Drifting Subpulses in PSR B0943+10

Gil, Janusz; Sendyk, M.

doi:10.1086/346079

Cited by 29 publications

(44 citation statements)

References 25 publications

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“…This interpretation is supported by detailed analysis of drifting data (Deshpande & Rankin 1999Asgekar & Deshpande 2001;Gil & Sendyk 2003). The RS75 model is the leading model to interpret the observations quantitatively.…”

Section: Introductionmentioning

confidence: 58%

“…The numbers of the subbeams are calculated theoretically, and the drifting rates can be obtained from the simulations, which would be used to infer the dynamical structure of both gaps. Gil & Sendyk (2000) suggest that the number of sparks that can be observed in the drifting pattern is given by N Ӎ , where N is the number of sparks, h is the height of 2pr /h for the ICG, where R is the stellar radius and is the radius R lc of the light cylinder. For a resonance ICS gap, the gap height is (Zhang et al…”

Section: Simulations Of Subpulse Driftingmentioning

confidence: 99%

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A Model for the Challenging "Bi-drifting" Phenomenon in PSR J0815+09

Qiao

Lee

Zhang

et al. 2004

ApJ

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A new drifting pulsar, PSR J0815ϩ09, was discovered in the Arecibo drift-scan searches. An intriguing feature of this source is that within the four pulse components in the integrated pulse profile, the subpulse drifting direction in the two leading components is opposite from that in the two trailing components. In the view that the leading theoretical model for pulsar subpulse drifting can only interpret one-direction subpulse drifting, the observed bi-drifting phenomenon from PSR J0815ϩ09 poses a great challenge to the pulsar theory. The inner annular gap (IAG), a new type of inner particle accelerator, was recently proposed to explain both g-ray and radio emission from pulsars. Here we show that the coexistence of the IAG and the conventional inner core gap offers a natural interpretation to the bi-drifting phenomenon. In particular, the peculiar drifting behavior in PSR J0815ϩ09 can be reproduced within the inverse Compton scattering model for pulsar radio emission.

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Section: Introductionmentioning

confidence: 58%

Section: Simulations Of Subpulse Driftingmentioning

confidence: 99%

A Model for the Challenging "Bi-drifting" Phenomenon in PSR J0815+09

Qiao

Lee

Zhang

et al. 2004

ApJ

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“…This carousel of spark plasma filaments can be observed as so-called drifting subpulses in the radio lightcurves of many pulsars. However, the predictions of the vacuum gap model yielded much faster drift rates of subpulses than were found in the observations (van Leeuwen et al 2003;Gil & Sendyk 2003). In order to reconcile observations with theoretical predictions the partially screened gap model (PSG) has been developed.…”

Section: Partially Screened Gapmentioning

confidence: 99%

Magneto–Thermal Evolution of Neutron Stars with Emphasis to Radio Pulsars

Geppert¹

2017

J Astrophys Astron

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The magnetic and thermal evolution of neutron stars is a very complex process with many, also non-linear, interactions. For a decent understanding of neutron star physics, these evolutions cannot be considered isolated. A brief overview is presented, which describes the main magneto -thermal interactions that determine the fate both of isolated neutron stars and accreting ones. Special attention is devoted to the interplay of thermal and magnetic evolution at the polar cap of radio pulsars. There, a strong meridional temperature gradient is maintained over the lifetime of radio pulsars. It may be strong enough to drive thermoelectric magnetic field creation which perpetuate a toroidal magnetic field around the polar cap rim. Such a local field component may amplify and curve the poloidal surface field at the cap, forming a strong and small scale magnetic field there as required for the radio emission of pulsars.Key words: stars: neutron -stars: magnetic fields -pulsars: general -stars: interiors PREFACEWhen I started to try to understand some aspects of neutron star physics, one of the first papers I read was Srinivasan & van den Heuvel (1982) about the evolution of millisecond pulsars. Then the connection between the (at that time in optical light) invisible pulsars and the fascinating manifestations of supernova remnants (Srinivasan et al. 1984) increased my interest in this branch of astrophysics. The observation of millisecond pulsars in the early eighties was a challenge, which was met by Prof. Srinivasan and his colleagues (see e.g. Bhattacharya & Srinivasan (1986);Srinivasan (1989)). Later the pioneering work of Srinivasan et al. (1990) triggered my interest to understand how the very long-lived core magnetic field is affected by the rotational history of neutron stars and how the evolutions of core and crustal field are coupled to each other. Meanwhile Prof. Srinivasan enriched our knowledge about neutron stars by many contributions, among others about their evolution in accreting binary systems, about the recycling of old pulsars to millisecond pulsars, about the supernova remnants and pulsar wind nebulae which are results of neutron star births, about the use of radiotelescope for pulsar observations and about many other topics. As far as I can see being a far distant observer, Prof. Srinivasan succeeded also in the formation of a group of excellent and worldwide renown Indian scientists working in the field of neutron star physics.⋆ E-mail:ulrich.geppert@dlr.deMay be there exists a not yet discovered age-relativistic effect that makes the time running faster when seen by an aging person. It seems to be this effect that made me surprised to recognize that Prof. Srinivasan celebrates already his 75th birthday. This special issue is a good opportunity to esteem his life-work and I am happy that I can contribute to it. THE MANY FACETS OF MAGNETO -THERMAL INTERACTIONS

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Section: Charge-depleted Inner Acceleration Regionmentioning

confidence: 99%

“…If the plasma above the polar cap is fragmented into filaments (sparks) that determine the intensity structure of the instantaneous pulsar radio beam, then, at least in principle, the tertiary periodicityP 3 can be measured/ estimated from the pattern of the observed drifting subpulses (e.g., DR99; Gil & Sendyk 2003). In practiceP 3 is very difficult to measure (mainly because of aliasing, which is a severe problem even in pulsars with high signal-to-noise ratio; e.g., DR99; Gil & Sendyk 2003) and its value is known at the moment only in few cases. It is much easier to measure the primary drift periodicity P 3 , which in high signal-to-noise ratio is just a distance between the observed drift bands measured in pulsar periods P (there are also clever techniques that allow the measurement of P 3 even in cases with very low signal-to-noise ratio; see Edwards & Stappers 2002;WES06).…”

Section: Charge-depleted Inner Acceleration Regionmentioning

confidence: 99%

Formation of a Partially Screened Inner Acceleration Region in Radio Pulsars: Drifting Subpulses and Thermal X‐Ray Emission from Polar Cap Surface

Gil

Melikidze

Zhang

2006

ApJ

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The subpulse drifting phenomenon in pulsar radio emission is considered within the partially screened inner gap model, in which the sub-Goldreich-Julian thermionic flow of iron ions or electrons coexists with the spark-associated electron-positron plasma flow. We derive a simple formula that relates the thermal X-ray luminosity L X from the sparkheated polar cap and the E < B subpulse periodicityP 3 (polar cap carousel time). For PSRs B0943+10 and B1133+16, the only two pulsars for which bothP 3 and L X are known observationally, this formula holds well. For a few other pulsars, for which only one quantity is measured observationally, we predict the value of the other quantity and propose relevant observations that can confirm or discard the model. Then we further study the detailed physical conditions that allow such partially screened inner gap to form. By means of the condition T c /T s > 1 (where T c is the critical temperature above which the surface delivers a thermal flow to adequately supply the corotation charge density, and T s is the actual surface temperature), it is found that a partially screened gap (PSG) can be formed given that the near surface magnetic fields are very strong and curved. We consider both curvature radiation (CR) and resonant inverse Compton scattering (ICS) to produce seed photons for pair production, and find that the former is the main agency to produce gamma rays to discharge the PSG.

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Drifting Subpulses in PSR B0943+10

Cited by 29 publications

References 25 publications

A Model for the Challenging "Bi-drifting" Phenomenon in PSR J0815+09

A Model for the Challenging "Bi-drifting" Phenomenon in PSR J0815+09

Magneto–Thermal Evolution of Neutron Stars with Emphasis to Radio Pulsars

Formation of a Partially Screened Inner Acceleration Region in Radio Pulsars: Drifting Subpulses and Thermal X‐Ray Emission from Polar Cap Surface

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