Montana State University Solar REU Program 2010
Dustin Hickey
Home Log

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Friday, June 25

When looking at March 27, 2002 I saw that there once again was an area of interest around 360. I did the same thing that I did for March 4. It is interesting to compare these two maps since they are almost a full rotation of the sun apart.

Thursday, June 24

I continued doing the same type of thing today that I was doing yesterday. I looked at times around January 2, 1998 and I also looked at March 2002. I also changed the program and started creating save files of the magnetic field data. It takes a long time to run the magnetic field program so by running it once and creating a save file I was able to save time when looking at different coronal holes wihtin a sun's rotation.

The image below is shifted over because the interesting part is right at 360. I had to rework the program and rerun the magnetic field program in order to produce it, which takes a little while.

Wednesday, June 23

I started today by looking at the different times around the August 15, 2001 date that I had been looking at. The magnetic data is the same during a rotation of the sun so my idea was to compare the different coronal hole data for the same magnetic data. I have provided on here a couple of different examples of some of the plots I made. I went in increments of two days in order to look at them.

Next I looked at a full rotation of the sun during early October 2001. Below are some plots comparing times during the rotation.

Tuesday, June 22

I continued working to integrate the magnetic field programs into the coronal hole program. I was able to successfully integrate them. I then had to adjsut some things in order to create plots that are easier to look at, as in it is easy to see what is going on in them. Below I have an example of a low resolution carrington map of the magnetic field lines.

This is the low resolution image that was used to create the plot from yesterday. The white lines are the magnetic field lines. The areas where there are no field lines are where there are open magnetic field lines, ones that go out from the sun and don't loop back. The pixelation of the background is a good indicator of the low resolution of this image. When I run the program it makes contour lines of the open field regions. Below I have a higher resolution map that is taken from data around August 15.

There are more field lines in this image and looking at the background it can be seen that it is less pixelated. The area where there is an open field is also more obvious in this image. I used this resolution to produce maps of the open field regions with coronal holes plotted on top. Today I did that for three dates that I have been looking at. Below I have the same map that I tried to create yesterday but now it is much better.

The gray areas in the background are the areas of open magnetic field as determined by Dana's program. The coronal holes at the south pole overlap with the open field regions but the rest of the holes don't. Below I have the same type of map for August 15, 2001.

Again there is some overlap between the open fields and the coronal holes but they don't always coincide. The same is also true for the map below which is from January 2, 1998.

Monday, June 21

Today I started working with magnetic data. Dana Longcope showed me how to use his programs that model magnetic field lines. I spent most of today working with the programs and playing around with them in order to figure out how to use them with my programs. As I started to figure them out I then started to rework my coronal hole program in order to combine it with the magnetic field data. Below is an early version of what I am trying to create.

The light yellow lines that are separate from the rest of the colors are supposed to be the contour lines of open magnetic field lines on the sun. This graph is just an early step on my way to producing graphs that will be useful. There are open field areas that are missing and the colors aren't what I would like. I also have the ability to determine the resolution of the magnetic field lines. The higher the resolution, the longer the program takes to run. This plot was produced using low resolution in order to save time as I figure things out.