Bronze level automatically awarded US beta

This data has achieved Bronze level on 22 October 2015 which means this data makes a great start at the basics of publishing open data.

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

Summary

Type of release
a one-off release of a single dataset

Data Licence
Not Applicable

Content Licence
Creative Commons CCZero

Verification
automatically awarded

Release Date
9 April 2015
Modified Date
8 July 2015
Publishers
National Aeronautics and Space Administration
Keywords
active, nasa-headquarters, project
Identifier
a-fast-compton-telescope-for-detection-and-imaging-of-gamma-ray-line-flares-project
Landing Page
http://techport.nasa.gov/view/10853
Maintainers
Peter Bloser hq-techport@mail.nasa.gov
Language
en-US

Community verification

Other people can verify whether the answers on this certificate are correct.

This certificate is automatically awarded.

Sign in to verify or report this certificate

Description

<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  </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  </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="TimesNewRomanPSMT">spacecraft’s mass, power, and telemetry budgets.</font></font></p> <p align="LEFT"> <font face="TimesNewRomanPSMT"><font face="TimesNewRomanPSMT"><font face="TimesNewRomanPSMT">Three recent technological developments potentially allow us to combine the abilities of </font><font face="TimesNewRomanPSMT">these pioneering instruments: 1) Recently developed scintillator materials, in particular LaCl </font><font face="TimesNewRomanPSMT" size="1"><font face="TimesNewRomanPSMT" size="1">3</font></font><font face="TimesNewRomanPSMT">:Ce </font><font face="TimesNewRomanPSMT">and LaBr </font><font face="TimesNewRomanPSMT" size="1"><font face="TimesNewRomanPSMT" size="1">3</font></font><font face="TimesNewRomanPSMT">:Ce, offer a far more attractive mix of stopping power, energy resolution, and fast time </font><font face="TimesNewRomanPSMT">response than NaI and BGO scintillators. Energy resolution better than 3% above 0.6 MeV and </font><font face="TimesNewRomanPSMT">timing resolution well below 500 ps are now well established. 2) Recently developed Silicon <font face="TimesNewRomanPSMT">Photo-Multipliers (SiPMs) offer a compact, low-mass, and low-power alternative to PMTs. We </font><font face="TimesNewRomanPSMT">have already shown that detectors composed of LaBr </font><font face="TimesNewRomanPSMT" size="1"><font face="TimesNewRomanPSMT" size="1">3 </font></font><font face="TimesNewRomanPSMT">scintillator coupled to SiPM readouts </font><font face="TimesNewRomanPSMT">perform well as gamma-ray spectrometers (Bloser et al. 2008, 2010a). 3) Newly available </font><font face="TimesNewRomanPSMT">compact arrays of SiPMs, with sensing elements typically 3 – 4 mm in size, promise the </font><font face="TimesNewRomanPSMT">additional ability to achieve fine spatial resolution within scintillators in a compact Anger </font><font face="TimesNewRomanPSMT">camera configuration. Gamma-ray detectors of this nature are currently being developed by the </font><font face="TimesNewRomanPSMT">medical imaging community (e.g., Schaart et al. 2009), and position resolution of 1 mm or better </font><font face="TimesNewRomanPSMT">has been demonstrated</font></font></font></font></p> <p align="LEFT">  </p> <p align="LEFT"> <font face="TimesNewRomanPSMT"><font face="TimesNewRomanPSMT"><b><font face="TimesNewRomanPS-BoldMT">We propose a program of instrument development and modeling to show that a fast </font></b><b><font face="TimesNewRomanPS-BoldMT">Compton telescope based on an innovative combination of new scintillator detectors and </font></b><b><font face="TimesNewRomanPS-BoldMT">light readout devices, combined with an imaging grid or mask, is a scientifically </font></b><b><font face="TimesNewRomanPS-BoldMT">competitive solution to this instrumentation challenge  </font></b><font face="TimesNewRomanPSMT">In effect, we will attempt to combine </font><font face="TimesNewRomanPSMT">the best features of past solar gamma-ray instruments into an efficient, low-background, imaging </font><font face="TimesNewRomanPSMT">gamma-ray spectrometer. The RHESSI mission (Lin et al. 2002) made the first high-angularresolution </font><font face="TimesNewRomanPSMT">images at gamma-ray energies, adapting Fourier-synthesis methods previously used at </font><font face="TimesNewRomanPSMT">hard X-ray energies (e.g., the Yohkoh Hard X-ray Telescope; Kosugi et al. 1991) to image the </font><font face="TimesNewRomanPSMT">2.2 MeV neutron-capture line with a resolution of about 35 arcsec (Hurford et al. 2006). Earlier </font><font face="TimesNewRomanPSMT">gamma-ray spectrometers based on efficient inorganic scintillators, including those on the Solar </font><font face="TimesNewRomanPSMT">Maximum Mission (SMM; Forrest et al. 1980), Yohkoh (Yoshimori et al. 1992), and the </font><font face="TimesNewRomanPSMT">Compton Gamma Ray Observatory (e.g., Murphy et al. 1993), made sensitive spectral </font><font face="TimesNewRomanPSMT">observations up to >10 MeV over a large range of flare intensities. The most sensitive gammaray </font><font face="TimesNewRomanPSMT">flare spectrometer of all was the COMPton TELescope (COMPTEL) on CGRO (Schönfelder </font><font face="TimesNewRomanPSMT">et al. 1993; Ryan & McConnell 1996). As a scintillator-based Compton telescope, COMPTEL </font><font face="TimesNewRomanPSMT">was able to dramatically suppress background using a fast coincidence, time-of-flight (ToF) </font><font face="TimesNewRomanPSMT">measurements, and coarse imaging ability. COMPTEL was able to detect nuclear emission from </font><font face="TimesNewRomanPSMT">a C4 flare, the faintest such detection to date (Young et al. 2001).</font></font></font></p> <p>  </p> <p>  </p>

Información General

Información legal

This dataset has been created by US Government which means it is required to be in the public domain. However US copyright law only allows open access by US citizens, we have assumed the data is equivalently licensed as CC0 for the rest of the world as this is in the spirit of the US Government’s Open Data policy.

  • La declaración sobre derechos está en

    http://catalog.data.gov/dataset/a-fast-compton-telescope-for-detection-and-imaging-of-gamma-ray-line-flares-project Do you think this data is incorrect? Let us know

  • Under which licence can people outside the US reuse this data?

    CCZero Creative Commons Do you think this data is incorrect? Let us know

  • Existen

    yes, and the rights are all held by the same person or organisation Do you think this data is incorrect? Let us know

  • El contenido se encuentra disponible bajo

    CCZero Creative Commons Do you think this data is incorrect? Let us know

  • La declaración sobre derechos incluye información acerca de

    su licencia de datos Do you think this data is incorrect? Let us know

  • Estos datos contienen

    Ningún dato sobre individuos Do you think this data is incorrect? Let us know

Información práctica

  • Los datos aparecen en esta colección.

    http://catalog.data.gov/organization/nasa-gov Do you think this data is incorrect? Let us know

  • La precisión o la relevancia de estos datos

    Expiran pero están temporalizados Do you think this data is incorrect? Let us know

  • Los datos están

    Respaldo fuera del sitio Do you think this data is incorrect? Let us know

Información técnica

  • Estos datos son publicados en

    http://techport.nasa.gov/xml-api/10853 Do you think this data is incorrect? Let us know

  • Estos datos son

    Lectura mecánica Do you think this data is incorrect? Let us know

  • El formato de estos datos es

    Un formato abierto estandar Do you think this data is incorrect? Let us know

Información social

  • La documentación incluye datos legibles por máquina para

    Título Do you think this data is incorrect? Let us know

  • La documentación incluye datos legibles por máquina para

    Descripción Do you think this data is incorrect? Let us know

  • La documentación incluye datos legibles por máquina para

    Identificador Do you think this data is incorrect? Let us know

  • La documentación incluye datos legibles por máquina para

    Página de destino Do you think this data is incorrect? Let us know

  • La documentación incluye datos legibles por máquina para

    Editor Do you think this data is incorrect? Let us know

  • La documentación incluye datos legibles por máquina para

    Palabra(s) clave o etiqueta(s) Do you think this data is incorrect? Let us know

  • La documentación incluye datos legibles por máquina para

    Distribución Do you think this data is incorrect? Let us know

  • La documentación incluye datos legibles por máquina para

    Fecha de lanzamiento Do you think this data is incorrect? Let us know

  • La documentación incluye datos legibles por máquina para

    Fecha de modificación Do you think this data is incorrect? Let us know

  • La documentación incluye datos legibles por máquina para

    Cobertura temporal Do you think this data is incorrect? Let us know

  • La documentación incluye datos legibles por máquina para

    Idioma Do you think this data is incorrect? Let us know

  • La documentación acerca de cada distribución incluye datos legibles por máquina para

    Fecha de lanzamiento Do you think this data is incorrect? Let us know

  • La documentación acerca de cada distribución incluye datos legibles por máquina para

    Un URL para acceder a los datos Do you think this data is incorrect? Let us know

  • La documentación acerca de cada distribución incluye datos legibles por máquina para

    Un URL para descargar la base de datos Do you think this data is incorrect? Let us know

  • La documentación acerca de cada distribución incluye datos legibles por máquina para

    Tipos de medios de descarga Do you think this data is incorrect? Let us know

  • Encuentre la manera de contactar a alguien sobre estos datos en

    http://catalog.data.gov/dataset/a-fast-compton-telescope-for-detection-and-imaging-of-gamma-ray-line-flares-project Do you think this data is incorrect? Let us know

  • Encuentre cómo sugerir mejoras a una publicación en

    http://www.data.gov/issue/?media_url=http://catalog.data.gov/dataset/a-fast-compton-telescope-for-detection-and-imaging-of-gamma-ray-line-flares-project Do you think this data is incorrect? Let us know

Create a certificate

Don't have an account?

Don't worry, you can register later to save your work.

Create an account