Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.1715b&link_type=abstract
American Astronomical Society, HEAD meeting #11, #17.15; Bulletin of the American Astronomical Society, Vol. 41, p.685
Astronomy and Astrophysics
Astrophysics
Scientific paper
A determination of the differential emission measure (DEM) is a prerequisite for describing the temperature structure of stellar coronae. It relies on fitting the observed spectral emission with output from spectral modeling calculations and is highly sensitive to the accuracy of underlying calculations of the ionization equilibrium as a function of temperature. Measurements of coronal temperatures that do not invoke assumptions associated with the calculations of ionization equilibria are highly desirable but generally have not been applicable to Chandra grating spectrometer observations. The most reliable way to spectroscopically determine the electron temperature is to measure the strength of dielectronic recombination (DR) satellite lines relative to the associated resonance line, IDR/Ir. We have applied this method to the Fe XVII lines, which are very bright in the Capella spectrum. In particular, we have determined the intensity of the DR lines next to and under lines 3C and 3D. The atomic data (radiative and autoionization rates) needed to do this will be supplied by the publically available Flexible Atomic Code; energy levels are available from astrophysical observations and laboratory measurements. The temperature TDR we have derived from this method will be compared with TDEM for Fe XVII. The comparison provides a much needed test of the accuracy of the charge fraction calculations underlying TDEM.
This work was supported by NASA through Chandra Cycle 10 Award AR9-0002X.
Beiersdorfer Peter
Desai Prasun
Gu Min Feng
Lepson Jaan
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