Coronal plasma behaviour in C and

1997 ◽  
Author(s):  
S. V. Lebedev ◽  
R. Aliaga-Rossel ◽  
J. P. Chittenden ◽  
A. E. Dangor ◽  
M. G. Haines ◽  
...  
Keyword(s):  
Coronal Plasma

Structuring, Motions and Shapes of Corona Emission Line Profiles

1994 ◽  
Vol 144 ◽  
pp. 421-426
Author(s):  
N. F. Tyagun
Keyword(s):  
Emission Line ◽  
Filling Factor ◽  
Direct Relationship ◽  
Coronal Plasma ◽  
Line Of Sight ◽  
Line Profiles ◽  
The Difference ◽  
Yellow Line ◽  
Red Line

AbstractThe interrelationship of half-widths and intensities for the red, green and yellow lines is considered. This is a direct relationship for the green and yellow line and an inverse one for the red line. The difference in the relationships of half-widths and intensities for different lines appears to be due to substantially dissimilar structuring and to a set of line-of-sight motions in ”hot“ and ”cold“ corona regions.When diagnosing the coronal plasma, one cannot neglect the filling factor - each line has such a factor of its own.

Solar Filaments as Tracers of Subsurface Processes

2000 ◽  
Vol 179 ◽  
pp. 177-183
Author(s):  
D. M. Rust
Keyword(s):  
Magnetic Fields ◽  
Magnetic Flux ◽  
Coronal Mass Ejections ◽  
Interplanetary Space ◽  
Intermediate Stage ◽  
Coronal Plasma ◽  
Magnetic Helicity ◽  
The Sun ◽  
New Paradigm ◽  
Solar Filaments

AbstractSolar filaments are discussed in terms of two contrasting paradigms. The standard paradigm is that filaments are formed by condensation of coronal plasma into magnetic fields that are twisted or dimpled as a consequence of motions of the fields’ sources in the photosphere. According to a new paradigm, filaments form in rising, twisted flux ropes and are a necessary intermediate stage in the transfer to interplanetary space of dynamo-generated magnetic flux. It is argued that the accumulation of magnetic helicity in filaments and their coronal surroundings leads to filament eruptions and coronal mass ejections. These ejections relieve the Sun of the flux generated by the dynamo and make way for the flux of the next cycle.

scholarly journals ARE CHROMOSPHERIC NANOFLARES A PRIMARY SOURCE OF CORONAL PLASMA?

2014 ◽  
Vol 791 (1) ◽  
pp. 60 ◽  
Author(s):  
J. A. Klimchuk ◽  
S. J. Bradshaw
Keyword(s):  
Primary Source ◽  
Coronal Plasma

Numerical simulations of fast MHD waves in a coronal plasma

Solar Physics ◽  
1993 ◽  
Vol 144 (2) ◽  
pp. 255-266 ◽  
Author(s):  
K. Murawski ◽  
B. Roberts
Keyword(s):  
Numerical Simulations ◽  
Coronal Plasma ◽  
Mhd Waves

scholarly journals The cooling and condensation of flare coronal plasma

1982 ◽  
Vol 254 ◽  
pp. 343 ◽  
Author(s):  
S. K. Antiochos ◽  
P. A. Sturrock
Keyword(s):  
Coronal Plasma

Characterization of stellar activity using transits and its impact on habitability

2019 ◽  
Vol 15 (S354) ◽  
pp. 461-466
Author(s):  
Raissa Estrela ◽  
Adriana Valio ◽  
Sourav Palit
Keyword(s):  
Magnetic Field ◽  
Light Curve ◽  
Physical Properties ◽  
Crucial Role ◽  
Coronal Plasma ◽  
Habitable Zone ◽  
Stellar Activity ◽  
Magnetic Cycles ◽  
Living Organisms

AbstractStellar magnetic field is the driver of activity in stars and can trigger spots, energetic flares, coronal plasma ejections and ionized winds. These phenomena play a crucial role in understanding the internal mechanisms of the star, but can also have potential effects in orbiting planets. During the transit of a planet, spots can be occulted producing features imprinted in the transit light curve. Here, we modelled these features to characterize the physical properties of the spots (radius, intensity, and location). In addition, we monitor spots signatures on multiple transits to estimate magnetic cycles length of Kepler stars. Flares have also been observed during transits in active stars. We derive the properties of the flares and analyse their UV impact on possible living organisms in planets orbiting in the habitable zone.

Sign in / Sign up

Export Citation Format

Share Document