Anomalous Transport in Current Sheets

Huba, J. D.

doi:10.1007/978-94-009-6520-1_33

Cited by 18 publications

(9 citation statements)

References 30 publications

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“…The FP82 model merely predicts a proportion between electric field and inflow speed as a cause-effect relationship; i.e., whether the reconnection drives the inflow or vice versa remains unknown. In a theory developed for radio pulsations (Kliem et al 2000), however, the RCS area can, at least, be involved in a self-organized evolution, in such a way that increase of current density and thus anomalous resistivity (Huba 1985) makes the RCS area expand, leading in turn to a decrease in current density. A series of such self-organized cycles would, in this view, produce the multiple peaks in X-ray/microwave light curves as observed.…”

Section: Discussionmentioning

confidence: 99%

Magnetic Energy Release during the 2002 September 9 Solar Flare

Lee

Gary

Choe

2006

ApJ

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We study the magnetic energy release during the 2002 September 9 flare using the high-cadence (40 ms) H filtergram at Big Bear Solar Observatory (BBSO), along with hard X-ray and microwave data from the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI ) and the Owens Valley Solar Array (OVSA), respectively. We take the Poynting vector approach with the standard two-dimensional geometry of the reconnecting current sheet (RCS) but suggest a new technique to infer the area of the RCS, in order to complete the magnetic energy calculation entirely with observed quantities. We found five peaks of impulsive magnetic energy release, concentrated within 10-30 s periods, that are episodic with the peaks of the hard X-ray light curve. The maximum amount of energy released per peak reaches $2:6 ; 10 30 ergs s À1 , and the electron energy deposition rate derived from the RHESSI spectra falls into the range of 10%-80% of the magnetic energy release rate. We briefly discuss this result in comparison with other studies thus far made toward understanding of the magnetic reconnection in solar flares and suggest the pulsating current sheet model as the most plausible interpretation of our result.

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Section: Discussionmentioning

confidence: 99%

Magnetic Energy Release during the 2002 September 9 Solar Flare

Lee

Gary

Choe

2006

ApJ

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“…The critical current density was heuristically chosen as j c = 0.1 while the coefficient is chosen to be η 2 = 0.05. The formation of localized nonideal regions in dependence on the electric current is motivated by the concept of anomalous resistivity due to microturbulence where momentum transfer between the charged species is caused by turbulent electromagnetic fields (e.g., Huba 1985;Benz 1993).…”

Section: Numerical Modelmentioning

confidence: 99%

Plasma-neutral gas simulations of reconnection events in cometary tails

Konz

Birk²,

Lesch³

2004

A&A

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Abstract. The formation and dynamical evolution of cometary plasma tails and magnetic boundary layers is studied by the first numerical plasma-neutral gas simulations. It is shown that collisional interaction between the cometary neutral envelope and the solar wind plasma leads to the formation of a magnetic barrier that separates the entire cometary body from the solar wind. The overall dynamics, in particular, of the magnetotail are governed by magnetic reconnection. Multiple reconnection events are initiated by the localized excitation of anomalous resistivity modeled by η( j). If the comet encounters a heliospheric current sheet, strong disconnection events characterize the cometary plasma tail. But even in the case of homogeneous solar wind conditions, partial disruption of the tail is triggered by dayside reconnection.

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“…Two resistivity models were used' a constant resistivity (r/= %) and a current-dependent resistivity, r/•c max (0, IJI-Jo) 2. The latter resistivity model' has been used extensively to mimic the effect of anomalous resistivity due to plasma instabilities [Papadopoulos, 1980;Huba, 1985].…”

Section: Resultsmentioning

confidence: 99%

“…The actual mechanics of the reconnection process is a topic of active research especially in light of the neutral line model for substorms [Hones, 1973;McPherron et al, 1973]. There has been a great deal of theoretical work done on the stability of taillike magnetic configurations [e.g., Schindler, 1974;Galeev et al, 1978;Coroniti, 1985] and on the possible causes of the needed dissipation (e.g., anomalous resistivity) [Huba, 1985;Papadopoulos, 1980]. Even without detailed knowledge of the physics of the reconnection diffusion region, simulation studies have focused on the nonlinear behavior of fully developed reconnection.…”

Section: Introductionmentioning

confidence: 99%

The effect of different resistivity models on magnetotail dynamics

Lyon

Fedder²,

Huba

1986

J. Geophys. Res.

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Two-dimensional, time-dependent MHD simulations of the interaction between the solar wind and the earth's magnetosphere have been performed to study magnetotail dynamics with varying forms of anomalous resistivity. In general, the resulting models conform to the neutral line model proposed for substorms with near-earth x points and high-speed tailward flows occurring in the magnetotail. However, in the case where Joule heating is included in the physical description of the system, the near-earth x point never moves far down tail, and high-speed tailward flows never stop. Only in the case where there is no Joule heating does the x point move down tail. Simultaneously, the high-speed tailward flows cease. These results indicate that the mechanism of energy dissipation can have an important effect on reconnection processes and the global magnetospheric dynamics.

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Anomalous Transport in Current Sheets

Cited by 18 publications

References 30 publications

Magnetic Energy Release during the 2002 September 9 Solar Flare

Magnetic Energy Release during the 2002 September 9 Solar Flare

Plasma-neutral gas simulations of reconnection events in cometary tails

The effect of different resistivity models on magnetotail dynamics

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