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A Fast Compton Telescope for Detection and Imaging of Gamma-Ray Line Flares Project

Metadata Updated: November 12, 2020

<p align="LEFT"> <font face="TimesNewRomanPSMT">One of the major goals of high-energy solar physics, and therefore of the Solar and </font><font face="TimesNewRomanPSMT">Heliospheric Physics (SHP) Program, is a detailed understanding of the particle acceleration </font><font face="TimesNewRomanPSMT">processes taking place on the Sun during solar flares. Flares can accelerate electrons to tens of </font><font face="TimesNewRomanPSMT">MeV and ions to energies exceeding 1 GeV, as evidenced by the neutral radiation that can be </font><font face="TimesNewRomanPSMT">studied remotely. The intense scientific interest in understanding this process is evidenced by </font><font face="TimesNewRomanPSMT">the large number of wh ite papers dedicated to the topic that were submitted in response to the </font><font face="TimesNewRomanPSMT">current Heliophysics Decadal Survey. A recurring theme in many white papers is the central role </font><font face="TimesNewRomanPSMT">that new, sensitive observations of the </font><b><font face="TimesNewRomanPS-BoldMT">gamma-ray line emissions </font></b><font face="TimesNewRomanPSMT">from flares must play in </font><font face="TimesNewRomanPSMT">disentangling the problem of acceleration and transport of energetic particles (Lin et al. 2010; </font><font face="TimesNewRomanPSMT">Shih et al. 2010; Desai et al. 2010). More specifically, to significantly advance the study of solar </font><font face="TimesNewRomanPSMT">flare particle acceleration, it will be necessary to&nbsp; </font><b><font face="TimesNewRomanPS-BoldMT">compare in detail the spatial, spectral, and </font></b><b><font face="TimesNewRomanPS-BoldMT">temporal evolution of electron signatures&nbsp; </font></b><font face="TimesNewRomanPSMT">(hard X-ray and gamma-ray continuum emission </font><font face="TimesNewRomanPSMT">from bremsstrahlung) </font><b><font face="TimesNewRomanPS-BoldMT">and ion signatures </font></b><font face="TimesNewRomanPSMT">(gamma-ray lines and pion-decay continuum from </font><font face="TimesNewRomanPSMT">accelerated ions colliding with the solar atmosphere) </font><b><font face="TimesNewRomanPS-BoldMT">over a wide dynamic range </font></b><font face="TimesNewRomanPSMT">of flare sizes </font><font face="TimesNewRomanPSMT">and intensities.</font></p> <p align="LEFT"> <font face="TimesNewRomanPSMT"><font face="TimesNewRomanPSMT">For the gamma-ray lines, comprehensive measurements require angular resolution of ~10 </font><font face="TimesNewRomanPSMT">arcsec or better at energies up to ~10 MeV, energy resolution of a few percent or better, and </font><font face="TimesNewRomanPSMT">sensitivity at least 10 times better than that of previous instruments. Making such complex </font><font face="TimesNewRomanPSMT">measurements over a large dynamic range presents a serious challenge to gamma-ray </font><font face="TimesNewRomanPSMT">instrumentation, which must deal with large backgrounds for faint flares and high count rates for </font><font face="TimesNewRomanPSMT">bright flares. In addition, future missions to study flare particle acceleration, such as the Solar </font><font face="TimesNewRomanPSMT">Eruptive Events (SEE) 2020 concept presented by Lin et al. (2010), will contain entire suites of </font><font face="TimesNewRomanPSMT">instruments to ensure that complementary measurements are made in a coordinated manner. </font><font face="TimesNewRomanPSMT">Unprecedented gamma-ray measurements must therefore be made without consuming the </font><font face="T

Access & Use Information

Public: This dataset is intended for public access and use. License: No license information was provided. If this work was prepared by an officer or employee of the United States government as part of that person's official duties it is considered a U.S. Government Work.

Downloads & Resources

References

http://techport.nasa.gov/home
http://techport.nasa.gov/doc/home/TechPort_Advanced_Search.pdf
http://techport.nasa.gov/fetchFile?objectId=6561
http://techport.nasa.gov/fetchFile?objectId=3456
http://techport.nasa.gov/fetchFile?objectId=3447
http://techport.nasa.gov/fetchFile?objectId=6584
http://techport.nasa.gov/fetchFile?objectId=6560
http://techport.nasa.gov/fetchFile?objectId=3448

Dates

Metadata Created Date November 12, 2020
Metadata Updated Date November 12, 2020

Metadata Source

Harvested from NASA Data.json

Additional Metadata

Resource Type Dataset
Metadata Created Date November 12, 2020
Metadata Updated Date November 12, 2020
Publisher Science Mission Directorate
Unique Identifier Unknown
Maintainer
Identifier TECHPORT_10853
Data First Published 2011-10-01
Data Last Modified 2020-01-29
Public Access Level public
Bureau Code 026:00
Metadata Context https://project-open-data.cio.gov/v1.1/schema/catalog.jsonld
Metadata Catalog ID https://data.nasa.gov/data.json
Schema Version https://project-open-data.cio.gov/v1.1/schema
Catalog Describedby https://project-open-data.cio.gov/v1.1/schema/catalog.json
Harvest Object Id 3501f115-edb7-4843-bd96-418c36fc776a
Harvest Source Id 58f92550-7a01-4f00-b1b2-8dc953bd598f
Harvest Source Title NASA Data.json
Homepage URL http://techport.nasa.gov/view/10853
Program Code 026:000
Related Documents http://techport.nasa.gov/home, http://techport.nasa.gov/doc/home/TechPort_Advanced_Search.pdf, http://techport.nasa.gov/fetchFile?objectId=6561, http://techport.nasa.gov/fetchFile?objectId=3456, http://techport.nasa.gov/fetchFile?objectId=3447, http://techport.nasa.gov/fetchFile?objectId=6584, http://techport.nasa.gov/fetchFile?objectId=6560, http://techport.nasa.gov/fetchFile?objectId=3448
Source Datajson Identifier True
Source Hash 706868b9d15dac80e383d49503a29fd75b9f9028
Source Schema Version 1.1
Temporal 2011-10-01T00:00:00Z/2014-09-01T00:00:00Z

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