scholarly journals Discrepancies in the prediction of solar wind using potential field source surface model: An investigation of possible sources

2004 ◽  
Vol 109 (A8) ◽  
Author(s):  
Bala Poduval
Keyword(s):  
Solar Wind ◽  
Potential Field ◽  
Surface Model ◽  
Source Surface ◽  
Field Source

scholarly journals Cyclic Evolution of Coronal Fields from a Coupled Dynamo Potential-Field Source-Surface Model

Solar Physics ◽  
2015 ◽  
Vol 291 (2) ◽  
pp. 339-355 ◽  
Author(s):  
Mausumi Dikpati ◽  
Akshaya Suresh ◽  
Joan Burkepile
Keyword(s):  
Potential Field ◽  
Surface Model ◽  
Source Surface ◽  
Field Source

scholarly journals An elliptic expansion of the potential field source surface model

2020 ◽  
Vol 638 ◽  
pp. A109
Author(s):  
M. Kruse ◽  
V. Heidrich-Meisner ◽  
R. F. Wimmer-Schweingruber ◽  
M. Hauptmann
Keyword(s):  
Magnetic Field ◽  
Potential Field ◽  
Three Dimensional ◽  
Coronal Magnetic Field ◽  
Magnetic Configuration ◽  
Surface Model ◽  
Source Surface ◽  
Field Source ◽  
Numerical Solver ◽  
Elliptical Models

Context. The potential field source surface model is frequently used as a basis for further scientific investigations where a comprehensive coronal magnetic field is of importance. Its parameters, especially the position and shape of the source surface, are crucial for the interpretation of the state of the interplanetary medium. Improvements have been suggested that introduce one or more additional free parameters to the model, for example, the current sheet source surface model. Aims. Relaxing the spherical constraint of the source surface and allowing it to be elliptical gives modelers the option of deforming it to more accurately match the physical environment of the specific period or location to be analyzed. Methods. A numerical solver is presented that solves Laplace’s equation on a three-dimensional grid using finite differences. The solver is capable of working on structured spherical grids that can be deformed to create elliptical source surfaces. Results. The configurations of the coronal magnetic field are presented using this new solver. Three-dimensional renderings are complemented by Carrington-like synoptic maps of the magnetic configuration at different heights in the solar corona. Differences in the magnetic configuration computed by the spherical and elliptical models are illustrated.

scholarly journals A Comparison between Global Solar Magnetohydrodynamic and Potential Field Source Surface Model Results

2006 ◽  
Vol 653 (2) ◽  
pp. 1510-1516 ◽  
Author(s):  
Pete Riley ◽  
J. A. Linker ◽  
Z. Mikić ◽  
R. Lionello ◽  
S. A. Ledvina ◽  
...  
Keyword(s):  
Potential Field ◽  
Surface Model ◽  
Source Surface ◽  
Field Source

Source-dependent properties of the background slow solar wind encountered by Parker Solar Probe

2021 ◽  
Author(s):  
Léa Griton ◽  
Sarah Watson ◽  
Nicolas Poirier ◽  
Alexis Rouillard ◽  
Karine Issautier ◽  
...  
Keyword(s):  
Solar Wind ◽  
Extreme Ultraviolet ◽  
Plasma Heating ◽  
Coronal Holes ◽  
Slow Solar Wind ◽  
Source Surface ◽  
Field Source ◽  
Flux Tubes ◽  
Field Lines

<p>Different states of the slow solar wind are identified from in-situ measurements by Parker Solar Probe (PSP) inside 50 solar radii from the Sun (Encounters 1, 2, 4, 5 and 6). At such distances the wind measured at PSP has not yet undergone significant transformation related to the expansion and propagation of the wind. We focus in this study on the properties of the quiet solar wind with no magnetic switchbacks. The Slow Solar Wind (SSW) states differ by their density, flux, plasma beta and magnetic pressure. PSP's magnetic connectivity established with Potential Field Source Surface (PFSS) reconstructions, tested against extreme ultraviolet (EUV) and white-light imaging, reveals the different states under study generally correspond to transitions from streamers to equatorial coronal holes. Solar wind simulations run along these differing flux tubes reproduce the slower and denser wind measured in the streamer and the more tenuous wind measured in the coronal hole. Plasma heating is more intense at the base of the streamer field lines rooted near the boundary of the equatorial hole than those rooted closer to the center of the hole. This results in a higher wind flux driven inside the streamer than deeper inside the equatorial hole. </p>

scholarly journals Coronal magnetic fields from the inversion of linear polarization measurements

2009 ◽  
Vol 5 (S264) ◽  
pp. 96-98
Author(s):  
Yu Liu ◽  
Haosheng Lin ◽  
Jeff Kuhn
Keyword(s):  
Linear Polarization ◽  
Spatial Relation ◽  
Coronal Magnetic Field ◽  
Surface Model ◽  
Source Surface ◽  
Coronal Emission ◽  
Field Source ◽  
Close Relationship ◽  
The Difference ◽  
Ir Emission

AbstractReal 3-D coronal magnetic field reconstruction is expected to be made based on the technologies of IR spectrometry and tomography, in which the data from other wavelengths can be used as critical reference. Our recent studies focused on this issue are briefly reviewed in this paper. Liu & Lin (2008) first evaluated the validity of potential field source surface model applied to one of five limb regions in the corona by comparing the theoretical polarization maps with SOLARC observations in the IR Fe XIII 10747 Å forbidden coronal emission line (CEL). The five limb coronal regions were then studied together in order to study the spatial relation between the bright EUV features on the solar disk and the inferred IR emission sources, which were obtained from the inversion of the SOLARC linear polarization (LP) measurements (Liu 2009). The inversion for each fiber data in the field of view was made by finding the best location where the difference between the synthesized and the observed polarizations reaches the minimum in the integration path along the line of sight. We found a close relationship between the inferred IR emission source locations and the EUV strong emission positions.

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