The Solar Atmosphere
Effects of partial ionisation in the solar atmosphere
... These governing equations were then recast for the partially ionised plasma of the Sun’s atmosphere, and estimates of transport parameters were made. A Lagrangian Remap MHD code was then adapted to simulate the ...
186
Thermal and resistive instabilities in the solar atmosphere
... The magnetic field greatly influences the plasma in the solar atmosphere and.in this thesis we consider the effect of the field on the stability of the plasma. The many observations that have been made ...
274
Compressive magnetohydrodynamic waves in the solar atmosphere
... the solar atmo- sphere, induced by the rearrangement of the complex magnetic field in the ...that solar flares affect all layers of the solar atmosphere, while most CMEs originate from the active ...
162
Magnetohydrodynamic surface waves in the solar atmosphere
... stratified atmosphere is severely complicated and therefore a theory of such modes in a non-gravitational medium is a useful preliminary study to a fuller understanding of the more complicated ...
210
The nonuniform magnetohydrodynamic nature of the solar atmosphere
... Chapter 6 : Flows In Closed And Partially Open Magnetic Structures. 6.1 Introduction As noted in chapter one, the magnetic field in the solar atmosphere can be classified as being either 'closed' or 'open'. ...
227
Nuclear-Chemical Processes in the Solar Atmosphere
... powerful solar bursts as a result of nuclear processes involving protons accelerated in these regions and carbon, nitrogen, oxygen, and iron nuclei, and also as a consequence of fusion of the helium-4 and helium-3 ...
5
Is magnetic topology important for heating the solar atmosphere?
... the solar atmosphere and powers events, large and small, from solar flares and coronal mass ejections down to X-ray bright points and nanoflares, comes from convective motions below the solar ...
22
The effects of magnetic fields on oscillations in the solar atmosphere
... the solar core to sophisticated versions of the equation of ...the solar p-modes are generally ...the solar atmosphere, where the magnetic fie ld dominates the gas pressure, fib ril fields fan ...
206
The propagation and damping of slow magnetoacoustic waves in the solar atmosphere
... By using a range of spectral lines, waves can be observed as they propagate through the solar atmosphere. With the addition of an equilibrium temperature gradient the forward modelling results vary more ...
164
The Generation and Damping of Propagating MHD Kink Waves in the Solar Atmosphere
... upper solar atmosphere to temperatures in excess of a million degrees and the acceleration of the solar wind to hundreds of kilometers per second is still ...the solar atmosphere, but, ...
11
The Liquid Metallic Hydrogen Model of the Sun and the Solar Atmosphere VII.
... the Solar Atmosphere ...the solar atmosphere should be viewed as the result of the simulta- neous transfer of protons and electrons onto condensed hydrogen structures, ...true solar ...
7
Empirical mode decomposition analysis of random processes in the solar atmosphere
... The other SDO / AIA data set taken from a lower level of ROI 1, namely the intensity signals at 1600 Å, shows similar spectral energy distribution well localised inside the general con- fidence interval with α ≈ 0 and α ...
10
Dynamical processes in the solar atmosphere
... hagai followed Kostyuk and Pikel'ner in attaching a mocel atmosphere and succeeded in avoiding the problem of time-step size. However, Craig (1961) has cast doubt on Magai’s grid spacing in the transition zone. ...
263
MHD flows in the solar atmosphere
... the solar wind is free to escape, stream ers contain a denser plasma, basically static, trapped inside large magnetic closed arcades, loops are clearly the result of curved magnetic flux tubes emerging from the ...
189
Observations of oscillatory motions in the solar atmosphere
... Light scattered perpendicular to the spectrum to various points on the slit.(a}unimaged sunlight on entrance slit; (b) 17 cm solar image centered at position X on [r] ...
196
The Structure and Dynamic nature of the Solar Atmosphere
... The frequencies are observed as oscillations in the chro- mosphere and transition region, and propagations in the emerging coronal loops, due to the combined effect of the temperature s[r] ...
216
Reflection-Driven MHD Turbulence in the Solar Atmosphere and Solar Wind
... going wave packet, it approximately follows—i.e., is advected by—the total ( perturbed plus unperturbed) magnetic field lines. induced by the w þ. Therefore, oppositely directed wave pac[r] ...
48
Magnetic braids in eruptions of a spiral structure in the solar atmosphere
... Abstract We report on high-resolution imaging and spectral observations of eruptions of a spiral structure in the transition region, which were taken with the Interface Region Imaging Spectrograph, and the Atmospheric ...
14
DEPARTMENT 4: Solar Physics SECTIONS 8 & 9: Structure and Dynamics of the Solar Atmosphere & Solar Activity
... An important factor for CME studies is the pre-eruption configuration of the coronal magnetic field. It is well-known that most of the CMEs originate from inside the streamer belt of the solar corona. A study of ...
43
Alfven Waves in the Lower Solar Atmosphere
... The flow of energy through the solar atmosphere and the heating of the Sun’s outer regions are still not understood. Here, we report the detection of oscillatory phenomena associated with a large ...
5