4 Stereoscopic and Tomographic Observations

In this section we describe the application of stereoscopic and tomographic methods to a variety of coronal observations, grouped by phenomena, with emphasis on observational and physical results, while the technical details of the methods are referred to the previous Section 3.

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Figure 15: Examples of tomographic reconstructions of the solar corona, visualized as synoptic density maps at a specific height level. Top left: Synoptic map of coronal density at a height of r = 2.55 R⊙, reconstructed with 87 pB images from LASCO C-2 (Frazin et al., 2007Jump To The Next Citation Point); Bottom left: Synoptic electron density map at a heigth of r = 1.075 R ⊙, reconstructed with a DEM method and STEREO/A and B observations (Frazin et al., 2009bJump To The Next Citation Point); Right: Density reconstruction ne(l,b) at r = 2.5 R⊙ from LASCO C-2 total brightness images B (top right) and density difference Δne (l,b) after subtraction of polarized brightness images, B − pB, at the same height level (bottom right) (from Frazin et al., 2010Jump To The Next Citation Point).
 4.1 3D reconstruction of the large-scale corona
 4.2 Coronal streamers
 4.3 Active regions
 4.4 Coronal loops
  4.4.1 Hydrostatic scale height of loops
  4.4.2 Hydrodynamics of loops
  4.4.3 Magnetic fields of loops
 4.5 MHD oscillations in coronal loops
 4.6 MHD waves in coronal loops
 4.7 Quiescent filaments and prominences
 4.8 Erupting filaments and prominences
 4.9 Bright points, jets, and plumes
 4.10 Solar flares
 4.11 CME source regions and EUV dimming
 4.12 Global coronal waves

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