Acceleration and collimation of relativistic plasmas ejected by fast rotators

Bogovalov, S. V.

doi:10.1051/0004-6361:20010201

Cited by 60 publications

(96 citation statements)

References 55 publications

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“…It only happens for a small value 37 of the magnetization ∼ 10 −3 . This contrasts strongly the expectations of pulsar wind electrodynamics 47,48,49,50 , which suggest that the magnetization in the wind, at best, with minor deviations from radial outflow, could be ∼ 1 at the typical distance of the nebulae 51 . Moreover 1-D models fail to explain the relative size of X-ray an Radio in the Crab Nebula 52 , and the correct softening of the spectrum with the distance from the pulsar 53 .…”

Section: -D Modelscontrasting

confidence: 92%

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Pulsar Wind Nebulae Modeling

Bucciantini

2014

Int. J. Mod. Phys. Conf. Ser.

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Pulsar Wind Nebulae (PWNe) are ideal astrophysical laboratories where high energy relativistic phenomena can be investigated. They are close, well resolved in our observations, and the knowledge derived in their study has a strong impact in many other fields, from AGNs to GRBs. Yet there are still unresolved issues, that prevent us from a full clear understanding of these objects. The lucky combination of high resolution X-ray imaging and numerical codes to handle the outflow and dynamical properties of relativistic MHD, has opened a new avenue of investigation that has lead to interesting progresses in the last years. Despite all of this, we do not understand yet how particles are accelerated, and the functioning of the pulsar wind and pulsar magnetosphere, that power PWNe. I will review what is now commonly known as the MHD paradigm, and in particular I will focus on various approaches that have been and are currently used to model these systems. For each I will highlight its advantages, limitations, and degree of applicability.

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Section: -D Modelscontrasting

confidence: 92%

“…This is confirmed both by theoretical 67,49 and numerical 68,50,69,70,71,72 studies. Such a wind would naturally drive a complex dynamics at least in the inner region.…”

Section: -D Modelssupporting

confidence: 72%

Pulsar Wind Nebulae Modeling

Bucciantini

2014

Int. J. Mod. Phys. Conf. Ser.

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“…Astrophysical relativistic MHD winds were simulated successfully for large Lorentz factors and magnetization parameters by [6,8]. Numerically the interaction of the pulsar winds with the ISM has been modeled by [33] and [15].…”

Section: Numerical Modeling Methodsmentioning

confidence: 99%

“…Relativistic winds from pulsars flow radially. Their magnetic collimation is infinitesimally small [4,8]. The toroidal magnetic field B ϕ generated at the rotation of the pulsar is proportional to θ , where θ is the polar angle [7].…”

Section: Magnetic Breakingmentioning

confidence: 99%

Interaction of pulsar winds with interstellar medium

Bogovalov¹,

Chechetkin²,

Koldoba³

et al. 2005

AIP Conference Proceedings

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Abstract. Time dependent numerical simulations show that the anisotropy of the energy flux and a weak magnetization of the pulsar winds result into formation of the most spectacular features in the central part of the plerions, namely the X-ray tore and jet-like outflows. We present the results of such simulations performed by our group. One of the most important conclusions following from this study is the fact that these structures are a direct observational proof that the rotational losses of the rotation powered pulsar are not due to magnetodipole radiation but instead they are due to magnetic breaking of a relativistic wind ejected by the pulsars. In this regard we discuss the direct physical consequences from this conclusion for the pulsar physics. OBSERVATIONSOnly a small fraction of the rotational energy of rotation powered pulsars (RPP) is released in the form of electromagnetic radiation. The largest part of this energy is transformed into energy of the electromagnetic field and kinetic energy of the particles. In someway this energy is finally injected into the interstellar medium (ISM) surrounding the pulsar. The particles in the ISM are accelerated up to 10 15 eV. They start to emit synchrotron and inverse Compton radiation forming a plerion (or synchrotron nebula).The plerions emit electromagnetic radiation in a wide range of frequencies from the radio to high energy gamma-rays [30,17,3]. In the last few years telescopes on the Hubble, Chandra and XMM observatories bring us new observational data about the central part of plerions. Observations in X-rays [13,20] and in the optics [26] have discovered a remarkable torus and jet-like structures in the central part of the Crab Nebula. The same structures were found by Chandra around the Vela pulsar [25,41,42].It appears that along with the rather close similarity between the Crab and Vela plerions there are at the same time remarkable differences. The bolometric Crab Nebula luminosity is equal to dozens of percentages of the pulsar rotational losses. In the Crab Nebula the X-ray torus consists of two parts: the inner ring with a small radius and an outer diffuse ring with a larger radius. The Vela nebula is rather compact and has low luminosity compared with the rotational losses of the pulsar, ∼ 5 · 10 −5 [25]. The torus in the Vela nebula consists of two rings as well. The radii of the rings are almost the same. No outer diffuse torus was observed in the Vela Nebula in X-rays. However, some signature of the outer torus has been found in the radio [19]. Attempts to find the plerionic structure around Vela in the optical are still not successful [39].Toroidal and jet-like structures were found in several other plerions as well: around 117 CP745, High Energy Gamma-Ray Astronomy, edited by

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“…The ratio between the energy fluxes of them is defined as the magnetization parameter σ = WEM/Wpart. Studies with magnetohydrodynamic (MHD) theory demonstrated that particles can not be effectively accelerated in pulsar wind (Usov 1975;Melatos & Melrose 1996; Beskin et al 1998; Chiueh et al 1998;Bogovalov & Tsinganos 1999;Bogovalov 2001;Lyubarsky & Eichler 2001;Lyubarsky 2002), therefore σ 1. However large kinetic energy of e ± in pulsar wind is needed in modeling the observations in high energy.…”

Section: Introductionmentioning

confidence: 99%

Probing the properties of the pulsar wind via studying the dispersive effects in the pulses from the pulsar companion in a double neutron-star binary system

Cheng

2017

Monthly Notices of the Royal Astronomical Society

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The velocity and density distribution of e ± in the pulsar wind are crucial distinction among magnetosphere models, and contains key parameters determining the high energy emission of pulsar binaries. In this work, a direct method is proposed, which might probe the properties of the wind from one pulsar in a double-pulsar binary. When the radio signals from the first-formed pulsar travel through the relativistic e ± flow in the pulsar wind from the younger companion, the components of different radio frequencies will be dispersed. It will introduce an additional frequency-dependent time-of-arrival delay of pulses, which is function of the orbital phase. In this paper, we formulate the above-mentioned dispersive delay with the properties of the pulsar wind. As examples, we apply the formula to the double pulsar system PSR J0737-3039A/B and the pulsar-neutron star binary PSR B1913+16. For PSR J0737-3039A/B, the time delay in 300 MHz is 10µs near the superior-conjunction, under the optimal pulsar wind parameters, which is ∼ half of the current timing accuracy. For PSR B1913+16, with the assumption that the neutron star companion has a typical spin down luminosity of 10 33 ergs/s, the time delay is as large as 10 ∼ 20µs in 300 MHz. The best timing precision of this pulsar is ∼ 5µs in 1400 MHz. Therefore, it is possible that we can find this signal in archival data. Otherwise, we can set an upper-limit on the spin down luminosity. Similar analysis can be apply to other eleven known pulsar-neutron star binaries.

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Acceleration and collimation of relativistic plasmas ejected by fast rotators

Cited by 60 publications

References 55 publications

Pulsar Wind Nebulae Modeling

Pulsar Wind Nebulae Modeling

Interaction of pulsar winds with interstellar medium

Probing the properties of the pulsar wind via studying the dispersive effects in the pulses from the pulsar companion in a double neutron-star binary system

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