Active Space Experiments with Electron Beam Injection: Whistler Wave Emission and Compatible on-Board VLF Receiver

1995 ◽  
Vol 31 (9) ◽  
pp. 579-583
Author(s):  
C Krafft ◽  
B Lundin
2005 ◽  
Vol 48 (9) ◽  
pp. 650-660 ◽  
Author(s):  
T. M. Zaboronkova ◽  
C. Krafft ◽  
A. V. Kudrin ◽  
M. Yu. Lyakh

1994 ◽  
Vol 72 (5) ◽  
pp. 649-652 ◽  
Author(s):  
C. Krafft ◽  
P. Thévenet ◽  
G. Matthieussent ◽  
B. Lundin ◽  
G. Belmont ◽  
...  

2002 ◽  
Vol 9 (4) ◽  
pp. 1401-1411 ◽  
Author(s):  
A. V. Kudrin ◽  
M. Yu. Lyakh ◽  
T. M. Zaboronkova ◽  
C. Krafft

1999 ◽  
Vol 6 (5) ◽  
pp. 1427-1434 ◽  
Author(s):  
M. Starodubtsev ◽  
C. Krafft ◽  
P. Thévenet ◽  
A. Kostrov

Author(s):  
C. Béghin ◽  
Y. Arnal ◽  
P. Gille ◽  
D. Henry ◽  
J. L. Michau ◽  
...  

1982 ◽  
Vol 51 (2) ◽  
pp. 650-657 ◽  
Author(s):  
Hiroharu Fujita ◽  
Shinya Yagura ◽  
Eiichi Yamada ◽  
Akira Aoyagi

2015 ◽  
Vol 11 (S320) ◽  
pp. 239-242
Author(s):  
Jianxia Cheng ◽  
Mingde Ding

AbstractSolar flares produce radiations in very broad wavelengths. Spectra can supply us abundant information about the local plasma, such as temperature, density, mass motion and so on. Strong chromospheric lines, like the most studied Hα and Ca II 8542 Å lines are formed under conditions of departures from local thermodynamic equilibrium in the lower atmosphere subject to flare heating. Understanding how these lines are formed is very useful for us to correctly interpret the observations. In this paper, we try to figure out the response of chromospheric lines heated by different periodic non-thermal electron beams. Our results are based on radiative hydrodynamic simulations. We vary the periods of electron beam injection from 1.25 s to 20 s. We compare the response times to different heating parameters. Possible explanations are discussed.


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