The animation here is 27 frames taken over 44 minutes. Surface features were inverted (white/black). It is loaded in full resolution, so please zoom in fully--you should be able to see 8 out of the Top 10, minus any flares or Ellerman bombs. This animation also shows the floating prominence that I previously posted a close-up for here.

I acquired SER 16-bit 15 s videos of about 350 frames, each at 7.5ms, gain of 100, and ROI of 2600x2600 px. There was a delay of 75s between frames starting at 10 AM local time. I stacked in AutoStakkert with a 1.5x drizzle, selecting the best 25% of frames (about 87 frames). I sharpened the stacks using wavelets in Registax. The surface white/black inversion, red Ha coloration and the gif animation were all done in Photoshop.

Top Ten Things to See in Solar Halpha
Our Sun in Ha has so many interesting features that it challenging to understand exactly what one is seeing.  I compiled this summary of as a viewing aid for myself: hopefully you may find it useful. In white light we only see the Sun’s 6000 Kelvin photosphere “landscape”, consisting of:

• Darker, cooler sunspots
• Granulation, consisting of hotter and brighter rising; and cooler and darker sinking convention cells, like boiling porridge.
• Faculae, bright hot patches of concentrated magnetic flux.

We see the chromosphere that in Ha, blocking out the Photosphere’s overwhelming white light. The chromosphere is a much hotter, 2000 km thick layer, lying above the Photosphere. With temperatures rising to 17000 K, the chromosphere efficiently excites hydrogen to produce Ha emission.

The chromosphere shows a very different “landscape” than the photosphere:

• Spicules, tiny bright spikes, form a 3,000-10,000 km layer of bright fuzz on the Sun’s limb, and darker spikes on the solar disk. They are dark on the disk as they are cooler than the chromosphere below them. Few last more than 15 min, but the Sun has 100s of thousands of them at any one time.
• Fibrils are tiny low contrast darker filament-like structures.
• Dark Mottles, comprised of fibrils and spicules, blanket the entire disk.
• Field Transition Arches are groups of longer fibrils that join areas of opposite magnetic polarity.
• Prominences loop out from the limb: these are glowing, but cooler, hydrogen gas lifted from the Sun by magnetic fields. Prominences rise 100s of thousands of km above the hotter chromosphere.
• Filaments are the darker clouds that seem to float on the solar disk. Filaments are prominences, appearing darker because they are cooler and higher, extending above the hotter chromosphere below them.
• Plage (French for beach) are irregular, bright patches on the disk, found around active regions. They mark nearly vertical emerging or reconnecting magnetic fields and can last several days.
• Ellerman bombs (named for the astronomer who studied them) are tiny, brighter spots that fluctuate in brightness, associated with large plage.
• Flares show a brightening within a sunspot group, often with a “comb-like” flow.  They last from a few minutes to hours and change in both intensity and area as you watch.
• Sunspot umbrae are the dark cores of sunspots, much like what is seen in white light. However, sunspot penumbrae branch out into whirls consisting of fibrils and spicules.

A bonus, not in the Top 10, because it is very difficult to observe:

• Chromospheric Network is outlined by filigree, which are very tiny bright spots that are less than 1 arc-second in size, and best observed off-band of Ha.

As I did here, it is common to invert light and dark on the solar surface, which provides improved contrast for the solar disk, and a better brightness match to the fainter prominences. It also has the advantage that the otherwise dark filaments on the surface (which are prominences) are now bright, matching the bright prominences at the limb. The disadvantage is it can get confusing, since the prominences and spicules on the limb are not inverted, while the surface is.