Measurement of plasma wave electric fields in solar flares

Davis, William D.

doi:10.1007/bf00146430

Cited by 23 publications

(9 citation statements)

References 12 publications

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“…Even more intensive electric fields (up to 700 V/cm) were measured by Davis. 25 Moreover, Foukal et al, 26 while analyzing two eruptive events, have found that the total electric field in such structures is less than 10 V/cm and about 40 V/cm in a post-flare loop.…”

Section: A Torsional Spine Reconnectionmentioning

confidence: 98%

Comparison of test particle acceleration in torsional spine and fan reconnection regimes

2014

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Magnetic reconnection is a common phenomenon taking place in astrophysical and space plasmas, especially in solar flares which are rich sources of highly energetic particles. Torsional spine and fan reconnections are important mechanisms proposed for steady-state three-dimensional nullpoint reconnection. By using the magnetic and electric fields for these regimes, we numerically investigate the features of test particle acceleration in both regimes with input parameters for the solar corona. By comparison, torsional spine reconnection is found to be more efficient than torsional fan reconnection in an acceleration of a proton to a high kinetic energy. A proton can gain as high as 100 MeV of relativistic kinetic energy within only a few milliseconds. Moreover, in torsional spine reconnection, an accelerated particle can escape either along the spine axis or on the fan plane depending on its injection position. However, in torsional fan reconnection, the particle is only allowed to accelerate along the spine axis. In addition, in both regimes, the particle's trajectory and final kinetic energy depend on the injection position but adopting either spatially uniform or non-uniform localized plasma resistivity does not much influence the features of trajectory. V C 2014 AIP Publishing LLC. [http://dx.

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Section: A Torsional Spine Reconnectionmentioning

confidence: 98%

Comparison of test particle acceleration in torsional spine and fan reconnection regimes

2014

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“…A formula for the "mean particle field" given by Griem (Griem 1974, p. 22) had been used by ourselves and by some other authors in this context (e.g., Jordan et al 1980, Davis 1977. This formula was found to lead to a field intensity estimate about 3.5 times as high, for a given observed broadening, as the .…”

Section: *"mentioning

confidence: 94%

Measurement of Macroscopic Electric Fields in Solar Plasma Structures

Foukal¹

1987

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Ba. NAME OF FUNDING I SPONSORING & b. OFFICE SYMBOL 9. PROCUREMENT INSTRUMENT IDENTIFICATION NUMBER ORGANIZATIOIN P (f appkabl.) ESD F 19628-87-C-0110 9C. ADDRESS (City, State, and ZAP Code) 10. SOURCE OF FUNDIN4G NUMBERS EEETN.N.No. CCESSION NO I1I TITLE (include Security Claication) Measurement of Macroscopic Electric Fields in Solar Plasma Structures 12 PERSONAL AUTHOR(S) P. Foukal 13a. TYPE OF REPORT 13b. TIME COVERED 14. DATE OF REPORT (YaW, Month, Day) S. PAGE COUNT FINA FROM 5 /27/87 TDll 2718 87/12/14 32 16 SUPPLEMENTARY NOTATION '7 COSATI CODES 1S. SUBJECT TERMS (Conwiu on juvmnh Nf necenary and Id*Ftfy by Niock numbw) FIELD GROUP SUBGROUP Electric Fields, Solar Flares 19 ABSTRACT (Candiwj. an raw,'. if necamty and kdfytI~ by block number) 20 DISTRIBUTION /AVAILAILITY OF ABSTRACT 21. ABSTRACT SECURITY CLASSIFICATION% OUNCLASSIFIED01UNUMITED 0 SAME AS RT. OTIC USERS Unclassified 22a NAME OF RESPONSIBLE INDIVIDUAL 22b TELEPHONE Onicudf AreaCo010) 22c. OFFICE SYMBOL DO FORM 1473.84MAR 93 APtedt nay be used 7:1 .h,.asted SECURITY CLASSIFICATION Of THIS PACE All othM editonS are obsoleftẽ

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“…Wien (1916) is the first author who pointed out the possibility of measuring electric field of solar plasma and measured the motional electric field using Stark effect. Around 1980s, some attempts to measure the electric field with helium and silicon spectra had been made, which suggested an electric field of 700 V/cm (Davis 1977) and 300 V/cm (Jordan et al 1980) respectively. Even so, Moran & Foukal (1991) pointed out that direct measurement of the electric field by Stark effect is hard to operate with the low sensitivity.…”

Section: Introductionmentioning

confidence: 99%

The induced electric field distribution in the solar atmosphere

Chen¹,

Yang²,

Deng³

2013

Res. Astron. Astrophys.

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A method of calculating induced electric field is presented in this paper. Induced electric field in solar atmosphere is derived by the time variation of magnetic field when the charged particle accumulation is neglected. In order to get the spatial distribution of magnetic field, several extrapolation methods are introduced. With observational data from Helioseismic and Magnetic Imager (HMI) aboard the NASA's Solar Dynamics Observatory (SDO) on May 20th, 2010, we extrapolate the magnetic field to the upper atmosphere from the photosphere. By calculating the time variation of magnetic field, we can get the induced electric field. The derived induced electric field can reach a value of 10 2 V/cm and the average electric field has a maximum point at the layer of 360 km above the photosphere. The Monte Carlo statistics method is used to compute the triple integration of induced electric field.

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Measurement of plasma wave electric fields in solar flares

Cited by 23 publications

References 12 publications

Comparison of test particle acceleration in torsional spine and fan reconnection regimes

Comparison of test particle acceleration in torsional spine and fan reconnection regimes

Measurement of Macroscopic Electric Fields in Solar Plasma Structures

The induced electric field distribution in the solar atmosphere

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