Magnetic fields in solar flares

2007 ◽  
Vol 13 (1s) ◽  
pp. 99-100
Author(s):  
V.G. Lozitsky ◽  
Keyword(s):  
1985 ◽  
Vol 107 ◽  
pp. 221-224
Author(s):  
J. J. Aly

We show that a sheared 2–D force–free field can evolve in a quasi–static way towards an open configuration, and apply this result to a qualitative theory of two–ribbon solar flares.


Solar Physics ◽  
1994 ◽  
Vol 155 (1) ◽  
pp. 99-112 ◽  
Author(s):  
Tongjiang Wang ◽  
Aoao Xu ◽  
Hongqi Zhang
Keyword(s):  

Solar Physics ◽  
1976 ◽  
Vol 47 (1) ◽  
pp. 261-266 ◽  
Author(s):  
Kunitomo Sakurai
Keyword(s):  

2015 ◽  
Vol 59 (8) ◽  
pp. 795-805 ◽  
Author(s):  
A. I. Podgorny ◽  
I. M. Podgorny ◽  
N. S. Meshalkina

2017 ◽  
Vol 30 (0) ◽  
pp. 232-235
Author(s):  
V. G. Lozitsky ◽  
E. A. Baranovsky ◽  
N. I. Lozitska ◽  
V. P. Tarashchuk

Author(s):  
Zety Sharizat Hamidi ◽  
S.N.U. Sabri ◽  
N.N.M. Shariff ◽  
C. Monstein

This event allows us to investigate how plasma–magnetic field interactions in the solar corona can produce suprathermal electron populations over periods from tens of minutes to several hours, and the interactions of wave-particle and wave-wave lead to characteristic fine structures of the emission. An intense and broad solar radio burst type IV was recorded by CALLISTO spectrometer from 240-360 MHz. Using data from a the KRIM observatory, we aim to provide a comprehensive description of the synopsis formation and dynamics of a a single solar burst type IV event due to active region AR2222. For five minutes, the event exhibited strong pulsations on various time scales and “broad patterns” with a formation of a group type III solar burst. AR 2222 remained the most active region, producing a number of minor C-Class solar flares. The speed of the solar wind also exceeds 370.8 km/second with 10.2 g/cm3 density of proton in the solar corona. The radio flux also shows 171 SFU. Besides, there are 3 active regions, AR2217, AR2219 and AR2222 potentially pose a threat for M-class solar flares. Active region AR2222 have unstable 'beta-gamma' magnetic fields that harbor energy for M-class flares. As a conclusion, we believed that Sun’s activities more active in order to achieve solar maximum cycle at the end of 2014.


1993 ◽  
Vol 141 ◽  
pp. 323-332 ◽  
Author(s):  
Haimin Wang

AbstractThis paper reviews observations on the evolution of magnetic fields and flows in active regions which produce major flares. It includes the following topics: (1) Relationship between magnetic shear and flares; (2) Relationship between electric currents and flares; (3) Flows in active regions, particularly the emergence of new flux inside sheared penumbrae, and the mixed magnetic polarity nature of this kind of flux emergence; and (4) Changes of magnetic structure immediately before and after major solar flares; in particular, I will describe some recent findings that shear may increase after major flares.


1998 ◽  
Vol 60 (1) ◽  
pp. 1-1
Author(s):  
John Dougherty

We record with sadness the death of Franz Kahn, a former Associate Editor of the Journal of Plasma Physics.Franz was born in Germany in 1926, but his family emigrated to England in 1938. He attended Oxford University, obtaining First Class Honours in Mathematics in 1947, and continuing as a research student there, eventually gaining his D.Phil. in 1950. His thesis work already involved him in plasma physics, under one of the pioneers of the subject. His supervisor was Sydney Chapman, and his topic was that of the production of plasma by solar flares, and its interaction with the Earth's atmosphere. This field had already been opened by Chapman and a previous pupil, Vincent Ferraro, in the 1930s. The idea had originally been phrased in terms of ‘corpuscles’, i.e. energetic ions and electrons, but it had gradually been realized that electrostatic forces give such a medium a coherence, so that it should be described as a fluid, notwithstanding the lack of collisions. This is of course the basic idea of plasma physics, and when the importance of magnetic fields was included, one had all the ingredients of magnetohydrodynamics.


Sign in / Sign up

Export Citation Format

Share Document