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Collisionless, phasemixed, dispersive, Gaussian Alfvén pulse in transversely inhomogeneous plasma 

David Tsiklauri Submitted: 20161222 10:19
In the previous works harmonic, phasemixed, Alfvén wave dynamics was
considered both in the kinetic and magnetohydrodynamic regimes. Up today only
magnetohydrodynamic, phasemixed, Gaussian Alfvén pulses were investigated. In
the present work we extend this into kinetic regime. Here phasemixed, Gaussian
Alfvén pulses are studied, which are more appropriate for solar flares, than
harmonic waves, as the flares are impulsive in nature. Collisionless,
phasemixed, dispersive, Gaussian Alfvén pulse in transversely inhomogeneous
plasma is investigated by particleincell (PIC) simulations and by an
analytical model. The pulse is in inertial regime with plasma beta less than
electrontoion mass ratio and has a spatial width of 12 ion inertial length.
The linear analytical model predicts that the pulse amplitude decrease is
described by the linear Korteweg de Vries (KdV) equation. The numerical and
analytical solution of the linear KdV equation produces the pulse amplitude
decrease in time as t^{1}. The latter scaling law is corroborated by full
PIC simulations. It is shown that the pulse amplitude decrease is due to
dispersive effects, while electron acceleration is due to Landau damping of the
phasemixed waves. The established amplitude decrease in time as t^{1} is
different from the MHD scaling of t^{3/2}. This can be attributed to the
dispersive effects resulting in the different scaling compared to MHD, where
the resistive effects cause the damping, in turn, enhanced by the
inhomogeneity. Reducing background plasma temperature and increase in ion mass
yields more efficient particle acceleration.
Authors: D. Tsiklauri
Projects:

Publication Status: Phys. Plasmas 23, 122906 (2016) doi: 10.1063/1.4972574
Last Modified: 20170104 12:18



The effect of longitudinal density gradient on electron plasma wake field acceleration 

David Tsiklauri Submitted: 20161118 05:51
3, 2 and 1dimensional, particleincell, fully electromagnetic simulations of electron plasma wake field acceleration in the blow out regime are presented. Earlier results are extended by (i) studying the effect of longitudinal density gradient; (ii) avoiding use of comoving simulation box; (iii) inclusion of ion motion; and (iv) studying fully electromagnetic plasma wake fields. It is established that injecting driving and trailing electron bunches into a positive density gradient of tenfold increasing density over 10 cm long Lithium vapor plasma, results in spatially more compact and three times larger, compared to the uniform density case, electric fields (6.4 x 10^{10} V/m), leading to acceleration of the trailing bunch up to 24.4 GeV (starting from initial 20.4 GeV), with an energy transfer efficiencies from leading to trailing bunch of 75 percent. In the uniform density case 2.5 x 10^{10} V/m wake is created leading to acceleration of the trailing bunch up to 22.4 GeV, with an energy transfer efficiencies of 65 percent. It is also established that injecting the electron bunches into a negative density gradient of tenfold decreasing density over 10 cm long plasma, results in spatially more spread and 2.5 smaller electric fields (1.0 x 10^{10} V/m), leading to a weaker acceleration of the trailing bunch up to 21.4 GeV, with an energy transfer efficiencies of 45 percent. It is shown that twodimensional simulation results are substantially different from the threedimensional ones, showing only 10 percent efficiency of trailing bunch acceleration, while in onedimensional case no acceleration is seen. Inclusion of ion motions into consideration shows that in the plasma wake ion number density can increase over few times the background value. We also show that transverse electromagnetic fields in plasma wake are of the same order as the longitudinal (electrostatic) ones. Applications of this mechanism to solar coronal flare MeV electron reacceleration will be also explored.
Authors: David Tsiklauri
Projects:

Publication Status: Proc. Roy. Soc. A, 472, 20160630 (2016), DOI:10.1098/rspa.2016.0630
Last Modified: 20161228 11:40



Particleincell simulations of the relaxation of electron beams in inhomogeneous solar wind plasmas 

David Tsiklauri Submitted: 20161118 05:42
Previous theoretical considerations of electron beam relaxation in inhomogeneous plasmas have indicated that the effects of the irregular solar wind may account for
the poor agreement of homogeneous modelling with the observations. Quasilinear theory and Hamiltonian models based on Zakharov?s equations have indicated that
when the level of density fluctuations is above a given threshold, density irregularities act to deresonate the beam?plasma interaction, restricting Langmuir wave growth on
the expense of beam energy. This work presents the first fully kinetic particleincell (PIC) simulations of beam relaxation under the influence of density irregularities.
We aim to independently determine the influence of background inhomogeneity on the beam?plasma system, and to test theoretical predictions and alternative models
using a fully kinetic treatment. We carry out onedimensional (1D) PIC simulations
of a bumpontail unstable electron beam in the presence of increasing levels of background inhomogeneity using the fully electromagnetic, relativistic EPOCH PIC code. We find that in the case of homogeneous background plasma density, Langmuir wave packets are generated at the resonant condition and then quasilinear relaxation leads to a dynamic increase of wavenumbers generated. No electron acceleration is seen ? unlike in the inhomogeneous experiments, all of which produce highenergy electrons. For the inhomogeneous experiments we also observe the generation of backwardspropagating Langmuir waves, which is shown directly to be due to the refraction of the packets off the density gradients. In the case of higheramplitude density fluctuations, similar features to the weaker cases are found, but also packets can also deviate from the expected dispersion curve in (omega,k)space due to nonlinearity. Our fully kinetic PIC simulations broadly confirm the findings of quasilinear theory and the Hamiltonian model based on Zakharov?s equations. Strong density fluctuations modify properties of excited Langmuir waves altering their dispersion properties.
Authors: J.O. Thurgood, D. Tsiklauri
Projects:

Publication Status: J. Plasma Phys. 82, 905820604 (2016), doi:10.1017/S0022377816000970
Last Modified: 20161228 11:40



Selfconsistent particleincell simulations of fundamental and harmonic plasma radio emission mechanisms 

David Tsiklauri Submitted: 20151124 07:11
Aims. The simulation of threewave interaction based plasma emission, thought to be the underlying mechanism for Type III solar radio bursts, is a challenging task requiring fullykinetic, multidimensional models. This paper aims to resolve a contradiction in past attempts, whereby some studies indicate that no such processes occur. Methods. We selfconsistently simulate threewaved based plasma emission through all stages by using 2D, fully kinetic, electromagnetic particleincell simulations of relaxing electron beams using the EPOCH2D code. Results. Here we present the results of two simulations; Run 1 (nb/n0 = 0.0057, vb/{Delta}vb = vb/Ve = 16) and Run 2 (nb/n0 = 0.05, vb/{Delta}vb = vb/Ve = 8), which we find to permit and prohibit plasma emission respectively. We show that the possibility of plasma emission is contingent upon the frequency of the initial electrostatic waves generated by the bumpintail instability, and that these waves may be prohibited from participating in the necessary threewave interactions due to frequency conservation requirements. In resolving this apparent contradiction through a comprehensive analysis, in this paper we present the first selfconsistent demonstration of fundamental and harmonic plasma emission from a singlebeam system via fully kinetic numerical simulation. We caution against simulating astrophysical radio bursts using unrealistically dense beams (a common approach which reduces run time), as the resulting nonLangmiur characteristics of the initial wave modes significantly suppresses emission. Comparison of our results also indicates that, contrary to the suggestions of previous authors, an alternative plasma emission mechanism based on two counterpropagating beams is unnecessary in an astrophysical context.
Authors: J.O. Thurgood, D. Tsiklauri
Projects:

Publication Status: A&A 584, A83 (2015) DOI http://dx.doi.org/10.1051/00046361/201527079
Last Modified: 20161130 11:25



Alfvén wave phase mixing in flows  why overdense solar coronal open magnetic field structures are cool? 

David Tsiklauri Submitted: 20150721 15:27
Our magnetohydrodynamic (MHD) simulations and analytical calculations show that, when a background flow is present, mathematical expressions for the Alfvén wave (AW) damping via phase mixing are modified by a following substitution C′A(x)→C′A(x)+V′0(x), where CA and V0 are AW phase and the flow speeds and prime denotes derivative in the direction across the background magnetic field. In uniform magnetic field and overdense plasma structures, in which CA is smaller compared to surrounding plasma, the flow, that is confined to the structure, in the same direction as the AW, reduces the effect of phase mixing, because on the edges of the structure C′A and V′0 have opposite sign. Thus, the wave damps via phase mixing {it slower} compared to the case without the flow. This is the consequence of the codirectional flow reducing the wave front stretching in the transverse direction. Although, the result is generic and is applicable to different laboratory or astrophysical plasma systems, we apply our finding to address the question why overdense solar coronal open magnetic field structures (OMFS) are cooler than the background plasma. Observations show that the overdense OMFS (e.g. solar coronal polar plumes) are cooler than surrounding plasma and that in these structures Doppler broadening of lines is consistent with bulk plasma motions, such as Alfvén waves (AW). If overdense solar coronal OMFS are heated by AW damping via phase mixing, we conjecture that, codirectional with AW, plasma flow in them, reduces the phase mixing induced heating, thus providing an explanation why they appear cooler than the background.
Authors: D. Tsiklauri
Projects: None

Publication Status: Astron. Astrophys. 586, A95 (2016) DOI http://dx.doi.org/10.1051/00046361/201527105
Last Modified: 20161130 11:15



Octupolar outofplane magnetic field structure generation during collisionless magnetic reconnection in a stressed Xpoint collapse 

David Tsiklauri Submitted: 20140617 03:19
The outofplane magnetic field, generated by fast magnetic reconnection, during collisionless, stressed Xpoint collapse, was studied with a kinetic, 2.5D, fully electromagnetic, relativistic particleincell numerical code, using both closed (flux conserving) and open boundary conditions on a square grid. It was discovered that the well known quadrupolar structure in the outofplane magnetic field gains four additional regions of opposite magnetic polarity, emerging near the corners of the simulation box, moving towards the Xpoint. The emerging, outer, magnetic field structure has opposite polarity to the inner quadrupolar structure, leading to an overall octupolar structure. Using Ampere's law and integrating electron and ion currents, defined at grid cells, over the simulation domain, contributions to the outofplane magnetic field from electron and ion currents were determined. The emerging regions of opposite magnetic polarity were shown to be the result of ion currents. Magnetic octupolar structure is found to be a signature of Xpoint collapse, rather than tearing mode, and factors relating to potential discoveries in experimental scenarios or spacecraft observations are discussed.
Authors: J. Graf von der Pahlen, D. Tsiklauri
Projects:

Publication Status: Phys. Plasmas 21, 060705 (2014); DOI: 10.1063/1.4885378
Last Modified: 20140702 12:59



The effect of guidefield and boundary conditions on collisionless magnetic reconnection in a stressed Xpoint collapse 

David Tsiklauri Submitted: 20140509 07:49
Works of D. Tsiklauri, T. Haruki, Phys. of Plasmas, 15, 102902 (2008) and D.
Tsiklauri and T. Haruki, Phys. of Plasmas, 14, 112905, (2007) are extended by
inclusion of the outofplane magnetic (guide) field. In particular, magnetic
reconnection during collisionless, stressed Xpoint collapse for varying
outofplane guidefields is studied using a kinetic, 2.5D, fully
electromagnetic, relativistic particleincell numerical code. Cases for both
open and closed boundary conditions are investigated, where magnetic flux and
particles are lost and conserved respectively. It is found that reconnection
rates and outofplane currents in the Xpoint increase more rapidly and peak
sooner in the closed boundary case, but higher values are reached in the open
boundary case. The normalized reconnection rate is fast: 0.100.25. In the open
boundary case an increase of guidefield yields later onsets in the
reconnection peak rates, while in the closed boundary case initial peak rates
occur sooner but are suppressed. The reconnection current increases for low
guidefields but then decreases similarly. In the open boundary case, for
guidefields of the order of the inplane magnetic field, the generation of
electron vortices occurs. Possible causes of the vortex generation, based on
the flow of particles in the diffusion region and localized plasma heating, are
discussed. Before peak reconnection onset, oscillations in the outofplane
electric field at the Xpoint are found, ranging in frequency from
approximately 1 to 2 ω_{pe} and coinciding with oscillatory
reconnection. These oscillations are found to be part of a larger wave pattern.
Mapping the outofplane electric field over time and applying 2D Fourier
transforms reveals that the waves predominantly correspond to the ordinary mode
and may correspond to observable radio waves such as solar radio burst fine
structure spikes.
Authors: J. Graf von der Pahlen, D. Tsiklauri
Projects: None

Publication Status: Phys. Plasmas 21, 012901 (2014)
Last Modified: 20140509 17:06



3D particleincell simulation of electron acceleration by Langmuir waves in an inhomogeneous plasma 

David Tsiklauri Submitted: 20140509 07:42
A possible solution to the unexplained high intensity hard xray (HXR) emission observable during solar flares was investigated via 3D fully relativistic, electromagnetic particleincell (PIC) simulations with realistic ion to electron mass ratio. A beam of accelerated electrons was injected into a magnetised, Maxwellian, homogeneous and inhomogeneous background plasma. The electron distribution function was unstable to the beamplasma instability and was shown to generate Langmuir waves, while relaxing to plateau formation. In order to estimate the role of the background density gradient on an unbound (infinite spatial extent) beam, three different scenarios were investigated: a) a uniform density background; b) a weak density gradient, n_R/n_L=3; c) a strong gradient case, n_R/n_L=10, where n_R and n_L denote background electron densities on the left and right edges of the simulation box respectively. The strong gradient case produced the largest fraction of electrons beyond 15 v_th. Further, two cases (uniform and strong gradient background) with spatially localized beam injections were performed aiming to show drifts of the generated Langmuir wave wavenumbers, as suggested in previous studies. For the strong gradient case, the Langmuir wave power is shown to drift to smaller wavenumbers, as found in previous quasilinear simulations.
Authors: R. Pechhacker, D. Tsiklauri
Projects: None

Publication Status: Phys. Plasmas 21, 012903 (2014)
Last Modified: 20140509 17:06



Whistler wave generation by nongyrotropic, relativistic, electron beams 

David Tsiklauri Submitted: 20140509 07:36
Particleincell code, EPOCH, is used for studying features of the wave component evident to propagate backwards from the front of the nongyrotropic, relativistic beam of electrons injected in the Maxwellian, magnetised background plasma with decreasing density profile. According to recent findings presented in Tsiklauri (2011), Schmitz & Tsiklauri (2013) and Pechhacker & Tsiklauri (2012), in a 1.5dimensional magnetised plasma system, the nongyrotropic beam generates freely escaping electromagnetic radiation with properties similar to the TypeIII solar radio bursts. In this study the backwards propagating wave component evident in the perpendicular components of the elecromagnetic field in such a system is presented for the first time. Background magnetic field strength in the system is varied in order to prove that the backwards propagating wave's frequency, prescribed by the whistler wave dispersion relation, is proportional to the specified magnetic field. Moreover, the identified whistlers are shown to be generated by the normal Dopplershifted relativistic resonance. Large fraction of the energy of the perpendicular electromagnetic field components is found to be carried away by the whistler waves, while a small but sufficient fraction is going into L and R electromagnetic modes.
Authors: Marina Skender, David Tsiklauri
Projects: None

Publication Status: Phys. Plasmas 21, 042904 (2014)
Last Modified: 20140509 17:06



3D MHD simulation of linearly polarised Alfvén wave dynamics in ArnoldBeltramiChildress magnetic field 

David Tsiklauri Submitted: 20140509 07:30
Previous studies [Malara et al ApJ, 533, 523 (2000)] considered smallamplitude Alfvén wave (AW) packets in ArnoldBeltramiChildress (ABC) magnetic field using WKB approximation. In this work linearly polarised Alfvén wave dynamics in ABC magnetic field via direct 3D MHD numerical simulation is studied for the first time. Gaussian AW pulse with lengthscale much shorter than ABC domain length and harmonic AW with wavelength equal to ABC domain length are studied for four different resistivities. While it is found that AWs dissipate quickly in the ABC field, surprisingly, AW perturbation energy increases in time. In the case of the harmonic AW perturbation energy growth is transient in time, attaining peaks in both velocity and magnetic perturbation energies within timescales much smaller than resistive time. In the case of the Gaussian AW pulse velocity perturbation energy growth is still transient in time, attaining a peak within few resistive times, while magnetic perturbation energy continues to grow. It is also shown that the total magnetic energy decreases in time and this is governed by the resistive evolution of the background ABC magnetic field rather than AW damping. On contrary, when background magnetic field is uniform, the total magnetic energy decrease is prescribed by AW damping, because there is no resistive evolution of the background. By considering runs with different amplitudes and by analysing perturbation spectra, possible dynamo action by AW perturbationinduced peristaltic flow and inverse cascade of magnetic energy have been excluded. Therefore, the perturbation energy growth is attributed to a new instability. The growth rate appears to be dependent on the value of the resistivity and spatial scale of the AW disturbance. Thus, when going beyond WKB approximation, AW damping, described by full MHD equations, does not guarantee decrease of perturbation energy.
Authors: D. Tsiklauri
Projects:

Publication Status: Phys. Plasmas 21, 052902 (2014) http://scitation.aip.org/content/aip/journal/pop/21/5/10.1063/1.4875920
Last Modified: 20140514 13:10



Three dimensional particleincell simulation of particle acceleration by circularly polarised inertial Alfvén waves in a transversely inhomogeneous plasma 

David Tsiklauri Submitted: 20120808 10:03
The process of particle acceleration by lefthand, circularly polarised inertial Alfvén waves (IAW) in a transversely inhomogeneous plasma is studied using 3D particleincell simulation. A cylindrical tube with, transverse to the background magnetic field, inhomogeneity scale of the order of ion inertial length is considered on which IAWs with frequency 0.3 omega_{ci} are launched that are allowed to develop three wavelength. As a result timevarying parallel electric fields are generated in the density gradient regions which accelerate electrons in the parallel to magnetic field direction. Driven perpendicular electric field of IAWs also heats ions in the transverse direction. Such numerical setup is relevant for solar flaring loops and earth auroral zone. This first, 3D, fullykinetic simulation demonstrates electron acceleration efficiency in the density inhomogeneity regions, along the magnetic field, of the order of 45% and ion heating, in the transverse to the magnetic field direction, of 75%. The latter is a factor of two times higher than the previous 2.5D analogous study and is in accordance with solar flare particle acceleration observations. We find that the generated parallel electric field is localised in the density inhomogeneity region and rotates in the same direction and with the same angular frequency as the initially launched IAW. Our numerical simulations seem also to suggest that the ''knee'' often found in the solar flare electron spectra can alternatively be interpreted as the Landau damping (Cerenkov resonance effect) of IAWs due to the waveparticle interactions.
Authors: D. Tsiklauri
Projects:

Publication Status: Phys. Plasmas 19, 082903 (2012)
Last Modified: 20120815 06:41



Particle acceleration by circularly and elliptically polarised dispersive Alfvén waves in a transversely inhomogeneous plasma in the inertial and kinetic regimes 

David Tsiklauri Submitted: 20110707 04:40
Dispersive Alfvén waves (DAWs) offer, an alternative to magnetic reconnection, opportunity to accelerate solar flare particles. We study the effect of DAW polarisation, L, R, circular and elliptical, in different regimes inertial and kinetic on the efficiency of particle acceleration. We use 2.5D PIC simulations to study how particles are accelerated when DAW, triggered by a solar flare, propagates in transversely inhomogeneous plasma that mimics solar coronal loop. (i) In inertial regime, fraction of accelerated electrons (along the magnetic field), in density gradient regions is ~20% by the time when DAW develops 3 wavelengths and is increasing to ~30% by the time DAW develops 13 wavelengths. In all considered cases ions are heated in transverse to the magnetic field direction and fraction of the heated particles is ~35%. (ii) The case of Rcircular, L and R elliptical polarisation DAWs, with the electric field in the nonignorable transverse direction exceeding several times that of in the ignorable direction, produce more pronounced parallel electron beams and transverse ion beams in the ignorable direction. In the inertial regime such polarisations yield the fraction of accelerated electrons ~20%. In the kinetic regime this increases to ~35%. (iii) The parallel electric field that is generated in the density inhomogeneity regions is independent of m_i/m_e and exceeds the Dreicer value by 8 orders of magnitude. (iv) Electron beam velocity has the phase velocity of the DAW. Thus electron acceleration is via Landau damping of DAWs. For the Alfvén speeds of 0.3c the considered mechanism can accelerate electrons to energies circa 20 keV. (v) The increase of mass ratio from m_i/m_e=16 to 73.44 increases the fraction of accelerated electrons from 20% to 3035% (depending on DAW polarisation). For the mass ratio m_i/m_e=1836 the fraction of accelerated electrons would be >35%.
Authors: David Tsiklauri
Projects: None

Publication Status: Phys. Plasmas 18, 092903 (2011)
Last Modified: 20110926 07:36



An alternative to the plasma emission model: ParticleInCell, selfconsistent electromagnetic wave emission simulations of solar type III radio bursts 

David Tsiklauri Submitted: 20101126 11:09
1.5D PIC, relativistic, fully electromagnetic (EM) simulations are used tomodel EM wave emission generation in the context of solar type III radiobursts. The model studies generation of EM waves by a superthermal, hot beamof electrons injected into a plasma thread that contains uniform longitudinalmagnetic field and a parabolic density gradient. In effect, a single magneticline connecting Sun to earth is considered, for which several cases arestudied. (i) We find that the physical system without a beam is stable and onlylow amplitude level EM drift waves (noise) are excited. (ii) The beam injectiondirection is controlled by setting either longitudinal or oblique electroninitial drift speed, i.e. by setting the beam pitch angle. In the case of zeropitch angle, the beam excites only electrostatic, standing waves, oscillatingat plasma frequency, in the beam injection spatial location, and only low levelEM drift wave noise is also generated. (iii) In the case of oblique beam pitchangles, again electrostatic waves with same properties are excited. However,now the beam also generates EM waves with the properties commensurate to typeIII radio bursts. The latter is evidenced by the wavelet analysis of transverseelectric field component, which shows that as the beam moves to the regions oflower density, frequency of the EM waves drops accordingly. (iv) When thedensity gradient is removed, electron beam with an oblique pitch angle stillgenerates the EM radiation. However, in the latter case no frequency decreaseis seen. Within the limitations of the model, the study presents the firstattempt to produce simulated dynamical spectrum of type III radio bursts infully kinetic plasma model. The latter is based on 1.5D nonzero pitch angle(nongyrotropic) electron beam, that is an alternative to the plasma emissionclassical mechanism.
Authors: David Tsiklauri
Projects: None

Publication Status: Physics of Plasmas 18, 052903 (2011)
Last Modified: 20110707 04:47



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Abstracts by Author

 Electron plasma wake field acceleration in solar coronal and chromospheric plasmas 
 Collisionless, phasemixed, dispersive, Gaussian Alfven pulse in transversely inhomogeneous plasma 
 The effect of longitudinal density gradient on electron plasma wake field acceleration 
 Particleincell simulations of the relaxation of electron beams in inhomogeneous solar wind plasmas 
 Role of electron inertia and reconnection dynamics in a stressed Xpoint collapse with a guidefield 
 Selfconsistent particleincell simulations of fundamental and harmonic plasma radio emission mechanisms 
 Alfven wave phase mixing in flows  why overdense solar coronal open magnetic field structures are cool? 
 The effects of ion mass variation and domain size on octupolar outofplane magnetic field generation in collisionless magnetic reconnection 
 Octupolar outofplane magnetic field structure generation during collisionless magnetic reconnection in a stressed Xpoint collapse 
 The effect of guidefield and boundary conditions on collisionless magnetic reconnection in a stressed Xpoint collapse 
 3D particleincell simulation of electron acceleration by Langmuir waves in an inhomogeneous plasma 
 Whistler wave generation by nongyrotropic, relativistic, electron beams 
 3D MHD simulation of linearly polarised Alfven wave dynamics in ArnoldBeltramiChildress magnetic field 
 The effect of initial conditions on the electromagnetic radiation generation in type III solar radio bursts 
 The effect of initial conditions on the electromagnetic radiation generation in type III solar radio bursts 
 Three dimensional particleincell simulation of particle acceleration by circularly polarised inertial Alfven waves in a transversely inhomogeneous plasma 
 Particle acceleration by circularly and elliptically polarised dispersive Alfven waves in a transversely inhomogeneous plasma in the inertial and kinetic regimes 
 Heating of solar chromosphere by electromagnetic wave absorption in a plasma slab model 
 Heating of solar chromosphere by electromagnetic wave absorption in a plasma slab model 
 An alternative to the plasma emission model: ParticleInCell, selfconsistent electromagnetic wave emission simulations of solar type III radio bursts 
 An alternative to the plasma emission model: Particleincell, selfconsistent electromagnetic wave emission simulations of solar type III radio bursts 
 Missing bits of the solar jigsaw puzzle: smallscale, kinetic effects in coronal studies 
 Physics of collisionless reconnection in a stressed Xpoint collapse 
 Physics of collisionless phase mixing 
 A new fast reconnection model in a collisionless regime 
 Physics of collisionless reconnection in a stressed Xpoint collapse 
 Magnetic reconnection during collionless, stressed, Xpoint collapse using ParticleinCell simulation 
 A minimal model of parallel electric field generation in a transversely inhomogeneous plasma 
 A fresh look at the heating mechanisms of the solar corona 
 Phase mixing of shear Alfvén waves as a new mechanism for electron acceleration in collisionless, kinetic plasmas 
 The Sun as a MHD generator: application of a new heating mechanism for the coronal loops and closed magnetic structures 
 ParticleInCell simulations of circularly polarised Alfven wave phase mixing: a new mechanism for electron acceleration in collisionless plasmas 
 Phase mixing of a three dimensional magnetohydrodynamic pulse 
 Phase mixing of a three dimensional magnetohydrodynamic pulse 
 A Three Dimensional Magnetohydrodynamic Pulse in a Transversely Inhomogeneous Medium 
 Lineofsight Effects on Observability of Kink and Sausage Modes in Coronal Structures with Imaging Telescopes 
 A Weakly Nonlinear Alfv'enic Pulse in a Transversely InhomogeneousMedium 
 WideSpectrum Slow Magnetoacoustic Waves in Coronal Loops 


