Vacuum gap model for PSR B0943+10

Gil, Janusz; Melikidze, George I.; Mitra, Dipanjan

doi:10.1051/0004-6361:20020475

Cited by 29 publications

(20 citation statements)

References 21 publications

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“…Whether, however, this model's other physical expectations (including that the primary particle acceleration occurs just above the magnetic polar cap) remain an open, but now actively debated, question (e.g. Asseo & Khechinashvili 2002; Gil, Melichidze & Mitra 2002; Wright 2002).…”

Section: Summary and Discussionmentioning

confidence: 99%

The topology and polarization of sub-beams associated with the 'drifting' subpulse emission of pulsar B0943 + 10 - III. Analysis of Pushchino 103/40-MHz observations

Rankin

Suleymanova

Deshpande

2003

Monthly Notices of the Royal Astronomical Society

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The rotating emission‐beam system of pulsar B0943 + 10 was explored in Paper I of this series using Arecibo observations at 430 and 111 MHz and in Paper II using Gauribidanur 35‐MHz data. Here, we have the opportunity to study simultaneous, dual‐frequency observations carried out at the Pushchino Radio Astronomy Observatory some 10 yr ago at frequencies of 103 and 40 MHz. The apparent modulation periods (P3) and circulation times derived from the 11 d of observations seem to fall into two distinct ranges, apparently correlated with profile modal effects. The 103‐MHz maps bear a strong resemblance to the 111‐MHz Arecibo sequence studied in Paper I, but show a variety of sub‐beam intensity patterns, whereas similar comments can be made about the 40‐MHz maps in relation to the 35‐MHz maps of Paper II. Most interesting here is the result that there is little correspondence between the sub‐beam maps at the two frequencies. Only for two of the observations do we find a correspondence between the pairs: one of the ‘B’‐mode sequences with an asymmetric pattern as well as a ‘Q’‐mode sequence occurring immediately prior to a transition to the ‘B’ mode. Finally, we find that our various ‘B’‐mode observations vary markedly in their profile linear polarization. The strongest sequences suggest differing proportions of secondary polarization mode power.

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Section: Summary and Discussionmentioning

confidence: 99%

The topology and polarization of sub-beams associated with the 'drifting' subpulse emission of pulsar B0943 + 10 - III. Analysis of Pushchino 103/40-MHz observations

Rankin

Suleymanova

Deshpande

2003

Monthly Notices of the Royal Astronomical Society

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“…In a later work Nishimura (2005) demonstrates that a linearly varying magnetic field is able to produce line non-harmonicity even for a 5 m thick slab of plasma above the NS. Such a configuration can be modeled by a combination of axial and crustal magnetic field, as proposed by Gil et al (2002).…”

Section: Structure Of the Cyclotron Harmonicsmentioning

confidence: 99%

Study of the accreting pulsar 4U 0115+63 using a bulk and thermal Comptonization model

Ferrigno

Becker

Segreto

et al. 2009

A&A

121

148

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Context. Highly magnetized pulsars accreting matter in a binary system are bright sources in the X-ray band (0.1-100 keV). Despite the early comprehension of the basic emission mechanism, their spectral energy distribution is generally described by phenomenological or simplified models. Aims. We propose a study of the spectral emission from the high mass X-ray binary pulsar 4U 0115+63 by means of thermal and bulk Comptonization models based on the physical properties of such objects. Methods.For this purpose, we analyze the BeppoSAX data in the energy range 0.7-100 keV of the 1999 giant outburst, 12 days after the maximum. We focus first on the phase averaged emission, and then on the phase resolved spectra, by modeling the system using a two-component continuum. Results. At higher energy, above ∼7 keV, the emission is due to thermal and bulk Comptonization of the seed photons produced by cyclotron cooling of the accretion column, and at lower energy, the emission is due to thermal Comptonization of a blackbody source in a diffuse halo close to the stellar surface. Phase resolved analysis establishes that most of the emission in the main peak comes from the column, while the low energy component gives a nearly constant contribution throughout the phase. Conclusions. From the best fit parameters, we argue that the cyclotron emission is produced ∼1.7 km above the stellar surface, and escapes from the column near its base, where the absorption features are generated by the interaction with the magnetic field in the halo. We find that in 4U 0115+63, the observed spectrum is dominated by reprocessed cyclotron radiation, whereas in other bright sources with stronger magnetic fields such as Her X-1, the spectrum is dominated by reprocessed bremsstrahlung.

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“…This is required, e.g., to explain the existence of long-period radio pulsars [27,28]. It is also supposed that the magnetic field near the surface of the neutron star must differ very strongly from a dipolar field in order for radio pulsars to operate in the Ruderman-Sutherland model [29][30][31].…”

Section: Non-dipolar Magnetic Fieldmentioning

confidence: 99%

Evolution of the angle between the magnetic moment and the rotation axis of radio pulsars

2009

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Abstract-It is shown that, when angular-momentum losses of a radio pulsar are represented as a sum of magnetic-dipole and current losses, the angle between the magnetic moment and rotation axis of the radio pulsar tends to some equilibrium value (near 45• ). This process takes place on a timescale of the order of the pulsar's characteristic age. Taking into account the non-dipolarity of the pulsar's magnetic field changes this equilibrium angle.PACS numbers: 97.60.Gb

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Vacuum gap model for PSR B0943+10

Cited by 29 publications

References 21 publications

The topology and polarization of sub-beams associated with the 'drifting' subpulse emission of pulsar B0943 + 10 - III. Analysis of Pushchino 103/40-MHz observations

The topology and polarization of sub-beams associated with the 'drifting' subpulse emission of pulsar B0943 + 10 - III. Analysis of Pushchino 103/40-MHz observations

Study of the accreting pulsar 4U 0115+63 using a bulk and thermal Comptonization model

Evolution of the angle between the magnetic moment and the rotation axis of radio pulsars

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