Monte Carlo Simulation of O<sup>+</sup>Behavior in the Auroral Ionosphere

Barghouthi, I. A.; Elias, Elias I.; Samra, Mahmoud Abu; Qatanani, Naji; Issa, Mazen S.

doi:10.1143/jpsj.72.3006

Cited by 3 publications

(5 citation statements)

References 24 publications

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“…The relative velocity, g , increases, and this decreases the role of O + –O polarization interactions (∝ g −1 ) which act to isotropize the O + velocity distribution function by transferring some of the energy from the field‐perpendicular to the field‐parallel direction. The role of O + –O + Coulomb self‐collisions also becomes less important because the collision frequency is temperature dependent [ Barghouthi et al , 2003a]. However, as altitude increases (i.e., the relative concentration of O + ions increases) the influence of O + –O + Coulomb self‐collision becomes dominant and is very effective in transferring energy from field‐perpendicular direction to the field‐parallel direction (i.e., it works to decrease the non‐Maxwellian features).…”

Section: O+ Ion Temperature Partition Coefficients β∥ and β⊥mentioning

confidence: 99%

“…[7] In a series of studies, Barghouthi et al [1991Barghouthi et al [ , 1994Barghouthi et al [ , 2003a…”

Section: Monte Carlo Modelmentioning

confidence: 99%

“…In a series of studies, Barghouthi et al [1991, 1994, 2003a] used Monte Carlo simulation to investigate the behavior of auroral O + ions that are E × B drifting through a background of neutrals O, with the effects of O + –O collisions (resonant charge exchange and polarization interaction) and O + –O + Coulomb self‐collisions included. Briefly, they considered 1000 O + ions, each of which is followed for a short period of time Δt (1% of the mean free time).…”

Section: Monte Carlo Modelmentioning

confidence: 99%

“…They found that Coulomb collisions act to Maxwellize (thermalize) the O + velocity distribution function. Barghouthi et al [1991, 1994, 2003a] used a Monte Carlo simulation to study the effect of O + –O + Coulomb self‐collisions on the O + behavior in the high‐latitude F region. Barghouthi et al [1994] used a realistic collision model (resonant charge exchange, polarization interaction, and O + –O + Coulomb self‐collisions) and compared their Monte Carlo results with the results of Tereshchenko et al [1991] and Kinzelin and Hubert [1992] to assess the effect of simplified collision models on the results.…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

O⁺ ion temperature partition coefficients β_∥ and β_⊥: The Effect of O⁺–O⁺ Coulomb self‐collisions

Barghouthi

2005

J. Geophys. Res.

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Section: O+ Ion Temperature Partition Coefficients β∥ and β⊥mentioning

confidence: 99%

“…[7] In a series of studies, Barghouthi et al [1991Barghouthi et al [ , 1994Barghouthi et al [ , 2003a…”

Section: Monte Carlo Modelmentioning

confidence: 99%

Section: Monte Carlo Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

O⁺ ion temperature partition coefficients β_∥ and β_⊥: The Effect of O⁺–O⁺ Coulomb self‐collisions

Barghouthi

2005

J. Geophys. Res.

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“…Effects of WPI were mainly studied for plasma flows along auroral field lines or along closed field lines (L = 4) (Ganguli et al, 1988). But WPI have also to be included in polar wind models like it was initiated by Barakat and Barghouthi (1994a) for O + ions and followed by several Monte carlo studies (Barakat and Barghouthi, 1994b;Barghouthi, 1997;Barghouthi et al, 1998;and Barghouthi et al, 2003). In their Monte Carlo simulations, Coulomb collisions were neglected since they assumed to be at high altitudes (i.e.…”

Section: Introductionmentioning

confidence: 99%

Effects of Wave-Particle Interactions on Double-Hump Distributions of the H + Polar Wind

Pierrard

Barghouthi²

2006

Astrophys Space Sci

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A Monte Carlo simulation is used in order to study the effects of wave-particle interactions (WPI) on H + distributions in the polar wind outflow. The simulation also considers effects of the gravity, the polarization electric field, the divergence of geomagnetic field lines and H + −O + Coulomb collisions. The proton velocity distribution function (VDF) and the profiles of its moments (density, bulk velocity, parallel and perpendicular temperatures, heat flux. . .) are found for different levels of WPI, i.e., for different values of the normalized diffusion rate in the velocity space (D ⊥ ). We find that the wave-particle interactions accelerate the polar wind and can have important effects on the double-hump H + distribution obtained in the transition region between the collision-dominated low altitudes and the collisionless high altitude regions.

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Hypergeometric function representation of transport coefficients for drifting bi-Maxwellian plasmas

Jubeh

Barghouthi

2017

Physics of Plasmas

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We derive the momentum, parallel energy, and perpendicular energy collisional transport coefficients for drifting bi-Maxwellian plasmas by using the Boltzmann collision integral approach and present them in the form of triple hypergeometric functions. In the derivation, we write the drift velocity u of the bi-Maxwellian plasma in terms of parallel and perpendicular components (i.e., u = u‖ + u⊥), parallel and perpendicular with respect to the ambient magnetic field, and we consider the Coulomb collision interactions. We consider two special cases: first, when the drift velocity is parallel to the ambient magnetic field (i.e., u = u‖), and second, when the drift velocity is perpendicular to the ambient magnetic field (i.e., u = u⊥). For the first case, the transport equations and consequently the transport coefficients are derived and presented in the form of double hypergeometric functions; these results are consistent with the findings of Hellinger and Trávníček [Phys. Plasmas 16(5), 054501 (2009)]. For the second case, the transport coefficients are obtained and found to be in the form of double hypergeometric functions. When we combine these two special cases, i.e., for general u, the transport coefficients are shown to be in the form of triple hypergeometric functions. Also, we investigate the above problem by using another approach, i.e., Fokker Planck approximation. We obtain similar results for both approaches.

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Monte Carlo Simulation of O⁺Behavior in the Auroral Ionosphere

Cited by 3 publications

References 24 publications

O⁺ ion temperature partition coefficients β_∥ and β_⊥: The Effect of O⁺–O⁺ Coulomb self‐collisions

O⁺ ion temperature partition coefficients β_∥ and β_⊥: The Effect of O⁺–O⁺ Coulomb self‐collisions

Effects of Wave-Particle Interactions on Double-Hump Distributions of the H + Polar Wind

Hypergeometric function representation of transport coefficients for drifting bi-Maxwellian plasmas

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Monte Carlo Simulation of O+Behavior in the Auroral Ionosphere

Cited by 3 publications

References 24 publications

O+ ion temperature partition coefficients β∥ and β⊥: The Effect of O+–O+ Coulomb self‐collisions

O+ ion temperature partition coefficients β∥ and β⊥: The Effect of O+–O+ Coulomb self‐collisions

Effects of Wave-Particle Interactions on Double-Hump Distributions of the H + Polar Wind

Hypergeometric function representation of transport coefficients for drifting bi-Maxwellian plasmas

Contact Info

Product

Resources

About

Monte Carlo Simulation of O⁺Behavior in the Auroral Ionosphere

O⁺ ion temperature partition coefficients β_∥ and β_⊥: The Effect of O⁺–O⁺ Coulomb self‐collisions

O⁺ ion temperature partition coefficients β_∥ and β_⊥: The Effect of O⁺–O⁺ Coulomb self‐collisions