One of the instruments on the Solar and Heliospheric Observatory (SOHO) is the Extreme ultraviolet Imaging Telescope. This is able to image in four bands of the extreme ultraviolet part of the EM spectrum. The lowest energy is sensitive to a band which includes an emission line of Helium -He II at 304 Å (30.4nm). The other three are at increasing ionisation emission lines of Iron - Fe XV at 284 Å (28,4nm), Fe XII at 195 Å (19.5nm) , and Fe IX, X at 171 Å (17.1nm). This compares to 656.3nm which the club's Ha filter lets through.
All this means that each camera can see different temperatures which means different energy events. The output from each camera is monochrome (black and white) but are coloured when they are put on the web so you can tell which camera they came from. The colouring is in colour order from the visible spectrum with red being the longest wavelength (30.4nm) and blue the shortest (17.1nm).
As magnetic fields burst out of the Sun, the four wavelengths recorded by the EIT reveal different temperatures in the event.
In the image above I have combined the four whole disk images in Photoshop. This example has been greatly reduced for the website. With practice you should be able to produce much better results. You can also layer in your own sunspot and Ha images.
Here the four images shown at the top of the page are combined. The white and the blue show the highest energy parts. Most of these are in the centre of intense magnetic fields (shown by the field lines). The flare is far cooler and only registers well on the He (II) 30.4nm red coded image.