Seems like a few of us actually managed to get some solar time on the 10th.
Some great images have already been uploaded. Well done to all.
Have some CaK, White light and DS Ha images. The seeing was better than usual!
AR 2770 showing evidence of breaking up. The main spot of a few days ago (which was showing the beginnings of a light bridge) has now split and both components are showing light bridge which may infer further splits. There's also evidence of some smaller "spots" north of the pair.
A nice filament is on show, and a couple of reasonably impressive proms.
Enjoy
I took a series of DS Ha images of AR2770 with the CWL (central wavelength) moving from the red wing to the blue wing and then onto the local continuum.
These may assist other imagers to determine the tuning of their Ha filter relative to the Ha centreline.
Glad to see that you got some sunny breaks, nice set of images. Makes a nice comparison seeing Cak, Ha and white light images of the same areas.
Still getting my head around what the tuning of the Etalon actually does, need to do a lot more reading I think.
Jeff, et al,
Tuning the conventional H alpha filters unfortunately is not well explained in the “manuals”. We have tilt tuned etalons and pressure tuned etalons, temperature tuning (Quark) different tuning “mechanism” which give different outcomes.
The bandwidth of the filter doesn’t change with the tuning.
The tuning moves the centreline (H alpha plus or minus some Angstrom) and allows us to observe solar features in and around the H alpha wavelength.
The issue, is knowing which way the “tuning” is moving and by how much.
With tilt etalon, the more the tilt the more the wavelength moves towards the blue.
With pressure tuning, the higher the tuning pressure the wavelength moves towards the red.
With the temperature tuning, the higher the temperature, the wavelength moves towards the blue.
Unfortunately it’s very (very) difficult to quantify the change in wavelength with the pretty coarse tuning mechanisms. (It’s much easier and far more accurate when you use a Spectroheliograph)
Obviously the details recorded in and around an H alpha feature will vary with wavelength. Activity like Ellerman bombs really needs access to the H alpha wings.
Practice, practice, practice......
