AAS 204th Meeting, June 2004
Session 56 Solar Active Regions and Coronal Heating
SPD Poster, Wednesday, June 2, 2004, 10:00am-7:00pm, Ballroom

[Previous] | [Session 56] | [Next]

[56.04] How does Background Subtraction Affect TRACE Loop Temperatures?

J.K. Roames, J.T. Schmelz, J.E. Beene (University of Memphis)

We have chosen a sample of 10 coronal loops that were visible in the 171 A and 195 A passband of TRACE, five on the limb and five on the disk. Our analysis was limited to 171/195 image observations taken when the instrument cycles through the different passbands during routine operations. The cycle takes only a few minutes, so each of these nonflaring structures did not appear to change significantly during the cycle. We chose between twenty to thirty pixels along each loop and background pixels to correspond with the loop pixels. Temperature analysis was done three different ways: (1) standard TRACE analysis of the loop pixels with no background subtraction;(2) constant background subtraction for each TRACE image; (3) pixel pair background subtraction. Each method produced a temperature estimate for the selected pixels. We are interested specifically in how these results may differ from he EIT loop temperature analysis that we have already completed. These results showed that background subtraction did not affect the EIT temperatures. EIT and TRACE have nearly identical temperature responses, but TRACE has high spatial resolution (0.5 arcsec pixels) compared with EIT (2.6 arcsec pixels). Does the higher spatial resolution change the results? Solar physics research at the University of Memphis is supported by NASA grants NAG5-9783 and NAG5-12096.

If you would like more information about this abstract, please follow the link to http://physics.memphis.edu/SOLAR. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.

[Previous] | [Session 56] | [Next]

Bulletin of the American Astronomical Society, 36 #2
© YEAR. The American Astronomical Soceity.