Solar flare forecasting model with active region photospheric magnetic field properties and sunspot factors

2013 ◽  
Vol 58 (19) ◽  
pp. 1845-1850
Author(s):  
YanMei CUI ◽  
Rong LI ◽  
Jie ZHU
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Solar Flare ◽  
Photospheric Magnetic Field ◽  
Forecasting Model

scholarly journals The Nonpotentiality of Active‐Region Coronae and the Dynamics of the Photospheric Magnetic Field

2005 ◽  
Vol 628 (1) ◽  
pp. 501-513 ◽  
Author(s):  
Carolus J. Schrijver ◽  
Marc L. DeRosa ◽  
Alan M. Title ◽  
Thomas R. Metcalf
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Photospheric Magnetic Field

CHOICE OF CONDITIONS FOR MHD SIMULATIONS ABOVE THE ACTIVE REGION, ALLOWING THE STUDY OF THE SOLAR FLARE MECHANISM

2021 ◽  
Vol 44 ◽  
pp. 92-95
Author(s):  
A.I. Podgorny ◽  
◽  
I.M. Podgorny ◽  
A.V. Borisenko ◽  
N.S. Meshalkina ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Solar Flare ◽  
Magnetic Energy ◽  
Solar Radius ◽  
Computational Domain ◽  
Mhd Simulations ◽  
Flare Energy ◽  
Numerical Instabilities ◽  
The Magnetic Field

Primordial release of solar flare energy high in corona (at altitudes 1/40 - 1/20 of the solar radius) is explained by release of the magnetic energy of the current sheet. The observed manifestations of the flare are explained by the electrodynamical model of a solar flare proposed by I. M. Podgorny. To study the flare mechanism is necessary to perform MHD simulations above a real active region (AR). MHD simulation in the solar corona in the real scale of time can only be carried out thanks to parallel calculations using CUDA technology. Methods have been developed for stabilizing numerical instabilities that arise near the boundary of the computational domain. Methods are applicable for low viscosities in the main part of the domain, for which the flare energy is effectively accumulated near the singularities of the magnetic field. Singular lines of the magnetic field, near which the field can have a rather complex configuration, coincide or are located near the observed positions of the flare.

scholarly journals The Formation of a Moat Around a Sunspot as Observed on Longitudinal–Field Magnetograms (?)

1993 ◽  
Vol 141 ◽  
pp. 75-77
Author(s):  
L.V. Ermakova
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Spatial Resolution ◽  
Sunspot Group ◽  
Longitudinal Magnetic Field ◽  
Photospheric Magnetic Field ◽  
Longitudinal Field ◽  
Maximum Area ◽  
Spot Group

In this paper the dynamics of the photospheric magnetic field near the sunspot of the active region McMath 15508 is considered on the basis of longitudinal magnetic field B11 magnetograms. The magnetograms were obtained at the panoramic magnetograph of the Sayan Observatory. The time taken to obtain one magnetogram was 5 min. The spatial resolution was 1.8“ × 3.6“. In the active region McMath 15508 a new bipolar spot group formed westward of the existing sunspot group on September 1; the next day the main sunspots had penumbras, and on September 3 the new sunspot group reached a maximum area and began decaying thereafter.

Solar flare forecasting model using 3D magnetic field data

2020 ◽  
Author(s):  
Xin Huang
Keyword(s):  
Magnetic Field ◽  
Deep Learning ◽  
Solar Flare ◽  
Solar Flares ◽  
Field Data ◽  
Active Regions ◽  
Forecasting Model ◽  
Magnetic Field Data ◽  
The Magnetic Field

<p>Solar flares originate from the release of the energy stored in the magnetic field of solar active regions. Generally, the photospheric magnetograms of active regions are used as the input of the solar flare forecasting model. However, solar flares are considered to occur in the low corona. Therefore, the role of 3D magnetic field of active regions in the solar flare forecast should be explored. We extrapolate the 3D magnetic field using the potential model for all the active regions during 2010 to 2017, and then the deep learning method is applied to extract the precursors of solar flares in the 3D magnetic field data. We find that the 3D magnetic field of active regions is helpful to build a deep learning based forecasting model.</p>

scholarly journals Large-scale photospheric magnetic field: The diffusion of active region fields

Solar Physics ◽  
1972 ◽  
Vol 26 (2) ◽  
pp. 283-289 ◽  
Author(s):  
Kenneth H. Schatten ◽  
Robert B. Leighton ◽  
Robert Howard ◽  
John M. Wilcox
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Large Scale ◽  
Photospheric Magnetic Field

Solar Flare Acceleration of Solar Wind: Influence of Active Region Magnetic Field

Science ◽  
1981 ◽  
Vol 212 (4502) ◽  
pp. 1501-1502 ◽  
Author(s):  
H. LUNDSTEDT ◽  
J. M. WILCOX ◽  
P. H. SCHERRER
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Active Region ◽  
Solar Flare ◽  
Wind Influence

CHARACTERISTICS OF THE PHOTOSPHERIC MAGNETIC FIELD ASSOCIATED WITH SOLAR FLARE INITIATION

2014 ◽  
Vol 786 (1) ◽  
pp. 72 ◽  
Author(s):  
Ya-Hui Yang ◽  
P. F. Chen ◽  
Min-Shiu Hsieh ◽  
S. T. Wu ◽  
Han He ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Flare ◽  
Photospheric Magnetic Field

scholarly journals Solar Flare Prediction and Magnetic Field Evolution in Solar Active Region

2002 ◽  
Vol 12 ◽  
pp. 396-397
Author(s):  
H.N. Wang ◽  
G.Q. Zhang ◽  
C.L. Zhu ◽  
J.L. Sun
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Solar Flare ◽  
Solar Flares ◽  
Astronomical Observatory ◽  
Solar Active Region ◽  
Field Evolution

AbstractThe authors propose a number of empirical criteria for prediction of solar flares based on many years of observations at Huairou Solar Observing Station of Beijing Astronomical Observatory.

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