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Thursday, May 7, 2020 | History

3 edition of Hard X-ray/microwave spectroscopy of solar flares found in the catalog.

Hard X-ray/microwave spectroscopy of solar flares

Hard X-ray/microwave spectroscopy of solar flares

final report, 1 Mar. 1990 - 29 Feb 1992

  • 314 Want to read
  • 2 Currently reading

Published by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va .
Written in English

    Subjects:
  • X-ray spectroscopy.,
  • Solar flares.

  • Edition Notes

    Statementprincipal investigator, Dale E. Gary.
    SeriesNASA contractor report -- NASA CR-194399.
    ContributionsUnited States. National Aeronautics and Space Administration.
    The Physical Object
    FormatMicroform
    Pagination1 v.
    ID Numbers
    Open LibraryOL15386333M

    hard x-ray imaging of solar flares using interpolated visibilities Anna Maria Massone 1, A. Gordon Emslie 2, G. J. Hurford 3, Marco Prato 1, 4, Eduard P. Kontar 5, and Michele Piana 1, 6 1 CNR-INFM LAMIA, via Dodecan I Genova, Italy; [email protected] @article{osti_, title = {Plasma heating in solar flares and their soft and hard X-ray emissions}, author = {Falewicz, R., E-mail: [email protected]}, abstractNote = {In this paper, the energy budgets of two single-loop-like flares observed in X-ray are analyzed under the assumption that nonthermal electrons (NTEs) are the only source of plasma heating during all phases of both.

    1. SOLAR SCIENCE WITH THE MINIATURE X-RAY SOLAR SPECTROMETER (MINXSS) CUBESATS The solar corona is the interface between the solar surface (photosphere) and lower atmosphere (chromosphere), and the solar wind (interplanetary space), starting at roughly 2, km above the solar photosphere and extending to a few solar radii1. The conditions in. A burst of high‐energy radiation coincident with a solar flare has been detected during a balloon flight at 10 gm/cm 2 atmosphere depth and 30° geomagnetic latitude over Cuba. The flare occurred at UT on Ma and was associated with solar radio bursts on 1, Mc/s.

    The X-ray observations of the flare taken from the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) spacecraft reveal two phases of the flare evolution. The first phase is characterized by the altitude decrease of the X-ray looptop (LT) source for approx11 minutes. In the first stages of the development of X-ray spectroscopy by means of diffraction in crystals, the radiation from ordinary technical X-ray tubes was registered. W. H. and W. L. Bragg () used for the analysis a goniometer, where a rocksalt crystal was mounted on the rotating table.


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Hard X-ray/microwave spectroscopy of solar flares Download PDF EPUB FB2

For all three flares, the O VII source volume is found to be smallest at the beginning of the flare, near the time when the impulsive hard X-ray/microwave volume reaches its first maximum. The joint study of hard x ray and microwave observations of solar flares is extremely important because the two complementary ways of viewing the accelerated electrons yield information that cannot be obtained using hard x rays or microwaves alone.

The microwaves can provide spatial information lacking in the hard x rays, and the x ray data can give information on the energy distribution of Author: Dale E. Gary. RELATIVE TIMING AND SPECTRA OF SOLAR FLARE HARD X-RAY SOURCES SÄM KRUCKER 1 1,2 1Space Sciences Lab, University of California, Berkeley, CAU.S.A.

2Physics Department, University of California, Berkeley, CAU.S.A. (Received 7 August ; accepted 2 September ) Abstract. Hard X-ray lightcurves, spectrograms, images, and.

We analysed the hard X-ray and microwave flux spectra of the solar flare (BATSE No) on 2 Novemberwhich started at UT and ended at UT. In attempting to explain observed hard X-ray and microwave flux from solar flares by a single population of energetic electrons, one has met a serious disc In this paper it is shown that this discrepancy can be removed for impulsive flares by the assumption of a precipitation model for both X-ray and microwave sources and that the magnetic field of – G is required in the microwave emitting Cited by: The typical characteristics of the hard X-ray emission of impulsive solar flares are examined.

At times of hard X-ray peaks, spectra that break downward are the rule rather than the exception. This paper explores the time evolution of microwave and hard X-ray spectral indexes in the solar flare observed by Nobeyama Radio Polarimeters (NoRP) and the Ramaty High Energy Solar Spectroscopy.

The flare consists of a gradual component in soft X-rays and microwaves and a superposed impulsive burst accompanied by hard X-ray emission. The impulsive phase of the flare appears in the soft.

Abstract We analyze 10 flare events that radiate intense hard X-ray (HXR) emission with significant photons over keV to verify that the electrons that have a common origin of acceleration mechanism and energy power-law distribution with solar flares emit HXRs and microwaves.

Most of these events have the following characteristics. X-Ray Spectroscopy of Solar Active Regions during the Third Skylab Mission. Pye, R. Hutcheon, J. Parkinson, K. Pounds Fe xxiv Emission in Solar Flares Observed with the NRL/ATM XUV Slitless Spectrograph.

Kenneth G. Widing. The Interpretation of Spectra, Polarization, and Directivity of Solar Hard X-Rays. John C. Brown. About this book This book provides the first complete and up-to-date summary of the state of the art in HAXPES and motivates readers to harness its powerful capabilities in their own research.

The chapters are written by experts. They include historical work, modern instrumentation, theory and applications. Hard X-ray lightcurves, spectrograms, images, and spectra of three medium-sized flares observed by the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) are by: solar flares, through imaging and spectroscopy of X-ray/γ-ray continuum and γ-ray lines emitted by accelerated electrons and ions, respectively.

It provides the first hard X-ray imaging spectroscopy, the first high resolution spectroscopy of solar -ray lines, and the first imaging of solar. Hard X-ray/microwave spectroscopy of solar flares: final report, 1 Mar. Feb [Dale E Gary; United States.

National Aeronautics and Space Administration.]. Abstract. We analyze the time variation of microwave spectra and hard X-ray spectra of Ma which are obtained from the Solar Array at the Owens Valley Radio Observatory (OVRO) and the Hard X-Ray Burst Spectrometer (HXRBS) on the Solar Maximum Mission (SMM), respectively.

From this observation, it is noted that the hard X-ray spectra Cited by: THE ASTROPHYSICAL JOURNAL LETTERS, MANUAL EMULATION TEMPLATE doi: //XXX/X/LXX 1 HARD X-RAY IMAGING OF INDIVIDUAL SPECTRAL COMPONENTS IN SOLAR FLARES AMIR CASPI1, ALBERT Y.

SHIH2, JAMES M. MCTIERNAN3, AND SÄM KRUCKER3,4 1Southwest Research Institute, Boulder, COUSA 2Solar Physics Laboratory, NASA Goddard. The Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) satellite was launched on 5 February Its objective is to study the energy release and particle acceleration in solar flares through observations of X-rays and gamma rays.

Two novel technologies are combined to obtain both spectra and images over a broad energy range. It was obtained that, in accordance with the development of the active region, the X- and gamma-ray flux tended to increase at the flare maxima while the hard X-ray spectral index tended to decrease; flares with a harder radiation spectrum occurred in the sunspot umbra, i.e., in the region with the strongest magnetic by: 2.

MODELING IMAGES AND SPECTRA OF A SOLAR FLARE OBSERVED BY RHESSI ON 20 FEBRUARY LINHUI SUI1, GORDON D. HOLMAN2, BRIAN R. DENNIS2, SÄM KRUCKER3, RICHARD A. SCHWARTZ4 and KIM TOLBERT4 1CUA & Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Greenbelt, MDU.S.A.

(e-mail: [email protected]). Millimeter, Microwave, Hard X–ray and Soft X–ray Observations of Energetic Electron Populations in Solar Flares M.

Kundu1, S. White 1, N. Gopalswamy1 and J. Lim1,2 1Dept. of Astronomy, Univ. of Maryland, College Park MD 2Solar Astronomy –33, Caltech, Pasadena CA Submitted to the Astrophysical Journal Supplement, March. SOLAR MAXIMUM MISSION BENT CRYSTAL SPECTROMETER I I - -4 U ~ 10 14 JULY UT 14 Fig 5 I I I 12 16 Electron Temperature ( K) 18 X-Ray Spectroscopy of Solar Flares (11)7 1 ii) The Braaa Spectrometers on the Pi Mission (US NRLI A substantial programme of solar flare observations has been carried out with the Cited by: 2.ELECTRON FLUX SPECTRAL IMAGING OF SOLAR FLARES THROUGH REGULARIZED ANALYSIS OF HARD X-RAY SOURCE VISIBILITIES Michele Piana,1 Anna Maria Massone,2 G.

J. Hurford,3 Marco Prato,4 A. Gordon Emslie,5 Eduard P. Kontar,6 and Richard A. Schwartz7 Received March 16; accepted May 3Cited by: Solar Flares. A solar flare is a short-lived sudden increase in the intensity of radiation emitted in the neighborhood of sunspots.

Historically it was best monitored in the H-alpha wavelength and occurs in the chromosphere, though occasionally white light flares are seen in the photosphere.