The RHESSI Spectrometer

Smith, David M.; Lin, R. P.; Turin, P.; Curtis, D. W.; Primbsch, J. H.; Campbell, R. D.; Abiad, R.; Schroeder, P.; Cork, C.; Hull, Ethan L.; Landis, D.A.; Madden, N.; Malone, D.; Pehl, Richard H.; Raudorf, T. W.; Sangsingkeow, P.; Boyle, R.; Banks, I. S.; Shirey, Kimberly; Schwartz, R. A.

doi:10.1007/978-94-017-3452-3_2

Cited by 48 publications

(41 citation statements)

References 8 publications

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“…For five of the spectra, the electric field inside the runaway electron avalanche region was assumed to be uniform and directed vertically downward, resulting in an upward beam of runaway electrons. These spectra were propagated through the instrument, transforming them into counts spectra, with a detailed Monte Carlo simulation of the RHESSI spacecraft, using GEANT [Smith et al, 2002].…”

Section: Comparing the Model With The Datamentioning

confidence: 99%

A comparison between Monte Carlo simulations of runaway breakdown and terrestrial gamma‐ray flash observations

Dwyer

Smith

2005

Geophysical Research Letters

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255

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[1] Monte Carlo simulations of the runaway breakdown of air are used to calculate the spectra of terrestrial gamma-ray flashes (TGFs), which are then compared with RHESSI and CGRO/BATSE observations. It is found that the recent RHESSI spectrum is not consistent with a source altitude above 24 km but can be well fit by a source in the range of 15-21 km, depending upon the electric field geometry of the source. Because 15 km is not unusual for the tops of thunderstorms, especially at low latitudes, and is lower than typical minimum sprite altitudes, the RHESSI data imply that thunderstorms and not sprites may be the source of these TGFs. On the other hand, the soft energy spectrum seen in some BATSE TGFs is inconsistent with such large atmospheric depths, indicating that there may exist two distinct sources of TGFs, with altitudes below 21 km and above 30 km.

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Section: Comparing the Model With The Datamentioning

confidence: 99%

A comparison between Monte Carlo simulations of runaway breakdown and terrestrial gamma‐ray flash observations

Dwyer

Smith

2005

Geophysical Research Letters

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255

404

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“…The fluence of damaging cosmic rays in space is ~10 8 /cm 2 /year. To minimize the effects of radiation damage, the detector should be kept as cold as possible, ideally below 85 K. This strategy was employed successfully with the germanium detectors in both RHESSI (Reuven Ramaty High Energy Solar Spectroscopic Imager) and TGRS (Transient Gamma-Ray Spectrometer), providing excellent gamma-ray energy resolution for several years in space [4], [14].…”

Section: Radiation Damage and Annealing Capabilitymentioning

confidence: 99%

“…The second approach is to use mechanical cryocooling. However, there is limited experience with this approach for germanium detectors in space [4]. Furthermore, there are a limited number of choices of mechanical cryocoolers that provide the heat lift needed with the required specifications of low mass, low input power, and long lifetime.…”

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confidence: 99%

Thermal design and performance of the gamma-ray spectrometer for the MESSENGER spacecraft

Burks

Cork

Eckels

et al.

IEEE Symposium Conference Record Nuclear Science 2004.

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Abstract--A gamma-ray spectrometer (GRS) has been built and delivered to the MESSENGER spacecraft which launched on August 3, 2004, from Cape Canaveral, Florida. The GRS, a part of seven scientific instruments on board MESSENGER, is based on a coaxial high-purity germanium detector. Gamma-ray detectors based on germanium have the advantage of providing excellent energy resolution, which is critical to achieving the science goals of the mission. However, germanium has the disadvantage that it must operated at cryogenic temperatures (typically ~80 K). This requirement is easy to satisfy in the laboratory but difficult near Mercury, which has an extremely hot thermal radiation environment. To cool the detector, a Stirling cycle mechanical cooler is employed. In addition, radiation and conduction techniques are used to reduce the GRS heat load. Before delivering the flight sensor, a complete thermal prototype was built and tested. The results of these tests, including thermal design, radiative and conductive heat loads, and cooler performance, are described.

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“…The Spectrometer on INTEGRAL (SPI) [68] has coaxial germanium detectors with a characteristic size of 7 cm serving as pixels below a large coded mask (see Chapter 12), and the Imager on Board the INTEGRAL Spacecraft (IBIS) includes thick fingers of CsI serving as pixels beneath a finer mask than SPI's [66]. The large germanium detectors on the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) [61] sit below rotation modulation collimators (see Chapter 12) that do not require position sensitivity.…”

Section: Thin and Monolithic Detectorsmentioning

confidence: 99%

Hard X-ray and gamma-ray detectors

Smith

2013

Observing Photons in Space

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The detection of photons above 10 keV through MeV and GeV energies is challenging due to the penetrating nature of the radiation, which can require large detector volumes, resulting in correspondingly high background. In this energy range, most detectors in space are either scintillators or solid-state detectors. The choice of detector technology depends on the energy range of interest, expected levels of signal and background, required energy and spatial resolution, particle environment on orbit, and other factors. This section covers the materials and configurations commonly used from 10 keV to >1 GeV.

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The RHESSI Spectrometer

Cited by 48 publications

References 8 publications

A comparison between Monte Carlo simulations of runaway breakdown and terrestrial gamma‐ray flash observations

A comparison between Monte Carlo simulations of runaway breakdown and terrestrial gamma‐ray flash observations

Thermal design and performance of the gamma-ray spectrometer for the MESSENGER spacecraft

Hard X-ray and gamma-ray detectors

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