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EUV & X-ray Updates to FORWARD since our last meeting

EUV & X-ray Updates to FORWARD since our last meeting. Terry Kucera NASA/GSFC March 10, 2014. EUV & X-ray Imagers. AIA, XRT, EUVIA/B, TRACE, EIT If you want to add a new instrument you need to write a program like the ones in $FORWARD/OBSERVABLES/ for_calc _*_ response_grid.pro

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EUV & X-ray Updates to FORWARD since our last meeting

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  1. EUV & X-ray Updates to FORWARD since our last meeting Terry Kucera NASA/GSFC March 10, 2014

  2. EUV & X-ray Imagers AIA, XRT, EUVIA/B, TRACE, EIT If you want to add a new instrument you need to write a program like the ones in $FORWARD/OBSERVABLES/for_calc_*_response_grid.pro Which read in the pre-calculated spectra and convolve them with the instrumental response function.

  3. EUV and X-ray imager options ABUND: Can select abundance from following chianti options: • sun_coronal_1992_feldman_ext (default) • sun_coronal_2012_schmelz • sun_photospheric_2011_caffau or USERSPEC User supplied spectra files convolved with instrument response function. or PITEAM response (currently only for AIA)

  4. EUV Spectral Line Intensities Following suggestions of Enrico Landi and we have revamped how we do spectral lines. • Populations at different atomic levels are now pre-calculated for all ions. • User can select any line from 1-1410 Å. • User can select ioneq or abundance tables from chianti or their own files in the same format. • Still assumes thermal and ionization equilibrium, optically thin, collisionally dominated plasma.

  5. Automatic Line Blend Search • Blends automatically included by consulting the following line lists: T n_e 4.0 11 4.5 10 5.0 9 5.5 8 6 7 6.5 7 7 7 7.5 7 These are not used to calculate the actual intensities, just to estimate which lines might be present over a range of temperatures in the range Wavelength ± Lwidth/2 Would be easy to change

  6. Spectral Keywords • LINE : e.q., 'Fe12_195.12’ • IONEQ (default: chianti) • ABUND (default: Feldman 1992 extended) • LWIDTH (in Å) includelines for wavelength ± LWIDTH Default is instrument dependent • LLIM limit for blend inclusion (default 0.01) • CVERSION • INGOFNT – user specified G(n,T) file – bypasses all of the above. • OUTGOFNT – filename to save G(n,T) youused.

  7. FORWARD_DB • To implement these changes, especially the population files for the spectral lines we have now added a FORWARD_DB directory. • A $FORWARD_DB system variable must be defined just as $FORWARD is.

  8. Future The collisional spectral line calculations can be expanded to include scattering, which would be useful for visible band lines.

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