Stephen St.Vincent - Swarthmore College
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This is the final version of the image for ApJ.
20 July 2005
Attempt number 3, with a different color scheme
Attempt number 2. This time I've only done a contour at lot(t)=7.
My first try at the image to go in ApJ. I'm not terribly happy with having two temperature contours; I think maybe just one at log(t)=7 would do fine.
Here's my first histogram from the beta cephei simulation. It's the emission measure vs time histogram, with no tilt and no temperature threshold.
Here's another emission measure vs time histogram. This time, the tilt angle is 45 degrees and the temperature threshold is 106.
19 July 2005
My magnetic field contours now rotate along with the star. This took a significant bit of trickery, but there it is, all done.
In addition, I made my equatorial magnetic field drawing routine work through rotation.
18 July 2005
This is an image of magnetic field lines that begin at regular intervals along the magnetic equator instead of at regular intervals on the surface of the star (see previous days' images for examples of those). While plotting the magnetic field lines this way is less informative about the overall structure of the star's magnetic field, it does provide interesting results: namely, closed field lines around the more dense areas of plasma.
15 July 2005
A balck-and-white at time=0 from the full simulation, showing the original magnetic field lines. Looks pretty much as expected.
I fixed my magnetic field contours. Turns out that I was negating both the x- and y-coordinates, which of course threw everything off. I only wanted to negate the x-coordinates, since that's what was missing from the original simulation data.
14 July 2005
This is my first attempt at plotting both halves of the star. I killed the run early, so not all of the contours were plotted. Still, it is obvious that the left side is not correct; it should be a mirror image of the right side, but isn't. In addition, the lines appear to always join together as they get farther from the star. I'll have a more in-depth look at this tomorrow and try to get it right.
This image is from d3grid.pro. At this point I've just ported the magnetic field contouring routine directly from zeuscontour.pro, so it's only capable of plotting one half of the star.
This is the first magnetic field contour that I've made with the new and improved routine. zeuscontour.pro made this lovely little image. As you can see, the overplotting now consists of field lines instead of lines of constant magnetic field strength, as desired.
13 July 2005
12 July 2005
I've added the threshold level to my EM vs Time plots so as to make them more directly informative.
11 July 2005
7 July 2005
Yet another double EM vs T histogram; this one is in color (obviously), and I've included dashed lines to indicate the value at t=0, or the value with no hot plasma.
An image showing emission measure vs time for &theta1 Ori C simulation. The solid line is without occultation, the dashed line is with occultation.
A plot of emission measure vs time for &theta1 Ori C created with d3t1oc.pro. There is no occultation present for this plot.
A plot of emission measure vs time for &theta1 Ori C created with d3t1oc.pro. There is occultation for this plot.
4 July 2005
Here is the VLOS histogram for an analytical distribution. The velocity dispersion statistics are included (top right). The calculated values are: line- center=0, line-width=0.288. Clearly, the values obtained by my program match the analytic values.
Here is another analytic distribution, this one of two delta-functions. Again, the analytic line-center is 0, and the analytic width is 0.5, so the numbers match up well once again.