scholarly journals Some Remarks on the Statics and Dynamics of Magnetic Field Structure Development in Active Regions

1971 ◽  
Vol 43 ◽  
pp. 201-211
Author(s):  
V. Bumba ◽  
J. Suda
Keyword(s):  
Magnetic Field ◽  
High Resolution ◽  
Active Regions ◽  
Field Structure ◽  
Structure Development ◽  
Magnetic Field Structure ◽  
Statics And Dynamics ◽  
Fine Structures

Some comments are given concerning the fine structures in the umbra and penumbra of sunspots and their changes on the basis of high resolution photographs.

A Discussion on the physics of the solar atmosphere - Physics of the solar atmosphere

1976 ◽  
Vol 281 (1304) ◽  
pp. 415-426
Keyword(s):  
Magnetic Field ◽  
Transition Region ◽  
Solar Atmosphere ◽  
Solar Rotation ◽  
Active Regions ◽  
Rotation Velocity ◽  
Coronal Magnetic Field ◽  
Velocity Fields ◽  
Field Structure ◽  
Magnetic Field Structure

A summary is given on recent results on the physics of the quiet solar atmosphere, and active regions. This includes: solar rotation, velocity fields and waves, magnetic field concentration, the transition region, coronal magnetic field structure, and prominences.

scholarly journals Tracing the physical conditions of planet formation with molecular excitation

2019 ◽  
Vol 15 (S350) ◽  
pp. 181-186
Author(s):  
Richard Teague
Keyword(s):  
Magnetic Field ◽  
High Resolution ◽  
Planet Formation ◽  
Physical Structure ◽  
Protoplanetary Disk ◽  
Field Structure ◽  
Magnetic Field Structure ◽  
Physical Conditions ◽  
Molecular Excitation ◽  
The Magnetic Field

AbstractUnderstanding the physical structure of the planet formation environment, the protoplanetary disk, is essential for the interpretation of high resolution observations of the dust and future observations of the magnetic field structure. Observations of multiple transitions of molecular species offers a unique view of the underlying physical structure through excitation analyses. Here we describe a new method to extract high-resolution spectra from low-resolution observations, then provide two case studies of how molecular excitation analyses were used to constrain the physical structure in TW Hya, the closest protoplanetary disk to Earth.

scholarly journals An Attempt to Associate Observed Photospheric Motions with the Magnetic Field Structure and Flare Occurrence in an Active Region

1971 ◽  
Vol 43 ◽  
pp. 435-442 ◽  
Author(s):  
M. J. Martres ◽  
I. Soru-Escaut ◽  
J. Rayrole
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Empirical Evidence ◽  
Active Regions ◽  
Field Structure ◽  
Magnetic Field Structure ◽  
Abrupt Changes ◽  
The Magnetic Field

We have tried to find empirical evidence for the role of photospheric motions in the building up of the flare productive magnetic patterns in Active Regions.The bright Hα faculae are associated with V∥ structures different from a classical Evershed flow and particularly ‘anomalous’ in the regions and periods of high flare occurrence. The flares observed occurred at ‘crossings’ of the lines V∥ = 0(V ≠ 0) and H∥ = 0 and at places where V∥ = 0 showed abrupt changes of direction. It is suggested that these anomalous V∥ structures are evidence of vortex motions.

scholarly journals High-resolution imaging polarimetry of HL Tau and magnetic field structure

2004 ◽  
Vol 352 (4) ◽  
pp. 1347-1364 ◽  
Author(s):  
P. W. Lucas ◽  
Misato Fukagawa ◽  
Motohide Tamura ◽  
A. F. Beckford ◽  
Yoichi Itoh ◽  
...  
Keyword(s):  
Magnetic Field ◽  
High Resolution ◽  
Field Structure ◽  
High Resolution Imaging ◽  
Magnetic Field Structure ◽  
Imaging Polarimetry ◽  
Resolution Imaging

scholarly journals Application of the Chromospheric Magnetograph to Active Regions

1971 ◽  
Vol 43 ◽  
pp. 237-242
Author(s):  
H. Zirin
Keyword(s):  
Magnetic Field ◽  
Magnetic Flux ◽  
Solar Surface ◽  
Active Regions ◽  
Field Structure ◽  
Form Complex ◽  
Magnetic Field Structure ◽  
Surface Field ◽  
The Magnetic Field

We show how to determine the magnetic field structure in active regions from the Hα morphology. We also show the role of the EFR (emerging flux region) as a bipolar region of velocity downflow. Finally, we point out that since all new magnetic flux emerges in strictly bipolar form, complex spot groups must result from surface interaction, hence most of the solar surface field may be produced on the surface.

scholarly journals Magnetic Field Structure of the CME Source Region

2001 ◽  
Vol 203 ◽  
pp. 393-395
Author(s):  
Y. Hanaoka
Keyword(s):  
Magnetic Field ◽  
Magnetic Energy ◽  
Source Region ◽  
Three Dimensional ◽  
Active Regions ◽  
Helical Structure ◽  
Field Structure ◽  
Dimensional Structure ◽  
Magnetic Field Structure ◽  
The Magnetic Field

The three-dimensional structure of the magnetic field in the source region of CMEs is the key to understand how the stored magnetic energy eventually causes an eruption. A CME accompanied by a filament eruption on 2000 February 26-27 is particularly a good event to study the three-dimensional magnetic field structure. This event was very well observed with the EIT and LASCO of SOHO and the SXT of Yohkoh, and shows the following clues of the magnetic field structure which caused the CME. (1) The filament had a helical structure before the eruption and it was kept throughout the eruption. (2) The coronal loop structure shows that this event was an eruption of a part of the quadrapolar magnetic field structure consisting of two active regions. In this proceeding, we present a brief overview of the event.

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