On the FRB Luminosity Function – II. Event Rate Density
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Massive Fast Rotating Highly Magnetized White Dwarfs: Theory and Astrophysical Applications
Massive Fast Rotating Highly Magnetized White Dwarfs: Theory and Astrophysical Applications Thesis Advisors Ph.D. Student Prof. Remo Ruffini Diego Leonardo Caceres Uribe* Dr. Jorge A. Rueda *D.L.C.U. acknowledges the financial support by the International Relativistic Astrophysics (IRAP) Ph.D. program. Academic Year 2016–2017 2 Contents General introduction 4 1 Anomalous X-ray pulsars and Soft Gamma-ray repeaters: A new class of pulsars 9 2 Structure and Stability of non-magnetic White Dwarfs 21 2.1 Introduction . 21 2.2 Structure and Stability of non-rotating non-magnetic white dwarfs 23 2.2.1 Inverse b-decay . 29 2.2.2 General Relativity instability . 31 2.2.3 Mass-radius and mass-central density relations . 32 2.3 Uniformly rotating white dwarfs . 37 2.3.1 The Mass-shedding limit . 38 2.3.2 Secular Instability in rotating and general relativistic con- figurations . 38 2.3.3 Pycnonuclear Reactions . 39 2.3.4 Mass-radius and mass-central density relations . 41 3 Magnetic white dwarfs: Stability and observations 47 3.1 Introduction . 47 3.2 Observations of magnetic white dwarfs . 49 3.2.1 Introduction . 49 3.2.2 Historical background . 51 3.2.3 Mass distribution of magnetic white dwarfs . 53 3.2.4 Spin periods of isolated magnetic white dwarfs . 53 3.2.5 The origin of the magnetic field . 55 3.2.6 Applications . 56 3.2.7 Conclusions . 57 3.3 Stability of Magnetic White Dwarfs . 59 3.3.1 Introduction . 59 3.3.2 Ultra-magnetic white dwarfs . 60 3.3.3 Equation of state and virial theorem violation . -
One Or Several Populations of Fast Radio Burst Sources?
One or several populations of fast radio burst sources? M. Caleb1, L. G. Spitler2 & B. W. Stappers1 1Jodrell Bank Centre for Astrophysics, the University of Manchester, Manchester, UK. 2Max-Planck-Institut fu¨r Radioastronomie, Bonn, Germany. arXiv:1811.00360v1 [astro-ph.HE] 1 Nov 2018 1 To date, one repeating and many apparently non-repeating fast radio bursts have been de- tected. This dichotomy has driven discussions about whether fast radio bursts stem from a single population of sources or two or more different populations. Here we present the arguments for and against. The field of fast radio bursts (FRBs) has increasingly gained momentum over the last decade. Overall, the FRBs discovered to date show a remarkable diversity of observed properties (see ref 1, http://frbcat.org and Fig. 1). Intrinsic properties that tell us something about the source itself, such as polarization and burst profile shape, as well as extrinsic properties that tell us something about the source’s environment, such as the magnitude of Faraday rotation and multi-path propagation effects, do not yet present a coherent picture. Perhaps the most striking difference is between FRB 121102, the sole repeating FRB2, and the more than 60 FRBs that have so far not been seen to repeat. The observed dichotomy suggests that we should consider the existence of multiple source populations, but it does not yet require it. Most FRBs to date have been discovered with single-pixel telescopes with relatively large angular resolutions. As a result, the non-repeating FRBs have typically been localized to no bet- ter than a few to tens of arcminutes on the sky (Fig. -
Detection of a Type Iin Supernova in Optical Follow-Up Observations of Icecube Neutrino Events Magellan Workshop, 17–18 March 2016, DESY Hamburg
Detection of a Type IIn Supernova in Optical Follow-Up Observations of IceCube Neutrino Events Magellan Workshop, 17{18 March 2016, DESY Hamburg Markus Voge, Nora Linn Strotjohann, Alexander Stasik 17 March 2016 Target: transient sources (< 100 s • neutrino burst): GRBs (Waxman & Bahcall 1997, Murase • & Nagataki 2006) SNe with jets (Razzaque, Meszaros, • Waxman 2005) More exotic phenomena? E.g. Fast • Radio Bursts (FRBs)? (Falcke & Rezzolla 2013) Online Neutrino Analysis Automatic search for interesting IceCube neutrino events • Realtime alerts sent to follow-up instruments • Multi-messenger: Combination with other data fruitful • Follow-up ensures access to data • 2 / 15 Online Neutrino Analysis Automatic search for interesting IceCube neutrino events • Realtime alerts sent to follow-up instruments • Multi-messenger: Combination with other data fruitful • Follow-up ensures access to data • Target: transient sources (< 100 s • neutrino burst): GRBs (Waxman & Bahcall 1997, Murase • & Nagataki 2006) SNe with jets (Razzaque, Meszaros, • Waxman 2005) More exotic phenomena? E.g. Fast • Radio Bursts (FRBs)? (Falcke & Rezzolla 2013) 2 / 15 The OFU and XFU system SN/GRB PTF (optical) Swift (X-ray) Alerts Alerts Madison/Bonn Iridium IceCube arXiv: 1309.6979 (p.40) 3 / 15 Online analysis scheme neutrino purity At least 8 coincident Trigger Level 0:0001% hits 2000 Hz ∼ Basic muon event se- Level 1 35 Hz 0:01% lection (tracks only) ∼ Up-going tracks Level 2 2 Hz 0:1% ∼ Neutrino selection OFU Level 3 mHz 90% (BDT) ∼ Neutrino multiplet ( 2ν): ≥ Time -
Magnetodynamics Inside and Outside Magnetars
Magnetodynamics Inside and Outside Magnetars Xinyu Li Submitted in partial fulfillment ofthe requirements for the degree of Doctor of Philosophy in the Graduate School of Arts and Sciences COLUMBIA UNIVERSITY 2019 ©2019 Xinyu Li All Rights Reserved Abstract Magnetodynamics Inside and Outside Magnetars Xinyu Li The ultra-strong magnetic fields of magnetars have profound implications for their radiative phenomena. We study the dynamics of strong magnetic fields inside and outside magnetars. Inside the magnetar, the strong magnetic stress can break the crust and trigger plastic failures. The interaction between magnetic fields and plastic failures is studied in two scenarios: 1. Internal Hall waves launched from the core-crust interface can initiate plastic failures and lead to X-ray outbursts. 2. External Alfven waves produced by giant flares can also initiate crustal plastic failures which dissipate the waves and give rise to delayed thermal afterglow. The crustal dissipation of Alfven waves competes with the magnetospheric dissipation outside the magnetar. Using a high order simulation of Force-Free Electrodynamics (FFE), we found that the magnetospheric dissipation of Alfven waves is generally slow and most wave energy will dissipate inside the magnetar. Contents List of Figures v Chapter 1 Introduction 1 1.1 Neutrons Stars . 2 1.1.1 Theoretical and observational discovery . .2 1.1.2 Structure of neutron stars . 5 1.2 Magnetars . 10 1.2.1 Discovery . 10 1.2.2 Magnetar Activities . 12 1.2.3 Theoretical Models . 16 1.3 This Dissertation . 24 Chapter 2 Magnetohydrodynamics (MHD) 26 2.1 Ideal MHD . 26 2.1.1 Nonrelativistic ideal MHD . -
The Discovery of Frbs
Credit: Swinburne in Fast Radio Burst detection detection Burst FastRadio in Strategic uses of single dishes (and GB) (and singledishes uses of Strategic DuncanLorimer, Dept. Physics and of Astronomy, WestVirginia University FRB lowdown • 21 published so far • Flux > 0.5 Jy @ 1.4 GHz • Pulse widths > few ms • Highly dispersed • Weakly scattered • One FRB so far repeats! • Few arcmin localization • One counterpart so far • ~few x 1000/day/sky Credit: Thornton et al. (2013) What might FRBs probe? • New/exciting physics • Cosmological NS census? • Non-stellar origin? • Fundamental tests? • The intergalactic medium • Electron content → missing baryons? • Magnetic field || to line of sight • Cosmology • Rulers • DM halos, DM/DE parameterization Single-pulse search pipeline DM Cordes & McLaughlin (2003) Credit: Spitler et al. (2014) 2014: FRB 121102 at Arecibo at FRB 121102 2014: Credit: Masui et al. (2015) 2015: FRB 110523 at GBT at FRB 110523 2015: • More “theories” than bursts! • Colliding compact objects (e.g. NS-NS) • Supernovae • Collapsing NS → BH (blitzar) • Black hole absorbing NSs • Giant pulses from pulsars/magnetars • Neutron star – asteroid belt interaction • More exotic (strange) star interactions • Galactic Flare Stars • Light sails from ET • Dark matter • Cosmic strings • White holes No! Maybe? No! → → → or maybesomethingor else? … … 2016: FRB 121102 repeats! 121102 FRB 2016: Credit: Spitler et al. and Scholz et al. (2016) 2017: FRB 121102 localized! Credit: NRAO Credit: Chatterjee et al. (2017) z = 0.19 (2.3 billion yr) We -
Search for Neutrino Emission from Fast Radio Bursts with Icecube
Search for Neutrino Emission from Fast Radio Bursts with IceCube Donglian Xu Samuel Fahey, Justin Vandenbroucke and Ali Kheirandish for the IceCube Collaboration TeV Particle Astrophysics (TeVPA) 2017 August 7 - 11, 2017 | Columbus, Ohio Fast Radio Bursts - Discovery in 2007 2 e2 Lorimer et al.,Science 318 (5851): 777-780 2 ∆tdelay = 3 DM w− 2⇡mec · · 24 2 =1.5 10− s DM w− ⇥ · · 3 DM = n dl = 375 1cm− pc e ± Z “very compact” SMC J0045−7042 (70) J0111−7131 (76) J0113−7220 (125) “extragalactic”? J0045−7319 (105) J0131−7310 (205) Figure 2: Frequency evolution and integrated pulse shape of!the radio burst.4 The.8 survey0.4 data, collected on 2001δ Augusttwidth 24, are=4 shown. here6 ms as a two-dimensio ( nal ‘waterfall)− plot’± of intensity as a function of radio frequency versus time. The dispersion1.4GHzis clearly seen as a quadratic sweep across the frequency band, with broadening towards lower frequencies. From a measurement of the pulse delay across the receiver band using standard pulsar timing techniques, we determine the DM to be 375 dtI1 cm−3!pc. The two150 white lines50Jy separated byms 15 ms @ that 1 bound.4 GHz the pulse show the expected behavior± for the' cold-plasma dispersion± law assuming a DM of 375 cm−3 pc. The horizontal line at 1.34 GHz is an artifact in the data caused by a malfunctioning frequency Z ∼ channel. This plot is for one of the offset beams in which the digitizers were not saturated. By splitting the data into four frequency sub-bands we have measured both the half-power Galactic DM: pulse width• andA fluxtotal density spectrumof ~ over23 the observingFRBs bandwidth. -
Neutron Star Collapse Times, Gamma-Ray Bursts and Fast Radio Bursts
MNRAS 441, 2433–2439 (2014) doi:10.1093/mnras/stu720 The birth of black holes: neutron star collapse times, gamma-ray bursts and fast radio bursts ‹ Vikram Ravi1,2 and Paul D. Lasky1 Downloaded from https://academic.oup.com/mnras/article-abstract/441/3/2433/1126394 by California Institute of Technology user on 24 June 2019 1School of Physics, University of Melbourne, Parkville, VIC 3010, Australia 2CSIRO Astronomy and Space Science, Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, Australia Accepted 2014 April 8. Received 2014 April 7; in original form 2013 November 29 ABSTRACT Recent observations of short gamma-ray bursts (SGRBs) suggest that binary neutron star (NS) mergers can create highly magnetized, millisecond NSs. Sharp cut-offs in X-ray afterglow plateaus of some SGRBs hint at the gravitational collapse of these remnant NSs to black holes. The collapse of such ‘supramassive’ NSs also describes the blitzar model, a leading candidate for the progenitors of fast radio bursts (FRBs). The observation of an FRB associated with an SGRB would provide compelling evidence for the blitzar model and the binary NS merger scenario of SGRBs, and lead to interesting constraints on the NS equation of state. We predict the collapse times of supramassive NSs created in binary NS mergers, finding that such stars collapse ∼10–4.4 × 104 s (95 per cent confidence) after the merger. This directly impacts observations targeting NS remnants of binary NS mergers, providing the optimal window for high time resolution radio and X-ray follow-up of SGRBs and gravitational wave bursts. -
81 EMBARGOED UNTILLTHURSDAY JULY 4 20:00 CET Nijmegen, July 2, 2013 Farewell Greeting from a Dying Star
PB 2012 - 81 EMBARGOED UNTILLTHURSDAY JULY 4 20:00 CET Nijmegen, July 2, 2013 Farewell greeting from a dying star – Scientists suggest explanation for mysterious radio flashes Mysterious bright radio flashes that appear for only a brief moment on the sky and do not repeat could be the final farewell greetings of a massive star collapsing into a black hole, astronomers from Nijmegen and Potsdam argue. Radio telescopes have picked up some bright radio flashes that appear for only a brief moment on the sky and do not repeat. Scientists have since wondered what causes these unusual radio signals. An article in this week’s issue of ‘Science’ suggests that the source of the flashes lies deep in the early cosmos, and that the short radio burst are extremely bright. However, the question of which cosmic event could produce such a bright radio emission in such a short time remained unanswered. The astrophysicists Heino Falcke from Radboud University Nijmegen and Luciano Rezzolla from the Max Planck Institute for Gravitational Physics in Potsdam provide a solution for the riddle. They propose that the radio bursts could be the final farewell greetings of a supramassive rotating neutron star collapsing into a black hole. Spinning star withstands collapse Neutron stars are the ultra-dense remains of a star that has undergone a supernova explosion. They are the size of a small city but have up to two times the mass of our Sun. However, there is an upper limit on how massive neutron stars can become. If they are formed above a critical mass of more than two solar masses, they are expected to collapse immediately into a black hole. -
Fast Radio Bursts
UvA-DARE (Digital Academic Repository) Fast radio bursts Petroff, E.; Hessels, J.W.T.; Lorimer, D.R. DOI 10.1007/s00159-019-0116-6 Publication date 2019 Document Version Final published version Published in Astronomy and Astrophysics Review License CC BY Link to publication Citation for published version (APA): Petroff, E., Hessels, J. W. T., & Lorimer, D. R. (2019). Fast radio bursts. Astronomy and Astrophysics Review, 27(1), [4]. https://doi.org/10.1007/s00159-019-0116-6 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 The Astronomy and Astrophysics Review (2019) 27:4 https://doi.org/10.1007/s00159-019-0116-6 REVIEW ARTICLE Fast radio bursts E. Petroff1,2 · J. -
The Discovery of Frbs
Credit: Swinburne Fast Radio Bursts : The Story SoStory Far... Bursts: The Fast Radio DuncanLorimer, Dept. Physics and of Astronomy, WestVirginia University Credit: Joeri van Leeuwen Phinney & Taylor (1979) Credit: Aurore Simonet “...the next few decades will undoubtedly bring about a greater understanding of radio-bursting objects, including Crab-like pulsars in other galaxies, counterparts to high-energy bursting sources, and other classes of objects that are yet to be discovered.” Rotating Radio Transients (RRATs) Credit: Froney Crawford Credit: ATNF Credit: Credit: Maura McLaughlin Credit: fas.org End up with a search over “DM” a search upwith End Single-pulse search pipeline DM Cordes & McLaughlin (2003) An unexpected signal! An unexpected signal! Interference Questions: * Why so bright? * Why no weaker events? * Detectable in other surveys? Even my own wife begins to doubt... “Moreover, the lack of highly dispersed celestial signals is the evidence that the Lorimer burst is unlikely to belong to a cosmological source population.” DM = 746 pc/cc 746 = DM ms W=8 eane et al. 2011/2012 Credit: K but then, in 2012, alongcame then,in2012, this but The burst is also consistent with the radio signal theorised … from an annihilatingfrom mini black hole.” “ … more good news followed in 2013 • Lorimer bursts? • Sparkers? • FARTS? • FRBs Cosmological redshift Cosmological redshift Credit: Thornton et al. (2013) DM delay in FRB 110220 FRB in delay DM Energy and redshift estimates Credit: Spitler et al. (2014) 2014: an FRB atArecibo an 2014: • Credit: Masui et al. (2015) 2015: an FRB atGBT an 2015: • Credit: Masui et al. (2015) 2015: an FRB atGBT an 2015: Scattering andScattering scintillation seen! • Credit: Petroff et al. -
Giant Sparks at Cosmological Distances?
The Astrophysical Journal, 797:70 (31pp), 2014 December 10 doi:10.1088/0004-637X/797/1/70 C 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. GIANT SPARKS AT COSMOLOGICAL DISTANCES? S. R. Kulkarni1,E.O.Ofek2,J.D.Neill3, Z. Zheng4,andM.Juric5 1 Caltech Optical Observatories 249-17, California Institute of Technology, Pasadena, CA 91125, USA 2 Department of Particle Physics & Astrophysics, Weizmann Institute of Science, Rehovot 76100, Israel 3 Space Radiation Laboratory 290-17, California Institute of Technology, Pasadena, CA 91125, USA 4 Department of Physics & Astronomy, University of Utah, 115 South 1400 East 201, Salt Lake City, UT 84112, USA 5 Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA Received 2014 February 28; accepted 2014 September 23; published 2014 November 25 ABSTRACT Millisecond-duration bright radio pulses at 1.4 GHz with high dispersion measures (DMs) were reported by Lorimer et al., Keane et al., and Thornton et al. Their all-sky rate is ≈104 day−1 above ∼1 Jy. Related events are “Perytons”—similar pulsed, dispersed sources, but most certainly local. Suggested models of fast radio bursts (FRBs) can originate in Earth’s atmosphere, in stellar coronae, in other galaxies, and even at cosmological distances. Using physically motivated assumptions combined with observed properties, we explore these models. In our analysis, we focus on the Lorimer event: a 30 Jy, 5 ms duration burst with DM = 375 cm−3 pc, exhibiting a steep frequency-dependent pulse width (the Sparker). To be complete, we drop the assumption that high DMs are produced by plasma propagation and assume that the source produces pulses with frequency-dependent arrival time (“chirped signals”). -
Lawrence Berkeley National Laboratory Recent Work
Lawrence Berkeley National Laboratory Recent Work Title THE DETECTION of A SN IIn in OPTICAL FOLLOW-UP OBSERVATIONS of ICECUBE NEUTRINO EVENTS Permalink https://escholarship.org/uc/item/9m60266f Journal Astrophysical Journal, 811(1) ISSN 0004-637X Authors Aartsen, MG Abraham, K Ackermann, M et al. Publication Date 2015-09-20 DOI 10.1088/0004-637X/811/1/52 Peer reviewed eScholarship.org Powered by the California Digital Library University of California PREPRINT ACCEPTED FOR PUBLICATION IN THE ASTROPHYSICAL JOURNAL Preprint typeset using LATEX style emulateapj v. 01/23/15 DETECTION OF A TYPE IIN SUPERNOVA IN OPTICAL FOLLOW-UP OBSERVATIONS OF ICECUBE NEUTRINO EVENTS M. G. AARTSEN1, K. ABRAHAM2, M. ACKERMANN3, J. ADAMS4, J. A. AGUILAR5, M. AHLERS6, M. AHRENS7, D. ALTMANN8, T. ANDERSON9, M. ARCHINGER10, C. ARGUELLES6, T. C. ARLEN9, J. AUFFENBERG11, X. BAI12, S. W. BARWICK13, V. BAUM10, R. BAY14, J. J. BEATTY15,16, J. BECKER TJUS17, K.-H. BECKER18, E. BEISER6, S. BENZVI6, P. BERGHAUS3, D. BERLEY19, E. BERNARDINI3, A. BERNHARD2, D. Z. BESSON20, G. BINDER21,14, D. BINDIG18, M. BISSOK11, E. BLAUFUSS19, J. BLUMENTHAL11, D. J. BOERSMA22, C. BOHM7, M. BORNER¨ 23, F. BOS17, D. BOSE24, S. BOSER¨ 10, O. BOTNER22, J. BRAUN6, L. BRAYEUR25, H.-P. BRETZ3, A. M. BROWN4, N. BUZINSKY26, J. CASEY27, M. CASIER25, E. CHEUNG19, D. CHIRKIN6, A. CHRISTOV28, B. CHRISTY19, K. CLARK29, L. CLASSEN8, S. COENDERS2, D. F. COWEN9,30, A. H. CRUZ SILVA3, J. DAUGHHETEE27, J. C. DAVIS15, M. DAY6, J. P. A. M. DE ANDRE´ 31, C. DE CLERCQ25, H. DEMBINSKI32, S. DE RIDDER33, P. DESIATI6, K. D.