22May2014 SHG images: 2nd installment.
- p_zetner
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22May2014 SHG images: 2nd installment.
More images from the 22May session.
1. H alpha (comparison with ChroTel telescope image).
2. H beta comparison with H alpha.
3. He D3 (comparison with ChroTel telescope He 1083nm image).
1. H alpha (comparison with ChroTel telescope image).
2. H beta comparison with H alpha.
3. He D3 (comparison with ChroTel telescope He 1083nm image).
Last edited by p_zetner on Mon Jun 09, 2014 5:10 pm, edited 2 times in total.
- marktownley
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Re: 22May2014 SHG images: 2nd installment.
These really are excellent Peter!
http://brierleyhillsolar.blogspot.co.uk/
Solar images, a collection of all the most up to date live solar data on the web, imaging & processing tutorials - please take a look!
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Re: 22May2014 SHG images: 2nd installment.
Looking really good there, Peter.
Nice work.
Stu.
Nice work.
Stu.
H-alpha, WL and Ca II K imaging kit for various image scales.
Fluxgate Magnetometers (1s and 150s Cadence).
Radio meteor detector.
More images at http://www.flickr.com/photos/solarcarbon60/
Fluxgate Magnetometers (1s and 150s Cadence).
Radio meteor detector.
More images at http://www.flickr.com/photos/solarcarbon60/
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Re: 22May2014 SHG images: 2nd installment.
Thanks, Stu and Wah.
Wah: The He D3 line is 587.6 nm. The absorption process in He is similar for the 587.6nm and 1083nm lines so the images should look similar (hence, the comparison with the ChroTel image). The lower (absorbing) level in both cases has an excitation energy around 21eV. These are very interesting absorptions and worth reading about. You should be able to see the D3 line in your instrument. I'd say a bandwidth of somewhere around 0.2A should be sufficient. As you've found, the on-disk He D3 absorption is extremely weak and basically, impossible to see. The trick is to take the on-band image and subtract or divide the nearby continuum. Strictly, division by the continuum is preferable but I've found this difficult to do! Subtraction gives me something to work with.
Cheers.
Peter.
Wah: The He D3 line is 587.6 nm. The absorption process in He is similar for the 587.6nm and 1083nm lines so the images should look similar (hence, the comparison with the ChroTel image). The lower (absorbing) level in both cases has an excitation energy around 21eV. These are very interesting absorptions and worth reading about. You should be able to see the D3 line in your instrument. I'd say a bandwidth of somewhere around 0.2A should be sufficient. As you've found, the on-disk He D3 absorption is extremely weak and basically, impossible to see. The trick is to take the on-band image and subtract or divide the nearby continuum. Strictly, division by the continuum is preferable but I've found this difficult to do! Subtraction gives me something to work with.
Cheers.
Peter.
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Re: 22May2014 SHG images: 2nd installment.
Hi Peter
wonderful results
wonderful results
Only stardust in the wind, some fine and some less fine scopes, filters and adapters as well. Switzerland 47 N, 9 E, in the heart of EUROPE
from 7 am - 7 pm http://www.nanosys.ch
from 7.01 pm - 6.59 am http://www.wastronomiko.com some times vice versa
from 7 am - 7 pm http://www.nanosys.ch
from 7.01 pm - 6.59 am http://www.wastronomiko.com some times vice versa
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Re: 22May2014 SHG images: 2nd installment.
Last pic from the 22May2014 session.
It's an image in the Mg "b" lines, presented as a median average of images made in the b1 (5184A), b2 (5173) and b4 (5167) lines.
Cheers.
Peter.
It's an image in the Mg "b" lines, presented as a median average of images made in the b1 (5184A), b2 (5173) and b4 (5167) lines.
Cheers.
Peter.
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- marktownley
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Re: 22May2014 SHG images: 2nd installment.
Cool addition!
http://brierleyhillsolar.blogspot.co.uk/
Solar images, a collection of all the most up to date live solar data on the web, imaging & processing tutorials - please take a look!
- fulvio.mete
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Re: 22May2014 SHG images: 2nd installment.
All beatiful images, Peter, but I'm very interested in the Helium I 5876 A one!
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Re: 22May2014 SHG images: 2nd installment.
Hi Fulvio.
Yes, I find the He D3 images very interesting as well. Apparently, the dark absorption features (correlated with the chromospheric plage) are never visible in coronal holes. The lower absorbing level of He D3 is produced by extreme ultraviolet radiation generated in the corona and passing downward, back to the surface.
You won't be able to see the absorption line on the solar disk in your instrument. You can calculate where it is relative to the Na D lines. You can also see this line in strong emission near the solar limb. As the Sun's limb sweeps into view of your spectrometer, the He D3 line will become, momentarily, quite bright. It's one way to locate the line.
Cheers.
Peter.
Yes, I find the He D3 images very interesting as well. Apparently, the dark absorption features (correlated with the chromospheric plage) are never visible in coronal holes. The lower absorbing level of He D3 is produced by extreme ultraviolet radiation generated in the corona and passing downward, back to the surface.
You won't be able to see the absorption line on the solar disk in your instrument. You can calculate where it is relative to the Na D lines. You can also see this line in strong emission near the solar limb. As the Sun's limb sweeps into view of your spectrometer, the He D3 line will become, momentarily, quite bright. It's one way to locate the line.
Cheers.
Peter.
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Re: 22May2014 SHG images: 2nd installment.
All good Peter .It would be interesting in all these wavelengths if you captured a large flaring region for comparison.Just have to hope you're in the right place when it happens.
Thanks Derek
Thanks Derek
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Re: 22May2014 SHG images: 2nd installment.
Absolutely, Derek!
There's a photo in Zirin's book of a flare taken in several wavelengths. Don't have the book with me at present, but remember being struck by the wavelength comparison.
Cheers.
Peter.
There's a photo in Zirin's book of a flare taken in several wavelengths. Don't have the book with me at present, but remember being struck by the wavelength comparison.
Cheers.
Peter.
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Re: 22May2014 SHG images: 2nd installment.
Yes, Peter. I know that, but till now I wasn'able to locate the He I line.Your suggestion to use the NaD lines as reference is very good.You won't be able to see the absorption line on the solar disk in your instrument. You can calculate where it is relative to the Na D lines. You can also see this line in strong emission near the solar limb. As the Sun's limb sweeps into view of your spectrometer, the He D3 line will become, momentarily, quite bright. It's one way to locate the line.
Cheers
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Re: 22May2014 SHG images: 2nd installment.
I also use Na line to find the HeD3, the line on solar edge is brightfulvio.mete wrote:Yes, Peter. I know that, but till now I wasn'able to locate the He I line.Your suggestion to use the NaD lines as reference is very good.You won't be able to see the absorption line on the solar disk in your instrument. You can calculate where it is relative to the Na D lines. You can also see this line in strong emission near the solar limb. As the Sun's limb sweeps into view of your spectrometer, the He D3 line will become, momentarily, quite bright. It's one way to locate the line.
Cheers
http://solarchat.natca.net/viewtopic.php?f=8&t=9829
But my SHG is not high resolution enough to get good surface details…