scholarly journals Driving Layer of Solar Activity

2002 ◽  
Vol 12 ◽  
pp. 371-377
Author(s):  
Jingxiu Wang
Keyword(s):  
Magnetic Field ◽  
Solar Activity ◽  
Magnetic Energy ◽  
Field Measurements ◽  
Basic Structure ◽  
The Sun ◽  
Flux Emergence ◽  
Vector Magnetic Field ◽  
Elementary Processes ◽  
Magnetic Field Measurements

AbstractThere should be a driving layer on the Sun, in which the interaction between magnetic field and plasma motion would provide enough magnetic energy and necessary topology for the explosion of solar activity in the corona.Although the exact location of the driving layer is not known, phenomenologically, the photosphere is acting, in many aspects, as the driving layer. Vector magnetic field measurements on the photosphere are greatly needed in clarifying the nature of the driving.Two elementary processes, flux emergence and cancellation, andone basic structure, magnetic interface between topology-independent magnetic loops, are key elements in the driving.

scholarly journals Modelling coronal electron density and temperature profiles of the Active Region NOAA 11855

2016 ◽  
Vol 12 (S328) ◽  
pp. 149-151
Author(s):  
J. M. Rodríguez Gómez ◽  
L. E. Antunes Vieira ◽  
A. Dal Lago ◽  
J. Palacios ◽  
L. A. Balmaceda ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Magnetic Flux ◽  
Physical Mechanism ◽  
Magnetic Energy ◽  
Plasma Temperature ◽  
Coronal Magnetic Field ◽  
Flux Emergence ◽  
Vector Magnetic Field ◽  
Atmospheric Phenomena ◽  
Coronal Electron

AbstractThe magnetic flux emergence can help understand the physical mechanism responsible for solar atmospheric phenomena. Emerging magnetic flux is frequently related to eruptive events, because when emerging they can reconnected with the ambient field and release magnetic energy. We will use a physic-based model to reconstruct the evolution of the solar emission based on the configuration of the photospheric magnetic field. The structure of the coronal magnetic field is estimated by employing force-free extrapolation NLFFF based on vector magnetic field products (SHARPS) observed by HMI instrument aboard SDO spacecraft from Sept. 29 (2013) to Oct. 07 (2013). The coronal plasma temperature and density are described and the emission is estimated using the CHIANTI atomic database 8.0. The performance of the our model is compared to the integrated emission from the AIA instrument aboard SDO spacecraft in the specific wavelengths 171Å and 304Å.

scholarly journals Improved Current Density and Magnetization Reconstruction Through Vector Magnetic Field Measurements

2020 ◽  
Vol 14 (2) ◽  
Author(s):  
D.A. Broadway ◽  
S.E. Lillie ◽  
S.C. Scholten ◽  
D. Rohner ◽  
N. Dontschuk ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Current Density ◽  
Field Measurements ◽  
Vector Magnetic Field ◽  
Magnetic Field Measurements

Observing the Sun with the Atacama Large Millimeter/submillimeter Array – from continuum to magnetic fields

2019 ◽  
Vol 15 (S354) ◽  
pp. 24-37
Author(s):  
Sven Wedemeyer ◽  
Mikolaj Szydlarski ◽  
Jaime de la Cruz Rodriguez ◽  
Shahin Jafarzadeh
Keyword(s):  
Magnetic Field ◽  
Time Series ◽  
Solar Magnetic Field ◽  
Extended Period ◽  
Field Measurements ◽  
The Sun ◽  
Post Processing ◽  
Magnetic Field Measurements ◽  
Scientific Results ◽  
Temperature Maps

AbstractThe Atacama Large Millimeter/submillimeter Array offers regular observations of our Sun since 2016. After an extended period of further developing and optimizing the post-processing procedures, first scientific results are now produced. While the first observing cycles mostly provided mosaics and time series of continuum brightness temperature maps with a cadence of 1-2s, additional receiver bands and polarization capabilities will be offered in the future. Currently, polarization capabilities are offered for selected receiver bands but not yet for solar observing. An overview of the recent development, first scientific results and potential of solar magnetic field measurements with ALMA will be presented.

scholarly journals Two Kinds of Activity in Late-type Stars

1991 ◽  
Vol 130 ◽  
pp. 440-442
Author(s):  
M.M. Katsova
Keyword(s):  
Magnetic Field ◽  
Active Regions ◽  
Field Measurements ◽  
Spherically Symmetric ◽  
The Sun ◽  
Late Type ◽  
X Ray ◽  
Magnetic Field Measurements ◽  
Local Magnetic Fields ◽  
Uniform Manner

Several years ago we proposed a method for the analysis of X-ray observations of late-type stars. It allowed the determination in a uniform manner of coronal base electron densities for more than 40 late-type stars, in terms of a one-temperature consideration of homogeneous spherically symmetric coronae (Katsova et al., 1987). Fig. 1 shows the results as a function of spectral type. Comparison of our results with values for different kinds of solar regions shows that physical characteristics of F and G star coronae correspond to densities less than those in active regions on the Sun. Values for the active K-M0 stars are comparable with those of dense steady condensations found directly above large sunspots.On this basis, activity can be explained as an increase in that part of the stellar surface that is occupied by strong local magnetic fields. This is illustrated in the table where we compare magnetic field measurements by Saar and Linsky (1988) with our calculations.

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