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Monday, October 12, 2020 | History

3 edition of High resolution X- and gamma-ray spectroscopy of solar flares found in the catalog.

High resolution X- and gamma-ray spectroscopy of solar flares

High resolution X- and gamma-ray spectroscopy of solar flares

final report, February 1, 1979-October 31, 1983

  • 161 Want to read
  • 20 Currently reading

Published by The Administration in Washington, D.C .
Written in English

    Subjects:
  • Solar flares.,
  • High resolution spectroscopy.

  • Edition Notes

    Statementsubmitted by Space Sciences Laboratory, University of California ; principal investigator, Robert P. Lin ; prepared for NASA Headquarters.
    SeriesNASA-CR -- 173150., NASA contractor report -- NASA CR-173150.
    ContributionsUniversity of California, Berkeley. Space Sciences Laboratory., United States. National Aeronautics and Space Administration.
    The Physical Object
    FormatMicroform
    Pagination1 v.
    ID Numbers
    Open LibraryOL17831608M

    To study solar flares in the wide energy band of the electromagnetic spectrum ranging from UV to high-energy gamma rays ( MeV), three Roentgen telescopes were developed by Dr. A. Raghu Rao of the astronomy and astrophysics department at Tata Institute of Fundamental Research in Mumbai, India, and a team of Indian researchers. The instruments were . Figure 1. Effective areas of high-resolution X-ray spectroscopy missions as functions of X-ray energy. The curve for the SXS is the present best estimate for a point source, where we assumed to sum all photons detected on the whole array, ’ HPD of the X-ray mirrors, and no contamination of the optical blocking filters.

    Buy The Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) - Mission Description and Early Results on FREE SHIPPING on qualified orders The Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) - Mission Description and Early Results: Robert P. Lin, Brian R. Dennis, Arnold O. Benz: : Books. @article{osti_, title = {Neutron and 2. MeV gamma-ray line emission from solar flares}, author = {Hua, X.M.}, abstractNote = {Systematic calculations of the neutron and MeV gamma-ray line production in solar flares and their escape fluxes as a function of angle, energy, and time were carried out. With a connected system of Monte Carlo programs, the .

    High Resolution Gamma Ray Spectroscopy Measurements of the Fast Ion Energy Distribution in JET 4He plasmas “This document is intended for publication in the open literature. It is made available on the understanding that it may not be further circulated and extracts or references may not be published. A massive thermal detector consisting of a 73 g TeO 2 crystal, to be used to search for double beta decay of Te and to detect high energy gamma-rays, is operating at aprox. 15 mK in the Gran Sasso Underground Laboratory. The FWHM resolution achieved with this detector is KeV, slightly dependent on energy from KeV to 3 MeV, showing the competitive Cited by: 1.


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High resolution X- and gamma-ray spectroscopy of solar flares Download PDF EPUB FB2

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 particleCited by: 8. Get this from a library. High resolution X- and gamma-ray spectroscopy of solar flares: final report, February 1, Octo [Robert P Lin; University of California, Berkeley.

Space Sciences Laboratory.; United States. National Aeronautics and Space Administration.]. Fine-structure measurements of solar gamma-emission lines are possible in the framework of high-resolution and sensitivity (HRS) spectroscopy only. Here we present the project of HRS instrument which includes Germanium and scintillator spectrometers.

The Ge-spectrometer will cover the range –10 MeV with a resolution of ∼% at 1 by: 2. The balloon-borne Gamma-Ray Imager/Polarimeter for Solar flares (GRIPS) instrument will provide a near-optimal combination of high-resolution.

"A high resolution X-ray spectrometer and large area Phoswich detector were designed and co-aligned in a common elevation mounting in order to measure solar and cosmic X-ray and gamma ray emission in the 13 to KeV energy range from a balloon.

High-Resolution Gamma-Ray Spectroscopy Fig. 60Co Spectrum Showing Resolutions and Peak-to-Compton Ratios for an HPGe Coaxial Detector and an NaI(Tl) Detector. Fig. Relative Probability of Each of the Three Types of Interactions as a Function of Energy.

The Transient Gamma-Ray Spectrometer (TGRS) to be flown aboard the WIND spacecraft is primarily designed to perform high resolution spectroscopy of transient γ-ray events, such as cosmic γ-ray bursts and solar flares over the energy range 25 keV to MeV with an expected spectroscopic resolution of ∼ 3 keV at 1 MeV.

The detector itself consists of a Cited by: RHESSI – The Reuven Ramaty High Energy Solar Spectral Imager was designed to image solar flares in energetic photons from soft X rays (ca. 3 keV) to gamma rays (up to ca. 20 MeV) and to provide high resolution spectroscopy up to gamma-ray energies of ca.

20 MeV. Furthermore, it had the capability to perform spatially resolved spectroscopy. in solar flares through imaging and spectroscopy of hard X-ray (HXR)/gamma-ray continua emitted by energetic electrons, and of gamma-ray lines produced by energetic ions.

The single RHESSI instrument provides ground-breaking imaging and spectroscopy measurements over the broad energy range from soft X-rays (3 keV) to gamma-rays (17 MeV).

Mission concept. RHESSI was designed to image solar flares in energetic photons from soft X-rays (~3 keV) to gamma rays (up to ~20 MeV) and to provide high resolution spectroscopy up to gamma-ray energies of ~20 MeV.

Furthermore, it had the capability to perform spatially resolved spectroscopy with high spectral or: NASA / Goddard, Space. My research aims to expand this small set gamma-ray flare observations by (1) using new techniques to study flares obscured by high-background counts in the existing RHESSI dataset and (2) providing new observations through the development and flight of the Gamma-Ray Imager/Polarimeter for Solar Flares (GRIPS) by: 1.

Recent reviews can be found on energetic ions in solar flares from gamma-ray and neutron observations (Vilmer et al. ()), on electron acceleration and propagation in.

A high-resolution gamma-ray and hard X-ray spectrometer for solar flare observations in Max Max Flare Research at the Next Solar Maximum.

Workshop 1: Scientific Objectives; p ; Gamma Ray Spectroscopy on Long Duration Balloon Flights in Antarctica ASP Conference Series; Vol. ;p and He3 in flares and they attempted to deduce the number of protons released from the flare ofAugust 4 by combining the He3 and gamma-ray obser- vat ions.

In the present paper we wish to summarize the above material md to present updated calculations on the production of gamma-ray lines in solar Size: 1MB.

The first high-res,lution spectrometers In be I'lown were lithium-drifted germanium used by Jacobson [4] for observations of the Crab Ne2ula and by Womack and Overbcck [5] for the first attempt at high-resolution observati~ ns of gamma-ray emission from solar flares. Presently, high-purity germanium is being empioyed in hoth satellite and Cited by: 4.

RHESSI provides high-resolution spectroscopy and imaging of solar flares from about 3 keV to about 20 MeV. RHESSI is expected to operate throughout the onset of the next activity cycle.

GLAST, launched in Juneis the next-generation high-energy gamma-ray observatory covering the photon energy range from 10 keV to more than GeV. Two new missions will be launched in andeach carrying X-ray and gamma ray detectors capable of high spectral resolution at room temperature.

The Argentine Satelite de Aplicaciones Cientificas (SAC-B) and the Small Spacecraft Technology Initiative (SSTI) Clark missions will each carry. Information on the highest energies of particles produced during solar flares, measured in gamma-ray wavelengths with photon energies of E ≳ keV, has been obtained by very few instruments on a.

Solar flare imaging in X-rays of two large X-class two ribbon flares: Thermal and non-thermal X-ray emissions are shown in red and blue contours, respectively.

For the Janu flare (top) the flare loop is seen mostly from the side, while for the Octo flare that occurred. Smith et al [1] reported the first high energy resolution meas-urements of nuclear de-excitation lines in the solar flare of July 23rd using data from the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) – a spacecraft designed to ob-serve the solar flares with high resolution X ray− and −ray im-aging spectroscopy.

– Chupp et al. detect gamma-ray emission lines from solar flares in August via an experiment aboard OSO This includes the keV positron annihilation line, the MeV neutron-capture line, and the weak detection of C & O de-excitation lines at & MeV.provide unique high-resolution X-ray and gamma-ray imaging spectroscopy observations over the range of energies from 3 keV to 17 MeV, with high spatial resolution (down to 2 arcseconds), spectral resolution (as fine as 1 keV FWHM), and time resolution (as fine as 2 s for imaging and.presented the first high resolution observation of the gamma ray spectrum in JET discharges with 4He beams accelerated by ICRH at the 3d harmonic resonance.

Gamma ray spectroscopy measures the γ-ray emission spectrum caused by reactions of fast particles with fuel ions or with impurities (carbon and beryllium) [1]. The γ-ray spectrum depends.