Parallel 3-D Electromagnetic Particle Code Using High Performance FORTRAN: Parallel TRISTAN

Cai, Dongsheng; Li, Yaoting; Nishikawa, Ken‐Ichi; Xiao, Chijie; Yan, Xiaoyang; Pu, Z.

doi:10.1007/3-540-36530-3_2

Cited by 14 publications

(19 citation statements)

References 7 publications

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“…To minimize the possible undesired influence of boundaries on the plasma dynamics, we try to keep the edges of the simulation domain as far as possible from the localized plasma element. A detailed description of the PIC-3D code and the boundary conditions used in our simulations can be found in Voitcu (2014); for details about the original TRISTAN code see Buneman (1993) and Cai et al (2003). …”

Section: Simulation Setupmentioning

confidence: 99%

Transport and entry of plasma clouds/jets across transverse magnetic discontinuities: Three‐dimensional electromagnetic particle‐in‐cell simulations

Voitcu

Echim

2016

JGR Space Physics

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In this paper we use three‐dimensional electromagnetic particle‐in‐cell simulations to investigate the interaction of a small Larmor radius plasma cloud/jet with a transverse nonuniform magnetic field typical to a tangential discontinuity in a parallel geometry. The simulation setup corresponds to an idealized, yet relevant, magnetospheric configuration likely to be observed at the magnetopause during northward orientation of the interplanetary magnetic field. The numerical simulations are adapted to study the kinetic effects and their role on the transport and entry of localized plasma jets similar to those identified inside the Earth's magnetosheath propagating toward the magnetopause. The simulations reveal the formation of a perpendicular polarization electric field inside the main bulk of the plasma cloud that enables its forward transport and entry across the transverse magnetic field. The jet is able to penetrate the transition region when the height of the magnetic barrier does not exceed a certain critical threshold. Otherwise, the forward transport along the injection direction is stopped before full penetration of the magnetopause. Moreover, the jet is pushed back and simultaneously deflected in the perpendicular plane to the magnetic field. Our simulations evidence physical processes advocated previously by the theoretical model of impulsive penetration and revealed in laboratory experiments.

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Section: Simulation Setupmentioning

confidence: 99%

Transport and entry of plasma clouds/jets across transverse magnetic discontinuities: Three‐dimensional electromagnetic particle‐in‐cell simulations

Voitcu

Echim

2016

JGR Space Physics

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“…Plasma instabilities can be efficiently reduced with the strong condition on the plasma frequency ω p .Δt ≤ 0.25 (Tskhakaya et al 2007). In addition, to avoid the classical problems of grid heating and instabilities, we ensured that the Debey length did not reach values below a critical size defined by λ D ≥ Δr π (Cai et al 2003;Tskhakaya et al 2007). To enforce the shielding effect of charges on the Debye volume, we assumed an initial particle density of five pairs per simulation cell (Reimann & Fajans 2002).…”

Section: Pic Simulation Of Magnetosphere and Comparison With Observatmentioning

confidence: 99%

HubbleSpace Telescope detection of oxygen in the atmosphere of exoplanet HD 189733b

Ben‐Jaffel

Ballester

2013

A&A

110

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Detecting heavy atoms in the inflated atmospheres of giant exoplanets that orbit close to their parent stars is a key factor for understanding their bulk composition, their evolution, and the processes that drive their expansion and interaction with the impinging stellar wind. Unfortunately, very few detections have been made thus far. Here, we use archive data obtained with the Cosmic Origins Spectrograph onboard the Hubble Space Telescope to report an absorption of ∼6.4%±1.8% by neutral oxygen during the HD 189733b transit. Using published results from a simple hydrodynamic model of HD 189733b, and assuming a mean temperature of ∼(8−12) × 10 3 K for the upper atmosphere of the exoplanet, a mean vertical integrated O I density column of ∼8 × 10 15 cm −2 produces only a 3.5% attenuation transit. Much like the case of the hot-Jupiter HD 209458b, super-solar abundances and/or super-thermal broadening of the absorption lines are required to fit the deep transit drop-off observed in most far-ultraviolet lines. We also report evidence of short-time variability in the measured stellar flux, a variability that we analyze using time series derived from the time-tagged exposures, which we then compare to solar flaring activity. In that frame, we find that non-statistical uncertainties in the measured fluxes are not negligible, which calls for caution when reporting transit absorptions. Despite cumulative uncertainties that originate from variability in the stellar and sky background signals and in the instrument response, we also show a possible detection for both a transit and early-ingress absorption in the ion C II 133.5 nm lines. If confirmed, this would be the second exoplanet for which an early ingress absorption is reported. In contrast, such an early ingress signature is not detected for neutral O I. Assuming the HD 189733b magnetosphere to be at the origin of the early absorption, we use the Parker model for the stellar wind and a particle-in-cell code for the magnetosphere to show that its orientation should be deflected ∼10−30• from the planet-star line, while its nose's position should be at least ∼16.7 R p upstream of the exoplanet in order to fit the C II transit light curve. The derived stand-off distance is consistent with a surface magnetic field strength of ∼5.3 Gauss for the exoplanet, and a supersonic stellar wind impinging at ∼250 km s −1 , with a temperature of 1.2 × 10 5 K and a density ∼6.3 × 10 6 cm −3 at the planetary orbit, yet the fit is not unique.

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“…[43] Our simulation code is an updated version, in terms of numerical stability and computer CPU (resource usage), of an existing PIC EM particle code that has been used in the past to simulate the macrostructure of the Earth's magnetosphere [Buneman, 1993;Nishikawa et al, 1995;Wodnicka, 2001]. However, in terms of boundary conditions, charge conservation, grid cells, and number of particles per cell, our code's version is similar to the one used by Buneman [1993], Buneman et al [1995], Villasenor and Buneman [1992], Nishikawa [1997], Nishikawa [1998], Nishikawa et al [1995], Nishikawa and Ohtani [2000], and Cai et al [2003]. Recent work by Cai et al [2006] improved the statistics of the code by using a higher density of particles per cell and a better resolution for the field description (0.5 R e scale compared to 1 R e in our case).…”

Section: Discussionmentioning

confidence: 99%

Sensitivity of the Earth’s magnetosphere to solar wind activity: Three‐dimensional macroparticle model

Baraka

Ben‐Jaffel

2007

J. Geophys. Res.

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[1] A new approach is proposed to study the sensitivity of the Earth's magnetosphere to the variability of the solar wind bulk velocity. The study was carried out using a three-dimensional electromagnetic particle-in-cell code, with the microphysics interaction processes described by Maxwell and Lorentz equations, respectively, for the fields and particles. Starting with a solar wind with zero interplanetary magnetic field (IMF) impinging upon a magnetized Earth, the formation of the magnetospheric cavity and its elongation around the planet were modeled over time until a steady state structure of a magnetosphere was attained. The IMF was then added as a steady southward magnetic field. An impulsive disturbance was applied to the system by changing the bulk velocity of the solar wind to simulate a decrease in the solar wind dynamic pressure, followed by its recovery, for both zero and southward IMF. In response to an imposed drop in the solar wind drift velocity, a gap (air pocket) in the incoming solar wind plasma appeared moving toward Earth. The orientation of the cusps was highly affected by the depression of the solar wind for all orientation of IMF. The magnetotail lobes flared out with zero IMF due to the ''air pocket'' effect. With the nonzero IMF, as soon as the gap hit the initial shock of the steady magnetosphere, a reconnection between the Earth's magnetic field and the IMF was noticed at the dayside magnetopause. During the expansion phase of the system, the outer boundary of the dayside magnetopause broke up in the absence of the IMF, yet it sustained its bullet shape when a southward IMF was included. The expansion/ contraction of the magnetopause nose is almost linear in the absence of the IMF but evolves nonlinearly with a southward IMF. The system recovered its initial state on the dayside soon after the impulsive disturbance was beyond Earth for both cases of zero and nonzero IMF. Comparison with existing observations from Cluster and Interball-1 seems to confirm many of our simulation results.Citation: Baraka, S., and L. Ben-Jaffel (2007), Sensitivity of the Earth's magnetosphere to solar wind activity: Three-dimensional macroparticle model,

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Parallel 3-D Electromagnetic Particle Code Using High Performance FORTRAN: Parallel TRISTAN

Cited by 14 publications

References 7 publications

Transport and entry of plasma clouds/jets across transverse magnetic discontinuities: Three‐dimensional electromagnetic particle‐in‐cell simulations

Transport and entry of plasma clouds/jets across transverse magnetic discontinuities: Three‐dimensional electromagnetic particle‐in‐cell simulations

HubbleSpace Telescope detection of oxygen in the atmosphere of exoplanet HD 189733b

Sensitivity of the Earth’s magnetosphere to solar wind activity: Three‐dimensional macroparticle model

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