To Do List
My reminders for daily/weekly tasks to accomplish
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• Finish presentation about how many time steps we need for time-dependent simulations
Try different initial conditions (starting level populations) and see if results change
Add plots of the CV fraction
Show ionization state fractions and spectra at 50 μs, since this is around the time of reconnection (what we care about)
Look at line strength ratios at 50 μs
• Compare time-dependent and time-independent runs
Figure out a way to quantify how different the two sets of runs are (what matters is differences at late times, i.e. 50 μs)
• Do simulations with CV included
Look at the line at 97 nm (find out whether its a CIII or CV line)
• Try a non-constant temperature profile (Doc suggested having the electrons cool from 30 eV to 15 eV during the 20
μs that the plasma is expanding--PrismSPECT plasma temperature means electron temperature for us)
Maybe try different densities as well (SSX plasma density is still somewhat uncertain because particles come out of the walls, etc.)
• Take new data with VUV monochromator--measure strength of 97.7 nm, 155 nm, and 229.7 nm lines
Work on code for post-processing data (integrate over spikes in voltage, subtract baseline, find point of strongest emission)
Present results for group meeting Monday
Modify code to process SXR data and calculate filter ratios
• Begin working on SXR modeling
Goal is to create a routine that allows one to calculate plasma temperature from the observed filter ratios
Write an IDL code that synthesizes signal levels in each of the four SXR channels and then compares the simulated spectra to SXR data (should channels with a strong signal be counted more in determining a best-fit temperature?)
Determine best-fit by minimizing the chi square statistic
Write out an algorithm in plain English, then figure out what variables I need, then start implementing the code (use lots of functions)
Start by running time-dependent simulations with basically constant temperatures, and then try simulations with varying temperature (e.g. a spike in T right after reconnection)
Get a new data set from Chris where all 4 filters have strong signals
Be careful with unit conversions between emissivity (simulations) and amperes (data) (talk to Chris if necessary)
• Try PrismSPECT simulations with lower densities to see if the time taken to reach equilibrium scales as we would expect
• Modify excitation time calculation according to David and Chris's suggestions.
• Calculate dependence of 97.7 nm / 155 nm line ratio on temperature using a PrismSPECT steady-state simulation
• Modify my 229.7 nm line anamoly presentation and send it to Joe McFarlane
• Talk to Peter about honors meeting that I missed
• Work on glossary of terms
• Read Abram Falk's thesis
• Read PrismSPECT documentation and figure out how the time scales for collisions and de-excitations are calculated
• Ask Doc and Chris for suggestions about papers I should read
• Process SSX interferometer data using code from Chris
• Write up description of my SXR unit conversion for my thesis
• Process SXR data and calculate temperatures with the tin filter left out and see if it makes sense
• Make final changes to APS-DPP abstract and submit it
• Post evidence on my results page that my PrismSPECT SXR ratios are correct
• Make powerpoint detailing the differences between spectra units in the zero-width and planar PrismSPECT simulations
• Look for papers that talk about the spectral lines we're looking at (229.7 nm in particular) (look for papers that cite Turner paper)
• Figure out how detailed my atomic models need to be
• Try PrismSPECT simulations with additional impurity elements (nitrogen alone, N+C+O, He, metals...)
Calculate total power emitted in the form of radiation (SSX has 1 kJ of energy lost over 1e-4 s, so ~10 MW)
Use "frequency integrated power in band" tool in PrismSPECT line intensity viewer
• Process SXR data from week of July 10-14 and see if filter ratios make sense
• Take new VUV monochromator data
  Do 25 shots looking at 97 nm and 155 nm lines for both single spheromak and counter-helicity
  Take some shots looking at NIV 76.5 nm, NV 123.9 nm, OIV ~55.4 nm (4 lines), OV 63.0 nm, OIV 79 nm (2 lines), and OVI ~103.5 nm (2 lines)
  Make sure to take at least one baseline shot with the entrance slit closed
  Run interferometer to get precise densities for all the shots
• Use the 97.7 nm / 155 nm line ratio to calculate the temperature evolution over an SSX shot--see if I get something plausible
  Add plots of line ratios to the plot of T vs. t
  Calculate error range using standard deviations and add propogated error to T plot
• Make plot of VUV monochromator calibration
• Recalculate error on TfromVUV calculation using formal error propogation
• Process SXR lollipop data from August 1
• Email Joe MacFarlane with details about the ionization state fraction viewer problem we found
• Write 1-2 page summer research summary
• Send ionization state fraction density dependence presentation to Joe MacFarlane
• Finish thesis intro
• Write thesis section about excitation kinematics
• Use Saurav's thesis as a template to start putting together an outline for mine in Latex (figures, tables, etc.)
Work on intro and theory sections