It was mentioned that the latest Quark is designed to observe the Mg I (b2) absorption line in the solar spectrum.
http://daystarfilters.com/Quark/MgIQuark.shtml
This line is the middle of the Mg I Triplet at 5172.8A, the b1, b2, b3 etc. comes from Fraunhofer's recording of the more prominent lines in the early 1800.
https://www.wikiwand.com/en/Fraunhofer_lines
Mg I (b2) is in the green region of the solar spectrum.
http://fermi.jhuapl.edu/liege/s02_0002.html
The b2 line has extended wings with a deep core and the main line is <1.5A.
Should be an easy target in an SHG.
Mg (b2) absorption line
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Mg (b2) absorption line
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Re: Mg (b2) absorption line
Will be interesting to see the disks you get in Mg Ken. I purchased (and sent back) an Mg Quark a few years ago.
http://brierleyhillsolar.blogspot.co.uk/
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Re: Mg (b2) absorption line
Thanks for the info Ken, I look forward to the images
A quick question, how do you know which line you are imaging in?
Alexandra
A quick question, how do you know which line you are imaging in?
Alexandra
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Re: Mg (b2) absorption line
Alexandra,
The whole of the solar spectrum can accessed by rotating the diffraction grating. The higher the rotation angle the further into the Red and NIR, so you can have a marked “dial” showing the approximate wavelength after calibration.
This is the setup with the Sol’Ex. (https://i.ibb.co/YD8BFjn/IMG-5212.jpg)
Calibration means working your way through the solar spectrum and comparing the view (usually around 100-200A wide) to a reference solar spectrum. I use the BASS spectrum (https://bass2000.obspm.fr/solar_spect.php). Once you recognise the main Fraunhofer lines it’s pretty easy to home in on any nominated line/wavelength.
The whole of the solar spectrum can accessed by rotating the diffraction grating. The higher the rotation angle the further into the Red and NIR, so you can have a marked “dial” showing the approximate wavelength after calibration.
This is the setup with the Sol’Ex. (https://i.ibb.co/YD8BFjn/IMG-5212.jpg)
Calibration means working your way through the solar spectrum and comparing the view (usually around 100-200A wide) to a reference solar spectrum. I use the BASS spectrum (https://bass2000.obspm.fr/solar_spect.php). Once you recognise the main Fraunhofer lines it’s pretty easy to home in on any nominated line/wavelength.
"Astronomical Spectroscopy - The Final Frontier" - to boldly go where few amateurs have gone before
https://groups.io/g/astronomicalspectroscopy
http://astronomicalspectroscopy.com
"Astronomical Spectroscopy for Amateurs" and
"Imaging Sunlight - using a digital spectroheliograph" - Springer
https://groups.io/g/astronomicalspectroscopy
http://astronomicalspectroscopy.com
"Astronomical Spectroscopy for Amateurs" and
"Imaging Sunlight - using a digital spectroheliograph" - Springer