Abstract
RHESSI observes solar photons over three orders of magnitude in energy (3 keV to 17 MeV) with a single instrument: a set of nine cryogenically cooled coaxial germanium detectors. With their extremely high energy resolution, RHESSI can resolve the line shape of every known solar gamma-ray line except the neutron capture line at 2.223 MeV. High resolution also allows clean separation of thermal and non-thermal hard X-rays and the accurate measurement of even extremely steep power-law spectra. Detector segmentation, fast signal processing, and two sets of movable attenuators allow RHESSI to make high-quality spectra and images of flares across seven orders of magnitude in intensity. Here we describe the configuration and operation of the RHESSI spectrometer, show early results on in-flight performance, and discuss the principles of spectroscopic data analysis used by the RHESSI software.
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References
Arnaud, K.: 1996, in G. Jacoby and J. Barnes (eds.), Astronomical Data Analysis Software and Systems V, Astronomical Society of the Pacific, San Francisco, U.S.A., p. 17.
Curtis, D.W. et al.: 2002, Solar Phys., this volume.
Freeland, S. L. and Handy, B. N.: 1998, Solar Phys. 182, 497.
Hull, E. L.: 1998, Ph. D. dissertation, Indiana University, U.S.A.
Hurford, G. et al.: 2002, Solar Phys., this volume.
Johns, C. M. and Lin, R. P.: 1992, Solar Phys. 137, 121 (Erratum: Solar Phys. 142, 219).
Koenen, M., Bruckner, J., Korfer, M., Taylor, I. and Wanke, H.: 1995, IEEE Trans. Nucl. Sci. 42, 653.
Krucker, S., Christe, S., Lin, R.P., Hurford, G.J., and Schwartz, R.A.: 2002, Solar Phys., this volume.
Landis, D. A., Cork, C. P., and Goulding, F. S.: 1982, IEEE Trans. Nucl. Sci. 29, 1125.
Lin, R. P. and Schwartz, R.: 1987, Astrophys. J. 312, 462.
Lin, R. P. et al.: 2002, Solar Phys., this volume.
McConnell, M.L., Ryan, J.M., Smith, D.M., Lin, R.P., and Emslie, A.G.: 2002, Solar Phys., this volume.
Schwartz, R. A. 1996, ‘Compton Gamma Ray Observatory Phase 4 Guest Investigator Program: Solar Flare Hard X-ray Spectroscopy,’ Technical Report, NASA Goddard Space Flight Center.
Share, G. H., Murphy, R. J., and Ryan, J.: 1997, in C. D. Dermer, M. S. Strickman, and J. D. Kurfess (eds.), Proceedings of the Fourth Compton Symposium, American Institute of Physics, Woodbury, New York, U.S.A., p. 17.
Share, G. H. et al.: 2002, Solar Phys., this volume.
Smith, D.M. et al.: 1995, J. Geophys. Res. 100, 19675.
Smith, D.M. et al.: 2000, ‘Extra-Solar Astrophysics with the High-Energy Solar Spectroscopic Imager (HESSI),’ AIP Conf. Proc., The 5th Compton Symposium, AIP New York, AIP), pp. 510, 671.
Smith, D.M. et al.: 2002, ‘Non-solar Astronomy with the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI),’ SPIE Conf. Proc. 4851, in press.
Vestrand, W. T. et al.: 1999, Astrophys. J. Suppl. 120, 409.
Yoshimori, M. et al.: 1994, Astrophys. J. Suppl. 90, 639.
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Smith, D., Lin, R., Turin, P. et al. The RHESSI Spectrometer. Sol Phys 210, 33–60 (2002). https://doi.org/10.1023/A:1022400716414
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DOI: https://doi.org/10.1023/A:1022400716414