View Full Version : Solar Spectroscopy - Lines needed

2005-Jul-09, 03:43 PM
I am requesting info on Fraunhoffer lines and lines (i.e. sentences) useable in a seminar presentation, probably.

A university of peculiar forsight has asked me to do a seminar. Yikes! Fact is stranger than fiction. In my case, my facts are stranger than physics. :-? :roll: I need to correct this.

Therefore, please adopt me into your cyber classroom, hereby established (this thread). I humbly request nourishment in Zeeman Anomalies, absorption/emission lines, limb red & blueshifts, optic depths, nucleosynthesis, spectroscopy history, SOHO and all other solar space scopes, terrestial solar sites, etc.

Maybe I should start with some requests....

Are the number of known solar elements 83 now?

By comparing sunspot spectroscopy with photosphere spectroscopy, the Zeeman lines are apparent. Where can I go to get images of this? Do they vary with sunspot size? Do flares produce more lines?

Can I simply use any image off the internet for a simple seminar presentation? If so, I presume I must, or should, reference the source somehow. What is taboo to copy for a non-income seminar presentation?

It's been too long since I was in college. What level do I need to be to advance them? If you are in physics, what would you lilke to learn on this topic. #-o

I hope to visit the physicists in charge of this soon. Near as I can tell, they are still interested in my colorful work, so I have a green light so far. :)

I do plan to demonstrate the SPACC (http://www.badastronomy.com/phpBB/viewtopic.php?p=479663#479663). This will cut-down on my speech time (thank goodness). But, what if it rains? :o

2005-Jul-09, 03:48 PM
Hey! Quit laughin'! :P

Manchurian Taikonaut
2005-Jul-09, 05:19 PM
a bit on the Zeeman effect


2005-Jul-09, 06:46 PM
a bit on the Zeeman effect
Thanks greatly!

1) http://aanda.u-strasbg.fr:2002/papers/aa/full/2001/46/aadi072/node2.html
Can this knowledge be transitioned to a ground state, let's call it - "georgeeze"? :roll: :)
Is the mag. field increasing the spin of the electrons into modified transition states, which alter their absorption wavelength?

Are the new changes in wavelength for the absorption regions linear across the visible spectrum? In other words, will Fe and H lnes also vary by the same percentage as the OH? I suspect not.

Is there a simple explanation in the difference between electronic spin and angular momenta of the electron cloud?


Then, in August of 1886, Dutch physicist Pieter Zeeman observed the spectrum from a sodium flame which had been placed between magnets. Remarkably, the emission lines were broadened or split into two or three lines.
Nice link! Was he just fiddlin' around like me and the SPACC - curious "like a cat" [Don't call me "whiskers". I am still laughing at the BA's Slacker Astronomy visit. Hillarious! :) ]


Cooler means darker! Brightness, or flux, is given by F=sigma*T4. This is the Boltzman equation, and F is the flux, sigma is the Stephan-Boltzman constant, and T is temperature. The strong dependence on temperature is why the spot looks dim in comparison to the surrounding surface; even a small change in temperature can have a significant affect on the brightness. Don't be fooled, though: if isolated, a large spot as seen from Earth would be a brilliant orange pinpoint whose total brightness would be comparable to that of the full moon!

I have wondered about this. If I am fortunate enough to determine the sun's intrinsic color, what color do I make the sunspots? Since they would be seen as dark, I plan to leave them as they appear as normally known. Yet, I could alter the mask to match their spectral irradiance and "see" if indeed they would look orange if observed independently from the rest of the surface.

The APOD illustration is wonderful.

I am curious if entropy plays much of a roll in the temperature differential due to organization by the mag. field.