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Proceedings Article

The Gamma-Ray Imager/Polarimeter for Solar flares (GRIPS)

[+] Author Affiliations
Albert Y. Shih

NASA Goddard Space Flight Ctr. (United States)

Robert P. Lin

Space Sciences Lab. and Univ. of California, Berkeley (United States)

Gordon J. Hurford, Nicole A. Duncan, Pascal Saint-Hilaire, Hazel M. Bain, Steven E. Boggs, Andreas C. Zoglauer

Univ. of California, Berkeley (United States)

David M. Smith

Univ. of California, Santa Cruz (United States)

Hiroyasu Tajima

Solar Terrestrial Environment Lab., Stanford Univ. (United States)

Mark S. Amman

Lawrence Berkeley National Lab. (United States)

Tadayuki Takahashi

Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (Japan)

Proc. SPIE 8443, Space Telescopes and Instrumentation 2012: Ultraviolet to Gamma Ray, 84434H (September 7, 2012); doi:10.1117/12.926450
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From Conference Volume 8443

  • Space Telescopes and Instrumentation 2012: Ultraviolet to Gamma Ray
  • Tadayuki Takahashi; Stephen S. Murray; Jan-Willem A. den Herder
  • Amsterdam, Netherlands | July 01, 2012

abstract

The balloon-borne Gamma-Ray Imager/Polarimeter for Solar flares (GRIPS) instrument will provide a near-optimal combination of high-resolution imaging, spectroscopy, and polarimetry of solar-flare gamma-ray/hard X-ray emissions from ~20 keV to >~10 MeV. GRIPS will address questions raised by recent solar flare observations regarding particle acceleration and energy release, such as: What causes the spatial separation between energetic electrons producing hard X-rays and energetic ions producing gamma-ray lines? How anisotropic are the relativistic electrons, and why can they dominate in the corona? How do the compositions of accelerated and ambient material vary with space and time, and why? The spectrometer/polarimeter consists of sixteen 3D position-sensitive germanium detectors (3D-GeDs), where each energy deposition is individually recorded with an energy resolution of a few keV FWHM and a spatial resolution of <0.1 mm3. Imaging is accomplished by a single multi-pitch rotating modulator (MPRM), a 2.5-cm thick tungstenalloy slit/slat grid with pitches that range quasi-continuously from 1 to 13 mm. The MPRM is situated 8 meters from the spectrometer to provide excellent image quality and unparalleled angular resolution at gamma-ray energies (12.5 arcsec FWHM), sufficient to separate 2.2 MeV footpoint sources for almost all flares. Polarimetry is accomplished by analyzing the anisotropy of reconstructed Compton scattering in the 3D-GeDs (i.e., as an active scatterer), with an estimated minimum detectable polarization of a few percent at 150–650 keV in an X-class flare. GRIPS is scheduled for a continental-US engineering test flight in fall 2013, followed by long or ultra-long duration balloon flights in Antarctica. © (2012) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Citation

Albert Y. Shih ; Robert P. Lin ; Gordon J. Hurford ; Nicole A. Duncan ; Pascal Saint-Hilaire, et al.
" The Gamma-Ray Imager/Polarimeter for Solar flares (GRIPS) ", Proc. SPIE 8443, Space Telescopes and Instrumentation 2012: Ultraviolet to Gamma Ray, 84434H (September 7, 2012); doi:10.1117/12.926450; http://dx.doi.org/10.1117/12.926450


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