I have enough counts to make images for energy intervals 6-12 Kev, 12-25 Kev, and barley enough for 25-50 but I made an image for it anyways.

I mimicked Angela’s dissertation and did a RHESSI image for the beginning of the flare. 

June 16,2009



I continued to make corrected images and graphs of my flare.

I made an overlay of lower energy intervals over the foot point to show the movement of X ray flux.

Before the overlay I had to make RHESSI Images of each energy interval from 6-50 keV.
    




                Energy range: 6-12 keV



                          

             Energy range: 12-25 keV

                           

            Energy range: 25-50 keV

         
                           






The final product with the overlay of the four different energy levels including 30-100 keV.

The contour intervals are 90 and 70 percent of the max.


                                   








I made another spectrum graph from time 2:03:07 to 2:06 because
the original spectrum graph start at 2:03 and it was beginning an
attenuator change. The graph did not look as clear as this one below.

                         



                                    







I continued to work on the second half of the
 OSPEX tutorial.
As I was reading I realized how important the
spectral images are going to be for my research
and how this is going to be the challenging part of my project.
I learned that I needed to make another spectral graph
that included a wider range of time plus night time
up to 50-100 keV for background radiation. 

I continued to do the OSPEX tutorial and making notes of certain areas that were not clear to me so I was able to pick Angela’s brain.   She made the “Fit” part of the tutorial a little clear. Basically I will be playing with four different parameters to make a line that will best fit the spectral in 20-sec intervals.  Apparently the way you can tell if each component fits the line correctly is through a residual map which is a graph of the fit and the chi-square helps as well.
The different components are as follow:



Variable Thermal- optically thin thermal bremsstrahlung radiation function as differential spectrum seen at Earth units of photon per cm^2 s keV

2 Lines- Single Gaussian function (high) quality width in sigma


bpow-   Broken Power-law function with/without discontinuities in the derivatives.






I also realized I needed to make another spectral image with a higher range of energy.
Energy range- 3-300 keV

                              






I produced an imaged using the various components and a residual map but I’m not too sure if it is correct. Then I made the program loop through the time intervals starting from the one I was previously looking at.  By the end of the working day the program was still looping so I left it running over night.




                                             
                 

I was interested to see if the loop was finished since I never left a program running over night and to my surprise it was not finished. It finally finished and I was able to finish the tutorial. 

After I spoke to Angela I learned that I didn’t have to do any looping initially but now I know the procedure to do it.  We went over more details on how get a good fit of the spectrum. Unfortunately, the program was cutting of my spectrum curve in the smaller time intervals but after restarting the OSPEX GUI it proceeded to work and I was able to ask questions. I learned how to make smaller adjustment on the parameters of each component to get a decent fit for my curve.


For the time being I am to work on one time interval at a time to figure out the parameters. I know if I have a good fit by looking at the residual graph and the chi-square. The graph calculates the total components and the actual data to calculate the best fit.  When there is a good fit the line on the residual graph would have a maximum and minimum of 5 but it is centered at origin and goes across the x axis.  The chi-square value should be around one for a good fit. The residual map below had a chi-square value of 79 and I managed to lower its value to 64.39 (this mean it is a horrible fit). The fit map only has the thermal, line 1, line 2, and it is missing the broken power law component.










                         


















June 19, 2009







I went to an amazing lecture presented by Dana Longcope about the radiation zone and the convection zone. The lecture gave me more insight of how the sun is operating and creating a magnetic field.

I met with Angela and went over the spectrum graph I produced with the fit line and discussed the next step in the process.
  

         -Loop other time intervals:
            * with the thermal component only
            *with thermal and broken power law component
  
     - From the thermal component find the relationship between the energy and temperature using the
        Equipartition theorem- E= (3/2) *Kboltzman*T.

    -Use two thermal components without the broken power law after 2:05



Then Angela and I discussed my agenda for next week in her absence.
               -continue working on the spectrum graph with fit lines
               -continue working on the topology overlay
              - Look at the TRACE tutorial