Glitches in radio pulsars
|
|
- Arabella Bryant
- 5 years ago
- Views:
Transcription
1 Frequency (Hz) ? MJD (Days) Glitches in radio pulsars Cristóbal Espinoza Jodrell Bank Centre for Astrophysics
2 ν 10 3 ν 100 µhz!! ("Hz) Glitch ν! (10-15 Hz s -1 ) Days from MJD=53737
3 What can produce a glitch? Caused by crust rearrangements; cooling, slowdown re-shaping. (Baym et al. 1969) Caused by rapid angular momentum exchange between the inner superfluid and the Crust; result of halted vortex migration. (Anderson & Itoh 1975; Alpar et al. 1984; many many others) Caused by magnetic field stresses on the crust, driven by vortex migration. (Ruderman et al. 1998) M. Ruderman (2009) INTERNAL OR CRUST PROCESS
4 Glitch 100 TG -10 Glitch detected Magnetar Detections TG 315 glitches in plot Kyr 378 detected so far pulsar/glitches.html log(period derivative) Kyr 0.01 TG -17 ~130 pulsars Myr Gyr MG Period (s)
5 Glitch spin-up rate (integrated glitch activity) [Lyne, Shemar & Graham-Smith (2000)] Separate pulsars according to their spindown rate and estimate their spin-up rate: ν glitch = i j ν ij k T k ν j counts the glitches on pulsar i Tk is the total time for which pulsar k has been observed (and sums over ALL pulsars in the group) 622 pulsars observed for more than 3 yr
6 ! (10-15 Hz s -1 ) x (a) Glitch spin-up rate (10-15 Hz s -1 ) x x10 6! N g " (yr -1 ) Glitching rate log! (10-15 Hz s -1 ) % of! reversed by glitches (b) log! (10-15 Hz s -1 ) Espinoza, Lyne, Stappers & Kramer (2011) Glitch activity grows linearly with spindown rate
7 3 regimes young pulsars ν glitch ν ν glitch ν old pulsars pulsar evolution?
8 glitches 315 glitches (smaller bin) Magnetars!! ["Hz] Bi-modal: two types of glitches? 40 Number Large glitches: seen mostly in Vela-like pulsars log(!!) ["Hz] (Espinoza et al. 2011) Distribution of Frequency steps
9 young pulsars Giant glitchers selected for showing large frequency and spindown rate steps 100 ν glitch ν 10 1 old pulsars!! ("Hz) Positive df1 jump Negative df1 jump !! (10-15 Hz s -1 )
10 Waiting time (days) Giant glitchers Narrow size distributions. Quasi periodic behaviour. Waiting times consistent with reaching critical lag. Permanent spindown rate changes B J Vela J e-13 1e-12 1e-11 1e-10 1e-09!!! (10-15 Hz s -1 )!! ("Hz)!! ("Hz)! (10-15 Hz s -1 )!! ("Hz)! (10-15 Hz s -1 ) B J model should relax the rigid rotation assumption for the charged component and include the effect of Ekman pumping. Further developments should also include more realistic models for the drag parameters in the star, as the density dependence of the coupling strength clearly has an impact on the amount of angular momentum that can be exchanged on different timescales. Truly quantitative results could then J be obtained with thej use of realistic equations J of state together with consistent estimates of the pinning force, such B as those of (Grill & Pizzochero 2011) and (Grill 2011). Note that we have assumed that a giant glitch only occurs when the maximum critical lag is reached. If unpinning could be triggered earlier, this could generate smaller glitches. In fact cellular automaton models have shown that the waiting time and size distributions of pulsar glitches can be successfully explained by vortex avalanche dynamics, related -500 to 0 random unpinning events (Warszawski & Melatos ; Days from Melatos Glitch & Warszawski Days from 2009; Glitch Warszawski Days & Melatos from Glitch Days from Glitch 2011). It would thus be of great interest to use our long-term hydrodynamical models, with realistic pinning forces, as a background for such cellular automaton models that model J P(!!) B J B Crab J B B !! ["Hz] Modelling pulsar glitches J Vela J ! (Hz/s) (Haskell et al. 2012) (Espinoza et al. 2011) Figure 14. We plot the approximate waiting time between glitches for the pulsars that have shown multiple giant glitches, as afunctionofthespindownrate.wealsoincludetwopulsarsthat J
11 CRAB ν(t) VELA ν(t) RESIDUALS RESIDUALS ~36 YR ~14 YR ν PERMANENT CHANGES ( ) THE CRAB AND VELA PULSARS ν p
12 Small glitches 100 Meet detection issues 10 Present in all pulsars, but preferably in low spin-down rate ones ν jumps appear smaller...!! ("Hz) days 1 day Do not seem to show significant permanent steps. ν Small glitches with large ν jumps may go undetected ph ph !! (10-15 Hz s -1 )
13 Residuals for ν = µhz (ν, ν fit until glitch epoch) 10 Residuals for ν = µhz (ν, ν fit entire data span) fit until glitch ν = 0.00 ν = 0.01 ν = 0.1 Increasing ν ν = 0.3 ν = 1.0 overall fit ν = 0.00 ν = 0.1 ν = 0.01 Increasing ν Hz s 1 Residuals for ν = 0.0 µhz ν = 0.00 ν = 0.01 (ν, ν fit until glitch epoch) ν = 0.3 ν = 0.1 Residuals for ν = 0.0 µhz ν = 0.00 ν = 1.0 ν = 0.01 ν = 1.0 Hz s 1 ν > 0 Timing noise ν = 0.3 & ν < 0 (ν, ν fit entire data span) ν = 0.1 ν = 0.3 ν = 1.0 ν < 0 ν > 0 ν = 0.00 ν = 0.01 ν = 0.1 ν = 0.3 ν = 0.3 ν = 0.01 ν = 0.00 ν = 0.1August 2012 IAU Symposium 291 Beijing, ν = 1.0 Timing noise refers to unmodelled deviations from a simple spindown model, appearing as a random wandering of the phase residuals. As pictured by Lyne+2010, most timing noise could be caused by changes, with both signs, of the spindown rate. ν = 1.0 Glitches and timing noise can be confused. Small glitches might remain undetected because they look like timing noise and timing noise might be confused with glitches (and reported as glitches with unusual properties). Characterising glitches and timing irregula in pulsars and magnetars C. M. Espinoza1*, D. Antonopoulou2^, B. W. Stappers1, A. Watts2 ν > 0 Glitches Study of the small glitches population is complicated Glitches are unresolved positive steps in pulsar spin because of accompanied contamination other phenomena frequency, normally by a changeby in the spindown Here is w 0 rate. After some glitches the frequency and the spin-down rate relax back to the pre-glitch state on timescales of up to ~100 days. These events are thought to be caused by the interaction of the neutron star crust with the internal neutron superfluid. Many recent detections of small events show unusual f Glitch ν JUMPS BECOMES IMPORTANT Phase residuals UNDERSTANDING OF tup φm
14 Summary: what we know about glitches All pulsars can glitch. But different pulsars glitch different. Pulsar with faster spindown rates glitch more often. The cumulative pulsars with large ~%1 of the spindown rate. ν ν ν effect over time is larger for (linearly) and it represents -distribution is bimodal. Some pulsars only exhibit large glitches.
15 Future work...or in progress Any trend involving improve error determinations. ν -jumps? Re-measure and Are all glitches followed by a permanent ν change? How is the size distribution towards lower end?
16 FIN
Statistical study of neutron star glitches
International Journal of Astrophysics and Space Science 2014; 2(2): 16-21 Published online May 20, 2014 (http://www.sciencepublishinggroup.com/j/ijass) doi: 10.11648/j.ijass.20140202.11 Statistical study
More informationarxiv: v2 [astro-ph.he] 27 Sep 2017
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed April 22, 2018 (MN LATEX style file v2.2) Minimum Glitch of the Crab Pulsar and the Crustquake as a Trigger Mechanism O. Akbal 1 & M.A. Alpar 1 arxiv:1707.01160v2
More informationarxiv: v1 [astro-ph.ga] 22 Dec 2009
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 22 December 2009 (MN LATEX style file v2.2) An analysis of the timing irregularities for 366 pulsars arxiv:0912.4537v1 [astro-ph.ga] 22 Dec 2009 G.
More informationarxiv: v1 [astro-ph.ga] 10 Jan 2010
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 8 September 2018 (MN LATEX style file v2.2) 29 Glitches Detected at Urumqi Observatory arxiv:1001.1471v1 [astro-ph.ga] 10 Jan 2010 J. P. Yuan, 1,2
More informationNonlinear interglitch dynamics, the braking index of the Vela pulsar and the time to the next glitch
Advance Access publication 2017 May 6 doi:10.1093/mnras/stx1095 Nonlinear interglitch dynamics, the braking index of the Vela pulsar and the time to the next glitch O. Akbal, 1 M. A. Alpar, 1 S. Buchner
More informationModelling pulsar glitches with realistic pinning forces: a hydrodynamical approach
Mon. Not. R. Astron. Soc. 420, 658 671 (2012) doi:10.1111/j.1365-2966.2011.20080.x Modelling pulsar glitches with realistic pinning forces: a hydrodynamical approach B. Haskell, 1,2 P. M. Pizzochero 3,4
More informationTiming Noise and The Long-term Stability of Pulsar Profiles
Timing Noise and The Long-term Stability of Pulsar Profiles Andrew Lyne Jodrell Bank Centre for Astrophysics The University of Manchester, UK IAU Symposium 291, Beijing 23 August 2012 Timing Noise Timing
More informationNew measurements of pulsar braking indices (obtained via phase-coherent timing)
New measurements of pulsar braking indices (obtained via phase-coherent timing) Collaborators: Vicky Kaspi (McGill) Fotis Gavriil (GSFC) Richard Manchester (ATNF) Eric Gotthelf (Columbia) Lucien Kuiper
More informationarxiv: v3 [astro-ph.he] 2 Jun 2017
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed June 18, 2018 (MN LATEX style file v2.2) Nonlinear interglitch dynamics, the braking index of the Vela pulsar and the time to the next glitch O. Akbal
More informationarxiv: v1 [astro-ph.sr] 30 Nov 2009
Compact stars in the QCD phase diagram II (CSQCD II) May 20-24, 2009, KIAA at Peking University, Beijing - P. R. China http://vega.bac.pku.edu.cn/rxxu/csqcd.htm The timing behaviour of radio pulsars arxiv:0911.5534v1
More informationGravitational waves from neutron stars: theoretical challenges. Ian Jones University of Southampton IGWM, 17 th May 2017
Gravitational waves from neutron stars: theoretical challenges Ian Jones University of Southampton IGWM, 17 th May 2017 Three gravitational wave emission mechanisms Mountains non-axisymmetric deformation
More informationNeutron Stars: Observations
Neutron Stars: Observations Ian Jones School of Mathematics, University of Southampton, UK Neutron star observations: overview From the observational point of view, neutron stars come in many different
More informationPulsar braking indices, glitches and energy dissipation in neutron stars
Mon. Not. R. Astron. Soc. 372, 489 496 (2006 doi:10.1111/j.1365-2966.2006.10893.x Pulsar braking indices, glitches and energy dissipation in neutron stars M. Ali Alpar 1 and Altan Baykal 2 1 Sabancı University,
More informationarxiv: v1 [astro-ph.he] 27 Dec 2018
Manuscript for Revista Mexicana de Astronomía y Astrofísica (2007) arxiv:1812.10815v1 [astro-ph.he] 27 Dec 2018 ENTRAINMENT FACTOR ON INDIVIDUAL GLITCH FRACTIONAL MOMENT OF INERTIA I. O. Eya, 1,3 J. O.
More informationRadio pulsar glitches as a state-dependent Poisson process
1 Radio pulsar glitches as a state-dependent Poisson process W. Fulgenzi 1, A. Melatos 1, B. D. Hughes 2, 1 School of Physics, The University of Melbourne, Parkville, VIC 31, Australia 2 School of Mathematics
More informationPhase Oscillation between Superfluid and Normal State of Neutrons in Neutron Stars The Origin of Glitches of Pulsars 1
Phase Oscillation between Superfluid and Normal State of Neutrons in Neutron Stars The Origin of Glitches of Pulsars Qiu-he Peng a,b ( qhpeng@nju.edu.cn ) Zhi quan Luo a,c a School of Physics and electronic
More informationGlitches and precession
Glitches and precession What is a glitch? A sudden increase of rotation rate. ATNF catalogue gives ~120 normal PSRs with glitches. The most known: Crab and Vela ΔΩ/Ω~ 10 9 10 6 Spin down rat e can change
More informationNot-Quite-Continuous Gravitational Waves
Not-Quite-Continuous Gravitational Waves Challenges and Opportunities Reinhard Prix Albert-Einstein-Institute Hannover INT Workshop on Astro-solids and GWs 18 April 2018 LIGO-G1800726-v3 1 Outline 1 Why
More informationarxiv:gr-qc/ v1 10 Dec 2003
Searching for gravitational waves from the Crab pulsar - the problem of timing noise arxiv:gr-qc/0312057v1 10 Dec 2003 Matthew Pitkin and Graham Woan Department of Physics and Astronomy, Kelvin Building,
More informationContinuous-wave gravitational radiation from pulsar glitch recovery
1 Continuous-wave gravitational radiation from pulsar glitch recovery Mark Bennett Anthony van Eysden & Andrew Melatos University of Melbourne 1 September 2010, ET WG4 Nice Meeting 2 Talk Outline Pulsar
More informationarxiv:astro-ph/ v2 8 Nov 2002
Radio Pulsars ASP Conference Series, Vol. to be determined, 23 M. Bailes, D. J. Nice, & S. E. Thorsett, eds. Precession of Isolated Neutron Stars arxiv:astro-ph/282v2 8 Nov 22 Bennett Link Department of
More informationPulsar glitch dynamics in general relativity
Pulsar glitch dynamics in general relativity Jérôme Novak (jerome.novak@obspm.fr) Laboratoire Univers et Théories (LUTH) CNRS / Observatoire de Paris / Université Paris-Diderot Sourie, Novak, Oertel &
More informationarxiv:astro-ph/ v5 31 Oct 2006
Predicting the Starquakes in PSR J0537 6910 J. Middleditch 1, F. E. Marshall 2, Q. D. Wang 3, E. V. Gotthelf 4, and W. Zhang 2 jon@lanl.gov arxiv:astro-ph/0605007v5 31 Oct 2006 ABSTRACT We report the results
More informationNeutron Star and Superfluidity
Neutron Star and Superfluidity Ka Wai Lo Department of Physics, University of Illinois at Urbana-Champaign December 13, 2010 Abstract It is expected that under high density, nucleons in neutron star can
More informationarxiv: v2 [astro-ph.he] 25 Jul 2013
Modeling the Evolution and Distribution of the Frequency s Second Derivative and Braking Index of Pulsar Spin with Simulations Yi Xie 1,2, Shuang-Nan Zhang 1,3 arxiv:1307.6413v2 [astro-ph.he] 25 Jul 2013
More informationCorrelated spin-down rates and radio emission in PSR B
doi:10.1093/mnras/stv2403 Correlated spin-down rates and radio emission in PSR B1859+07 B. B. P. Perera, 1 B. W. Stappers, 1 P. Weltevrede, 1 A. G. Lyne 1 andj.m.rankin 2 1 Jodrell Bank Centre for Astrophysics,
More informationMissing pieces in the r-mode puzzle
Missing pieces in the r-mode puzzle Southampton Theory Astronomy Gravity Centre for Fundamental Physics Nils Andersson accreting systems Accreting neutron stars in LMXBs may be relevant gravitational-wave
More informationarxiv: v2 [astro-ph.he] 15 Jun 2016
MNRAS, 1 9 (216) Preprint 16 April 218 Compiled using MNRAS LATEX style file v3. arxiv:166.498v2 [astro-ph.he] 15 Jun 216 A glitch in the millisecond pulsar J613 2 J. W. McKee, 1 G. H. Janssen, 2 B. W.
More informationarxiv: v1 [astro-ph] 29 Jun 2008
A cellular automaton model of pulsar glitches L. Warszawski 1 and A. Melatos 1 1 School of Physics, University of Melbourne, Parkville, VIC 3010, Australia arxiv:0806.4738v1 [astro-ph] 29 Jun 2008 1 INTRODUCTION
More informationOn the statistical implication of timing noise for pulsar braking index. A. E. Chukwude 1,2,
A&A 406, 667 671 (2003) DOI: 10.1051/0004-6361:20030789 c ESO 2003 Astronomy & Astrophysics On the statistical implication of timing noise for pulsar braking index A. E. Chukwude 1,2, 1 Hartebeesthoek
More informationDense matter equation of state and rotating neutron stars
Dense matter equation of state and rotating neutron stars ANG LI (李昂) with R.-X. Xu & H. Gao (Beijing) W. Zuo & J.-M. Dong (Lanzhou) B. Zhang (UNLV) J.-B. Wang (Urumqi) N.-B. Zhang & B. Qi (Weihai) T.
More informationGravitational Waves from Neutron Stars
Gravitational Waves from Neutron Stars Astronomical Institute Anton Pannekoek Elastic outer crust Neutron star modelling Elastic inner curst with superfluid neutrons Superfluid neutrons and superconducting
More informationInteractions between gravitational waves and photon astronomy (periodic signals)
Interactions between gravitational waves and photon astronomy (periodic signals) Ben Owen October 20, 2007 LSC-VIRGO / NS meeting 1 Intro We can look for things better if we know more about them from photon
More informationStudy of superfluidity in magnetars by van Hoven and Levin
Study of superfluidity in magnetars by van Hoven and Levin Overview What is a superfluid and how does it look like in neutron stars? What can happen when both a superfluid and a strong magnetic field are
More informationNeutron Stars. We now know that SN 1054 was a Type II supernova that ended the life of a massive star and left behind a neutron star.
Neutron Stars Neutron Stars The emission from the supernova that produced the crab nebula was observed in 1054 AD by Chinese, Japanese, Native Americans, and Persian/Arab astronomers as being bright enough
More informationVela Pulsar Glitches and Nuclear Superfluidity
Vela Pulsar Glitches and Nuclear Superfluidity Nicolas Chamel Institute of Astronomy and Astrophysics Université Libre de Bruxelles, Belgium March 214 Vela pulsar In October 1968, astronomers from the
More informationWhat can X-ray observations tell us about: The role of Gravitational Waves in Low Mass X-ray Binaries
What can X-ray observations tell us about: The role of Gravitational Waves in Low Mass X-ray Binaries Astronomical Institute Anton Pannekoek Low Mass X-ray Binaries Mass is stripped from the donor Forms
More informationOBSERVATIONS OF MICROGLITCHES IN HartRAO RADIO PULSARS
Available at: http://publications.ictp.it IC/2008/093 United Nations Educational, Scientific and Cultural Organization and International Atomic Energy Agency THE ABDUS SALAM INTERNATIONAL CENTRE FOR THEORETICAL
More informationSUPERFLUID MAGNETARS AND QPO SPECTRUM
SUPERFLUID MAGNETARS AND QPO SPECTRUM Andrea Passamonti Osservatorio Astronomico di Roma INAF. In collaboration with L. Stella, S. Lander SAIt Bologna 9/5/23 Magnetars Neutron stars with a strong magnetic
More informationarxiv:astro-ph/ v1 16 Aug 2001
Mon. Not. R. Astron. Soc. 000, 1 6 (2001) Printed 19 February 2004 (MN LATEX style file v1.4) Vortex Unpinning in Precessing Neutron Stars B. Link 1 and C. Cutler 2 1 Montana State University, Department
More informationThe pulsar population and PSR/FRB searches with MeerKAT Slow boring pulsars
The pulsar population and PSR/FRB searches with MeerKAT Slow boring pulsars Aris Karastergiou with contributions from Simon Johnston, Ben Stappers and the TRAPUM team P and Pdot are the observables. Lines
More informationTHE NEUTRON STAR CRUST AND SURFACE WORKSHOP. Quantum calculation of nucleus-vortex interaction in the inner crust of neutron stars
THE NEUTRON STAR CRUST AND SURFACE WORKSHOP Seattle 25-29 June 2007 Quantum calculation of nucleus-vortex interaction in the inner crust of neutron stars P. Avogadro, F.Barranco, R.A.Broglia, E.Vigezzi
More informationMicroscopic Calculation of Vortex-Nucleus Interaction for Neutron Star Glitches
INT Program INT-16-2b The Phases of Dense Matter July 11 - August 12, 2016 Microscopic Calculation of Vortex-Nucleus Interaction for Neutron Star Glitches Kazuyuki Sekizawa 1 in collaboration with G. Wlazłowski
More informationVariations of the harmonic components of the X-ray pulse profile of PSR B
RAA 205 Vol. 5 No., XX XX doi: 0.088/674 4527/5//00X http://www.raa-journal.org http://www.iop.org/journals/raa Research in Astronomy and Astrophysics Variations of the harmonic components of the X-ray
More informationPoS(Confinement X)260
The Hottest Superfluid and Superconductor in the Universe: Discovery and Nuclear Physics Implications, a Nils Andersson, a Cristóbal M. Espinoza, b Kostas Glampedakis, c Brynmor Haskell, d,e and Craig
More informationJames Clark For The LSC
A search for gravitational waves associated with the August 2006 timing glitch of the http://arxiv.org/abs/1011.1357 Vela pulsar James Clark For The LSC Introduction This talk: first search for GWs associated
More informationTHERMAL EVOLUTION OF ORDINARY NEUTRON STARS AND MAGNETARS
THERMAL EVOLUTION OF ORDINARY NEUTRON STARS AND MAGNETARS D.G. Yakovlev Ioffe Physical Technical Institute, Saint-Petersburg, Russia Introduction Thermal evolution of ordinary neutron stars Thermal evolution
More informationSearching for gravitational waves from neutron stars
Searching for gravitational waves from neutron stars Ian Jones D.I.Jones@soton.ac.uk General Relativity Group, Southampton University Ian Jones Searching for gravitational waves from neutron stars 1/23
More informationRotating RAdio Transients (RRATs) ApJ, 2006, 646, L139 Nature, 2006, 439, 817 Astro-ph/
Rotating RAdio Transients (RRATs) ApJ, 2006, 646, L139 Nature, 2006, 439, 817 Astro-ph/0608311 Introduction 11 Rotating RAdio Transients (RRATs) (Mclaughlin et al 2006) Repeated, irregular radio bursts
More informationThe Secret Life of Neutron Stars. Jeremy Heyl Harvard-Smithsonian CfA
The Secret Life of Neutron Stars Jeremy Heyl Harvard-Smithsonian CfA The Life of a 10 M Star PNS 10 5 yr 10 6 yr 10 7 yr 10 8 yr 10 9 yr 10 10 yr PMS MS Radio Pulsars Thermal Accretion-, Nuclear-, GWpowered
More informationarxiv: v1 [astro-ph.he] 28 Sep 2018
The Physical Essence of Pulsar Glitch arxiv:1810.01743v1 [astro-ph.he] 28 Sep 2018 Qiu-He Peng 1, Jing-Jing Liu 2 and Chih-Kang, Chou 3 qhpeng@nju.edu.cn, zsyuan@nao.cas.cn, and syjjliu68@126.com ABSTRACT
More informationarxiv: v2 [astro-ph.sr] 8 Jul 2015
Mon. Not. R. Astron. Soc. 000, 1 7 (2015) Printed 9 July 2015 (MN LATEX style file v2.2) Magnetic field growth in young glitching pulsars with a braking index Wynn C. G. Ho, 1 1 Mathematical Sciences and
More informationMagnetic fields of neutron stars: the AMXP connection
Recent Trends in the Study of Compact Objects: Theory and Observation ASI Conference Series, 2013, Vol. 8, pp 89 95 Edited by Santabrata Das, Anuj Nandi and Indranil Chattopadhyay Magnetic fields of neutron
More informationSimulations of Glitches in Isolated Pulsars
Utah State University DigitalCommons@USU All Physics Faculty Publications Physics 2002 Simulations of Glitches in Isolated Pulsars Michelle B. Larson Utah State University Bennett Link Follow this and
More informationChapter 14. Outline. Neutron Stars and Black Holes. Note that the following lectures include. animations and PowerPoint effects such as
Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). Chapter 14 Neutron
More information21. Neutron Stars. The Crab Pulsar: On & Off. Intensity Variations of a Pulsar
21. Neutron Stars Neutron stars were proposed in the 1930 s Pulsars were discovered in the 1960 s Pulsars are rapidly rotating neutron stars Pulsars slow down as they age Neutron stars are superfluid &
More informationINNER CRUST. s Lz2 \ 0, (1) f ] oj ] ALu
THE ASTROPHYSICAL JOURNAL, 563:267È275, 21 December 1 ( 21. The American Astronomical Society. All rights reserved. Printed in U.S.A. VORTEX CONFIGURATIONS, OSCILLATIONS, AND PINNING IN NEUTRON STAR CRUSTS
More informationParticle acceleration during the gamma-ray flares of the Crab Nebular
Particle acceleration during the gamma-ray flares of the Crab Nebular SLAC Accelerator seminar SLAC 15 June 2011 R. Buehler for the LAT collaboration and A. Tennant, E. Costa, D. Horns, C. Ferrigno, A.
More informationFermi Large Area Telescope:
Fermi Large Area Telescope: Early Results on Pulsars Kent Wood Naval Research Lab kent.wood@nrl.navy.mil for the Fermi LAT Collaboration Tokyo Institute of Technology 7 March 2009 K. Wood (NRL) 1/30 Fermi
More informationA pulsar wind nebula associated with PSR J as the powering source of TeV J
A pulsar wind nebula associated with PSR J2032+4127 as the powering source of TeV J2032+4130 Javier Moldón Netherlands Institute for Radio Astronomy Extreme Astrophysics in an Ever-Changing Universe Crete,
More informationarxiv: v1 [astro-ph.he] 19 Aug 2017
Phase Evolution of the Crab Pulsar between Radio and X-ray L.L. Yan 1,2,3, M.Y. Ge 1, J.P. Yuan 4, S.J. Zheng 1, F.J. Lu 1, Y. L. Tuo 1,2, H. Tong 4, S.N. arxiv:1708.05898v1 [astro-ph.he] 19 Aug 2017 Zhang
More informationTwo types of glitches in a solid quark star model
Two types of glitches in a solid quark star Enping Zhou Supervisor: Prof. Renxin Xu & Prof. Luciano Rezzolla 2015.01.13 1 Outline Motivation The The result D & C Challenges to the theories on pulsar glitches
More informationEmission-rotation correlation in pulsars: new discoveries with optimal techniques
Preprint 17 November 2015 Compiled using MNRAS LATEX style file v3.0 Emission-rotation correlation in pulsars: new discoveries with optimal techniques P. R. Brook, 1,2 A. Karastergiou, 1,3 S. Johnston,
More informationarxiv: v2 [astro-ph.he] 8 Jan 2010
Timing Behavior of the Magnetically Active Rotation-Powered Pulsar in the Supernova Remnant Kesteven 75 arxiv:0905.3567v2 [astro-ph.he] 8 Jan 2010 Margaret A. Livingstone 1, Victoria M. Kaspi Department
More informationDo soft gamma repeaters emit gravitational waves?
Astron. Astrophys. 336, 397 401 (1998) ASTRONOMY AND ASTROPHYSICS Do soft gamma repeaters emit gravitational waves? J.A. de Freitas Pacheco Observatoire de la Côte d Azur, B.P. 4229, F-06304 Nice Cedex
More informationTime-correlated structure in spin fluctuations in pulsars
Mon. Not. R. Astron. Soc. 426, 2507 2521 (2012) doi:10.1111/j.1365-2966.2012.21863.x Time-correlated structure in spin fluctuations in pulsars S. Price, 1 B. Link, 1 S. N. Shore 2 and D. J. Nice 3 1 Department
More informationEXTREME NEUTRON STARS
EXTREME NEUTRON STARS Christopher Thompson Canadian Institute for Theoretical Astrophysics University of Toronto SLAC Summer Institute 2005 Extreme Magnetism: B ~ 10 8-9 G (Low-mass X-ray binaries, millisecond
More informationPulsar Glitches: Gravitational waves at r-modes frequencies
Pulsar Glitches: Gravitational waves at r-modes frequencies LIGO-G1100022 I. Santiago 1, J. Clark 2, I. Heng 1, I. Jones 3, Graham Woan 1 1 University of Glasgow, 2 Cardiff University, 3 University of
More informationX-ray Properties of Rotation Powered Pulsars and Thermally Emitting Neutron Stars
X-ray Properties of Rotation Powered Pulsars and Thermally Emitting Neutron Stars George Pavlov (Penn State; Polytech.Univ SPb) Collaborators: Oleg Kargaltsev (George Washington Univ.) Bettina Posselt
More informationETA Observations of Crab Pulsar Giant Pulses
ETA Observations of Crab Pulsar Giant Pulses John Simonetti,, Dept of Physics, Virginia Tech October 7, 2005 Pulsars Crab Pulsar Crab Giant Pulses Observing Pulses --- Propagation Effects Summary Pulsars
More informationThe Same Physics Underlying SGRs, AXPs and Radio Pulsars
Chin. J. Astron. Astrophys. Vol. 6 (2006), Suppl. 2, 273 278 (http://www.chjaa.org) Chinese Journal of Astronomy and Astrophysics The Same Physics Underlying SGRs, AXPs and Radio Pulsars Biping Gong National
More informationVictoria Kaspi (McGill University, Montreal, Canada)
Victoria Kaspi (McGill University, Montreal, Canada) C. Espinoza M. Gonzalez M. Kramer M. Livingstone A. Lyne M. McLaughlin S. Olausen C.Y. Ng G. Pavlov W. Zhu Victoria Kaspi (McGill University, Montreal,
More informationSuperfluid instability in precessing neutron stars
Superfluid instability in precessing neutron stars Kostas Glampedakis SISSA, Trieste, Italy in collaboration with Nils Andersson & Ian Jones Soton October 2007 p.1/15 This talk Precessing neutron stars
More informationarxiv: v1 [astro-ph.he] 31 Mar 2015
Compact Stars in the QCD Phase Diagram IV (CSQCD IV) September 26-30, 2014, Prerow, Germany http://www.ift.uni.wroc.pl/~csqcdiv Braking index of isolated pulsars: open questions and ways forward arxiv:1503.09110v1
More informationThe Parkes Multibeam Pulsar Survey II. Discovery and timing of 120 pulsars
Mon. Not. R. Astron. Soc. 335, 275 290 (2002) The Parkes Multibeam Pulsar Survey II. Discovery and timing of 120 pulsars D. J. Morris, 1 G. Hobbs, 1 A. G. Lyne, 1 I. H. Stairs, 1,2 F. Camilo, 3 R. N. Manchester,
More informationX-ray emission properties vary with spin-down age. Crab-like pulsars (< 10 4 yrs)
X-ray emission properties vary with spin-down age Crab-like pulsars (< 10 4 yrs) X-ray emission properties vary with spin-down age Crab-like pulsars (< 10 4 yrs) Cooling neutron stars ( ~10 5-10 6 yrs)
More informationDeveloping a model for neutron star oscillations following starquakes
doi:10.1093/mnras/stu13 Developing a model for neutron star oscillations following starquakes L. Keer and D. I. Jones Mathematical Sciences, University of Southampton, University Road, Southampton SO17
More informationarxiv: v1 [astro-ph.he] 17 Dec 2015
Astronomy& Astrophysics manuscript no. 0000_FINAL_MAX_v2_printer c ESO 2018 February 10, 2018 What brakes the Crab pulsar? A. Čadež 1, L. Zampieri 2, C. Barbieri 2, 3, M. Calvani 2, G. Naletto 2, 4, 5,
More informationMagnetic Fields of Neutron Stars. Dipankar Bhattacharya IUCAA, Pune
Magnetic Fields of Neutron Stars Dipankar Bhattacharya IUCAA, Pune Neutron Stars harbour the strongest known magnetic fields in the universe: 10 8-10 15 G Magnetic fields determine their interaction with
More informationComponents of Galaxies Stars What Properties of Stars are Important for Understanding Galaxies?
Components of Galaxies Stars What Properties of Stars are Important for Understanding Galaxies? Temperature Determines the λ range over which the radiation is emitted Chemical Composition metallicities
More informationThe Parkes Multibeam Pulsar Survey - III. Young Pulsars and the Discovery and Timing of 200 Pulsars
Haverford College Haverford Scholarship Faculty Publications Physics 2003 The Parkes Multibeam Pulsar Survey - III. Young Pulsars and the Discovery and Timing of 200 Pulsars M. Kramer J. F. Bell R. N.
More informationarxiv:astro-ph/ v1 16 Oct 2003
Young Neutron Stars and Their Environments IAU Symposium, Vol. 218, 2004 F. Camilo and B. M. Gaensler, eds. Observational manifestations of young neutron stars: Spin-powered pulsars arxiv:astro-ph/0310451v1
More informationFlux-Vortex Pinning and Neutron Star Evolution
J. Astrophys. Astr. (September 2017) 38:44 Indian Academy of Sciences DOI 10.1007/s12036-017-9473-6 Review Flux-Vortex Pinning and Neutron Star Evolution M. ALI ALPAR Faculty of Engineering and Natural
More informationThe Parkes Multibeam Pulsar Survey II. Discovery and Timing of 120 Pulsars
Mon. Not. R. Astron. Soc. 000, 000 000 (2002) The Parkes Multibeam Pulsar Survey II. Discovery and Timing of 120 Pulsars D. J. Morris, 1 G. Hobbs, 1 A. G. Lyne, 1 I. H. Stairs, 2,1 F. Camilo, 3 R. N. Manchester,
More informationGravitational waves from neutron stars and the nuclear equation of state
Gravitational waves from neutron stars and the nuclear equation of state Ian Jones School of Mathematics, University of Southampton, UK University of Surrey, 18th October 2011 Context: the hunt for gravitational
More informationAn Introduction to Radio Astronomy
An Introduction to Radio Astronomy Second edition Bernard F. Burke and Francis Graham-Smith CAMBRIDGE UNIVERSITY PRESS Contents Preface to the second edition page x 1 Introduction 1 1.1 The role of radio
More informationPulsars and Radio Transients. Scott Ransom National Radio Astronomy Observatory / University of Virginia
Pulsars and Radio Transients Scott Ransom National Radio Astronomy Observatory / University of Virginia TIARA Summer School on Radio Astronomy 2016 Radio Transients Non-thermal emission Emission types
More informationarxiv: v2 [astro-ph.he] 31 Aug 2017
Draft version August 26, 2018 Preprint typeset using L A TEX style AASTeX6 v. 1.0 TIMING SOLUTIONS AND SINGLE-PULSE PROPERTIES FOR EIGHT ROTATING RADIO TRANSIENTS B.-Y. Cui 1 Department of Physics and
More information(Anomalous) X-Ray Pulsars. Vicky Kaspi. Montreal, Canada. Stanford December 16, 2004
(Anomalous) X-Ray Pulsars Vicky Kaspi Montreal, Canada Texas @ Stanford December 16, 2004 Summary Introduction to AXPs Evidence that AXPs are magnetars Open Issues and Recent Results: IR emission Transient
More informationarxiv:astro-ph/ v1 10 Nov 1999
Pulsar Astronomy 2000 and Beyond ASP Conference Series, Vol. e iπ + 1, 2000 M. Kramer, N. Wex, and R. Wielebinski, eds. The Parkes Multibeam Pulsar Survey arxiv:astro-ph/9911185v1 10 Nov 1999 F. Camilo
More informationThe Eight-meter-wavelength Transient Array
The Eight-meter-wavelength Transient Array Steve Ellingson Cameron Patterson John Simonetti Dept. of Electrical & Computer Engineering Dept. of Electrical & Computer Engineering Dept. of Physics Virginia
More informationA Major SGR-like Outburst and Rotation Glitch in the No-Longer-So-Anomalous X-ray Pulsar 1E
A Major SGR-like Outburst and Rotation Glitch in the No-Longer-So-Anomalous X-ray Pulsar 1E 2259+586 V. M. Kaspi, 1,2,3 F. P. Gavriil, 1 P. M. Woods, 4 J. B. Jensen 5 M. S. E. Roberts, 1,2 D. Chakrabarty
More informationarxiv: v1 [astro-ph.im] 3 Oct 2017
Starovoit E.D. Rodin A.E. On The Existence of Planets Around the Pulsar PSR B0329+54 E. D. Starovoit 1, 2, * 1, ** and A. E. Rodin 1 Pushchino Radio Astronomy Observatory, arxiv:1710.01153v1 [astro-ph.im]
More informationHigh Energy Astrophysics
High Energy Astrophysics Gamma-ray Bursts Giampaolo Pisano Jodrell Bank Centre for Astrophysics - University of Manchester giampaolo.pisano@manchester.ac.uk May 2011 Gamma-ray Bursts - Observations - Long-duration
More informationFermi-LAT Searches for gamma-ray pulsars
Fermi-LAT Searches for gamma-ray pulsars Pablo Saz Parkinson (pablo@scipp.ucsc.edu) for the LAT Collaboration Santa Cruz Institute for Particle Physics (SCIPP) IAU Symposium 291 Beijing, 20 August 2012
More informationComposite Supernova Remnants: Multiwavelength Observations and Theoretical Modelling
Composite Supernova Remnants: Multiwavelength Observations and Theoretical Modelling Okkie de Jager & Stefan Ferreira (NWU, South Africa) Regis Terrier & Arache Djannati-Ataï (Univ. of Paris VII, France)
More informationPulsars. The maximum angular frequency of a spinning star can be found by equating the centripetal and gravitational acceleration M R 2 R 3 G M
Pulsars Pulsating stars were discovered in 1967 via radio dipole antennae by Jocelyn Bell and Anthony Hewish Pulse period of PSR 1919+21 is 1.337 s Most pulsars have periods between 0.25 s and 2 s The
More informationPulsar Observations in Urumqi
Pulsar Observations in Urumqi Na Wang Xinjiang Astronomical Observatory, CAS Jul 8-12, 2013 FAN4, Hongkong University 1 Pulsar Observations Pulsar timing Pulsar emission The Future Jul 8-12, 2013 FAN4,
More informationDouble neutron star evolution from geometric constraints
Double neutron star evolution from geometric constraints Robert Ferdman University of East Anglia Bonn NS Workshop X 14 November 2016 A tale of two DNSs PSR J0737-3039A/B J1756 2251 Spin period (s) 0.0227
More informationGeneralized equation of state for cold superfluid neutron stars. Abstract
Generalized equation of state for cold superfluid neutron stars N. Chamel, 1 J. M. Pearson, 2 and S. Goriely 1 1 Institut d Astronomie et d Astrophysique, CP-226, Université Libre de Bruxelles, 1050 Brussels,
More information