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Radio Pulsars Chania, Crete 26–29 August 2002 Schedule, Abstracts, & Participant List A meeting to honor the contributions of Andrew Lyne, Dick Manchester, and Joe Taylor, celebrating a century of combined work on pulsars on the occasion (more or less) of their sixtieth birthdays. Meeting Chairs: Matthew Bailes, David Nice, Steve Thorsett. Scientific Organizing Committee: Zaven Arzoumanian, Matthew Bailes, Dipankar Bhattacharya, Fernando Camilo, Vicky Kaspi, Michael Kramer, Dunc Lorimer, David Nice, Fred Rasio, Ingrid Stairs, Steve Thorsett.

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Page 1: Radio Pulsars Chania, Crete 26–29 August 2002 › research › conferences › ... · the work by Kaspi, Taylor, & Ryba (1994) and other authors. The results required combining

Radio PulsarsChania, Crete

26–29 August 2002

Schedule, Abstracts, & Participant List

A meeting to honor the contributions of Andrew Lyne, DickManchester, and Joe Taylor, celebrating a century of combined workon pulsars on the occasion (more or less) of their sixtieth birthdays.

Meeting Chairs:Matthew Bailes, David Nice, Steve Thorsett.

Scientific Organizing Committee:Zaven Arzoumanian, Matthew Bailes, Dipankar Bhattacharya, Fernando Camilo,Vicky Kaspi, Michael Kramer, Dunc Lorimer, David Nice, Fred Rasio, Ingrid Stairs,Steve Thorsett.

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Monday, 26 August

Morning Session Chair: John Seiradakis

Opening9:00 Welcome9:05 Donald Backer Pulsars: Old Puzzles–New Challenges

Timing and Binary Observations 19:50 Matthew Bailes Parkes Precision Pulsar Timing

10:20 Willem van Straten Annual-Orbital Parallax and Nearby Binary Millisecond Pulsars10:40 Break

Timing and Binary Observations 211:00 Zaven Arzoumanian PSR B0655+64: A Stalwart Control Experiment11:20 David Nice Binary Pulsar Timing at Arecibo11:50 Andrea Lommen New Limits on Gravitational Wave Background Using Pulsars12:10 Alex Wolszczan Pulsar Planets: Status and Future Prospects

Afternoon Session Chair: Roger Romani

Timing and Binary Observations 316:00 Ingrid Stairs The Massive Binary Pulsar J1740−305216:20 Steve Ord The Scintillation Velocity of the Relativistic Binary J1141−654516:40 Joel Weisberg Binary Pulsar B1913+16: Twenty-Seven Years and Going Strong17:10 Michael Kramer Geodetic Precession in PSR B1913+1617:40 Break

Timing and Binary Observations & Theory 418:00 Na Wang Pulsar Timing and Scintillation Observations at Urumqi Observatory18:20 Johnson Urama Long-Term Timing Analysis of Some Pulsars18:40 Sergei Kopeikin Relativistic Effect of Retardation of Gravity19:00 Graham Woan The Search for Gravitational Waves from Pulsars

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Tuesday, 27 August

Morning Session Chair: Ingrid Stairs

Searches9:00 Andrew Lyne The Development of Pulsar Search Techniques9:40 Joseph Taylor Reflections on 34 Years of Finding Pulsars

10:00 Maura McLaughlin New Pulsars from Arecibo Drift Scan Searches10:20 Bryan Jacoby A Search for Millisecond Pulsars at High Galactic Latitude10:40 Break

Young Neutron Stars11:00 Fernando Camilo Deep Searches for Young Pulsars11:30 Victoria Kaspi Magnetars12:00 Andrea De Luca The Radio Quiet Neutron Star 1E1207−5209 Observed with XMM-Newton12:20 David Kaplan The Radio Quiet RXJ0720.4−3125

Afternoon Session Chair: Joel Weisberg

The Pulsar Signal16:00 Yashwant Gupta Emission Beam Geometry of Multi-Component Pulsars16:20 Fredrick Jenet The Radio Pulsar Signal: Statistics of Single Pulses16:40 Simon Johnston High Time Resolution Observations of the Vela Pulsar17:00 Don Melrose What Causes the Circular Polarization in Pulsars?17:20 Guojun Qiao Radio and Gamma-ray Emission from Pulsars17:40 Break

Astrometry18:00 George Hobbs Jodrell Bank Timing Astrometry18:20 Andrew Fruchter VLA Astrometry18:40 Walter Brisken VLBI Techniques in Pulsar Astrometry19:10 Shami Chatterjee Probing the Galaxy with Pulsar Parallaxes and Proper Motions

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Wednesday, 28 August

Morning Session Chair: Yashwant Gupta

Pulsars at Parkes9:00 Richard Manchester Pulsars at Parkes

Glitches & Precession9:45 Francis Graham Smith The Incidence and Cumulative Effect of the Crab Glitches

10:05 Fabio Frescura Precession in Isolated Pulsars10:25 Bennett Link Precessing Neutron Stars10:55 Break

The Interstellar Medium11:15 Dan Stinebring The Scintillation Arc Phenomenon11:35 Robert Benjamin The Distribution of Warm Ionized Medium in the Milky Way11:55 JinLin Han Galactic Magnetic Structure Derived from Pulsar Rotation Measures12:15 Richard Wielebinski Galactic Magnetic Fields and Foreground Effects

Afternoon Session Chair: Frank Verbunt

Binary Evolution & Accretion 116:00 Deepto Chakrabarty Millisecond Pulsars in Low-Mass X-ray Binaries16:30 Andrew Cumming Magnetic Field Evolution in Neutron Stars17:00 Philipp Podsiadlowski X-ray Binaries and the Formation of Binary Millisecond Pulsars17:30 Break

Binary Evolution & Accretion 217:50 Lars Bildsten Gravitational Wave Limitations to Neutron Star Spin-Up18:20 Philip Chang Diffuse Nuclear Burning in Neutron Star Envelopes18:40 Vicky Kalogera Binary Coalescence Rates19:10 Dong Lai Core-Collapse Supernovae and Neutron Star Kicks

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Thursday, 29 August

Morning Session Chair: Simon Johnston

Radio Telescope Instrumentation9:00 Bhal Chandra Joshi Coherent On-Line Baseband Receiver for Astronomy:

A New Instrument for Pulsar Research9:20 Adrian Tiplady Development of a Digital Pulsar Timer9:40 Paulo Freire Pulsar Surveys with ALFA

Across the Spectrum 110:00 Roger Romani The Rest of the Story: Connecting Radio Pulsars to

IR–Gamma-ray Emission10:30 Break

Across the Spectrum 210:50 Mallory Roberts Pulsar Searches of Unidentified EGRET Sources11:10 Luciano Nicastro Reviewing the BeppoSAX Observations of Radio Pulsars11:30 Ocker C. de Jager Next Generation Ground Based Telescopes for Pulsar Studies in

the EGRET Range11:50 Marco Tavani AGILE and Pulsar Studies12:10 Stephen Thorsett Pulsars and GLAST

Afternoon Session Chair: Vicky Kalogera

Globular Clusters 116:00 Duncan Lorimer The Radio Pulsars in 47 Tucanae16:20 Craig Heinke X-ray and Optical Studies of Millisecond Pulsars in 47 Tucanae16:40 Scott Ransom Recent Globular Cluster Searches Using Arecibo and the GBT17:00 Nichi D’Amico The Parkes Search of Globular Clusters for Millisecond Pulsars17:20 Andrea Possenti PSR J1740−5340 in NGC6397 and PSR J1911−5958A in NGC6752:

Two New Attractions in the Millisecond Pulsar Zoo17:40 Break

Globular Clusters 218:00 Fred Rasio Formation and Evolution of Millisecond Pulsars in Clusters18:30 Steinn Sigurdsson Black Holes and Pulsar Binaries

Closing19:00 Edward van den Heuvel Conference Summary

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Poster Presentations

Dimitris Athanasiadis Pulsar Polarisation Observations at Jodrell BankRobert Benjamin An Unusually Straight and Narrow H-alpha FilamentOlga Bitzaraki On the Formation of Binary PulsarsTzihong Chiueh Probing the Clumpiness of Synchrotron Electrons with the Polarization MapRussell Edwards Unusual Subpulse Modulation in PSR B0320+39Ocker C. de Jager Constraining the Pair Production Multiplicity and Pulsar Wind Magnetization

Parameters from Multiwavelength ObservationsFredrick Jenet High Time Resolution Observations of Radio Pulsars and the First Detection of

non-Gaussian Coherent EmissionBhal Chandra Joshi A Search for Giant Pulses in Millisecond PulsarsAris Karastergiou Simultaneous Single-Pulse Observations of Radio PulsarsJarek Kijak Structure of Pulsar BeamsHaydon Knight A Baseband Survey for Ultrafast PulsarsJoeri van Leeuwen Nulling-drifting interaction in PSR B0809+74Qinghuan Luo Propagation Effects on Pulsar Radio EmissionDonald Payne Magnetic Field Evolution in Accreting Neutron Star BinariesAlberto Pellizzoni Optical Study of the Radio Quiet Pulsar Candidate Associated with SNR

G266.1−1.2Gerard Petit Looking for Submillisecond Pulsars: A Progress ReportJerome Petri Structure and Stability of Pulsars’ ElectrospheresJohn-Hugh Seiradakis Converting EPN-formatted Data to XML FormatIngrid Stairs High Resolution Observations of PSR B1828−11Dan Stinebring Frequency Dependence of Scintillation ArcsFrank Verbunt

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Donald Backer (University of California, Berkeley) Monday 9:05Pulsars: Old Puzzles–New Challenges

Searches for pulsars are the engine of progress in our subfield. The Parkes Multi-Beam effort hasprovided a dramatic advance; the planned Arecibo effort will do likewise. The scientific case for aSquare Kilometer Array points to prospects for further advances.

“Timing” known pulsars leads to a myriad of results about the star itself, about the interveningmedium and about fundamental physics and cosmology. Rotation instabilities remain an unsolvedproblem. Small scale structure in the ISM neutral and ionized phases and in magnetic field is not wellunderstood although there is recent theoretical progress. We’ll hear about detailed probes of binarysystems and the next step toward detection of a stochastic background of gravitational radiation.

New instruments and a new generation of investigators will tackle old questions about thefundamental emission mechanism in pulsars. Orthogonal polarization modes, memory in pulseto pulse fluctuations and radio/X-ray/Gamma-ray connections all pose questions and provideconstraints to make progress.

Matthew Bailes (Swinburne University) Monday 9:50Parkes Precision Pulsar Timing

The Parkes precision pulsar timing programme has been running for almost ten years now and inthat time the precision attainable on the brightest millisecond pulsars has increased by about afactor of 50 through improvements in instrumentation. I will summarise recent timing highlightsincluding the mass of a neutron star from a low-mass progenitor and a binary millisecond pulsarwith unusually high eccentricity. Finally I will describe a new 128MHz baseband recorder (CPSR2)with an in-built supercomputer capable of real-time coherent dedispersion for pulsar timing, fastpulsar surveys and polarimetry.

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Willem van Straten (Swinburne University) Monday 10:20Annual-Orbital Parallax and Nearby Binary Millisecond Pulsars

High-precision timing of the closest and brightest millisecond pulsar, PSR J0437−4715, has yieldedthe first detection of annual-orbital parallax, providing an accurate estimation of the orbitalinclination and a significant constraint on the shape of the Shapiro delay in this system. Thelong-term timing stability of this MSP is analysed and discussed, and the newly-developed timingmodel is applied to another binary system, PSR 1713+0747, yielding an estimation of its orbitalinclination and component masses.

Zaven Arzoumanian (USRA/NASA-GSFC) Monday 11:00PSR B0655+64: A Stalwart Control Experiment

I will report on the status of a two-decade-long timing study of the mildly relativistic binary pulsarthat has served as a control experiment to observed orbital decay due to gravitational radiation inthe close double-neutron-star binaries.

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David Nice (Princeton University) Monday 11:20Binary Pulsar Timing at Arecibo

I will discuss high precision timing observations of five pulsar–white dwarf binary systems at Arecibo:PSRs J0621+1002, J0751+1807, J1713+0747, B1855+09, and J2019+2425. (In some cases, theArecibo observations are augmented by data from Green Bank, Jodrell Bank, or Effelsberg.) Ourobservations place significant constraints on the component masses of the systems. We havemeasured the Shapiro delay in J0751+1807, J1713+0747, and B1855+09. The non-detection ofShapiro delay in the other two systems is also significant. We have measured the relativisticprecession of J0621+1002. In the widest two binaries, J1713+0747 and J2019+2425, we havedetected secular changes in the projected orbital semi-major axes due to the changing inclinationangles which result from proper motion. The tightest of these binaries, J0751+1807, holds greatpromise for detection of general relativistic orbital decay within a few years; the present upper limiton orbital period change already places modest constraints on the system masses.

Andrea Lommen (University of Amsterdam) Monday 11:50New Limits on Gravitational Wave Background Using Pulsars

Pulsar timing is uniquely sensitive to gravitational radiation with periods near one year. The primarysources emitting at these frequencies are Massive Black Hole binaries throughout the universe thatare on their way to coalescence. The final coalescence events of these binaries will be detected inthe future by orbiting laser interferometer arrays. Other contributions to the stochastic backgroundof gravitational radiation from the chaotic processes in the early universe are more speculative.

We present a new upper limit on the stochastic background of gravitational radiation using timingresiduals from PSRs B1855+09 (17 y), B1937+21 (18 y) and J1713+0747 (9 y) which improves onthe work by Kaspi, Taylor, & Ryba (1994) and other authors. The results required combining datafrom 3 different observing projects: 2 with the Arecibo telescope and 1 with the 140ft telescope inGreen Bank. This project represents early results from the “Pulsar Timing Array” which will soonbe able detect the stochastic background from Massive Black Hole binaries.

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Alex Wolszczan (Penn State University) Monday 12:10Pulsar Planets: Status and Future Prospects

I will discuss the current status of the Arecibo timing of the planets pulsar, PSR B1257+12,and briefly describe basic constraints on the origin of neutron star planets resulting from theseobservations.

Ingrid Stairs (University of British Columbia) Monday 16:00The Massive Binary Pulsar J1740−3052

The young pulsar PSR J1740−3052 is in an 8-month eccentric orbit with a companion of at least 11solar masses. I present multifrequency GBT and Parkes timing observations, and discuss implicationsfor the nature of the companion.

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Steve Ord (Swinburne University) Monday 16:20The Scintillation Velocity of the Relativistic Binary J1141−6545

We report a dramatic orbital modulation in the scintillation timescale of the relativistic binary pulsarJ1141−6545 that both confirms the validity of the scintillation speed methodology and enables usto derive important physical parameters. We have determined the space velocity, orbital inclinationand even longitude of periastron of the binary system, which we find to be in good agreement withthat obtained from pulse timing measurements.

Joel Weisberg (Carleton College) Monday 16:40Binary Pulsar B1913+16: Twenty-Seven Years and Going Strong

The first binary pulsar, B1913+16, continues to yield new relativistic results. I will summarizeprevious and current observations and relativistic analyses, and discuss future prospects.

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Michael Kramer (Jodrell Bank Observatory) Monday 17:10Geodetic Precession in PSR B1913+16

I will present some latest Effelsberg data and their modelling for PSR B1913+16. I will discuss theirimplication for tests of relativity and pulsar physics.

Na Wang (Urumqi Observatory, NAOC-CAS) Monday 18:00Pulsar Timing and Scintillation Observations at Urumqi Observatory

We present the status and results of pulsar observations at Urumqi Observatory. Observationscommenced with a pulsar timing system at the 25-m Urumqi Nanshan telescope in mid-1999;these were the first regular and high-quality pulsar observations in China. The center frequencyof this system is 1540 MHz, and de-dispersion is provided by a 2×128×2.5 MHz filterbank/digitisersystem. Observations over more than one year have resulted in updated rotation parameters for 74pulsars. Comparing with earlier observations we showed that long-term period and period-derivativefluctuations may be dominated by unseen glitches. Taking advantage of the available telescope time,we are also monitoring the variation of pulsar scintillation dynamic spectra for a few strong pulsars.Scintillation parameters are measured and their variations are under study. We are planning to builda new system at a lower frequency so that frequency-dependent pulsar properties can be investigated.

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Johnson Urama (University of Nigeria, Nsukka) Monday 18:20Long-Term Timing Analysis of Some Pulsars

An analysis of the combined JPL and HartRAO timing data spanning about 30 years is presentedfor some radio pulsars. The time evolution of the rotational parameters for some of these pulsarsshow “unusual” behaviour. The implications of these behaviours are discussed.

Sergei Kopeikin (University of Missouri, Columbia) Monday 18:40Relativistic Effect of Retardation of Gravity

Gravity propagates with finite speed. In the case of a time-dependent gravitational field, the finitespeed of propagation of gravity can be measured, for example, by making use of timing observationsof a pulsar in a binary system. The propagation of gravity leads to a small correction to the Shapirotime delay that can be observed in the case of binary pulsars with nearly edgewise orbits.

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Graham Woan (University of Glasgow) Monday 19:00The Search for Gravitational Waves from Pulsars

The new generation of gravitational wave detectors are reaching sensitivities at which the detectionof rotational gravitational radiation from neutron stars is a viable possibility. Search algorithmshave been developed to carry out all-sky searches and searches targeted at known pulsars. He wereport on progress with the targeted searches, using data from the GEO 600 detector in Hannover,Germany and the LIGO detectors in Hanford, Washington and Livingston, Louisiana.

Andrew Lyne (Jodrell Bank Observatory) Tuesday 9:00The Development of Pulsar Search Techniques

The search for radio pulsars has always been limited by the availability of electronic and computerdata processing technology. This talk will review the incredible development of the field over thepast 35 years and what the future might hold.

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Joseph Taylor (Princeton University) Tuesday 9:40Reflections on 34 Years of Finding Pulsars

Maura McLaughlin (Jodrell Bank Observatory) Tuesday 10:00New Pulsars from Arecibo Drift Scan Searches

I discuss new pulsars discovered in drift-scan data taken during the latter stages of the Areciboupgrade period. These data were taken with the Penn State Pulsar Machine (PSPM) and are beingprocessed on the COBRA cluster at Jodrell Bank. Thus far, processing has resulted in the detectionof 10 new and 23 known pulsars, in addition to a number of pulsar candidates. The new pulsarsdiscovered thus far include one MSP with a period of 5.79ms and one pulsar with a period of 55.6 ms.

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Bryan Jacoby (Caltech) Tuesday 10:20A Search for Millisecond Pulsars at High Galactic Latitude

We are conducting a search for radio pulsars using the Parkes 64 m telescope, covering ∼4500 squaredegrees in the galactic latitude range 15◦ < |b| < 30◦. Each pointing is observed for 265 s with the13-beam multibeam system at a frequency of 1374 MHz. The signal from each beam is processed bya 2×96 channel filterbank sampled every 125 µs, with a bandwidth of 288 MHz. This strategy affordsrapid sky coverage and good sensitivity to pulsars with periods as short as ∼1 ms, whose existencewould constrain the neutron star equation of state. Data are analyzed offline using the workstationcluster at the Swinburne Centre for Astrophysics and Supercomputing. Analysis of ∼3000 squaredegrees of the survey has been completed, yielding 21 new pulsars including four binary recycledpulsars. Three of these objects have great potential for high precision timing experiments, and onehas an unusual massive white dwarf companion.

Fernando Camilo (Columbia University) Tuesday 11:00Deep Searches for Young Pulsars

We are undertaking a large (∼30 objects) set of deep observations (∼10 hours/each) of young pulsarcandidates (mostly PWNe), and the results so far are quite encouraging, resulting in the discoveryof several very young and very low-luminosity (L1400 < 1 mJy kpc2) pulsars. I plan to describe theresults of this survey, which should be largely complete by the time of this meeting.

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Victoria Kaspi (McGill University) Tuesday 11:30Magnetars

I will review the evidence for the existence of the hypothesized population of young, isolated, ultrahigh magnetic field neutron stars that has come to be known as “magnetars.” The existing evidenceincludes observations of Soft Gamma Repeaters (SGRs) as well as Anomalous X-ray Pulsars (AXPs).The talk will focus on the latter, in particular on recently discovered SGR-like bursts from twoAXPs. These bursts greatly solidify the relationship between SGRs and AXPs, and provide verystrong support that both classes of object are indeed magnetars.

Andrea De Luca (CNR-IASF Milan) Tuesday 12:00The Radio Quiet Neutron Star 1E1207−5209 Observed with XMM-Newton

The X-ray source 1E 1207−5209 belongs to the emerging class of radio-quiet neutron stars. Itsneutron star nature, suggested by its location at the geometrical center of the supernova remnantG296.5+10.0, has been confirmed by the Chandra discovery of pulsations at 424 ms. We presentthe spectral and timing results of an XMM-Newton observation of this source. In particular, thephase-resolved spectral analysis made possible by the large collecting area of the EPIC instrumentallows us to constrain the properties of the neutron star.

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David Kaplan (Caltech) Tuesday 12:20The Radio Quiet RXJ0720.4−3125

We review the soft, nearby, 8-s X-ray pulsar RX J0720.4−3125. Using timing data and optical/UVphotometry combined with cooling models, we have been able to reject the popular magnetar modelfor this source, and instead suggest that it is an off-beam radio pulsar. This source would thenbe either a (1) 1013 G pulsar born with P ∼ 0, or a (2) 1012 G pulsar that was injected with abirth period very close to its current period. The proximity of this source (< 500 pc) argues for asubstantial population of similar objects.

Yashwant Gupta (NAIC, Arecibo and NCRA, Pune) Tuesday 16:00Emission Beam Geometry of Multi-Component Pulsars

Results are presented from an analysis of single-pulse data for several pulsars with prominentmulti-component profiles at metre wavelengths. Using a new method of analysis that is suitablefor detecting weak emission components, we are able to detect new emission components in mostpulsar profiles. From a careful determination of the total number of emission components and theirlocations in pulse longitude, we find that all the pulsars show clear evidence for retardation andaberration effects in the conal emission beams. From this, using a dipolar field geometry, we obtainestimates of the height and transverse location in the magnetosphere, for each of the cones. Wefind that successive outer cones are emitted at higher altitudes in the magnetosphere. The range ofinferred heights is from ∼ 160 km to ∼ 2500 km. The set of active field lines from which the conalemissions originate are located in the region ∼ 0.23 to ∼ 0.77 of the polar cap radius. At the starsurface, these conal rings map to radii of a few tens of metres and the separation between successiverings is about 10 metres. The implications of these findings for pulsar emission mechanisms arediscussed.

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Fredrick Jenet (Caltech) Tuesday 16:20The Radio Pulsar Signal: Statistics of Single Pulses

High time resolution (100 ns) observations of several radio pulsars were made with the CaltechBaseband Recorder (CBR) at the Arecibo Radio Observatory in Puerto Rico. New analysistechniques have been developed in order to study the single pulse properties of “weak” orlow-intensity pulsars. These techniques have been used to analyze the pulse-to-pulse amplitudeand pulse shape variations of the fastest millisecond pulsar PSR B1937+21. Techniques have alsobeen developed in order to search for the presence of coherent non-Gaussian emission statistics. Suchstatistics have been detected in pulsars B0823+26, B0950+08, and B1133+16. This is the first timesuch a phenomenon has been observed, and these results place significant constraints on the radiopulsar emission mechanism.

Simon Johnston (University of Sydney) Tuesday 16:40High Time Resolution Observations of the Vela Pulsar

I will present observations of the Vela pulsar at 1.4 and 2.3 GHz at a resolution of 22 microseconds.We have detected microstructure, a new pulse component and quasi-giant pulses not previously seendespite 30 years of observations of Vela.

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Don Melrose (University of Sydney) Tuesday 17:00What Causes the Circular Polarization in pulsars?

Guojun Qiao (Peking University) Tuesday 17:20Radio and Gamma-ray Emission from Pulsars

The radiation of radio pulsars has been observed from radio to gamma-rays for many years.Observations present an abundance of information. Theoretical models for radio and gamma-rayshave been presented separately. Until now we have not found a model which shows emission fromradio to gamma-rays at the same time in detail. For certain pulsars, the emission from radio togamma-rays can be observed at the same time (such as Crab pulsar and so on), so a reasonablemodel should present the emission from radio to gamma-rays at the same time in detail. A jointmodel for emission from radio to gamma-rays is presented in this paper, which can show emissioncharacters for both radio and gamma-ray emission band. Core and cone emission beams at the radioemission band, and gamma-rays for Geminga-like, Crab-like and Vela-like emission beams can beshown at the same time. First of all, an inverse Compton scattering model (ICS model, partly seeICS I A & A 1998; ICS II A & A 2001; ICS III ApJ 2000) of radio pulsars will be introduced indetail. Then a new model for gamma-ray emission will be introduced. In this model both radio andgamma-ray emission mechanisms are jointed, and the emission beams from radio to gamma-rays canbe presented. Various kind of pulse profiles and other observational characteristics can be shown,and the theory is in agreement with these observations.

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George Hobbs (Jodrell Bank Observatory) Tuesday 18:00Jodrell Bank Timing Astrometry

More than 500 pulsars are regularly observed using the 76-m Lovell radio telescope at Jodrell BankObservatory. Precise positional and rotational parameters have been obtained from observationsspanning between 6 and 34 years for over 300 pulsars. This talk introduces the analysis by presentingnew proper motion measurements and a description is given of the timing noise present in the timingresiduals.

Andrew Fruchter (Space Telescope Science Institute) Tuesday 18:20VLA Astrometry

We have used gated observations at the VLA to study a sample of pulsars that contains a relativelylarge number of high-z but low-b pulsars. We use these observations to constrain the velocitydistribution of the pulsar population.

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Walter Brisken (National Radio Astronomy Observatory) Tuesday 18:40VLBI Techniques in Pulsar Astrometry

The proper motions and parallaxes that can be derived from accurate astrometry of pulsars havenumerous applications which justify the difficulty of the measurements. Pulsars quickly decline inradio brightness as the observing frequency is increased, forcing a compromise between attainableresolution and detectability. This results in typical observing frequencies in the 1.5GHz band, wherethe ionosphere introduces large astrometric shifts and distortions. Two solutions to the ionosphereproblem have been very successful, producing several new pulsar parallaxes over the last four years.These techniques are discussed, as are the future prospects of VLBI pulsar astrometry.

Shami Chatterjee (Cornell University) Tuesday 19:10Probing the Galaxy with Pulsar Parallaxes and Proper Motions

We are in the process of measuring parallaxes and proper motions of a large sample of pulsars. Newparallaxes and proper motions will enable a whole range of scientific applications, such as accuratemodeling of the velocity distribution of pulsars, calibrating models of Galactic electron density,probing the local ISM, establishing constraints on the neutron star Equation of State, verification ofreference frame ties and supernova remnant associations, etc. A new model of the Galactic electrondensity distribution is introduced, and we discuss recent results using bow shocks to probe the ISMand hybrid ISS-VLBI methods to constrain the distribution of matter along specific lines of sight.

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Richard Manchester (ATNF-CSIRO) Wednesday 9:00Pulsars at Parkes

A review of the role of Parkes in pulsar astronomy, highlighting results which are scientifically and/orpersonally significant.

Francis Graham Smith (Jodrell Bank Observatory) Wednesday 9:45The Incidence and Cumulative Effect of the Crab Glitches

The sequence of 14 glitches in 33 years suggests a simple two components system. The effect onslowdown is to reduce the braking index to n=2.45.

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Fabio Frescura (Hartebeesthoek Radio Astronomy Obs.) Wednesday 10:05Precession in Isolated Pulsars

18 years of pulsar timing data gathered at the Hartebeesthoek Radio Astronomy Observatory areused to investigate some precession models.

Bennett Link (Montana State University) Wednesday 10:25Precessing Neutron Stars

Recent data indicate that some isolated neutron stars undergo precession of their spin axes. Iwill discuss the observational evidence for precession, theoretical efforts at modeling the data,how precession might be excited and damped, and what precession can tell us about the materialproperties of the crust.

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Dan Stinebring (Oberlin College) Wednesday 11:15The Scintillation Arc Phenomenon

Low-intensity scattering (far out in the wings of an image) probes the physics of the scatteringprocess. Scintillation arcs arise from this sort of scattering and are widespread in high dynamicrange spectral observations of pulsars. I will present the observational basics of this phenomenonand put forward a physical interpretation of it. The potential for milliarcsecond “imaging” of theISM using this technique will be briefly discussed.

Robert Benjamin (University of Wisconsin, Madison) Wednesday 11:35The Distribution of Warm Ionized Medium in the Milky Way

The warm ionized medium is a major component of the interstellar medium of the Galaxy, providinga significant fraction of the total weight and a large power requirement. Understanding its spatialdistribution is also important in estimating the distance to pulsars. I will present a simple modelof the distribution of this gas using a set of 109 pulsars of known distance. This revised modelmatches the available data as well as the more complex Taylor-Cordes model. However, even in thisreduced dataset, there is evidence for the need of non-axisymmetric features. I will compare thisto the recent revised model of Cordes & Lazio (2002) and the results from the Wisconsin H-alphaMapper (Reynolds et al 2001).

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JinLin Han (National Astronomical Observatory) Wednesday 11:55Galactic Magnetic Structure Derived from Pulsar Rotation Measures

Pulsars are the best probes for the large scale structure of Galactic magnetic fields. In early daysthe investigation of the fields were limited to a few kpc due to pulsar sample distribution. Therecent Parkes pulsar survey discovered many more distant pulsars, and hence enabled to reveal themagnetic field in almost half of the Galactic disk. We present a brief overview of historical researchon this direction and also the most recent results.

Richard Wielebinski (MPI for Radioastronomy, Bonn) Wednesday 12:15Galactic Magnetic Fields and Foreground Effects

We have made new observations of rotation measures of a sample of northern pulsars. We havealso studied the foreground emission in Hα and radio continuum. It is clear that serious effects arecaused by the Galactic foreground. We must combine radio continuum polarization data and pulsarRMs to give us a model of the Galactic magnetic field.

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Deepto Chakrabarty (MIT) Wednesday 16:00Millisecond Pulsars in Low-Mass X-ray Binaries

I will review the observational properties of the three known accretion-powered binary millisecondX-ray pulsars, two of which were discovered only in the last 5 months. These systems are presumablyprogenitors of millisecond radio pulsars. All three are X-ray transients in very close binaries withextremely low mass transfer rates, which may provide a clue to why millisecond pulsars are so elusiveamong the over 50 known low-mass X-ray binaries containing neutron stars (NS/LMXBs). I willalso discuss the properties of the 10 so-called “burst oscillation” sources, which are NS/LMXBs thatshow nearly coherent millisecond oscillations during thermonuclear X-ray bursts.

Andrew Cumming (University of California, Santa Cruz) Wednesday 16:30Magnetic Field Evolution in Neutron Stars

I discuss two aspects of magnetic field evolution in neutron stars, with an eye on the global picture.The first is whether the neutron star magnetic field may be “buried” or “screened” by accretion. Ishow that for accretion to be rapid enough to overcome ohmic diffusion, the accretion rate must be atleast 1/100 of the Eddington rate. This has interesting implications for the lack of X-ray pulsationsfrom low mass X-ray binary neutron stars. In addition, I show that instabilities limit the strengthof the buried field, and discuss the reemergence timescale of the field once accretion switches off.Secondly, I discuss the non-linear evolution of the field due to the Hall effect, which might lead tomagnetic field changes on a 10 million year timescale, relevant for evolution in the P − P diagram. Ioutline the regimes where the Hall effect is important, and describe ongoing numerical and analyticstudies of the Hall cascade, both in the solid crust and fluid core.

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Philipp Podsiadlowski (University of Oxford) Wednesday 17:00X-ray Binaries and the Formation of Binary Millisecond Pulsars

We present the results of a systematic study of low- and intermediate-mass X-ray binaries and theirimplications for the population of millisecond pulsars using binary stellar evolution calculationsand binary population synthesis modelling. The results show that the so-called standard model isuntenable and that most millisecond pulsars probably originate from intermediate-mass systems.However, even with the inclusion of intermediate-mass systems the model does not explainvarious key features of the the observed X-ray binary and ms pulsar population. We show howirradiation-driven mass-transfer cycles can alleviate many of these problems. (Co-authors: S.Rappaport, E. Pfahl.)

Lars Bildsten (Kavli Institute for Theoretical Physics) Wednesday 17:50Gravitational Wave Limitations to Neutron Star Spin-Up

I will review the theoretical progress over the last five years on the halting by gravitationalwave emission of neutron star spin-up through accretion. Prior to this theoretical work and themeasurements of rotation rates in accreting neutron stars, the community was confident that mostaccreting neutron stars would be spun-up to rotation rates near breakup, motivating searches forsub-millisecond objects. I will argue that such systems will be rare, as there are now strongtheoretical reasons to believe that gravitational wave emission intervenes to slow-down or arrestthe accretion spin-up. The gravitational waves will either be emitted transiently as r-modes orpersistently from a crustal quadrupole. This theoretical idea will be tested by LIGO by the end ofthis decade. Millisecond pulsar observers would likely “discover” this phenomena as a dropoff in thenumber of pulsars beyond 600 Hz.

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Philip Chang (University of California, Santa Barbara) Wednesday 18:20Diffuse Nuclear Burning in Neutron Star Envelopes

The origin and evolution of the surface abundances of young neutron stars is just now being probedby observing their thermal emission. These observations suggest an apparent transition in surfaceabundances from predominantly H/He at young ages to a more opaque element for ages in excess of105 years. The photospheric temperatures and densities are far too low to burn H locally, so we arecalculating the burning of hydrogen in the exponentially suppressed tail that extends into the hotterregions of the envelope. We show that this Diffusive Nuclear Burning (DNB) can change the totalcolumn of hydrogen in the envelope on astrophysically relevant timescales. It has clear implicationsfor the effective temperature-core temperature relation and for the thermal X-ray spectra.

Vicky Kalogera (Northwestern University) Wednesday 18:40Binary Coalescence Rates

I will present results from a collaboration with my student Chunglee Kim and with Dunc Lorimer onthe probability distribution of coalescence rates for binary pulsars. For a variety of pulsar populationmodels, we calculate the ranges of rate values at different statistical confidence levels as well as thevalue with the highest likelyhood.

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Dong Lai (Cornell University) Wednesday 19:10Core-Collapse Supernovae and Neutron Star Kicks

Despite decades of investigations, our understanding of core-collapse supernovae remains significantlyincomplete. Observations in recent years have revealed many new puzzles. I will discuss severalproblems related to core-collapse SNe, including the origin of pulsar kicks and supernova asymmetry,and how neutron star kicks are intimately connected to the other fundamental parameters of youngneutron stars (such as the initial spin and initial magnetic field).

Bhal Chandra Joshi (Jodrell Bank Observatory) Thursday 9:00Coherent On-Line Baseband Receiver for Astronomy–A New Instrument forPulsar Research

Coherent On-line Baseband Receiver for Astronomy is a software based receiver implemented in aBeowulf cluster consisting of 182 Pentium III processors. It will be capable of processing 80MHzbandwidth on line (320 Mbytes per second). This instrument is particularly useful for pulsar timingas it provides high time resolution coherently dedispersed profiles. It also acts as a polarimeter. Thedesign of the instrument is described in this talk followed by preliminary results obtained in the lastfew weeks.

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Adrian Tiplady (Rhodes University) Thursday 9:20Development of a Digital Pulsar Timer

The current Hartebeeshoek Radio Astronomy Observatory (HartRAO, South Africa) pulsar timeris a fixed 10 MHz bandwidth, single channel device which is used in the continuation of the presentglitch detection program and the measurement of timing noise. However, high dispersion measureand weak pulsars are difficult to detect and so the need arose to develop a new pulsar timer which isable to take advantage of modern electronics and the scheduling model of the HartRAO telescope.The new timer is a multi-channel, wide bandwidth digital radiometer that is modularised, scalableand generalised, allowing for easy expansion (2 channels at a time) without further design effortrequired. It is inexpensive, using COTS (consumer-off-the-shelf) components designed for cellularphones, high speed analogue to digital converters, FPGAs (Field Programmable Gate Arrays) andmicrocontrollers. The timer communicates via an ethernet network, making it highly accessibleand easy to use. The design and implementation of and initial measurements from the timer arepresented.

Paulo Freire (NAIC, Cornell University) Thursday 9:40Pulsar Surveys with ALFA

In this talk, we report on the present status of the Arecibo L-band Feed Array (ALFA) project. Thisis a 7-beam system due to become operational at the Arecibo Observatory in about 21 months time.Pulsar searches with this array have the potential to find many hundreds of new pulsars. We presentthe feed configuration chosen for ALFA, the system specifications and expected performance. Wealso describe the back-ends now being developed at NAIC, their suitability for pulsar searches, andthe expected L-band RFI situation at Arecibo. Finally, we describe the consortium now being formedfor pulsar searches. Input from the pulsar community will be needed to further define the backendrequirements. We also provide details on the upcoming workshop at the Arecibo Observatory onALFA pulsar searches.

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Roger Romani (Stanford University) Thursday 10:00The Rest of the Story: Connecting Radio Pulsars to IR–Gamma-ray Emission

Recent instrumental progress has let us detect a number of young pulsars from the power peak inthe gamma ray band to the incoherent photon peak in the optical/IR. With a wide variation oflight curves between the bands the story is complex, but I’ll argue we are making progress on themultiwavelength phenomenology of pulsar emission and beaming. Of course, without the pioneeringand continued work of Andrew, Dick and Joe we would have little idea of where to look and no cluehow to fold what we found there...

Mallory Roberts (McGill University/MIT) Thursday 10:50Pulsar Searches of Unidentified EGRET Sources

The majority of Galactic high energy gamma-ray sources continue to elude identification. Currently,we have a handful of firm pulsar identifications, one of which is radio-quiet, and a few marginaldetections, including one millisecond pulsar. Recently, both blind searches of EGRET error boxesand targeted searches of X-ray counterpart candidates have had some success in finding new pulsars.I will review these results, and discuss our current program of searching mid-Galactic latitudeEGRET error boxes using the Parkes multi-beam system.

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Luciano Nicastro (IASF-CNR) Thursday 11:10Reviewing the BeppoSAX Observations of Radio Pulsars

Exactly six years after its launch, the Italian-Dutch X-ray satellite BeppoSAX was switched offon April 30, 2002. Some 20 pulsars (Crab-like, Vela-like, cooling, MSPs) were observed with itsnarrow field instruments. The results were very interesting, especially in the energy band 1-10 keV(where the sensitivity of BeppoSAX is higher). For example for the first time we were able to detectand study the double peak profiles of the two MSPs J0218+4232 and B1937+21. I will review theobservational results and briefly discuss the implications for emission mechanisms.

Ocker C. de Jager (Potchefstroom Univ.) Thursday 11:30Next Generation Ground Based Telescopes for Pulsar Studies in the EGRETRange

New large mirror area telescopes such as H.E.S.S. (Namibia) and MAGIC (La Palma) should allowus to trigger on gamma-ray showers at the upper energy range of EGRET, where the spectral cutoffsfrom a few gamma-ray pulsars were seen. H.E.S.S. First Light already realized during June 2002.Background rejection techniques should allow us to detect some of these pulsars within a few hours’integration, as opposed to EGRET’s week-long exposures. Apart from studying the cutoff energiesfrom such pulsars, we can also survey a proposed class of low-multiplicity, older pulsars, for whichthe pulsed photon energies are expected to cluster near the spectral cutoff, expected to be above aGeV, or even as high as 50 GeV (e.g. PSR B1951+32 and PSR B1706−44).

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Marco Tavani (IASF-CNR, Milano) Thursday 11:50AGILE and Pulsar Studies

The gamma-ray astrophysics space mission AGILE operating in the energy bands 10-40 keV and30 MeV-30 GeV is planned to be operational in the year 2004. Pulsars are a major topic ofinvestigation of AGILE, and the talk will present the prospects for future research.

Stephen Thorsett (University of California, Santa Cruz) Thursday 12:10Pulsars and GLAST

NASA will support radio pulsar timing observations needed to support the GLAST gamma-raytelescope. The radio community has been asked to help define priorities and to plan observations.

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Duncan Lorimer (Jodrell Bank Observatory) Thursday 16:00The Radio Pulsars in 47 Tucanae

The radio pulsar population of the globular cluster 47Tucanae currently stands at 20 millisecondpulsars close to the cluster core. In this talk I will briefly review what studies of these pulsarshave taught us about 47Tuc. Time permitting, some remarks about the underlying population willbe made, as well as an outlook of what we can look forward to in the future search and timingobservations of this fascinating cluster.

Craig Heinke (Harvard University) Thursday 16:20X-ray and Optical Studies of Millisecond Pulsars in 47 Tucanae

Our Chandra X-ray observation of the globular cluster 47 Tuc clearly detected most of the 16 MSPswith precise radio positions, and indicates probable X-ray emission from the remainder. The MSPsare soft (BB kT ∼ 0.2 − 0.3 keV) and faint (LX ∼ few 1030 ergs/s), and generally consistent withthermal emission from small polar caps. An additional 40 soft X-ray sources are consistent with theknown MSPs in X-ray colors, luminosity, and radial distribution within the cluster (and thus mass).We note that these MSPs display a flatter LX to E relation than PSRs and MSPs in the field, whichis consistent with polar cap heating models for younger MSPs and may suggest the surface magneticfield has been modified by repeated accretion episodes to include multipole components. CorrelatingHST images, radio timing positions, and the Chandra dataset has allowed optical searches for MSPbinary companions. The MSP 47 Tuc-U is coincident with a blue star exhibiting sinusoidal variationsthat agree in period and phase with the heated face of the WD companion. Another blue variablestar (and X-ray source) agrees in period and phase with the companion to 47 Tuc-W (which lacksan accurate timing position); this companion is probably a main sequence star.

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Scott Ransom (McGill University) Thursday 16:40Recent Globular Cluster Searches Using Arecibo and the GBT

We present initial results (and several new millisecond pulsars) from 20 cm searches of numerousglobular clusters using Arecibo and the GBT. We also summarize the prospects for similar searcheswith these instruments in the future.

Nichi D’Amico (Cagliari Astronomical Observatory) Thursday 17:00The Parkes Search of Globular Clusters for Millisecond Pulsars

In the last few years we have carried out a sensitive search for millisecond pulsars in globular clustersusing the Parkes radio telescope. In this paper we describe the experiment motivation, the hardwareand software systems adopted, and the survey plan. So far we have discovered 12 new millisecondpulsars in 6 clusters in which no associated pulsars were previously known.

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Andrea Possenti (Astronomical Observatory of Bologna) Thursday 17:20PSR J1740−5340 in NGC6397 and PSR J1911−5958A in NGC6752: Two NewAttractions in the Millisecond Pulsar Zoo

It is well known that the globular clusters are a fertile ground for finding unusual binaries. I discussthe cases of two such systems comprising a millisecond pulsar. PSR J1740−5340 is a binary in whichthe Roche lobe overflow stage is not ended yet, but the pulsar is already active. It could representthe missing link between the X-ray bright phase of the “recycling” and the canonical millisecondpulsar orbiting a white dwarf. PSR J1911−5958A is the most displaced known millisecond pulsar(with respect to the cluster center) allowing to infer intriguing scenarios for its formation and currentlocation.

Fred Rasio (Northwestern University) Thursday 18:00Formation and Evolution of Millisecond Pulsars in Clusters

Close to 50 radio pulsars have now been observed in globular clusters, the number in 47 Tucanae alonehaving recently increased to more than 20. Globular clusters contain some of the most interestingand unusual recycled and binary pulsars known, including many single millisecond pulsars, eclipsingbinaries with periods as short as an hour and companions as small as brown dwarfs, one doubleneutron star system, and one triple system containing a neutron star, a white dwarf, and a giantplanet! Most of these systems are located inside or near the inner cores of the densest clusters, wherestrong dynamical interactions between stars and binaries are taking place at high rates. The mostfrequent interactions involving neutron stars are probably exchange interactions with primordialbinaries, and direct physical collisions with main-sequence stars. In this talk I will discuss thetheoretical implications of the latest observations of globular cluster pulsars for our understandingof the formation and evolution of recycled pulsars in general, as well as dynamical processes in densestellar systems and the overall dynamical evolution of globular clusters.

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Steinn Sigurdsson (Penn State) Thursday 18:30Black Holes and Pulsar Binaries

A black hole-pulsar binary would provide an interesting testbed for general relativity, and possiblesources of high frequency gravitational radiation. I briefly discuss formation of BH-PSR binaries,and BH-PSR interactions in globular clusters.

Edward van den Heuvel (University of Amsterdam) Thursday 19:00Conference Summary

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Dimitris Athanasiadis (Jodrell Bank Observatory) PosterPulsar Polarisation Observations at Jodrell Bank

I will summarise the polarisation observations at Jodrell Bank with particular attention to PSRB1828−11 and/or using COBRA.

Robert Benjamin (University of Wisconsin, Madison) PosterAn Unusually Straight and Narrow H-alpha Filament

We discuss progress on understanding an unusually straight and narrow ionized filament detectedin H-alpha and first presented in McCullough and Benjamin (2001, AJ, Vol. 122, p. 1500). Thisfilament has been detected in three independent H-alpha images, and is 2.5 degrees long and has anH surface brightness of 0.5 rayleighs, and is located at (l, b)=(139,38). Spectroscopic observationsusing WHAM appear to rule out the possibility that it is normal interstellar filamentation. Wesuggest, therefore, that is a “Fossil Stromgren Trail” left by a high velocity white dwarf or neutronstar. We discuss the search for an associated ionizing source, resulting in one inconclusive candidate:RSXJ094247.2+700238. We also discuss how this structure might be useful to constrain the thermaland velocity structure of the nearby interstellar medium.

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Olga Bitzaraki (University of Athens) PosterOn the Formation of Binary Pulsars

Tzihong Chiueh (National Taiwan University) PosterProbing the Clumpiness of Synchrotron Electrons with the Polarization Map

Radio synchrotron electrons are long-lived. They have time to stream along and drift across themagnetic field lines and thus tend to distribute homogeneously in the light emitting cloud. By usingthe geometrical property of synchrotron polarization, I present a method to probe the small-scalespatial variation of synchrotron electron distribution in a cloud even with random 3D magneticfields.

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Ocker C. de Jager (Potchefstroom University) PosterConstraining the Pair Production Multiplicity and Pulsar Wind MagnetizationParameters from Multiwavelength Observations

Radio to X-ray constraints on the flux from the compact nebulae of pulsar driven plerions allow usto probe the injection rates and magnetization parameters in the convection dominated region wherethe number of free parameters are a minimum, compared to diffusion dominated flow, governed bymulti-parameter transport equations. We derive empirical confidence contours for the multiplicityand “sigma” parameters, which serve to constrain models for the electromagnetic pair cascades abovepulsar polar caps. We apply this technique to Vela and PSR B1706−44. These parameters are alsouseful in predicting the gamma-ray fluxes for observations by H.E.S.S. and the new CANGAROOtelescopes in the near future.

Russell Edwards (University of Amsterdam) PosterUnusual Subpulse Modulation in PSR B0320+39

We report on an analysis of the drifting subpulses of PSR B0320+39 that indicates a sudden step of∼ 160 degrees in subpulse phase near the centre of the pulse profile. The phase step, in combinationwith the attenuation of the periodic subpulse modulation at pulse longitudes near the step, suggeststhat the patterns arise from the addition of two superposed components of nearly opposite driftphase and differing longitudinal dependence. We argue that since there cannot be physical overlapof spark patterns of the polar cap, the drift components must be associated with a kind of “multipleimaging” of a single polar cap “carousel” spark pattern. One possibility is that the two componentscorrespond to refracted rays originating from opposite sides of the polar cap. A second optionassociates the components with emission from two altitudes in the magnetosphere.

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Fredrick Jenet (Caltech) PosterHigh Time Resolution Observations of Radio Pulsars and the First Detectionof non-Gaussian Coherent Emission

High time resolution (100 ns) observations of several radio pulsars were made with the CaltechBaseband Recorder (CBR) at the Arecibo Radio Observatory in Puerto Rico. New analysistechniques have been developed in order to study the single pulse properties of “weak” orlow-intensity pulsars. These techniques have been used to analyze the pulse-to-pulse amplitudeand pulse shape variations of the fastest millisecond pulsar PSR B1937+21. Techniques have alsobeen developed in order to search for the presence of coherent non-Gaussian emission statistics. Suchstatistics have been detected in pulsars B0823+26, B0950+08, and B1133+16. This is the first timesuch a phenomenon has been observed and these results place significant constraints on the radiopulsar emission mechanism.

Bhal Chandra Joshi (Jodrell Bank Observatory) PosterA Search for Giant Pulses in Millisecond Pulsars

Giant pulses, which are occasional individual pulses with an intensity typically 100 times the averageintensity, have been seen in three pulsars to date. Recent studies suggest a connection between thestrength of magnetic field at light cylinder and the existence of such pulses. Since millisecond pulsarshave relatively larger magnetic field strength at light cylinder radius, these stars are more likely toshow giant pulses. We have obtained single pulse data on eight MSPs using GMRT. The detectionthreshold for our data is ∼ 6 Jy. The results of this study are summarised in the poster.

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Aris Karastergiou (MPIfR Bonn) PosterSimultaneous Single-Pulse Observations of Radio Pulsars

Simultaneous single-pulse observations of radio-pulsars at multiple frequencies (1.4GHz, 2.7 GHz and4.8GHz) provide an excellent opportunity to investigate the intricate problem of pulsar emission.We especially study the frequency evolution of polarization characteristics, for PSR B0329+54 andPSR B1133+16. We also specifically investigate the behaviour of orthogonal polarization modesin PSR B1133+16. Our results show us that polarization features exhibit a complex picture whenobserved simultaneously across a broad frequency range, suggesting the increased role of propagationeffects in the pulsar magnetosphere.

Jarek Kijak (Institute of Astronomy, Zielona Gora) PosterStructure of Pulsar Beams

Structure of mean pulsar radiation patterns is discussed within the nested-cones and patchy beammodels. Observational predictions of both these models are analyzed and compared with availabledata on pulsar waveforms. It is argued that observational properties of pulsar waveforms are highlyconsistent with the nested-cone model and, in general, inconsistent with the patchy beam model.

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Haydon Knight (Swinburne University) PosterA Baseband Survey for Ultrafast Pulsars

Utilising the increased 64MHz bandwidth and 2-bit sampling of the newly commissioned CPSR-IIbaseband recorder at the Parkes Radio Telescope we recently undertook a survey of 6 globularclusters of known dispersion measure. Nyquist sampled for around 8 hours, each observation wascentred at 660MHz and produced a dataset of approximately 2 TB. An appropriately large syntheticcoherent filterbank was formed, with each channel typically sampled faster than 64 microseconds.Full acceleration searches and custom RFI mitigation techniques were then applied to each dataset.Novel acceleration search strategies are to be applied off-line at a later date. Although resultsare still forthcoming, preliminary analyses suggest that the raw dataset taken will be significantlymore sensitive to the putative pulsar populations in highly dispersed clusters such as Terzan 5. Theapplication of broad bandwidth coherent dedispersion has allowed us to eliminate dispersive smearingas a limiting factor to the survey sensitivity. Exact figures depend on the nature of interstellarscattering effects, but a theoretical sensitivity of 0.2mJy for the long-hailed sub-millisecond pulsaris expected. This experiment will place significant constraints upon the ultrafast pulsar population.

Qinghuan Luo (University of Sydney) PosterPropagation Effects on Pulsar Radio Emission

It is generally believed that a pulsar magnetosphere is populated with pair plasmas produced throughacceleration near the polar cap. Any radio emission produced inside the magnetosphere must besubject to various propagation effects due to the intervening plasma. I will discuss in particular theabsorption effect on the radio beam by the cyclotron resonance in co-rotating pulsar plasma. A raytracing model has been developed including the co-rotation effect. It is shown that such effect canlead to observable features in the pulse profile.

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Joeri van Leeuwen (Utrecht Astronomical Institute) PosterNulling-drifting interaction in PSR B0809+74

Using high-quality single pulse sequences, taken with Westerbork/PuMa, we accurately identify thenulls of PSR B0809+74. We then determine the alias order of the subpulse drift, using its interactionwith these nulls. We find that the subpulse drift is not aliased but directly reflects the actual motionof the subbeams.

We use this to show that the carousel-rotation time must be longer than 200 seconds, much longerthan predicted by theory. Furthermore, we show that after nulls, the subbeam carousel is reducedin size, suggesting that it originates lower in the pulsar magnetosphere. This indicates an increaseof the particle velocity and/or a decrease in plasma frequency after nulls

Donald Payne (Melbourne University) PosterMagnetic Field Evolution in Accreting Neutron Star Binaries

We model the field reduction by magnetic field burial, maintaining strict flux-freezing. We find thatan accreted mass of 10−5 solar masses is required before significant reduction in the dipole momentoccurs. This negates earlier work which found 10−10 because the equatorward magnetic stresseswere neglected.

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Alberto Pellizzoni (IstIASF/CNR) PosterOptical Study of the Radio Quiet Pulsar Candidate Associated with SNRG266.1−1.2

The shell-like SNR G266.1−1.2 appears projected against the much more extended Vela remnant.The inferred hydrogen column density suggests a location farther than the latter (1-2 kpc) althoughthe possible detection of the short-lifetime 44Ti gamma-ray line at 1.156 MeV might imply avery young age and a distance of only 200 pc. The quest for the compact remnant associatedto G266.1−1.0 started with the detection of possible X-ray candidates by ROSAT, ASCA andBeppoSAX. This was recently identified with a soft X-ray source localized with an accuracy of 2′′

with Chandra. The spectrum and luminosity of this source are difficult to explain with a very youngand nearby neutron star as suggested by gamma-ray line observations of the associated SNR. Wewill report our results on the possible optical counterparts of this interesting X-ray source belongingto the emerging class of radio/gamma-quiet neutron stars.

Gerard Petit (BIPM) PosterLooking for Submillisecond Pulsars: A Progress Report

A millisecond pulsar survey has been started to search for very fast and dispersed millisecond pulsars.A data acquisition system and associated processing techniques have been developed and surveyobservations have been conducted at Nancay in 1998. Observations of known millisecond pulsarshave been used to validate the system and assess the sensitivity of the survey. About 400 parasite-freescans, corresponding to 10 square degrees in the galactic plane, have been processed, searching forperiods down to 0.67 ms, DM up to 300 cm−3pc and moderate binary configuration. No new pulsarhas been found so far. Re-observations of a few candidate signals and re-processing of the datasearching for extreme binary configurations are under way.

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Jerome Petri (Observatoire Astronomique de Strasbourg) PosterStructure and Stability of Pulsars’ Electrospheres

I will speak about the construction of pulsar electrospheric models. I will show that this structureis unstable against an electrostatic instability, the diocotron instability. The consequences of thisinstability for the electric current in the magnetosphere will also be discussed. Finally, we study ofthe pair creation in the vacuum gaps by photon-photon interaction and by photon disintegration.

John-Hugh Seiradakis (University of Thessaloniki, Greece) PosterConverting EPN-formatted Data to XML Format

Before the creation of the European Pulsar Network (EPN), the lack of a common standard formatfor pulsar data had seriously hampered collaborative research attempts. Since 1998 the EPN dataformat has been used in several observatories facilitating an easy exchange of data between pulsarresearchers. With the present work, we have extended the portability of pulsar data creating a toolto convert EPN formatted pulsar data to XML (Extensible Markup Language) format. The tool,written in Fortran code, automatically converts EPN files to XML Physical Structure (xml) andXML Document Type Definition (dtd) files. XML is a tree-structured language and is expected toplay a pivotal role in the exchange of any kind of data in the web in the near future. The datais annotated using tags (similar to the tags used in HTML) that describe what each piece of datais. The MS Explorer (V ≥ 5.5) already reads XML files. Other browsers are expected to follow.The Cambridge University Press is ready to accept publications in XML format. Several tools forreducing data in XML format are being built at the moment.

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Ingrid Stairs (University of British Columbia) PosterHigh Resolution Observations of PSR B1828−11

We present high-time-resolution observations of the young precessing pulsar B1828−11, which yieldclues to the true beam shape and the fundamental precession period.

Dan Stinebring (Oberlin College) PosterFrequency Dependence of Scintillation Arcs

A thin-screen model for the production of scintillation arcs predicts that the curvature of the arcs(fν/f2

t ) should scale as observing wavelength squared. I will present recent Arecibo observationsthat confirm this prediction for several pulsars.

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Frank Verbunt (Astronomical Institute Utrecht) Poster

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Zaven ArzoumanianUSRA/[email protected]: +1-301-286-2547fax: +1-301-286-1684X-Ray Astrophysics Branch, Code 662Greenbelt, MD 20771, USA

Dimitris AthanasiadisJodrell Bank [email protected]: +441477572678Jodrell Bank ObservatoryMacclesfield, Cheshire, SK11 9DL, UK

Donald BackerUniversity of California, [email protected]: +1-510-642-5128fax: +1-510-642-3411Astronomy Department601 Campbell HallUniversity of CaliforniaBerkeley, CA 94720-3411 USA

Matthew BailesSwinburne [email protected]: +61-3-9214 8782fax: +61-3-9214 8797Astrophysics and SupercomputingPO Box 218Hawthorn, Vic 3122, Australia

Robert BenjaminUniversity of Wisconsin, [email protected]: +1-608-262-5916fax: +1-608-263-0361Dept of PhysicsUniversity of Winsconsin-Madison1150 University Ave.Madison, WI 53706 USA

Lars BildstenKavli Institute for Theoretical [email protected]: +1-805-893-3979fax: +1-805-893-2431KITP, Kohn HallUCSBSanta Barbara, CA 93106, USA

Olga BitzarakiUniversity of [email protected]: 0107276898fax: 01 7276725Section of Astrophysics, Astronomy andMechanicsUniverity of AthensPanepistimiopolis, ZografosAthens, GR 157 84

Walter BriskenNational Radio Astronomy [email protected]: +1-505-835-7133fax: +1-505-835-7027PO Box OSocorro, NM 87801, USA

Marta BurgayAstronomical Observatory of [email protected]: +39 051 2095719fax: +39 051 2095700Via Ranzani 140127 Bologna, Italy

Fernando CamiloColumbia [email protected]: +1-212-854-2540fax: +1-212-854-8121Columbia Astrophysics LabColumbia University550 West 120th StreetNew York, NY 10027, USA

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Deepto [email protected]: +1 617 253 3840fax: +1 617 253 0861Department of PhysicsMITRoom 37-626ACambridge, MA 02139, USA

Philip ChangUniversity of California, Santa [email protected] HallBuilding 572University of CaliforniaSanta Barbara, CA 93106-9530, USA

Shami ChatterjeeCornell [email protected]: +1 (607) 255 9020fax: +1 (607) 255 8803Cornell University518 Space SciencesIthaca, NY 14853, USA

Tzihong ChiuehNational Taiwan [email protected]: 886-3366-5190fax: 886-2367-03581 Roosevelt Rd. Sec.4Taipei, Taiwan

Augustine Ejikeme ChukwudeUniversity of Nigeria & HartRAO S/Aaus [email protected] of Physics & AstronomyUniversity of NigeriaNsukka. Nigeria

Andrew CummingUniversity of California, Santa [email protected]: +1-831-459-5246fax: +1-831-459-5265Department of Astronomy and AstrophysicsUniversity of CaliforniaSanta Cruz CA 95064, USA

Nichi D’AmicoCagliari Astronomical [email protected]: +39-070-71180208fax: +39-070-71180222Osservatorio Astronomico di CagliariStrada 54, Loc. Poggio dei Pini09012 Capoterra (Ca), Italy

Andrea De LucaCNR-IASF [email protected]: +39 02 23699329fax: +39 02 2666017Via Bassini 15I-20133 Milano, Italy

Russell EdwardsUniversity of [email protected]: +31-20-5257484Sterrenkundig Instituut ‘Anton Pannekoek’Kruislaan 4031098 SJ Amsterdam – Netherlands

Andrew FaulknerJodrell Bank [email protected]: +44 1477 571321fax: +44 1477 571618Jodrell Bank ObservatoryDept. of Physics & AstronomyThe University of ManchesterMacclesfield, Cheshire SK11 9DLUnited Kingdom

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Paulo FreireNAIC, Cornell [email protected]: +1 787 878 2612fax: +1 787 878 1861Arecibo ObservatoryHC 03 Box 53995Arecibo, Puerto Rico 00612, USA

Fabio FrescuraHartebeesthoek Radio Astronomy [email protected]: +27-11-717-6816fax: +27-11-339-2926Dept of PhysicsUniversity of the WitwatersrandWITS 2050 South Africa

Andrew FruchterSpace Telescope Science [email protected]: +1.410.338.5018fax: +1.410.338.47673700 San Martin DriveBaltimore, MD 21218, USA

Francis Graham SmithJodrell Bank [email protected]: +44-1477-571321fax: +44-1477-571618Jodrell Bank ObservatoryMacclesfield, Cheshire, SK11 9DL, UK

Yashwant GuptaNAIC, Arecibo and NCRA, [email protected]: +1-787-878-2612fax: +1-787-878-1861Arecibo ObservatoryHC3 Box 53995Arecibo, PR 00612, USA

JinLin HanNational Astronomical [email protected]: +86-10-6487.7723fax: +86-10-6487.7723 Jia-20, DaTun RoadChaoYang DistrictBeijing 100012, China

Craig HeinkeHarvard [email protected]: +1-617-495-5989Center for Astrophysics, MS-1060 Garden StreetCambridge MA 02138, USA

Edward van den HeuvelUniversity of [email protected]: +31-20-5257492fax: +31-20-5257484Astronomical InstituteKruislaan 4031098SJ Amsterdam, Netherlands

Antony HewishCavendish [email protected]: 01223 337299fax: 012233545999Cavendish LaboratoryMadingley RoadCambridge, CB3 0HE, UK

George HobbsJodrell Bank [email protected]: +44 1477 571617fax: +44 1477 571618Jodrell Bank ObservatoryMacclesfield, CheshireSK11 9DL, UK

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Aidan HotanSwinburne [email protected]: +61 (03) 9214 8502fax: +61 (03) 9214 8797Mail number 31Swinburne University of TechnologyPO Box 218Hawthorn Victoria 3122, Australia

Bryan [email protected]: +1 626 395 4026fax: +1 626 568 9352Caltech Astronomy 105-241201 East California Bl.Pasadena, CA 91125, USA

Ocker C. de JagerPotchefstroom [email protected]: +27-18-2992418fax: +27-18-2992421Unit for Space PhysicsPotchefstroom Univ. for CHEPotchefstroom 2520, South Africa

Fredrick [email protected]: +1 203 794 0142187 Scranton Ave.Lynbrook, NY 11563, USA

Simon JohnstonUniversity of [email protected] of PhysicsUniversity of SydneyNSW 2006, Australia

Bhal Chandra JoshiJodrell Bank [email protected]: +441477572677fax: +441477571618Jodrell Bank ObservatoryUniversity of ManchesterBomish LaneMacclesfield, Cheshire SK11 9DL, UK

Vicky KalogeraNorthwestern [email protected]

David [email protected]: +1-626-395-4051fax: +1-626-568-9352105-24 CaltechPasadena, CA 91125, USA

Aris KarastergiouMPIfR [email protected]

Victoria KaspiMcGill [email protected]: +1-514-398-6412fax: +1-514-398-3733Physics Department3600 University StreetMontreal, QC Canada H3W 2T8

Jarek KijakInstitute of Astronomy, Zielona [email protected]: +48 68 3202863fax: +48 68 3202863Institute of AstronomyUniversity of Zielona GoraLubuska 265-265 Zielona Gora, Poland

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Haydon KnightSwinburne [email protected]: +61 3 9214 8502fax: +61 3 9214 8797Mail number 31Swinburne University of TechnologyPO Box 218, HawthornVictoria 3122, Australia

Sergei KopeikinUniversity of Missouri, [email protected]: +1-573-882-6210fax: +1-573-882-4195Dept. of Physics and AstronomyUniversity of Missouri-Columbia223 Physics Bldg.Columbia, MO 65211, USA

Michael KramerJodrell Bank [email protected]: +44-1477-572622fax: +44-1477-571618Jodrell Bank ObservatoryJodrell BankMacclesfield SK11 9DL, UK

Dong LaiCornell [email protected]: +1 607 255 4936fax: +1 607 255 6918Space Sciences Bldg.Dept. of AstronomyCornell Univ.Ithaca, NY 14853, USA

Joeri van LeeuwenUtrecht Astronomical Institutephone: +31-30-2535208fax: +31-30-2535201P.O. Box 80000NL-3508 TA Utrecht, The Netherlands

Dion LewisUniversity of Tasmania/ATNF - [email protected]: +61 3 6226 7529fax: +61 3 6226 2867University of TasmaniaPhysics DepartmentGPO Box 252-21Hobart TAS 7001, Australia

Bennett LinkMontana State [email protected]: +1-406-994-6174fax: +1-406-994-4452Department of PhysicsMontana State UniversityBozeman, Montana 59717, USA

Andrea LommenUniversity of [email protected]: +31 (0)20 525 7491fax: +31 (0)20 525 7494Astronomy InstituteKruislaan 4031098 SJ Amsterdam, the Netherlands

Duncan LorimerJodrell Bank [email protected]: +44-1477-571321fax: +44-1477-571618Jodrell Bank ObservatoryMacclesfield, Cheshire, SK11 9DL, UK

Qinghuan LuoUniversity of [email protected]: +61-2-93512546fax: +61-2-9351-7726School of PhysicsThe University of Sydney

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Andrew LyneJodrell Bank [email protected]: +44-1477-571321fax: +44-1477-571618Jodrell Bank ObservatoryMacclesfield, Cheshire, SK11 9DL, UK

Richard [email protected]: 02-9372-4313fax: 02-9372-4310PO Box 76Epping NSW 1710 Australia

Maura McLaughlinJodrell Bank [email protected]: +44 1477 572672fax: +44 1477 571618Jodrell Bank ObservatoryMacclesfield, Cheshire, SK11 9DL, UK

Don MelroseSydney [email protected]: +61 2 9351 2537fax: +61 2 9351 7726School of PhysicsUniversity of SydneyNSW 2006 Australia

Luciano [email protected]: +39-091-6809562fax: +39-091-6882258Via U. La Malfa 15390146 Palermo, ITALY

David NicePrinceton [email protected]: +1-609-258-6347fax: +1-609-258-6853Physics DepartmentPrinceton UniversityBox 708Princeton, NJ 08544, USA

Steve OrdSwinburne [email protected] for Astrophysics and SupercomputingPO Box 218Hawthorn, Vic 3122, Australia

Donald PayneMelbourne [email protected]: 61 3 9509 7428fax: 61 3 9347 4783Astrophysics GroupMelbourne UniversityParkville, Vic, 3010, Australia

Alberto PellizzoniIstIASF/[email protected]: +39 2 23 699 493via Bassini, 15I-20133 Milano Italy

Gerard [email protected]: +33-145077067fax: +33-145077059Pavillon de Breteuil92312 Sevres, France

Jerome PetriObservatoire Astronomique de [email protected]: +33 290242400fax: +33 29024243211, rue de l’Universite67000 Strasbourg, France

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Fabio PizzolatoUniversita dell’insubria and IASF/[email protected]: +39-02-23699-329fax: +39-02-2666017IASF/CNR (Milano)Sez. “G. Occhialini”Via E. Bassini 15/A20133 Milano, Italy

Philipp PodsiadlowskiUniversity of [email protected]: +441865273343fax: +441865273390St. Edmund HallOxford, OX1 4Ar, United Kingdom

Andrea PossentiAstronomical Observatory of Bolognal [email protected]: +39-051-2095796fax: +39-051-2095700Osservatorio Astronomico di Bolognavia Ranzani 140127 Bologna, Italy

Guojun QiaoPeking [email protected]: +86-10-62758633fax: +86-10-62765031Dept. of AstronomyPeking UniversityBeijing, 100871, China

Aikaterini RadiotiUniversity of Thessaloniki, [email protected]: 30-310-816873

Scott RansomMcGill [email protected] Univ.Physics Dept.3600 University St.Montreal, QC H3A 2T8 Canada

Fred RasioNorthwestern [email protected]

Shaun ReidJodrell Bank [email protected]: +441477572657fax: +441477571618Jodrell Bank ObservatoryUniversity Of ManchesterMacclesfield, Cheshire, SK11 9DL, UK

Mallory RobertsMcGill / [email protected]: +1 514 398 6520fax: +1 514 398 37333600 University St.Montreal, QC H3A 2T8, Canada

Roger RomaniStanford [email protected]: +1(650)725-7595fax: +1(650)723-4840Dept of Physics MC 4060Stanford UniversityStanford, CA 94305, USA

John-Hugh SeiradakisUniversity of Thessaloniki, [email protected]: +30 310 998173fax: +30 310 995384University of ThessalonikiDepartment of PhysicsSection of Astrophysics, Astronomy andMechanicsGR-54006 Thessaloniki, Greece

Steinn SigurdssonPenn [email protected]: +1 814 863 6038fax: +1 814 863 3399525 Davey LaboratoryPenn StateUniversity Park, PA 16802, USA

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Ingrid StairsUniversity of British [email protected]: +1-304-456-2213fax: +1-304-456-2229Dept. of Physics and AstronomyUniversity of British Columbia6224 Agricultural RoadVancouver, BC V6T 1Z1 Canada

Dan StinebringOberlin [email protected]: +1-440-775-8331fax: +1-440-775-6379Dept. of Physics & AstronomyOberlin CollegeOberlin, OH 44074, USA

Willem van StratenSwinburne [email protected]: +61-3-9214 8758fax: +61-3-9214 8797Centre for Astrophysics and SupercomputingMail number 31PO Box 218Hawthorn, Victoria 3122, Australia

Marco TavaniIASF-CNR, [email protected]: +39-02-23699-345fax: +39-02-2367587IASF-CNRvia Bassini 1520133 Milano, Italy

Joseph TaylorPrinceton [email protected]: 609 258 3020fax: 609 258 21689 Nassau HallPrinceton UniversityPrinceton, NJ 08544, USA

Stephen ThorsettUniversity of California, Santa [email protected]: +1-831-459-5170Dept of Astronomy and Astrophysics1156 High StSanta Cruz, CA 95064, USA

Adrian TipladyRhodes [email protected]: 046-6038461fax: 046-6035049Dept. Physics and ElectronicsRhodes UniversityGrahamstown, 6140, South Africa

Johnson UramaUniversity of Nigeria, [email protected]: +234 42 771107Dept. of Physics & AstronomyUniversity of NigeriaNsukka, Enugu State, Nigeria

Frank VerbuntAstronomical Institute [email protected]: 31-30-2535207fax: 31-30-2535201Astronomical InstitutePostbox 80.0003508 TA Utrecht, Netherlands

Na WangUrumqi Observatory, [email protected]: +86-991-3846524fax: +86-991-3838628South Beijing Road, 40-5Urumqi ObservatoryUrumqi, Xinjiang 830011, China

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Joel WeisbergCarleton College [email protected]: +1 507 646 4367fax: +1 507 646 4384Physics & AstronomyCarleton College1 N. CollegeNorthfield MN 55057, USA

Craig WestSwinburne [email protected]: +61 (03) 9214 8502fax: +61 (03) 9214 8797Mail number 31Swinburne University of TechnologyPO Box 218Hawthorn Victoria 3122, Australia

Richard WielebinskiMPI for [email protected]: +49 228 525300fax: +49 228 525436mpifrauf dem hugel 69D-53121 Bonn, Germany

Graham WoanUniversity of [email protected]: +44 141 330 5897fax: +44 141 330 5183University of GlasgowGlasgow, G12 8QQ, UK

Alex WolszczanPenn State [email protected]: +49 228 525 496fax: +49 228 525 436Max-Planck-Institut fuer RadioastronomieAuf dem Huegel 6953121 Bonn, Germany

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