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Abstract
Aims. We compute the distribution of the magnetic field and the plasma in the global corona with a selfconsistent magnetohydrostatic (MHS) model.
Methods. Because direct measurements of the solar coronal magnetic field and plasma are extremely difficult and inaccurate, we use a modeling approach based on observational quantities, e. g. the measured photospheric magnetic field, to reconstruct the structure of the global solar corona. We take an analytic magnetohydrostatic model to extrapolate the magnetic field in the corona from photospheric magnetic field measurement. In the model, the electric current density can be decomposed into two components: one component is aligned with the magnetic field lines, whereas the other component flows in spherical shells. The second component of the current produces finite Lorentz forces that are balanced by the pressure gradient and the gravity force. We derive the 3D distribution of the magnetic field and plasma selfconsistently in one model. The boundary conditions are given by a synoptic magnetogram on the inner boundary and by a source surface model at the outer boundary.
Results. The density in the model is higher in the equatorial plane than in the polar region. We compare the magnetic field distribution of our model with potential and forcefree field models for the same boundary conditions and find that our model differs noticeably from both. We discuss how to apply the model and how to improve it.
Original language  English 

Pages (fromto)  827834 
Number of pages  8 
Journal  Astronomy & Astrophysics 
Volume  481 
DOIs  
Publication status  Published  Apr 2008 
Keywords
 Sun : corona
 Sun : magnetic fields
 magnetohydrodynamics (MHD)
 FREE MAGNETICFIELD
 ELECTRICCURRENT SYSTEMS
 GREENSFUNCTION METHOD
 MAGNETOSTATIC ATMOSPHERES
 3DIMENSIONAL STRUCTURES
 OPTIMIZATION APPROACH
 SPHERICAL GEOMETRY
 TRIPLE STRUCTURES
 HELMET STREAMERS
 CONSTANTALPHA
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Dive into the research topics of 'A first step in reconstructing the solar corona selfconsistently with a magnetohydrostatic model during solar activity minimum'. Together they form a unique fingerprint.Projects
 2 Finished


Solar&Magnetospheric Plasma Theory PP/E1: Solar and Magnetospheric Plasma Theory
Neukirch, T., Hood, A. W., Parnell, C. E., Priest, E., Roberts, B. & Wright, A. N.
1/04/07 → 31/03/12
Project: Standard