Turku Faculty of Science and Engineering Department of Physics and Astronomy Astronomy Doctoral Programme in Physical and Chemical Sciences Supervised by Prof. Juri Poutanen Docent Sergey Tsygankov Department of Physics and Astronomy Department of Physics and Astronomy University of Turku University of Turku Turku, Finland Turku, Finland PhD Joonas Nättilä Physics Dept. and Astrophysics Lab. Columbia University & Flatiron Institute New York, USA Reviewed by Prof. Denis Leahy Prof. Stephan Rosswog Department of Physics and Astronomy Astronomy and Oskar Klein Centre University of Calgary Stockholm University Calgary, Canada Stockholm, Sweden Opponent Prof. Marat Gilfanov Max Planck Institute for Astrophysics & Space Research Institute Garching, Germany & Moscow, Russia The originality of this publication has been checked in accordance with the University of Turku quality assurance system using the Turnitin OriginalityCheck service. ISBN 978-951-29-8277-6 (PRINT) ISBN 978-951-29-8278-3 (PDF) ISSN 0082-7002 (Print) ISSN 2343-3175 (Online) Painosalama Oy - Turku, Finland 2020 Acknowledgements First, I would like to thank my supervisors Prof.
    [Show full text]
  • Probing the Neutron Star Interior and the Equation of State of Cold Dense Matter with the SKA
    Probing the neutron star interior and the Equation of State of cold dense matter with the SKA Anna Watts∗1, Renxin Xu2, Cristóbal Espinoza3, Nils Andersson4, John Antoniadis5, Danai Antonopoulou1, Sarah Buchner7, Shi Dai8, Paul Demorest9, Paulo Freire6, Jason Hessels1;10, Jérôme Margueron11, Micaela Oertel12, Alessandro Patruno13;10, Andrea Possenti14, Scott Ransom9, Ingrid Stairs15, Ben Stappers16 1University of Amsterdam; 2KIAA Peking University; 3PUC, Chile; 4University of Southampton; 5University of Toronto 6 Max Planck Institute for Radio Astronomy; 7 HRAO, University of Witwatersrand; 8 ATNF; 9 NRAO Charlottesville; 10 ASTRON; 11 IPNL, CNRS/IN2P3, Université Lyon; 12 LUTH, CNRS, Observatoire de Paris, Université Paris Diderot; 13 Leiden University; 14 INAF-Osservatorio Astronomico di Cagliari; 15 University of British Columbia; 16 University of Manchester. E-mail: [email protected] With an average density higher than the nuclear density, neutron stars (NS) provide a unique test- ground for nuclear physics, quantum chromodynamics (QCD), and nuclear superfluidity. Deter- mination of the fundamental interactions that govern matter under such extreme conditions is one of the major unsolved problems of modern physics, and – since it is impossible to replicate these conditions on Earth – a major scientific motivation for SKA. The most stringent observational constraints come from measurements of NS bulk properties: each model for the microscopic be- haviour of matter predicts a specific density-pressure relation (its ‘Equation of state’, EOS). This generates a unique mass-radius relation which predicts a characteristic radius for a large range of masses and a maximum mass above which NS collapse to black holes. It also uniquely predicts other bulk quantities, like maximum spin frequency and moment of inertia.
    [Show full text]
  • 3 December 2019, 15:44 • From: Anna Watts • To: Division D High Energy
    • Date sent: 3 December 2019, 15:44 • From: Anna Watts • To: Division D High Energy Phenomena and Fundamental Physics • Subject: IAU Div D (High energy phenomena and fundamental physics) Bulletin - December 2019 ***IAU Division D Bulletin, December 2019*** INDEX *Upcoming Conferences, Meetings, Workshops and Schools ======================================= *Upcoming Conferences, Meetings, Workshops and Schools XLVIII International Workshop on Gross Properties of Nuclei and Nuclear Excitations, ‘Nuclear equation of state and neutron stars' 12-18 January, 2020 Hirschegg, Austria http://theorie.ikp.physik.tu-darmstadt.de/hirschegg/ Peculiar supernovae and neutron stars 17 February, 2020 Bonn, Germany https://events.mpifr-bonn.mpg.de/indico/event/143/ Jürgen Ehlers Spring School of Gravity and Gravitational Waves 2-13 March, 2020 Potsdam, Germany https://springschool.aei.mpg.de/ GGI PhD School on Theoretical Aspects of Astroparticle Physics, Cosmology and Gravitation 9-20 March, 2020 Arcetri, Florence, Italy http://www.ggi.infn.it/showevent.pl?id=340 Mapping the X-ray Sky with SRG: First Results from eROSITA and ART-XC 16-20 March, 2020 Garching, Germany https://events.mpe.mpg.de/event/SRG2020/ Polish-German WE-Heraeus-Seminar “The Variable Multi-Messenger Sky” 6-9 April, 2020 Cracow, Poland https://www.we-heraeus-stiftung.de/veranstaltungen/seminare/2020/the-variable-multi- messenger-sky/ THESEUS conference 2020 12-15 May, 2020 Malaga, Spain https://www.isdc.unige.ch/theseus/theseus-conference-2020.html The X-ray Universe 2020 25-29 May,
    [Show full text]
  • 7 October 2019, 09:51 • From: Anna Watts • Subject: IAU Div D (High Energy Phenomena and Fundamental Physics) Bulletin - October 2019
    • Date sent: 7 October 2019, 09:51 • From: Anna Watts • Subject: IAU Div D (High energy phenomena and fundamental physics) Bulletin - October 2019 ***IAU Division D Bulletin, October 2019*** INDEX *Fast Radio Burst Newsletter *Annual Report of the Office for Astronomy for Development *THESEUS Science Working Group registration now open * New book on Astronomical Polarization *Upcoming Conferences, Meetings, Workshops and Schools (new announcements) ======================================= * Fast Radio Burst Newsletter Emily Petroff and Shami Chatterjee have started an FRB Community Newsletter, an approximately monthly email newsletter dedicated to discoveries, developments, and news in the FRB community. To subscribe, please use the following link: https://docs.google.com/forms/d/e/1FAIpQLSdtLF6XJ4LNnoRRVRxcCXH6Le_luSLvdwGu8X SfiQNxE6g-FQ/viewform ======================================= * Annual Report of the Office for Astronomy for Development The 36 page Annual Report for the year 2018-19 summarises the activities of the OAD and its Regional Office over the last year, including an overview of the OAD, flagship themes, special projects and an analysis of the impact of previously funded OAD projects. The report can be downloaded on the OAD website at: http://www.astro4dev.org/downloads/ ======================================= * THESEUS Science Working Group registration now open The Transient High-Energy Sky and Early Universe Surveyor (THESEUS) is a space mission concept aiming at fully exploiting Gamma-Ray Bursts for investigating the early Universe and at providing a substantial advancement of multi-messenger and time-domain astrophysics, currently under Phase A study by the European Space Agency (ESA) as candidate M5 mission in view of a launch opportunity in 2032. See the THESEUS website (https://www.isdc.unige.ch/theseus) and main white papers for further details (Amati et al., 2018, Adv.
    [Show full text]
  • STROBE-X: X-Ray Timing and Spectroscopy on Dynamical
    STROBE-X March 11, 2019 STROBE-X : X-ray Timing and Spectroscopy on Dynamical Timescales from Microseconds to Years White Paper Submitted to Astro 2020 Decadal Survey Paul S. Ray U.S. Naval Research Laboratory [email protected] STROBE-X Steering Committee: Zaven Arzoumanian, David Ballantyne, Enrico Bozzo, Soren Brandt, Laura Brenneman, Deepto Chakrabarty, Marc Christophersen, Alessandra DeRosa, Marco Feroci, Keith Gendreau, Adam Goldstein, Dieter Hartmann, Margarita Hernanz, Peter Jenke, Erin Kara, Tom Maccarone, Michael McDonald, Michael Nowak, Bernard Phlips, Ron Remillard, Abigail Stevens, John Tomsick, Anna Watts, Colleen Wilson-Hodge, Kent Wood, Silvia Zane STROBE-X Science Working Group: Marco Ajello, Will Alston, Diego Altamirano, Vallia Antoniou, Kavitha Arur, Dominic Ashton, Katie Auchettl, Tom Ayres, Matteo Bachetti, Mislav Balokovi´c,Matthew Baring, Altan Baykal, Mitch Begelman, Narayana Bhat, Slavko Bogdanov, Michael Briggs, Esra Bulbul, Petrus Bult, Eric Burns, Ed Cackett, Riccardo Campana, Amir Caspi, Yuri Cavecchi, Jerome Chenevez, Mike Cherry, Robin Corbet, Michael Corcoran, Alessan- dra Corsi, Nathalie Degenaar, Jeremy Drake, Steve Eikenberry, Teruaki Enoto, Chris Fragile, Felix Fuerst, Poshak Gandhi, Javier Garcia, Adam Goldstein, Anthony Gonzalez, Brian Grefenstette, Victoria Grinberg, Bruce Grossan, Sebastien Guillot, Tolga Guver, Daryl Haggard, Craig Heinke, Sebastian Heinz, Paul Hemphill, Jeroen Homan, Michelle Hui, Daniela Huppenkothen, Adam In- gram, Jimmy Irwin, Gaurava Jaisawal, Amruta Jaodand, Emrah Kalemci,
    [Show full text]
  • Arxiv:1804.03380V1 [Astro-Ph.HE] 10 Apr 2018
    ,Draft version September 29, 2018 Typeset using LAT X twocolumn style in AASTeX61 , E THE INFLUENCE OF STELLAR SPIN ON IGNITION OF THERMONUCLEAR RUNAWAYS Duncan K. Galloway,1, 2 Jean J. M. in 't Zand,3 Jer´ ome^ Chenevez,4 Laurens Keek,5, 6 Celia Sanchez-Fernandez,7 Hauke Worpel,8 Nathanael Lampe,9 Erik Kuulkers,10 Anna Watts,11 and Laura Ootes11 The MINBAR collaboration 1School of Physics & Astronomy, Monash University, Clayton, VIC 3800, Australia 2Monash Centre for Astrophysics, Monash University, Clayton, VIC 3800, Australia 3SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, the Netherlands 4National Space Institute, Technical University of Denmark, Elektrovej 327-328, DK-2800 Lyngby, Denmark 5X-ray Astrophysics Laboratory, Astrophysics Science Division, NASA/GSFC, Greenbelt, MD 20771 6CRESST and the Department of Astronomy, University of Maryland, College Park, MD 20742 7European Space Astronomy Centre (ESA/ESAC), Science Operations Department, E-28691, Villanueva de la Ca~nada,Madrid, Spain 8Leibniz-Institut f¨urAstrophysik Potsdam (AIP), An der Sternwarte 16, Potsdam 14482, Germany 9CNRS, IN2P3, CENBG, UMR 5797, F-33170 Gradignan, France 10ESA/ESTEC, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands 11Anton Pannekoek Institute for Astronomy, University of Amsterdam, Postbus 94249, 1090GE Amsterdam, the Netherlands (Accepted April 9, 2018) Submitted to ApJL ABSTRACT Runaway thermonuclear burning of a layer of accumulated fuel on the surface of a compact star provides a brief but intense display of stellar nuclear processes. For neutron stars accreting from a binary companion, these events manifest as thermonuclear (type-I) X-ray bursts, and recur on typical timescales of hours to days.
    [Show full text]
  • Elisa: Gravitational Waves from Space an Astronomy/Physics Facility
    eLISA: Gravitational waves from Space An Astronomy/Physics facility A proposal for the KNAW committee for future large-scale facilities Acronym eLISA-NL Facility European Space Agency Gravitational Wave mission Main applicant Prof. dr. Gijs Nelemans Organisation Radboud University Function UHD Address Postbus 9010, 6500 GL, Nijmegen Telephone 024-3652983 Email [email protected] Co-applicants: SRON: Dr. Ir. G. de Lange Nikhef: Dr. N. van Bakel NOVA: Dr. W. Boland, Executive Director NOVA TNO: M. Maniscalco JD, MSc, LLM UTwente: Prof. dr. K-J. Boller eLISA-NL consortium: Ana Achucarro (Physics, UL) Niels van Bakel (Instrumentation, Nikhef) Daniel Baumann (Physics, UvA) Eric Bergshoef (Physics, RUG) Klaus Boller (Instrumentation, U Twente) Jo van den Brand (Physics, VU/Nikhef) Chris van den Broeck (Physics, Nikhef) Ernst-Jan Buis (Instrumentation, TNO) Henk-Jan Bulten (Physics, VU/Nikhef) Gert de Lange (Instrumentation, SRON) Carsten Fallnich (Instrumentation, U Twente/Münster) Paul Groot (Astrophysics, RU) Jan-Willem den Herder (Instrumentation/Astrophysics, SRON) Jan-Willem van Holten (Physics, UL/Nikhef) Gemma Janssen (Astrophysics, ASTRON) Peter Jonker (Astrophysics, SRON/RU) Marc Klein-Wolt (Astrophysics, RU) Michiel van der Klis (Astrophysics, UvA) Elmar Koerding (Astrophysics, RU) Rudolf Le Poole (Astrophysics, UL) Frank Linde (Physics, Nikhef/UvA) Renate Loll (Physics, RU) Matthew Maniscalco (Instrumentation, TNO) Mariano Mendez (Astrophysics, RUG) Selma de Mink (Astrophysics, UvA) Ramon Navarro (Instrumentation, NOVA) Gijs Nelemans (Astrophysics, RU) Onno Pols (Astrophysics, RU) Simon Portegies Zwart (Astrophysics, UL) Tomislav Prokopec (Physics, UU) Elena Maria Rossi (Astrophysics, UL) Joop Schaye (Astrophysics, UL) Marco Spaans (Astrophysics, RUG) Frank Verbunt (Astrophysics, RU) Anna Watts (Astrophysics, UvA) Frontpage: Artist impression of eLISA.
    [Show full text]