Drifting subpulse phenomenon in pulsars
|
|
- Emery Anthony
- 5 years ago
- Views:
Transcription
1 Drifting subpulse phenomenon in pulsars Lofar perspective Janusz Gil J. Kepler Astronomical Institute University of Zielona Góra, Poland Collaborators: G. Melikidze, B. Zhang, U. Geppert, F. Haberl, J. Kijak, M. Sendyk
2 LOFAR sensitivity for PSRs LOFAR sensitivity for PSRs
3 Broadening of the profile As frequency decreases Evidence of the radius-to-frequency mapping and dipolar nature of magentic field lines in the emission region Sensitive observations below 160 MHz would be highly desirable
4 40 years after discovery of pulsars the actual mechanism of their coherent radio emission is still a mystery. Drifting subpulses, which seem to be a common phenomenon in pulsar radiation, is also a puzzle. The mechanism for drifting subpulses cannot be very different from the mechanism of observed radio emission......intrinsic property of radiation mechanism (Weltevrede, Edwards & Stappers 2006, A&A 445,243)
5 LRFS longitude (deg) 2DFS f=ccp cycles per period ccp LRFS - Longitude Resolved Fluctuation Spectrum P2 = ± P / cpp 2DFS - Two Dimensional Fluctuation Spectrum calulated along various slopes
6 Unbiased search for drifting subpulses in 187 (191) pulsars About 55 % (more) of drifting subpulse pulsars Weltevrede, Edwards & Stappers et al. 2006, ATNF 20. S/N a= r a = rp / h At frequencies lower than 320 MHz (LOFAR range) the ratio of detected drifting subpulses should be even higher
7 m ρ D d h rem Ω γ 1 m γ 1 ρ NS - opening angle Subpulses (drifting) can be resolved if h rp ρ ρ > γ 1 d D rpc α at the emission altitude R rem P (γ 2 )3.76 P1.35
8 Unbiased search for drifting subpulses in 187 (191) pulsars About 55 % (more) of drifting subpulse pulsars Weltevrede et al. 2006, ATNF 20. P 15 = 52 (1.2)3.76 P a= r a = rp / h Lorentz factor γ = 120
9 Subpulse drift Carousel model Sub-beams of radio emission presumably related to sparks operating just above the Polar Cap circulate around the magnetic axis P 2 P3 Subpulses in subsequent pulses arrive in phases determined by the apparent drift rate D = P2 / P3 l of s P4 l of s l of s P4 Ω = Hot PC heated by sparks - circulational periodicity? 2π P Polar cap rpc = P 0.5 cm
10 150 PSR B Perhaps the best example of Drifting subpulses phenomenon in pulsars P2 Apparent subpulse drift-bands P3 11P Modulation of intensity along drift-bands consistent with carousel model that is Sub-beams continue to circulate beyond the observed pulse-window (after van Leuven, Stappers et al..)
11 B α = 175 β = 7
12 PSR B LRFS
13 P1, P2, P3, P4 Apparent drift rate P2 P4 P3 Intrinsic drift rate P1 = P N P4 = P3 N number of rotating sub-beams P4 P4 Ruderman & Sutherland 1975 distance between driftbands in longitude between P P3 distance 1 driftbands in D = P2 / P3 distance between the same driftbands time interval to complete one rotation around the pole very difficult to measure, only 8 cases known!!!
14 PSR B Deshpande&Rankin 1999 P=1.089 s P3 = 1.87 P ^ P4 = 37.35P Number of sub-beams circulating around B P ~37P 4 N = P4 / P3 = 20
15 PSR B MHz observations Asgekar & Deshpande MHz observations Deshpande & Rankin f4 f3 Phased-resolved fluctuation spectrum 1/37 f4 = 1/ 37P P4 = P = 41s. Spectral analysis fully consistent with carousel model. Sub-beams continue to circulate around the beam axis beyond the pulse-window and reapear after the period needed to complete one full circulation around the magnetic axis 1 / 2.f15 3 = 1 / P3 1/14 f4 1/37=0.027 N = P4 / P3 = =20 Low frequency observations (LOFAR range) are more sensitive to low frequency modulations possibly related to the carousel circulation times
16 Radius-to-frequency mapping PSR B Frequency dependent beam size 430 MHz 103 MHz 103 MHz 35 MHz Arecibo PRAO Gauribidanur
17 B Arecibo 327 MHz Rankin et al. 2007
18 B P = 1.19 s P 15 = MHz E = erg / s P3 = P P4 = P N = P4 / P3 = 22 Arecibo Observatory 327 MHz Rankin et al. 2007
19 B Cartographic map of 20 subpulse beams circulating around the pole in about 37 pulsar periods Deshpande & Rankin, 1999 P = s l-of-s P 15 = 3.52 E = 1032 erg / s 430 MHz P3 = 1.86 P P4 = P N = P4 / P3 = 20 α,β (Intensity; pulse longitude and pulse number) (Intensity; polar colatitude and azimuth) Clear manifestation of subpulse sub-beams circulating around the magnetic axis Pulsar geometry known
20 B MHz Q-mode Erratic No organized drift visible Cartographic map impossible to make
21 103 MHz 1/37=0.026 B Q-mode (erratic) Suleymanova & Rankin 2006 Clear feature at 37 P as in the B-mode
22 Spark plasma circulates around the local magnetic pole on the Polar Cap with a specific period P_4, regardless it is fragmented into equally spaced filaments or operates in much less organized manner. One cannot swich off the E x B drift, except when there is no E or B.
23 Natural mechanism of subpulse drift E B Natural state of the magnetospheric plasma frozen into electric and magnetic field is corotation with NS (global corotation) υ cor = c( Ec Bs ) / B 2 = cec / Bs if E Ec then υ υ cor ρ = ρ GJ ρ ρ GJ corotation Polar Gap charge depletion Non-corotation plasma lags behind pulsar rotation and drifts with respects the polar cap surface with velocity υ dr υ dr = c( E Bs ) / B 2 = c E / Bs E Electric field associated with charge depletion ρ = ρ GJ ρ If plasma has transversal structure (spark filaments) then this inevitable E B drift should be observed in the form of drifting subpulses, and/or specific features in the intensity fluctuation spectrum
24 E B spark plasma circulation drift rate Linear velocity of the E x B drift (RS75) υd = c E cη ( 2π / cp ) Bs h 2π = =η h [cm/s] Bs Bs P Bs -actual surface magnetic field Bd -dipolar magnetic field at PC E - component of electric field caused by charge depletion ρ = ρ GJ ρ th = η ρ GJ ω = ν d / d = η (2π / P)(h / d ) Carusel angular speed Time interval to complete one circulation around periphery of PC P d P rp P4 = 2η h 2η h Gil, Melikidze & Geppert 2003
25 Within the model of the inner acceleration region to surface of the PC is heated to high temperatures by the back-flow of particles produced in sparking discharges. The heating rate is determined by the same value of the electric field that is involved in the E x B drifting phenomenon. thus, the observed drifting rate P d P rp P 4 = 2π d / υ d = 2η h 2η h and the observed heating rate (thermal X-ray luminosity from hot PC) Lx = σ Ts4 Abol = σ Ts4 Apc ( Bd / Bs ) should be strongly correlated.
26 Thermal X-ray luminosity from spark-heated polar cap Lx = ( P 15 / P )( P 4 / P ) 31 Efficiency 3 2 erg/s E = IΩ Ω Lx / E = (0.63 / I 45 ) ( P 4 / P) 2. Spin-down power I = I g cm 2 I 45 = 1 ± 0.15
27 X-ray Multi Mirror (XMM) Newton satelite telescope One revolution on an excentric orbit around the Earth takes 48 hours observations are not performed close to the Earth due to strong noise contamination
28 I 45 = 1 ± 0.15 Lx / E = (0.63 / I 45 ) ( P 4 / P) 2
29 Further low frequency LOFAR observation using 2DFS techniques should result P4 in Detection drifting subpulse pulsars and pussible more of be In nearbymore pulsars, in which thermal X-ray component fromdetermination hot polar cap can determined. Then the polar gap relationship Lx P4 2 can be tested further.
30
31 B L_x=2.78 x 10^30 erg/s E_dot=1.5 x 10^32 erg/s P_4=6 P Weltevrede et al P_3=(7+/-1) P P_4=P_3
32 Ruderman & Sutherland 1975 Strong non-dipolar Surface magnetic field Charge depletion maximum possible gap height ~MK Pure vacuum gap ρ = ρ GJ E ~ V /h Very strong electric field E E B drift much too fast as compared with observations Within the acceleration region the spark generated positrons are moving towards the magnetosphere while back-flow of electrons bombard the polar cap surface and heat it to MK temperatures Polar cap heating too intense and subpulse drift was too fast as compared with observations Modification needed
33 Future work New XMM-Newton observations of PSR B Ks performed in November 2006 Zhang, Gil, Melikidze, Geppert, Haberl Non-detected P4 / P = 14 ± 1 (Gupta, Gil, Kijak, Sendyk 2004) Proposal for XMM-Newton observations of PSR B accepted observation in summer 2006 (simultaneous radio observations with GMRT planned) Very promissing P4 / P = 15 ± 1 (Asgekar, Deshapande 2005) Proposal for XMM-Newton observations of PSR B will be submitted for the next cycle Very promissing P4 / P = 10 ± 1 (Weltevrede 2006; GMRT planned)
34 Co-rotating magnetosphere Ec = (Ω r / c) Bs Ec Bs = 0 V = 0 Force-free magnetosphere GJ69, RS75 No acceleration along B ρ c = (1 / 2π ) dive c = = Ω B s /( 2π c ) = ± B s / cp 2 υ cor = c ( Ec Bs ) / B = cec / Bs Co-rotating charge density Linear co-rotation velocity
35 The only two cases existing with both measurements B Lx / E ~ B Lx / E ~ P 3 / P ~ 33 P 3/ P ~ 37
36 Gil, Melikidze & Zhang 2006 η = (1 / 2π )( P / P3 ) Screening factor ~( ) only few % of GJ plasma involved in acceleration Lx = ( P 15 / P )( P 3 / P ) X-ray bolometric luminosity erg/s 10( 28 29) erg / s Lx / E = 0.63 ( P 3 / P) 2 Ts = ( K ) A4 6 A4 = Abol /(10 4 m 2 ) ~ P 15 Efficiency ~ P 0.75 ( P3 / P ) 0.5 Ts ~ (2 3) MK
37 Pulsars are fast rotating and strongly magnetized Neutron Stars (NS) Corotation with NS E*B=0 Polar Cap (PC) region of NS surface connected to ISM via open magnetic field lines penetrating the Light Cylinder Charged particles will leave through LC due to inertia and create charge depletion just above the PC. If this charge cannot be re-supplied by the PC surface (strong binding) then huge accelerating potential drop will occur along the open magnetic field lines close to the PC surface.
38 1.4 GHz 0.32 GHz 1.4 GHz Weltevrede, Edwards & Stappers et al. 2006, 2007
Investigating Emission Mechanisms by Mapping Pulsar Magnetospheres in 3D
Investigating Emission Mechanisms by Mapping Pulsar Magnetospheres in 3D Candidacy Presentation, 22 Aug 2016 Sam McSweeney Supervisors: Ramesh Bhat Steven Tremblay Avinash Deshpande Trying to figure out
More informationFORMATION OF A PARTIALLY SCREENED INNER ACCELERATION REGION IN RADIO PULSARS: DRIFTING SUBPULSES AND THERMAL X-RAY EMISSION FROM POLAR CAP SURFACE
The Astrophysical Journal, 650:1048 1062, 2006 October 20 # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. FORMATION OF A PARTIALLY SCREENED INNER ACCELERATION REGION IN
More informationXMM-NEWTON OBSERVATIONS OF RADIO PULSARS B AND B AND IMPLICATIONS FOR THE PULSAR INNER ACCELERATOR
The Astrophysical Journal, 686:497 507, 2008 October 10 # 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A. XMM-NEWTON OBSERVATIONS OF RADIO PULSARS B0834+06 AND B0826 34
More informationDrifting2 or Analysis of temporal evolution of drifting subpulse phenomenon
Drifting2 or Analysis of temporal evolution of drifting subpulse phenomenon Maciej Serylak Ben Stappers Patrick Weltevrede 4th ESTRELA workshop Bologna Italy 19-22.01.2009 Outline Pulsar (very) short overview
More informationProbing drifting and nulling mechanisms through their interaction in PSR B
A&A 399, 223 229 (2003) DOI: 10.1051/0004-6361:20021630 c ESO 2003 Astronomy & Astrophysics Probing drifting and nulling mechanisms through their interaction in PSR B0809+74 A. G. J. van Leeuwen 1, B.
More informationarxiv: v1 [astro-ph.sr] 27 Jun 2012
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 10 September 2018 (MN LATEX style file v2.2) Radiation properties of extreme nulling pulsar J1502 5653 arxiv:1206.6156v1 [astro-ph.sr] 27 Jun 2012
More informationarxiv: v2 [astro-ph.sr] 28 Jul 2014
Mon. Not. R. Astron. Soc. 000, 1?? (2014) Printed 29 July 2014 (MN LATEX style file v2.2) arxiv:1402.2675v2 [astro-ph.sr] 28 Jul 2014 Explaining the subpulse drift velocity of pulsar magnetosphere within
More informationRadio Pulsar Phenomenology: What can we learn from pulsar profiles? Simon Johnston (ATNF, CSIRO) Aris Karastergiou (Oxford, UK)
Radio Pulsar Phenomenology: What can we learn from pulsar profiles? Simon Johnston (ATNF, CSIRO) Aris Karastergiou (Oxford, UK) Outline Brief tour through the basics P-Pdot diagram The Rotating Vector
More informationExplaining the subpulse drift velocity of pulsar magnetosphere within the space-charge limited flow model
doi:10.1093/mnras/stu1486 Explaining the subpulse drift velocity of pulsar magnetosphere within the space-charge limited flow model Viktoriya S. Morozova, 1,2 Bobomurat J. Ahmedov 3,4,5 and Olindo Zanotti
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 informationarxiv:astro-ph/ v1 30 Oct 2000
Vacuum gaps in pulsars and PSR J2144 3933 Janusz Gil 1 and Dipanjan Mitra 2 arxiv:astro-ph/0010603v1 30 Oct 2000 1 J. Kepler Astronomical Center, Lubuska 2, 65-265, Zielona Góra, Poland email: jag@astro.ca.wsp.zgora.pl
More informationSingle-Pulse Studies : Polar Maps of Pulsars B and B
Chapter 5 Single-Pulse Studies : Polar Maps of Pulsars B0943+10 and B0834+06 In the last chapter, we dwelled on the fluctuation properties of a few,bright pulsars observable using GEETEE at 35 MHz. We
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 informationGeometry: The Sine Qua Non For Understanding the Pulsar Magnetosphere (and Gamma-ray Emission) Matthew Kerr obo Many
Geometry: The Sine Qua Non For Understanding the Pulsar Magnetosphere (and Gamma-ray Emission) Matthew Kerr obo Many kerrm@stanford.edu Parkes 50 th Birthday Party, Parkes Telescope, November 2 nd, 2011
More informationWhat is the Physics of Pulsar Radio Emission? A white paper submitted to the Astro2010 Science Frontier Panel Stars and Stellar Evolution
What is the Physics of Pulsar Radio Emission? A white paper submitted to the Astro2010 Science Frontier Panel Stars and Stellar Evolution T. H. Hankins (575) 835-7326 New Mexico Institute of Mining and
More informationThe annular gap model: radio and Gamma-ray emission of pulsars. Qiao,G.J. Dept. of Astronomy, Peking Univ.
The annular gap model: radio and Gamma-ray emission of pulsars Qiao,G.J. Dept. of Astronomy, Peking Univ. The annular gap model of pulsars I. The Annular gap What is the Annular gap? What is the advantage
More informationUnderstanding the pulsar magnetosphere through first-principle simulations
Understanding the pulsar magnetosphere through first-principle simulations Alexander Y. Chen In collaboration with: Andrei Beloborodov Rui Hu The Many Faces of Neutron Stars August 25, 2015 Pulsars: Rotating
More informationThe topology and polarisation of subbeams associated with the drifting subpulse emission of pulsar B IV. Q-to-B-mode recovery dynamics
A&A 453, 679 686 (2006) DOI: 10.1051/0004-6361:20054140 c ESO 2006 Astronomy & Astrophysics The topology and polarisation of subbeams associated with the drifting subpulse emission of pulsar B0943+10 IV.
More informationAn Annular Gap Acceleration Model for γ-ray Emission of Pulsars
Chin. J. Astron. Astrophys. Vol. 7 (2007), No. 4, 496 502 (http://www.chjaa.org) Chinese Journal of Astronomy and Astrophysics An Annular Gap Acceleration Model for γ-ray Emission of Pulsars Guo-Jun Qiao
More informationdiscovers a radio-quiet gamma-ray millisecond Journal Group
Einstein@Home discovers a radio-quiet gamma-ray millisecond pulsar @CHEA Journal Group Contribution of the paper Contribution of the paper Millisecond Pulsars (MSPs) Ver y rapid rotating neutron star
More informationProgress in Pulsar detection
Progress in Pulsar detection With EINSTEIN & EXOSAT: 7 radio pulsars detected in X-rays With ROSAT, ASCA & BSAX: 33 radio pulsars detected in X-rays After ~8 yrs with XMM & Chandra: 81 radio pulsars detected
More informationAn empirical model for the beams of radio pulsars
Mon. Not. R. Astron. Soc. 380, 1678 1684 (2007) doi:10.1111/j.1365-2966.2007.12237.x An empirical model for the beams of radio pulsars Aris Karastergiou 1 and Simon Johnston 2 1 IRAM, 300 rue de la Piscine,
More informationarxiv: v1 [astro-ph.he] 3 Nov 2011
2011 Fermi Symposium, Roma., May. 9-12 1 Gamma-Ray Pulsar Light Curves in Vacuum and Force-Free Geometry Alice K. Harding 1, Megan E. DeCesar 1,2, M. Coleman Miller 2, Constantinos Kalapotharakos 1,2,
More informationMagneto-Thermal Evolution of Isolated Neutron Stars
Magneto-Thermal Evolution of Isolated Neutron Stars Ulrich R.M.E. Geppert J. Gil Institute of Astronomy Zielona Gòra 1 B t = c2 4πσ B + c 4πen e B B Ԧv hyd + Ԧv amb B Q T Ohmic decay: σ = σ(t) Ԧv hyd ~
More informationElectrodynamics of neutron star magnetospheres
of neutron star magnetospheres An example of non-neutral plasma in astrophysics Centre d Étude des Environnements Terrestre et Planétaires - Vélizy, FRANCE Laboratoire de Radio Astronomie, École Normale
More informationThe Radio and X-ray Mode-Switching Pulsar PSR B
J. Astrophys. Astr. (September 2017) 38:54 Indian Academy of Sciences DOI 10.1007/s12036-017-9464-7 Review The Radio and X-ray Mode-Switching Pulsar PSR B0943+10 SANDRO MEREGHETTI 1, and MICHELA RIGOSELLI
More informationSimultaneous XMM-Newton Radio Observations of the Mode-switching Radio Pulsar PSR B Wim Hermsen 1,2
Simultaneous XMM-Newton Radio Observations of the Mode-switching Radio Pulsar PSR B1822-09 Wim Hermsen 1,2 Collaborators: J.W.T. Hessels 3,2, L. Kuiper 1, J. van Leeuwen 3,2, D. Mitra 4, J.M. Rankin 2,5,
More informationA New Model for the Beams of Radio Pulsars
, IRAM, France E-mail: aris.karastergiou@gmail.com Simon Johnston, ATNF, Australia With the discovery of new classes of radio-emitting neutron stars, such as RRATS and the radio emitting magnetar, understanding
More informationSpectral Analysis of the Double Pulsar PSR J with XMM-Newton
Spectral Analysis of the Double Pulsar PSR J0737-3039 with XMM-Newton * E. Egron, A. Pellizzoni, M.N. Iacolina, A. Pollock, et al. INAF - Osservatorio Astronomico di Cagliari, Italy * ESAC, Madrid, Spain
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 informationJoeri van Leeuwen An X-raydio switcheroo!
Joeri van Leeuwen Joeri van Leeuwen Joeri van Leeuwen Joeri van Leeuwen Joeri van Leeuwen Joeri van Leeuwen Team Wim Hermsen Lucien Kuiper Dipanjan Mitra Jason Hessels Jelle de Plaa Joanna Rankin Ben Stappers
More informationParticle acceleration and pulsars
Meudon, nov. 2013 p. 1/17 Particle acceleration and pulsars Fabrice Mottez LUTH - Obs. Paris-Meudon - CNRS - Univ. Paris Diderot Meudon, nov. 2013 p. 2/17 Pulsars (PSR) and pulsar wind nebulae (PWNe) Mostly
More informationThe Mystery of Fast Radio Bursts and its possible resolution. Pawan Kumar
The Mystery of Fast Radio Bursts and its possible resolution Outline Pawan Kumar FRBs: summary of relevant observations Radiation mechanism and polarization FRB cosmology Wenbin Lu Niels Bohr Institute,
More informationElectrodynamics of Magnetized Rotators Anatoly Spitkovsky,, UC Berkeley
Electrodynamics of Magnetized Rotators Anatoly Spitkovsky,, UC Berkeley Magnetized rotators are ubiquitous: pulsars, AGN, GRBs (?) Rotation very efficient at long-term energy storage Extraction of rotational
More informationX-ray Observations of Rotation Powered Pulsars
X-ray Observations of Rotation Powered Pulsars George Pavlov (Penn State) Oleg Kargaltsev (George Washington Univ.) Martin Durant (Univ. of Toronto) Bettina Posselt (Penn State) Isolated neutron stars
More informationTESTING PULSAR RADIATION MODELS USING AN α-weak-dependent ALTITUDE RATIO
The Astrophysical Journal, 703:507 56, 2009 September 20 C 2009. The American Astronomical Society. All rights reserved. Printed in the U.S.A. doi:0.088/0004-637x/703//507 TESTING PULSAR RADIATION MODELS
More informationRadio emission regions in pulsars
Mon. Not. R. Astron. Soc. 299, 855 861 (1998) Radio emission regions in pulsars Jaroslaw Kijak 1;2 and Janusz Gil 1 1 Astronomy Centre, Pedagogical University, Lubuska 2, PL-65-265 Zielona Góra, Poland
More informationCooling Limits for the
Cooling Limits for the Page et al. 2004 Youngest Neutron Stars Cooling from the Youngest NSs SNR Zone NSs younger than ~50 kyr offer strong constraints on rapid cooling - the associated physical processes
More informationarxiv: v1 [astro-ph] 17 Jul 2007
Mon. Not. R. Astron. Soc. 000, 1 8 (2005) Printed 6 November 27 (MN LATEX style file v2.2) An empirical model for the beams of radio pulsars Aris Karastergiou 1 & Simon Johnston 2 1 IRAM, 300 rue de la
More informationThe double pulsar as Jupiter: tomography of magnetosphere and a new test of General Relativity. Maxim Lyutikov (Purdue U.)
The double pulsar as Jupiter: tomography of magnetosphere and a new test of General Relativity Maxim Lyutikov (Purdue U.) The Double Pulsar: sixth most important scientific discovery of 2004 (Science)
More informationThe pulsars magnetospheres
The pulsars magnetospheres journée plasma UPMC - janvier 2009 Fabrice Mottez, très redevable à Jérôme Pétri (Obs. Strasbourg) qui a fourni un matériel abondant dérivé de sa présentation à Cargèse en 2005
More informationThe Nature of Coherent Radio Emission from Pulsars
J. Astrophys. Astr. (2017) 123: #### DOI 12.3456/s78910-011-012-3 The Nature of Coherent Radio Emission from Pulsars Dipanjan Mitra 123 1, National Center for Radio Astrophysics, TIFR, Pune 411007, India.
More informationThe Fermi Large Area Telescope View of Gamma-ray Pulsars
The Fermi Large Area Telescope View of Gamma-ray Pulsars 1 Tyrel J. Johnson, D.A. Smith2, M. Kerr3, & P. R. den Hartog4 on behalf of the Fermi Large Area Telescope Collaboration and the Pulsar Timing and
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 informationX-ray and Gamma-ray. Emission Pulsars and Pulsar Wind Nebulae. K.S. Cheng Department of Physics University of Hong Kong Hong Kong, China
X-ray and Gamma-ray Emission Pulsars and Pulsar Wind Nebulae K.S. Cheng Department of Physics University of Hong Kong Hong Kong, China X-ray luminosity (L x ) vs spin-down power (L sd ) Becker and Trumper
More informationarxiv: v1 [astro-ph.sr] 23 Jul 2014
Accepted for publication in The Astrophysical Journal Preprint typeset using L A TEX style emulateapj v. 5/2/11 INTER-RELATIONSHIP BETWEEN THE TWO EMISSION CONES OF B1237+25 Yogesh Maan and Avinash A.
More informationEmission Altitude r/r Pulsar Period P [s] 4.85 GHz
Mon. Not. R. Astron. Soc., { (1997) Radio emission regions in pulsars Jaroslaw Kijak 1;2 and Janusz Gil 1 1 Astronomy Centre, Pedagogical University, Lubuska 2, PL-65-265 Zielona Gora, Poland 2 Max-Planck-Institut
More informationNon-thermal emission from Magnetic White Dwarf binary AR Scorpii
Non-thermal emission from Magnetic White Dwarf binary AR Scorpii Jumpei Takata (Huazhong University of Science and Technology, China) On behalf of Y. Hui (HUST), C.-P. Hu, K.S. Cheng (HKU, HK), L.C.C.
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 information12 Pulsars: overview and some physics
Physics 426 Notes Spring 2009 59 12 Pulsars: overview and some physics Carroll & Ostlie present the basic picture in some detail; another good reference is Longair s High Energy Astrophysics. In these
More informationarxiv:astro-ph/ Feb 2000
The spark-associated soliton model for pulsar radio emission George I. Melikidze 1;, Janusz A. Gil 1 and Avtandil D. Pataraya gogi@astro.ca.sp.zgora.pl, jag@astro.ca.sp.zgora.pl ABSTRACT arxiv:astro-ph/000458
More informationCoherent and continuous radio emission from Magnetic Chemically Peculiar stars
Coherent and continuous radio emission from Magnetic Chemically Peculiar stars C. Trigilio 1 P. Leto 1, G. Umana 1, C.Buemi 1, F.Leone 2 1 INAF-OACT, 2 UNICT Magnetic Chemically Peculiar stars MS B-A type
More informationPulsars & Double Pulsars:! A Multiwavelength Approach!
Pulsars & Double Pulsars:! A Multiwavelength Approach! Marta Burgay INAF, Cagliari Observatory! X-Ray Astronomy 2009 Bologna 08/09/2009! Spin-Powered Pulsars! Radio! High Energy! RRATs! Magnetars! XDINS!
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 informationTheory of High Energy Emission from Pulsars. K.S. Cheng Department of Physics University of Hong Kong Hong Kong, China
Theory of High Energy Emission from Pulsars K.S. Cheng Department of Physics University of Hong Kong Hong Kong, China Outline Introduction :Accelerators polar gap, slot gap and outer gap Relevant observed
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 informationDistinct Features of Pulsar Polar-Gap Emission at the High-Energy Spectral Cutoff
The Universe Viewed in Gamma-Rays 1 Distinct Features of Pulsar Polar-Gap Emission at the High-Energy Spectral Cutoff Jaros law DYKS and Bronis law RUDAK Nicolaus Copernicus Astronomical Center, Rabiańska
More informationarxiv: v1 [astro-ph.he] 20 May 2016
Astronomy& Astrophysics manuscript no. psrsalsa c ESO 2016 May 23, 2016 Investigation of the bi-drifting subpulses of radio pulsar B1839 04 utilising the open-source data-analysis project PSRSALSA P. Weltevrede
More informationThe Structure of Integrated Pulse Profiles. Μ. Vivekanand and V. Radhakrishnan Raman Research Institute, Bangalore
J. Astrophys. Astr. (1980) 1, 119 128 The Structure of Integrated Pulse Profiles Μ. Vivekanand and V. Radhakrishnan Raman Research Institute, Bangalore 560080 Received 1980 July 8; accepted 1980 October
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 informationSubpulse modulation, moding and nulling of the five-component pulsar B
Mon. Not. R. Astron. Soc. 406, 237 246 (2010) doi:10.1111/j.1365-2966.2010.16703.x Subpulse modulation, moding and nulling of the five-component pulsar B1737+13 Megan M. Force 1 and Joanna M. Rankin 1,2
More informationRotation-Powered Pulsars
Rotation-Powered Pulsars As we discussed last time, the extreme properties of neutron stars (gravity, density, magnetic field) make them excellent objects to study to see how physics operates in unusual
More informationExplosive reconnection of the double tearing mode in relativistic plasmas
Explosive reconnection of the double tearing mode in relativistic plasmas Application to the Crab Jérôme Pétri 1 Hubert Baty 1 Makoto Takamoto 2, Seiji Zenitani 3 1 Observatoire astronomique de Strasbourg,
More informationPhenomenology of pulsar B s rotating subbeam system. II. Carousel configuration and polarization ABSTRACT
A&A 455, 215 221 (2006) DOI: 10.1051/0004-6361:20054417 c ESO 2006 Astronomy & Astrophysics Phenomenology of pulsar B0809+74 s rotating subbeam system II. Carousel configuration and polarization Joanna
More informationStudies of interstellar scintillation and scattering of pulsars using polish LOFAR stations
Studies of interstellar scintillation and scattering of pulsars using polish LOFAR stations Wojciech Lewandowski Janusz Gil Institute for Astronomy, University of Zielona Góra The interstellar medium (ISM)
More informationAstronomy 421. Lecture 23: End states of stars - Neutron stars
Astronomy 421 Lecture 23: End states of stars - Neutron stars 1 Outline Neutron stars Pulsars properties distribution emission mechanism evolution 2 Neutron stars Typical values: M ~ 1.4M R ~ 10 km ρ ~
More informationOuter-magnetospheric model for Vela-like pulsars: formation of sub-gev spectrum
Mon. Not. R. Astron. Soc. 348, 4 49 (004) Outer-magnetospheric model for -like pulsars: formation of sub-gev spectrum J. Takata, S. Shibata and K. Hirotani 3 Graduate School of Science and Engineering,
More informationSources of GeV Photons and the Fermi Results
Sources of GeV Photons and the Fermi Results 1. GeV instrumentation and the GeV sky with the Fermi Gamma-ray Space Telescope 2. First Fermi Catalog of Gamma Ray Sources and the Fermi Pulsar Catalog 3.
More informationLecture 3 Pulsars and pulsar wind nebulae
Lecture 3 Pulsars and pulsar wind nebulae Pulsars Characteristic parameters Pulsar wind nebulae Properties Evolution Exotic central compact objects - Magnetars The Crab Pulsar http://www.jb.man.ac.uk/~pulsar/education/sounds/sounds.html
More informationStudies of single pulses from two millisecond pulsars ares presented. The energy
Chapter 6 Individual Pulses in Millisecond Pulsars 6.1 Summary Studies of single pulses from two millisecond pulsars ares presented. The energy distribution of PSR B1534+12 is similar to that of slow pulsars,
More informationProbing the Pulsar Wind in the TeV Binary System
Probing the Pulsar Wind in the TeV Binary System -PSR B1259-63/SS2883- Jumpei Takata (University of Hong Kong) Ronald Taam (TIARA, Taiwan) 1 Outline 1, Introduction -TeV binaries -Fermi observation -PSR
More informationFERMI. YOUNG PULSAR SPECTRA WITH THE LAT FERMI TELESCOPE Ateliers pulsars. 25 novembre 2008 Damien Parent. Gamma-ray Large Area Space Telescope
FERMI Gamma-ray Large Area Space Telescope YOUNG PULSAR SPECTRA WITH THE LAT FERMI TELESCOPE Ateliers pulsars 25 novembre 2008 1 Topics 1. Young pulsars, our best candidates 2 examples : J0205+6449 and
More informationFermi-Large Area Telescope Observations of Pulsar Wind Nebulae and their associated pulsars
Fermi-Large Area Telescope Observations of Pulsar Wind Nebulae and their associated pulsars Marie-Hélène Grondin CENBG, Bordeaux (France) on behalf of the Fermi-LAT Collaboration and the Pulsar Timing
More informationarxiv:astro-ph/ v1 23 Aug 2005
Coherent Curvature Radiation and Proton Counterflow in the Pulsar Magnetosphere Katsuaki Asano arxiv:astro-ph/0508474v1 23 Aug 2005 Division of Theoretical Astronomy, National Astronomical Observatory
More informationPeriodic Nulls in Pulsar B
Mon. Not. R. Astron. Soc. 000, 1 7 (2007) Printed 22 April 2007 (MN LATEX style file v2.2) Periodic Nulls in Pulsar B1133+16 Jeffrey L. Herfindal and Joanna M. Rankin Physics Department, University of
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 informationPulsars and Timing. Lucas Guillemot, Ismaël Cognard.!! Rencontre CTA, Observatoire de Paris, 28/11/13
Pulsars and Timing Lucas Guillemot, Ismaël Cognard Rencontre CTA, Observatoire de Paris, 28/11/13 Pulsars radio emission cone γ-ray emission fan beam Pulsars are rapidly rotating highly magnetized neutron
More informationTerm Project: Magnetic Fields of Pulsars
Term Project: Magnetic Fields of Pulsars Jamie Lomax May 14, 2008 Contents Introduction-A brief introduction to pulsars. (Page 1) Observing Pulsars-An example of how pulsars are observed. (Page 1) Magnetic
More informationOn the pulse-width statistics in radio pulsars I. Importance of the interpulse emission
Mon. Not. R. Astron. Soc. 414, 1314 1328 (2011) doi:10.1111/j.1365-2966.2011.18471.x On the pulse-width statistics in radio pulsars I. Importance of the interpulse emission Krzysztof Maciesiak, 1 Janusz
More informationThe Double Pulsar:! A Decade of Discovery! (and what you can do over the next decade with FAST!)
The Double Pulsar:! A Decade of Discovery! (and what you can do over the next decade with FAST!) Maura McLaughlin West Virginia University 20 May 2014 : Double neutron star systems" The pulsar catalog
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 informationRadio Pulsar Death. Bing Zhang
Vol.44 Suppl. ACTA ASTRONOMICA SINICA Feb., 2003 Radio Pulsar Death Bing Zhang (The Pennsylvania State University, USA) ABSTRACT Pulsar radio emission is believed to be originated from the electronpositron
More informationPulsar Overview. Kevin Stovall NRAO
Pulsar Overview Kevin Stovall NRAO IPTA 2018 Student Workshop, 11 June, 2018 Pulsars Pulsars ~2,700 pulsars known Act as clocks, therefore provide a means for studying a variety of physical phenomena Strongly
More informationEmission from Isolated Neutron Stars. Observations and model applications
Thermal Emission from Isolated Neutron Stars Theoretical aspects Observations and model applications Slava Zavlin (MPE, Garching) A Short History Chi & Salpeter (1964) and Tsuruta (1964): thermal radiation
More informationELECTROMAGNETIC RADIATION FROM PULSARS : AND MAGNETARS 4
ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES Volume 466 J ELECTROMAGNETIC RADIATION FROM PULSARS : AND MAGNETARS 4 Proceedings of a conference held at University of Zielona Gora, Zielona Gora,
More informationRadio Emission Physics in the Crab Pulsar. J. A. Eilek & T. H. Hankins New Mexico Tech, Socorro NM, USA
Radio Emission Physics in the Crab Pulsar J. A. Eilek & T. H. Hankins New Mexico Tech, Socorro NM, USA Summary for Impatient Readers We are carrying out ultra-high time resolution observations in order
More information- Synchrotron emission: A brief history. - Examples. - Cyclotron radiation. - Synchrotron radiation. - Synchrotron power from a single electron
- Synchrotron emission: A brief history - Examples - Cyclotron radiation - Synchrotron radiation - Synchrotron power from a single electron - Relativistic beaming - Relativistic Doppler effect - Spectrum
More informationRecent Radio Observations of Pulsars
Recent Radio Observations of Pulsars R. N. Manchester Australia Telescope National Facility, CSIRO Sydney Australia Summary A pulsar census Recent pulsar surveys Pulse modulation and drifting subpulses
More informationPolarization of high-energy emission in a pulsar striped wind
Paris - 16/1/26 p.1/2 Polarization of high-energy emission in a pulsar striped wind Jérôme Pétri Max Planck Institut für Kernphysik - Heidelberg Paris - 16/1/26 p.2/2 Outline 1. The models 2. The striped
More informationToward an Empirical Theory of Pulsar Emission. XII. Exploring the Physical Conditions in Millisecond Pulsar Emission Regions
2017. The American Astronomical Society. All rights reserved. https://doi.org/10.3847/1538-4357/aa7b73 Toward an Empirical Theory of Pulsar Emission. XII. Exploring the Physical Conditions in Millisecond
More informationThe Stellar Graveyard Neutron Stars & White Dwarfs
The Stellar Graveyard Neutron Stars & White Dwarfs White Dwarfs White dwarfs are the remaining cores of low-mass (M < 8M sun ) stars Electron degeneracy pressure supports them against gravity Density ~
More informationEditorial comment: research and teaching at UT
Wednesday, March 23, 2017 Reading for Exam 3: Chapter 6, end of Section 6 (binary evolution), Section 6.7 (radioactive decay), Chapter 7 (SN 1987A), Background: Sections 3.1, 3.2, 3.3, 3.4, 3.5, 3.8, 3.10,
More informationPulsar Wind Nebulae. Pennsylvania State University. General outlook Chandra results Polarization in radio and optical X-ray polarization
Pulsar Wind Nebulae George Pavlov & Oleg Kargaltsev Pennsylvania State University General outlook Chandra results Polarization in radio and optical X-ray polarization Pulsar Wind Nebulae: extended objects
More informationPoS(Texas 2010)130. Geometric modelling of radio and γ-ray light curves of 6 Fermi LAT pulsars
Geometric modelling of radio and γ-ray light curves of 6 Fermi LAT pulsars A. S. Seyffert a,b, C. Venter a, O. C. de Jager a, and A. K. Harding b a Centre for Space Research, North-West University, Potchefstroom
More informationProbing Pulsar Winds With X-rays!
Probing Pulsar Winds With X-rays! Collaborators:! Bryan Gaensler! Steve Reynolds! David Helfand! Stephen Ng! Anne Lemiere! Okkie de Jager! Stephanie LaMassa! Jack Hughes! PWNe and Their SNRs! PWN Shock
More informatione - -e + pair production in pulsar magnetospheres
e - -e + pair production in pulsar magnetospheres Kouichi HIROTANI TIARA/ASIAA-NTHU, Taiwan IPMU December 8, 2009 Crab nebula: Composite image of X-ray [blue] and optical [red] 1 Introduction: The γ-ray
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 informationae Bhadik Singie-pulse Studies of Pulsars at Decameter Wavelengths DEPARTMENT OF PHYSICS BANGALORE (INDIA) &11PmiUM!
Singie-pulse Studies of Pulsars at Decameter Wavelengths ae Bhadik &11PmiUM! jnvr the depw 4 DEPARTMENT OF PHYSICS INDIAN INSTITUTE OF SCIENCE BANGALORE-560 012 (INDIA) Declaration I hereby declare that
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. in this talk. Pulsar timing. Pulsar timing. Pulsar timing. Pulsar timing. How to listen to what exotic. are telling us! Paulo César C.
How to listen to what exotic Pulsars are telling us! in this talk 1. 2. 3. Test of gravitational theories using binary pulsars 4. Probing the equation of state of super-dense matter Paulo César C. Freire
More information