Michael Mozina
Banned
- Joined
- Feb 10, 2009
- Messages
- 9,361
Actually RC, the RD image disk diameter makes or breaks both models. Only one is left standing, and I know for a fact it won't be the standard solar model. I've seen the light.
Actually Michael Mozina, the RD image disk diameter makes or breaks both models. Only one is left standing, and I know for a fact it won't be the Michael Mozina fantasy*. I've seen the basic physics thgat Michael Mozina is ignorant of.Actually RC, the RD image disk diameter makes or breaks both models. Only one is left standing, and I know for a fact it won't be the standard solar model. I've seen the light.
) and predicts absolutely nothing just makes it a joke. See the over 60 questions that Michael Mozina is incapable of answering.I've seen the light.
Read it again. It'll come to you.Actually his answer does seem to set minimum and maximum parameters and that seems to be a start.
Running difference images made from the color separated pairs of images above wouldn't show much contrast because the source images are only 10 frames apart. But with a 100 frame offset the running difference images would be what you see in any single frame from the videos below.
This first video was made by removing the green and blue from the source video leaving just the red. Then all the red was converted to grayscale. Then two frames are taken from the video 100 frames apart starting with frames 1 and 100. Then 50% gray is added to each pixel in the first image, and the second image is subtracted pixel by pixel from the first. The result becomes frame 1 in the output. Then move to frame 2 and frame 102 and repeat with all frame X and frame X+100... (These pixel values are numerical values of gray from 0 = black to 255 = white.)
Then of course these videos are sized down to 640x320 and letterboxed to 640x480 to make them fit YouTube and common video viewers. And I trimmed them down to just the first 20 seconds to make more reasonable download sizes.
The second video, above, is the same only I took out the red and the blue, leaving only the green from the original video. And the third, below, is the running difference video made from just the blue. I believe these red, green, and blue colors represent 211Å, 193Å, and 171Å source data respectively.
I use a proprietary script I wrote myself to do this processing, so I won't be more specific. Anyone with a little math background, a modicum of expertise in computer video and graphics, and some reasonable programming skills could certainly do this.
This is a very important point for this discussion. Although the running difference material we find at NASA and LMSAL probably is made pretty much exactly the way I've done it, they can look quite different by adjusting only a couple of things.
First, if you subtract frame x+1 from frame x+100 you get the videos we see above. If you instead subtract frame x+100 from frame x+1 you end up with something that looks like a negative of that video. Either the lighting comes from the other side of the mountain or your mountain turns into a valley. Take your pick.
Second, the contrast between images will obviously be affected by the offset, or how many frames apart you use for the compared images. And you need to remember that is based on the time difference between the original frames, too. A running difference video made with an offset of 10 frames might show so little change that it would look almost like a smooth gray throughout. Compare images 100 frames apart and you can see the changes between source images more clearly. You can shrink and grow your mountains by comparing frames closer or further apart in the sequence.
Many of the running difference images available from NASA and LMSAL have quite different sizes of mountains, some so huge that it's amazing we don't see them with the naked eye when there's a solar eclipse!![]()
Those are all different wavelengths emitted particularly strongly by ultrahot iron at different temperatures. 171 is particularly strong from 600,000K iron, 193 picks up two lines (one characteristic of 1,200,000K and one of 5,000,000K) and 211 picks up 2,000,000K. At any high enough temperature, all of these lines will be emitted, but the balance between them shifts in the way I said.
The orange? If you ovelaid a visible-light image of the Sun on this, those "orange" areas are above the surface. That's the corona. At the place it meets the green edge, there's about ONE PIXEL worth---a few hundred km in projection---of either lightening of the orange or darkening of the green or both---which is entirely buried in the JPEG artifacts. Is that what you think is "limb darkening", Michael? That one sometimes-darker row of pixels? Good heavens.
If that one row of pixels were to mean something (for example, if it's still there in a FITs image, and if it's wider than the telescope PSF), it's a perfectly normal standard model meaning. That's what you expect if there's a layer ~400km thick, above the green emitter and below the orange emitter, which emits neither green nor orange. Or alternatively it's what you expect if there's an extremely optically-thin layer (O = 0.001 or so) above the green emitter which is able to absorb the green light when it's in extreme projection.
Is that one row of pixels the exciting one, Michael?
About that "transparent layer" in the SDO picture . . . I got to thinking about what such a thing would look like, and it seemed to me that the bottom of the band should look different from the top of the band. After all we're looking through far more gas at the bottom of the green band than at the top of the green band.
So I threw together a little code to model the sun as a series of nested spherical shells with various opacities and emissivities, jiggled the numbers to get something vaguely like the SDO image, and I got a significant brightness gradient (2nd image). I'm not seeing any such gradient in the SDO image (1st image), and the only reason the gradient isn't stronger in my model is that I assumed a uniform density within each layer.
So, if we're looking through a nearly transparent layer at the limb in the SDO image, why isn't there a gradient?
There are mass flows (coronal loops) flowing all along the surface. It's *highly* electrically active. Those jagged areas are mass flows related to either coronal loops or twister like formations that form in the atmosphere.
Is there anyone that disagrees with the minimums and maximums that I have outlined related to diameter of the disk in the RD images?
Is GM prepared to commit his hair yet on anything with a number attached?
Ok, that is *finally* a quantified prediction and we can clearly tell the difference between standard theory and a Birkeland model. I appreciate you efforts Mr. Spock. You're redeemed.![]()
Ok, so can we at least agree on some minimum and maximum parameters to falsify both solar models?
I will accept that the maximum RD disk size in my solar model can be no larger the bottom of the chromosphere with a minimum size of the core (0), likewise the minimum distances related to the standard model should be the chromosphere with a maximum of infinity. These are the minimum and maximum of each models. Does anyone disagree?
Speak up now if you disagree.
Ok, so can we at least agree on some minimum and maximum parameters to falsify both solar models?
I will accept that the maximum RD disk size in my solar model can be no larger the bottom of the chromosphere with a minimum size of the core (0), likewise the minimum distances related to the standard model should be the chromosphere with a maximum of infinity. These are the minimum and maximum of each models. Does anyone disagree?
Speak up now if you disagree.
Under? What's this "under"? It's a 2-D photo. Either you're seeing it closer to the center of the photo, or closer to the edge. Please stick to that terminology---"under" is your intuitive interpretation which you haven't been able to justify at all---in part because your descriptions are maddeningly unclear, mixing bits of observable ("green") with bits of your guesswork ("under", "through") in a totally hashwork way.
Fix it. Here's an ASCII art cartoon of a SIDE VIEW of a simple opaque Sun with a green blob hovering in front of it. I've labeled (with letters) a bunch of lines-of-sight for an observer looking down at and past the limb. You can follow any given line of sight and figure out what the observer sees in that pixel. This is possible both for opaque features and transparent ones---I put in an example "g" to show. Then I gave you an ASCII "stem plot" where you can list what's in line-of-sight a, what's in line-of-sight b, what's in line-of-sight j, etc.
Please edit it to represent what YOU think the 3D structure is, and show how you think that 3D structure projects along the lines-of-sight. Replace the opaque 0s with "f" or "n" to represent iron or neon, for example.
Code:observer is up here lines of sight, looking down. |||||||||| abcdefghij This is a cartoon of a simple opaque sphere. The 0s are "opaque photospheric material". The "g" for example is a blob of transparent corona. 0 g What do we see along the lines of sight a-h? 000 g a: 0 0000 g b: 0 00000 c: 0 000000 d: 0 000000 e: 0 <- when you look at an opaque sphere you 0000000 f: 0 see the same thing right out to the edge. 0000000 g: 0+g <- when you're looking through the green blob 0000000 h: 0+g you see green + whatever's behind it. 00000000 i: b+g 00000000 j: b <- past the edge all you see is the background 00000000 which is "b" for black. 00000000 00000000 00000000 0000000 0000000 0000000 000000 000000 00000 0000 000 0 bbbbbbbbbbbb background is black bbbbbbbbbbbb bbbbbbbbbbbb
First, you haven't defined what you mean by "RD disk size".