Modeling a Coronal Loop Heated by Magnetohydrodynamic Turbulence Nanoflares | Zendy

F. Reale | Zendy; Giuseppiigro | Zendy; F. Malara | Zendy; G. Pérès | Zendy; P. Veltri | Zendy

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Modeling a Coronal Loop Heated by Magnetohydrodynamic Turbulence Nanoflares

Author(s) -

F. Reale,

Giuseppiigro,

F. Malara,

G. Pérès,

P. Veltri

Publication year - 2005

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/444409

Subject(s) - nanoflares , physics , coronal loop , magnetohydrodynamic drive , dissipative system , dissipation , magnetohydrodynamics , magnetohydrodynamic turbulence , plasma , corona (planetary geology) , loop (graph theory) , turbulence , magnetic field , mechanics , astrophysics , magnetic reconnection , computational physics , thermodynamics , solar wind , coronal mass ejection , nuclear physics , mathematics , combinatorics , quantum mechanics , astrobiology , venus

We model the hydrodynamic evolution of the plasma confined in a coronal loop, 30,000 km long, subject to the heating of nanoflares due to intermittent magnetic dissipative events in the MHD turbulence produced by loop footpoint motions. We use the time-dependent distribution of energy dissipation along the loop obtained from a hybrid shell model, occurring for a magnetic field of about 10 G in the corona; the relevant heating per unit volume along the loop is used in the Palermo-Harvard loop plasma hydrodynamic model. We describe the results, focusing on the effects produced by the most intense heat pulses, which lead to loop temperatures between 1 and 1.5 MK

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