I should write this up and save it or something because this isn't the first time I've written this, but here's the bottom line with SOHO: none of its instruments records data in a way that is going to produce images which you can analyze the same way as a photograph. Why is this? Well, Wikipedia lists its instruments as follows.

• Coronal Diagnostic Spectrometer (CDS) which measures density, temperature and flows in the corona.
• Charge Element and Isotope Analysis System (CELIAS) which studies the ion composition of the solar wind.
• Comprehensive SupraThermal and Energetic Particle analyser collaboration (COSTEP) which studies the ion and electron composition of the solar wind. COSTEP and ERNE are sometimes referred to together as the COSTEP-ERNE Particle Analyzer Collaboration (CEPAC).
• Extreme ultraviolet Imaging Telescope (EIT) which studies the low coronal structure and activity.
• Energetic and Relativistic Nuclei and Electron experiment (ERNE) which studies the ion and electron composition of the solar wind. (See note above in COSTEP entry.)
• Global Oscillations at Low Frequencies (GOLF) which measures velocity variations of the whole solar disk to explore the core of the Sun.
• Large Angle and Spectrometric Coronagraph (LASCO) which studies the structure and evolution of the corona by creating an artificial solar eclipse.
• Michelson Doppler Imager (MDI) which measures velocity and magnetic fields in the photosphere to learn about the convection zone which forms the outer layer of the interior of the Sun and about the magnetic fields which control the structure of the corona. The MDI is the biggest producer of data by far on SOHO. In fact, two of SOHO's virtual channels are named after MDI, VC2 (MDI-M) carries MDI magnetogram data, and VC3 (MDI-H) carries MDI Helioseismology data.
• Solar Ultraviolet Measurement of Emitted Radiation (SUMER) which measures plasma flows, temperature and density in the corona.
• Solar Wind Anisotropies (SWAN) which uses telescopes sensitive to a characteristic wavelength of hydrogen to measure the solar wind mass flux, map the density of the heliosphere, and observe the large-scale structure of the solar wind streams. UltraViolet Coronagraph Spectrometer (UVCS) which measures density and temperature in the corona. Variability of solar IRradiance and Gravity Oscillations (VIRGO) which measures oscillations and solar constant both of the whole solar disk and at low resolution, again exploring the core of the Sun.