scholarly journals The solar magnetic activity band interaction and instabilities that shape quasi-periodic variability

2015 ◽  
Vol 6 (1) ◽  
Author(s):  
Scott W. McIntosh ◽  
Robert J. Leamon ◽  
Larisza D. Krista ◽  
Alan M. Title ◽  
Hugh S. Hudson ◽  
...  
Keyword(s):  
Magnetic Activity ◽  
Solar Magnetic Activity ◽  
Activity Band

scholarly journals ‘Sumer’ – Solar Ultraviolet Measurements of Emitted Radiation

1994 ◽  
Vol 144 ◽  
pp. 619-624 ◽  
Author(s):  
K. Wilhelm ◽  
W. Curdt ◽  
A. H. Gabriel ◽  
M. Grewing ◽  
M. C. E. Huber ◽  
...  
Keyword(s):  
Spectral Resolution ◽  
Extreme Ultraviolet ◽  
Flow Characteristics ◽  
Magnetic Activity ◽  
High Accuracy ◽  
The Sun ◽  
Lower Corona ◽  
Doppler Shifts ◽  
Solar Magnetic Activity ◽  
Solar Ultraviolet

AbstractThe experiment Solar Ultraviolet Measurements of Emitted Radiation (SUMER) is designed for the investigations of plasma flow characteristics, turbulence and wave motions, plasma densities and temperatures, structures and events associated with solar magnetic activity in the chromosphere, the transition zone and the corona. Specifically, SUMER will measure profiles and intensities of extreme ultraviolet (EUV) lines emitted in the solar atmosphere ranging from the upper chromosphere to the lower corona; determine line broadenings, spectral positions and Doppler shifts with high accuracy; provide stigmatic images of selected areas of the Sun in the EUV with high spatial, temporal and spectral resolution and obtain full images of the Sun and the inner corona in selectable EUV lines, corresponding to a temperature range from 104to more than 1.8 x 106K. The spatial and spectral resolution capabilities of the instrument will be considered in this contribution in some detail, and a new detector concept will be introduced.

The generation of solar magnetic activity: Photospheric flows and coronal fields

1993 ◽  
Vol 13 (9) ◽  
pp. 15-22
Author(s):  
Gerard Van Hoven
Keyword(s):  
Magnetic Activity ◽  
Solar Magnetic Activity

scholarly journals Radio Flare Activity of RS CVn Stars

1980 ◽  
Vol 88 ◽  
pp. 403-403
Author(s):  
Paul A. Feldman
Keyword(s):  
Binary Star ◽  
Quantitative Model ◽  
Magnetic Activity ◽  
Flare Activity ◽  
Radio Observatory ◽  
X Ray ◽  
Rs Cvn Stars ◽  
Solar Magnetic Activity ◽  
Radio Flare ◽  
Systematic Program

For several years, a systematic program to observe RS CVn and similar binaries has been undertaken with the 46-m telescope of the Algonquin Radio Observatory. A number of large radio outbursts at 2.8 cm wavelength has been found from HR 1099, AR Lac, SZ Psc, UX Ari, and HR 5110. In several cases, simultaneous, or nearly simultaneous, observations of these stars were made by cooperating observers at (other) radio, optical, UV, and X-ray wavelengths. It is now clearly established that the mechanism responsible for the cm-wavelength radio emission is nonthermal gyrosynchrotron radiation in a volume whose characteristic dimension is comparable with the binary star separation. More generally, a semi-quantitative model for the radio flare activity of these stars seems to be possible using greatly scaled-up analogues of solar magnetic activity.

Non-axisymmetrical distributions of solar magnetic activity and irradiance

2002 ◽  
Vol 29 (12) ◽  
pp. 1941-1946 ◽  
Author(s):  
E.E. Benevolenskaya
Keyword(s):  
Magnetic Activity ◽  
Solar Magnetic Activity

scholarly journals On the Current Solar Magnetic Activity in the Light of Its Behaviour During the Holocene

Solar Physics ◽  
2015 ◽  
Vol 291 (1) ◽  
pp. 303-315 ◽  
Author(s):  
F. Inceoglu ◽  
R. Simoniello ◽  
M. F. Knudsen ◽  
C. Karoff ◽  
J. Olsen ◽  
...  
Keyword(s):  
Magnetic Activity ◽  
The Holocene ◽  
Solar Magnetic Activity

scholarly journals Reflection of Solar Activity Dynamics in Radionuclide Data

Radiocarbon ◽  
1992 ◽  
Vol 34 (2) ◽  
pp. 207-212 ◽  
Author(s):  
A. V. Blinov ◽  
M. N. Kremliovskij
Keyword(s):  
Nonlinear Dynamics ◽  
Solar Activity ◽  
Numerical Methods ◽  
Chaotic Behavior ◽  
Magnetic Activity ◽  
Data Sets ◽  
Cosmogenic Nuclide ◽  
Proxy Records ◽  
Solar Magnetic Activity ◽  
Activity Dynamics

Variability of solar magnetic activity manifested within sunspot cycles demonstrates features of chaotic behavior. We have analyzed cosmogenic nuclide proxy records for the presence of the solar activity signals. We have applied numerical methods of nonlinear dynamics to the data showing the contribution of the chaotic component. We have also formulated what kind of cosmogenic nuclide data sets are needed for investigations on solar activity.

scholarly journals Solar magnetic activity: Topologically explored

2009 ◽  
Vol 1 ◽  
pp. 225-234
Author(s):  
H. Lundstedt
Keyword(s):  
Magnetic Activity ◽  
Solar Magnetic Activity

scholarly journals Characterisation of flare Soft X-ray distribution with solar magnetic activity

2020 ◽  
Vol 1548 ◽  
pp. 012011
Author(s):  
R Foldes ◽  
F Berrilli
Keyword(s):  
Magnetic Activity ◽  
X Ray ◽  
Solar Magnetic Activity

scholarly journals Magnetic fields and dynamics of the Sun's interior

2008 ◽  
Vol 4 (S259) ◽  
pp. 147-158
Author(s):  
Alexander G. Kosovichev
Keyword(s):  
Magnetic Fields ◽  
Physical Mechanism ◽  
Active Regions ◽  
Magnetic Activity ◽  
Solar Interior ◽  
Global Dynamics ◽  
The Sun ◽  
New Knowledge ◽  
Solar Magnetic Activity ◽  
Key Questions

AbstractAdvances in helioseismology provide new knowledge about the origin of solar magnetic activity. The key questions addressed by helioseismology are: what is the physical mechanism of the solar dynamo, how deep inside the Sun are the magnetic fields generated, how are they transported to the surface and form sunspots? Direct helioseismic signatures of the internal magnetic fields are weak and difficult to detect. Therefore, most of the information comes from observations of dynamical effects caused by the magnetic fields. I review results of recent helioseismic observations of the magnetohydrodynamics of the solar interior on various scales, including global dynamics associated with the dynamo processes, and formation of sunspots and active regions.

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