3 edition of Determining the solar flare photosphereic scale height from SMM gamma-ray measurements found in the catalog.
Determining the solar flare photosphereic scale height from SMM gamma-ray measurements
by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va
Written in English
|Statement||Richard E. Lingenfelter.|
|Series||NASA contractor report -- NASA CR-194084.|
|Contributions||United States. National Aeronautics and Space Administration.|
|The Physical Object|
The photosphere is the visible surface of the Sun that we are most familiar with. Since the Sun is a ball of gas, this is not a solid surface but is actually a layer about km thick (very, very, thin compared to the , km radius of the Sun). Solar flares are observed at all wavelengths from decameter radio waves to gamma-rays beyond 1 GeV. This review focuses on recent observations in EUV, soft and hard X-rays, white light, and radio waves. Space missions such as RHESSI, Yohkoh, TRACE, SOHO, and more recently Hinode and SDO have enlarged widely the observational base. They have revealed a number of surprises: Coronal sources.
Gamma Ray Measurements of the November 15 Solar Flare Martina B. Arndt1, Kevin Bennett2, Alanna Connors1, Mark McConnell1, Gerhard Rank3, James M. Ryan1, Volker Schonfelder3, Raid Suleiman1, and C. Alex Young1 1 Space Science Center, University of New Hampshire, Durham, NH 2Astrophysics Division of ESA/Estec, NL AG Noordwijk, The Netherlands. These solar flares were imaged in extreme ultraviolet light by NASA's STEREO satellites, which at the time were viewing the side of the sun facing away from Earth.
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. from SMM, the local increase was several times higher. We compare the gamma ray line energies, widths, and intensities from the solar event and quiescent atmospheric spectra and discuss their identifications. From this comparison we confirm direct observations that the solar proton spectrum is considerably softer than the spectrum of cosmic rays.
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The diagnostic capabilities of the SMM/GRS measurements were extended by developing a new technique to directly determine the effective photospheric scale height in solar flares from the neutron capture gamma-ray line measurements, and critically test current atmospheric models in the flare Author: Richard E.
Lingenfelter. Determining the Solar-Flare Photospheric Scale Height from SMM Gamma-Ray Measurements Lingenfelter, R. E.; Hua, X. Abstract. Not Available. Publication: Bulletin of the American Astronomical Society. Pub Date: March Bibcode: BAAS L full text sources Author: Richard E.
Lingenfelter. Get this from a library. Determining the solar flare photosphereic scale height from SMM gamma-ray measurements: final technical report, NASA grant NAG (03/01/90 to 02/28/91).
[Richard E Lingenfelter; United States. National Aeronautics and Space Administration.]. Comparing the results of these calculations with the Solar Maximum Mission/Gamma Ray Spectrometer (SMM/GRS) measurements of gamma-ray line and neutron fluxes, the total number and energy spectrum of the flare-accelerated ions trapped on magnetic loops at the Sun were determined and the angular distribution, pitch angle scattering, and mirroring of the ions on loop fields were Author: Richard E.
Lingenfelter. scale height in solar flares from the neutron capture gamma-ray line measurements, and critically test current atmospheric models in the flare region.
Although the photosphere is not a simple exponential atmosphere with a single scale height, an effective scale height can nonetheless be determined at any depth. We show (Lingen. Comparing the results of these calculations with the Solar Maximum Mission/Gamma Ray Spectrometer (SMM/GRS) measurements of gamma-ray line and neutron fluxes, the total number and energy spectrum of the flare-accelerated ions trapped on magnetic loops at the Sun were determined and the angular distribution, pitch angle scattering, and mirroring of the ions on loop fields were.
A comparison of gamma-ray and radio emissions during the UT solar flare on June 3. 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. Based on SMM/GRS measurements of the positronium continuum and annihilation line (Share and Murphy, ) in 19 solar flares observed from tothey showed that gamma-rays from flares with the lowest low-FIP to high-FIP ratios were produced deep in the chromosphere where the abundances should be close to photospheric.
Solar Flares Post Flare Loops but are best seen in measurements of the "Doppler shift" where light from material moving toward us is shifted to the blue while light from material moving away from us is shifted to the red. These features also cover the entire Sun and are continually evolving.
Photospheric Features Review Articles. Technique For Determining the Solar-Flare Photospheric Scale Height From SMM Gamma-ray Measurements - Part 1, - Contains notes, drafts and.
The diagnostic capabilities of the SMM/GRS measurements were extended by developing a new technique to directly determine the effective photospheric scale height in solar flares. An overview of the flare phenomenon is shown in Fig. this view is generally correct is supported by the image obtained with the Yohkoh satellite (and confirmed more recently by RHESSI observations) shown in the upper left of the figure (Masuda et al., ).The gray-scale image shows soft X-ray emission, revealing the magnetic loop filled with hot plasma.
Download Citation | Determination of the Abundances of Subcoronal 4He and of Solar Flare-accelerated 3He and 4He from Gamma-Ray Spectroscopy | A series of narrow gamma-ray lines at, 0.
Spectral measurements of such hard X rays do indeed show a less steep fall-off than at lower energies, often with a power-law rather than an exponential shape. The bremsstrahlung spectrum can extend up into the gamma-ray range.
Indeed, in some of the biggest flares, the spectrum is seen to extend to energies in excess of MeV. Fermi Solar Flare X-Ray and Gamma-Ray Observations.
The Fermi Gamma-ray Space Telescope was launched in June to explore high-energy phenomena in the Universe. This GI program is targeted specifically at Fermi observations of high-energy solar phenomena, primarily solar flares.
In solar flare classification, X-class flares are the most powerful, and M-class flares are just behind them. Both flares were X-class flares. NASA's Fermi Gamma-ray Space Telescope has observed high-energy light from solar eruptions located on the far side of the sun -- light it shouldn't be able to see.
Terrestrial solar radiation measurements are based on pyranometers that respond to radiation within a 2-pi steradian (hemispherical) field of view, and/or pyrheliometers, narrow field of view instruments (° to °) that measure the nearly collimated (i.e. ANCHORAGE, Alaska — A massive flare that exploded from the solar surface in March unleashed the highest-energy light ever seen during a sun eruption, scientists say.
On March 7. Calculate the scaled planet diameters and planet-sun distances for a solar system model. Enter scale or diameter or distance, select to show table and/or map below, select options, then press Calculate.
Examples: Scale 1: or Sun Diameter = 10 cm or Neptune Distance from Sun = ft.Determining the solar flare photosphereic scale height from SMM gamma-ray measurements: final technical report, NASA grant NAG (03/01/90 to 02/28/91) by Richard E Lingenfelter (Book).A solar flare is a very hot, violent event that radiates energy across the electromagnetic spectrum.
The importance of the H-α line is due to the conveniences of observation. The spectral lines of hydrogen are outside the visible band except for the first four of the Balmer series, from the red H .