Weekly Report 18Feb2011 25Feb2011

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RHESSI Website Migration

The RHESSI Website Migration Project continued.

MESSENGER Data Analysis Project

Time series analysis was done on the 31Dec2007 flare using MESSENGER XRS data. Abundances were measured for various elements over the course of the flare.

The following shows the Iron-Nickel abundance as a function of time.

The Fe-Ni abundance as a function of time for the 31Dec2007 flare(XRS data)

The following shows the Calcium abundance as a function of time.

The Ca abundance as a function of time for the 31Dec2007 flare(XRS data)

The following shows the Sulfur abundance as a function of time.

The Sulfur abundance as a function of time for the 31Dec2007 flare(XRS data)

These abundances were measured using two vth_abun components. One component was used to fit the XRS data below 2 keV. All abundances for this component were held fixed. The second component fit the rest of the data above 2 keV. The abundances were allowed to vary in this component.

RHESSI Pixon Albedo Imaging Test

Calibrated eventlist files were created from maps consisting of a compact Gaussian source and an extended cosine cubed source. The total flux of the cosine cubed source was adjusted to different percentages of the total flux of the compact Gaussian source. Pixon and Clean images were made from each eventlist file. Using these images, plots were made of the flux as a function of the radial distance from the peak of the Gaussian source and the cosine cubed source.

The following plot shows the flux as a function of radial distance from the peak of Gaussian source and the cosine cubed source. The cosine cubed source is 50% of the total flux in the Gaussian source.

The flux as a function of radial distance from the peak of the compact Gaussian source and cosine cubed source.

There is a fall off of the compact Gaussian to approximately 2 arcsec, the Full Width Half Maximum of the Gaussian. The contribution of the cosine cubed source becomes apparent at this point.


The following plot shows the flux as a function of radial distance from the peak of Gaussian source and the cosine cubed source. The cosine cubed source is 75% of the total flux in the Gaussian source.

The flux as a function of radial distance from the peak of the compact Gaussian source and cosine cubed source.

Once again the the compact Gaussian source falls at it's FWHM of 2 arcsec. The contribution of the cosine cubed source is more pronounced in this case.


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