Thermal and Nonthermal Contributions to the Solar Flare X-ray Flux

 

B. R. Dennisa, K. J. H. Phillipsb, J. Sylwesterc, B. Sylwesterc, R. A. Schwartzd, and K. A. Tolbertd

 

 

aLaboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Code 682, Greenbelt, MD 20771, USA

bNational Research Council Senior Research Associate, NASA Goddard Space Flight Center, Code 682, Greenbelt, MD 20771, USA

cSpace Research Centre, Polish Academy of Sciences,ul. Kopernika 11, PL-51-622 Wroclaw, Poland

dSSAI, NASA Goddard Space Flight Center, Code 682, Greenbelt, MD 20771, USA

Abstract

The relative thermal and nonthermal contributions to the total energy budget of a solar flare are being determined through analysis of RHESSI X-ray imaging and spectral observations in the energy range from ~ 5 to ~ 50 keV. With its ~ 1-keV spectral resolution, intensities and equivalent widths of two line complexes, the Fe line group at 6.7 keV (mostly due to Fe  XXV lines and Fe  XXIV satellites) and the Fe/Ni line group at 8 keV (mostly due to higher-excitation Fe  XXV lines and Ni  XXVII lines) can be obtained as a function of time through a number of flares. With line and continuum intensities from the CHIANTI code, the thermal component of the flare emission can be more reliably separated from the nonthermal. The abundance of Fe can also be determined from RHESSI spectra. Comparisons of RHESSI spectra with those from the RESIK crystal spectrometer on CORONAS-F show very satisfactory agreement, giving much confidence in the intensity calibration of both instruments.

Key words: Sun, X-ray, spectra

1  Introduction

The RHESSI mission has been operating successfully since its launch on 2002 February 5, and has observed many thousands of solar flares. The instrument , which has been described by Lin et al. (2002), has nine cooled germanium detectors which enable flare spectra and images by modulation collimators to be obtained from the soft X-ray region (3 or 4 keV) to gamma-rays (17 GeV). Its relatively high resolution, ~ 1 keV at energies less than 20 keV, enable line features in the spectrum at 6.7 keV (Fe line feature) and 8.0 keV (Fe/Ni line feature) to be observed. These line features are on a flare continuum which, at the flare impulsive stage, consists of a nonthermal component with relatively flat energy dependence and a thermal component with steeper spectrum.

This paper is concerned with analysis of flare spectra in the energy range ~ 2 -20 keV, which has been observed by both RHESSI and the RESIK crystal spectrometer on the Russian CORONAS-F spacecraft. The 2-20 keV range is of great interest since it is where the nonthermal component begins to be evident over the thermal component. We report on attempts to derive parameters for the thermal component as well as the absolute abundance of Fe in the flare plasma from line emission during a flare on 2003 April 26.

2  Theoretical X-ray Spectra in the 3.8 keV - 10 keV Range

We first briefly describe line and continuum emission from thermal solar flare plasmas in the range 3.8 keV - 10 keV. More details are given by Phillips (2004). The emission has been calculated for solar plasmas by Mewe et al.(1985) (MEKAL code) and Dere et al. (1997) (CHIANTI code). In analyzing RHESSI spectral data, we have used both codes, though most of the illustrations here are from CHIANTI. In the RHESSI range, the thermal spectrum consists of free-free and free-bound continua and two line features at 6.7 keV and 8 keV that, for flare temperatures 20 MK, are made up of He-like Fe (Fe  XXV) lines (transitions 1s2 - 1snl, n 2, l=s, p etc.) and Fe  XXIV dielectronic satellites. At higher temperatures, Fe  XXVI and Ni  XXVII lines contribute to both features. Illustrations of theoretical spectra in the 1 keV - 12 keV range at various temperatures are given in Figure .

 

Figure 1: CHIANTI X-ray line and continuum spectra for temperatures indicated. Solid lines: spectral resolution (FWHM) 0.05 keV; dashed lines: FWHM 0.8 keV. Coronal abundances (Feldman & Laming 2000) and ion fractions of Mazzotta et al.(1998) are assumed.

With RHESSI's spectral resolution, individual lines, in particular the Fe  XXIV satellite structure at 6.6 - 6.7 keV, cannot be resolved. However, because the lines are all due to Fe and have a known dependence on temperature, and, as the continuum is well observed by RHESSI, we can find the Fe/H abundance. Spectral fits to the thermal spectrum, defined by the continuum slope and intensity, give temperature T and volume emission measure (Ne = electron density, V= emitting volume), which can be easily found, assuming an isothermal plasma. Other spectral fits, involving a multi-thermal plasma (i.e. two or more values of T) or a temperature distribution have been applied elsewhere in our analyses.

A convenient way of expressing the intensity of the two RHESSI line features is through the equivalent width (energy width of a portion of the continuum at the line's energy with flux equal to that of the line feature). The variation of equivalent width with T is given in Figure  (solid line) based on CHIANTI. There is a fast rise of equivalent width with T for T 16 MK.

 

Figure 2: Equivalent width (keV) of the Fe line feature plotted against T (smooth curve) as calculated from CHIANTI (assuming coronal abundances and Mazzotta et al. (1998) ion fractions). Observed RHESSI values in attenuator states A0, A1, and A3, for the flare of 2003 April 26 are shown as points connected by lines (see legend for line styles and plotting symbols).

3  RHESSI Observations

We illustrate our RHESSI flare thermal spectral analyses in the 4 keV - 10 keV range with observations made during an M2 flare with maximum at 03:08 UT on 2003 April 26. This flare was also observed by the RESIK instrument on CORONAS-F. There were several changes in the RHESSI attenuator state (see Smith et al. 2002), from A0 (no attenuator) to A1 (thin attenuator) to A3 (thick attenuator) and the reverse sequence.

 

Figure 3: RHESSI X-ray spectrum (thick black histogram) in A3 attenuator state near the peak of the flare on 2003 April 26, integrated over 03:07:44 - 03:09:24 U.T. This was fitted with a two-component thermal spectrum (T1 = 29.4 MK, T2=11.5 MK) and a nonthermal component with power-law energy dependence (grey histograms). Three line features were added with Gaussian profiles having centroid energies 6.70 keV, 8.36 keV, and 10.30 keV, identifiable with the Fe line and Fe/Ni line features and an instrumental feature.

RHESSI spectra were fitted with the RHESSI analysis software over the energy range 3-100 keV. In our investigations, we sometimes used the spectral output from individual detectors, while for some purposes data from seven of the nine detectors summed were more appropriate: in such cases, data from detectors 2 and 7, which have poorer spectral resolution, were omitted. A first-guess spectrum with appropriate parameters found from previous analysis was folded through the RHESSI spectral response matrix for each attenuator state, having subtracted a background spectrum.

The low-energy ( ~ 3 keV - 20 keV) part of the spectrum could generally be fitted during the A0 and A1 attenuator states with a thermal continuum and three line features with Gaussian profiles having a single value of T and EM. For higher-intensity spectra, the addition of a continuum with power-law dependence on energy E was found necessary to fit the spectrum at energies above ~ 30 keV. An iterative process was used to refine the parameters of the first-guess spectrum, minimizing the value of . This procedure is adequate for spectra in the A0 and A1 attenuator states, but less so for A3 spectra, which are better fitted with two-component thermal continua: see Figure 3. Two of the three line features can be identified with the flare Fe line feature (energy ~ 6.7 keV) and Fe/Ni line feature (energy ~ 8 keV), and the third with an instrumental (Ge) line. Parameters from the final iteration describing the two thermal components of the continuum and the nonthermal continuum are given in the Figure. The fit to the observed spectrum over the 3 keV - 100 keV range gave = 0.84, and can be regarded as satisfactory.

With observed fluxes of the continuum and Fe and Fe/Ni line features, the line equivalent widths can be evaluated (points in Figure 2) and the agreement with the theoretical curve examined. For observations in the A1 attenuator states, on the rise and decline of the flare, the observed equivalent widths of the Fe line feature approximately follow the theoretical curve, giving support for a coronal abundance of Fe in the flare plasma. However, the observed equivalent widths from the A3 attenuator state, analyzed with single-temperature fits (i.e. not the two-component fit as in Figure 3) vary widely, much more than is predicted by CHIANTI. This apparent discrepancy has been encountered in the analysis of several other spectra. The presence of a multi-thermal or two-component emission measure spectrum is likely to contribute to this discrepancy, but other possible explanations for this are also under investigation.

4  RESIK Observations and their Comparison with RHESSI

RESIK is a high-resolution crystal spectrometer (Sylwester et al., 2004) operating in the energy range 2.04 keV - 3.68 keV (3.37 Ǻ - 6.09 Ǻ) on the Russian CORONAS-F spacecraft launched on 2001 July 31. RESIK's spectral range includes diagnostically important lines of Ar, S, and Si ions, as well as `trace' elements (K and Cl). Unlike many previous crystal spectrometers, it observes the continuum in solar flares with a background that is negligible for two of its channels (that in the other 2 channels can be accounted for in analysis software). Normally, RESIK operates in first order Bragg diffraction, but by changing the instrument's gain, third-order spectra (with wavelength ranges one-third their first-order ranges) can be obtained. The instrument has been precisely calibrated, with 20% uncertainties at most in the measured fluxes, making RESIK spectra suitable for comparison with those from RHESSI.

RESIK observed a number of flares in 2002 and 2003 for which there are RHESSI observations. During the 2003 April 26 flare, RESIK was in third-order diffraction mode for a short interval near the event peak (03:03 U.T. - 03:05 UT), but in first-order mode at other times. Figure  shows RESIK (all four channels) and RHESSI spectra at 03:00 UT (RHESSI in A0 attenuator state). The RHESSI spectra show a thermal continuum, with the Fe line (6.7 keV) and Fe/Ni (8.0 keV) line features while the RESIK spectra show He-like Ar (3.1 keV) and He-like and H-like Si (2.4 keV) lines. The RESIK continuum agrees with the RHESSI spectrum at around 3.5 keV to within about 20%, within the expected intensity calibration uncertainties of RESIK. The agreement between two quite different instruments is very gratifying, and adds to our confidence in the calibration of both instruments.

 

Figure 4: Observed X-ray spectra for a time (03:00 U.T.) just preceding the main flare on 2003 April 26. RESIK spectra (four channels) cover 2.0 keV - 3.7 keV and include lines and continuum. Spectrum above 3 keV (histogram) is from RHESSI detector 4 (A0 attenuator) and shows the Fe line and Fe/Ni line features. The best-fit thermal spectral parameters for this spectrum are Te = 18.6 MK, EM = 2.1 1047 cm-3.

The Fe line was observed by RESIK in third-order diffraction when RHESSI was in its A1 attenuator state. The RHESSI spectrum gives the line flux as 7.83 104 photons cm-2 s-1, while RESIK spectra integrated over the same interval gives nearly the same flux: 8.22104 photons cm-2 s-1.

5  Conclusions and Summary

Observations of several flares, including the one discussed in detail here, suggest that RHESSI can measure equivalent widths of the Fe line to an accuracy that allows a preliminary estimate to be made of the abundance of Fe: this is close to the coronal value (1.2610-4). There is good agreement - within about 20% - of RHESSI spectral fluxes and those from the CORONAS-F RESIK crystal spectrometer in the region of overlap, around 3 - 4 keV. There is also agreement between RHESSI and RESIK estimates of the Fe line flux.

Acknowledgements

K.J.H.P. acknowledges a National Research Council Senior Research Associateship award at the NASA Goddard Space Flight Center. B.S. and J.S. acknowledge support from grants 2.P03D.002.22 and BPZ-KBN-054/P03/2001 of the Polish Committee for Scientific Research. CHIANTI is a collaborative project involving Naval Research Laboratory, Rutherford Appleton Laboratory (U.K.), and the Universities of Florence (Italy) and Cambridge (U.K.). We thank E. Landi for providing updates of the CHIANTI database.

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