TY - JOUR
T1 - A possible structure of the magnetic field in solar filaments obtained by flux emergence
AU - Magara, Tetsuya
PY - 2007
Y1 - 2007
N2 - We report a result, that the emergence of a subsurface magnetic field naturally reproduces the feature of the global magnetic configuration observed in solar filaments. This was obtained by performing a three-dimensional simulation of a twisted flux tube that emerges in the shape of a multi-Ω-loop in a highly stratified solar atmosphere, extending from the subsurface layer to the corona. One of the key findings is that a kinking of the twisted flux tube occurs at the site of a linkage between adjacent Ω-loops. This develops a magnetic structure mat has remarkable similarities to the structure of a filament, in that the inner part of the twisted flux tube can be applied to the main body of a filament, while the outer part is reminiscent of observations of filament feet and a coronal arcade overlying the main body of a filament. Based on the result, we concluded that the orientation of filaments observed on the Sun may have its origin in the handedness of a twisted magnetic field below the solar surface.
AB - We report a result, that the emergence of a subsurface magnetic field naturally reproduces the feature of the global magnetic configuration observed in solar filaments. This was obtained by performing a three-dimensional simulation of a twisted flux tube that emerges in the shape of a multi-Ω-loop in a highly stratified solar atmosphere, extending from the subsurface layer to the corona. One of the key findings is that a kinking of the twisted flux tube occurs at the site of a linkage between adjacent Ω-loops. This develops a magnetic structure mat has remarkable similarities to the structure of a filament, in that the inner part of the twisted flux tube can be applied to the main body of a filament, while the outer part is reminiscent of observations of filament feet and a coronal arcade overlying the main body of a filament. Based on the result, we concluded that the orientation of filaments observed on the Sun may have its origin in the handedness of a twisted magnetic field below the solar surface.
KW - Magnetohydrodynamics: MHD
KW - Methods: numerical
KW - Sun: filaments
KW - Sun: magnetic fields
UR - http://www.scopus.com/inward/record.url?scp=39149135264&partnerID=8YFLogxK
U2 - 10.1093/pasj/59.6.L51
DO - 10.1093/pasj/59.6.L51
M3 - Article
AN - SCOPUS:39149135264
SN - 0004-6264
VL - 59
SP - L51-L55
JO - Publication of the Astronomical Society of Japan
JF - Publication of the Astronomical Society of Japan
IS - 6
ER -