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  • 1
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    The difference in the energy spectra of galactic cosmic rays at the minima of the 19th and 20th solar activity cycles (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: The absorption curves of the cosmic ray charged component for solar minima in 1965 and 1975 to 1977 are analyzed on the basis of daily stratospheric measurements in Murmansk, Moscow, Alma-Ata and Mirny (Antarctic). Two distinct features in the energy spectra of galactic cosmic rays are revealed during these periods. At the 20th solar activity minimum there was the additional short range component of cosmic rays. Additional fluxes in the stratosphere at high latitudes caused by this component are probably protons and He nuclei with the energy 100 to 500 MeV/n. The fluxes are estimates as Approx. 300 sq m/s/sr. At the minimum in 1975 to 1977 the proton intensity in the energy range 1 to 15 GeV is 10 to 15% lower than that in the 1965 solar activity minimum.
    Keywords: SOLAR PHYSICS
    Type: SH-4.4-18 , 19th Intern. Cosmic Ray Conf - Vol. 5; p 79-82; NASA-CP-2376-VOL-5
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  • 2
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    Peculiarities of propagation of charged particles in solar corona (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: The influence of boundaries of the large scale unipolar magnetic regions (UMR) on the Sun upon the charged particle propagation in the solar corona and interplanetary space is investigated. Increases of the charged particle fluxes from solar flares on November 4 and 20, 1978 detected by Venera-11 and Prognoz-1 and on December 7, 1982 by Venera-13 and "GMS-2" were analyzed.
    Keywords: SOLAR PHYSICS
    Type: SH-3.1-6 , 19th Intern. Cosmic Ray Conf - Vol. 4; p 313-316; NASA-CP-2376-VOL-4
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  • 3
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    On the retention of high-energy protons and nuclei with charges Z or equal to 2 in large solar flares after the process of their acceleration (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Data which suggest that the protons with energies of up to several GeV should be retained on the Sun after the process of their acceleration are presented. The protons are on the average retained for 15 min, irrespectively of the solar flare heliolatitude and of the accelerated particle energy ranging from 100 MeV to several GeV. It is suggested that the particles are retained in a magnetic trap formed in a solar active region. No Z or = 2 nuclei of solar origin during large solar flares. The absence of the 500 MeV/nucleon nuclei with Z or = 2 may be due to their retention in the magnetic trap which also retains the high-energy protons. During the trapping time the approx. 500 MeV/nucleon nuclei with Z or = 2 may escape due to nuclear interactions and ionization loss.
    Keywords: SOLAR PHYSICS
    Type: SH-2.1-8 , 19th Intern. Cosmic Ray Conf - Vol. 4; p 229-232; NASA-CP-2376-VOL-4
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  • 4
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    Silicon to iron abundances in solar cosmic rays and in the sun (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Differential spectra of even charged nuclei between Si and Fe in the August 4, 1972 event were made in the energy region of 10 to 40 MeV/n-1 using rocket borne plastic detectors. The resulting relative abundances of elements and low energy enhancements are obtained and compared with spectroscopically determined photospheric abundances. The implications of the relative abundances on the acceleration mechanisms is discussed.
    Keywords: SOLAR PHYSICS
    Type: SH-2.1-6 , 19th Intern. Cosmic Ray Conf - Vol. 4; p 221-224; NASA-CP-2376-VOL-4
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  • 5
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    Observation of the fluxes of nuclei with energies 10-20 MEV per nucleon during the solar flare of April 26, 1984 (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Observations of the fluxes of low energy nuclei in the Earth's magnetosphere are reported. The energy distribution and the composition of the nuclear component of cosmic rays observed during the solar flare of April 26, 1984 are presented.
    Keywords: SOLAR PHYSICS
    Type: SH-2.1-1 , 19th Intern. Cosmic Ray Conf - Vol. 4; p 205-208; NASA-CP-2376-VOL-4
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  • 6
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    The vector structure of active magnetic fields (1985)
    In:  CASI
    Details
    Publication Date: 2006-02-14
    Description: Observations are needed to show the form of the strains introduced into the fields above the surface of the Sun. The longitudinal component alone does not provide the basic information, so that it has been necessary in the past to use the filamentary structure observed in H sub alpha to supplement the longitudinal information. Vector measurements provide the additional essential information to determine the strains, with the filamentary structure available as a check for consistency. It is to be expected, then, that vector measurements will permit a direct mapping of the strains imposed on the magnetic fields of active regions. It will be interesting to study the relation of those strains to the emergence of magnetic flux, flares, eruptive prominences, etc. In particular we may hope to study the relaxation of the strains via the dynamical nonequilibrium.
    Keywords: SOLAR PHYSICS
    Type: NASA. Marshall Space Flight Center Meas. of Solar Vector Magnetic Fields; p 7-16
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  • 7
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    High-resolution X-ray spectra of solar flares. VII - A long-duration X-ray flare associated with a coronal mass ejection (1985)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: It has been recognized that very long duration X-ray events (lasting several hours) are frequently associated with coronal mass ejection. Thus, Sheeley et al. (1983) found that the probability of the occurrence of a coronal mass ejection (CME) increases monotonically with the X-ray event duration time. It is pointed out that the association of long-duration, or long-decay, X-ray events (LDEs) with CMEs was first recognized from analysis of solar images obtained by the X-ray telescopes on Skylab and the Naval Research Laboratory (NRL) slitless spectroheliograph. Recently high-resolution Bragg crystal X-ray spectrometers have been flown on three spacecraft, including the Department of Defense P78-1 spacecraft, the NASA Solar Maximum Mission (SMM), and the Japanese Hinotori spacecraft. In the present paper, P78-1 X-ray spectra of an LDE which had its origin behind the solar west limb on November 14, 1980 is presented. The obtained data make it possible to estimate temperatures of the hottest portion of the magnetic loops in which the emission arises.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal, Part 1 (ISSN 0004-637X); 292; 309-318
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  • 8
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    White-light and radio sounding observations of coronal transients (1985)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: A concerted search for coronal transients was conducted with the 'Solwind' coronagraph during the solar occultations of the two Helios spacecraft in October/November 1979. The polarization angle and bandwidth of the linearly polarized S-band downlink signal were monitored at the three 64-m tracking stations of the NASA Deep Space Network to determine coronal Faraday rotation and spectral broadening. A one-to-one correspondence could be established between abrupt disturbances in the two signal parameters and the passage of a white-light transient through the signal ray path from spacecraft to earth. The white-light morphology and the additional information provided by the radio sounding coverage are presented for each of the five distinct events recorded. Although no specific example could be observed in sufficient detail in both white light and Faraday rotation to derive the small-scale magnetic structure, some qualitative descriptions of the orientation and rough estimates of the magnitude of the transient magnetic field could be made.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics (ISSN 0038-0938); 98; 341-368
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  • 9
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    Great microwave bursts and hard X-rays from solar flares (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: In the present study of the microwave and hard X-ray characteristics of 13 solar flares emitting microwave fluxes greater than 500 solar flux units, simultaneous 3-35 GHz and hard X-ray observations were conducted in the 30-500 keV energy range. An analysis is conducted to determine whether the same distribution of energetic electrons can explain both emissions; tests for any correlations between them yield results suggesting that optically thick microwave emission, near the peak frequency, originates in the same electron population that produces the hard X-rays. A single temperature model and a multitemperature model were tested for consistency with the coincident X-ray and microwave spectra at microwave burst maximum; neither model, however, attempts to explain the high frequency component of the microwave spectrum.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics (ISSN 0038-0938); 96; 339-356
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  • 10
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    Doppler scintillation observations of interplanetary shocks within 0.3 AU (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: It is pointed out that more definitive shock velocity observations near the sun are needed for an improved determination of the extent of shock deceleration from the sun to earth. Woo and Armstrong (1981) have demonstrated the use of radio scattering and scintillation observations, using spacecraft signals, for measuring interplanetary shock waves near the sun. Woo and Armstrong provided the first near-sun profiles of solar wind speed and electron density fluctuation for a shock wave produced by a solar flare. The present investigation has the objective to demonstrate the use of Doppler or phase scintillations for monitoring and observing interplanetary shocks. It is also shown that Doppler noise, a parameter which is routinely observed and recorded by the NASA Deep Space Network, is essentially a measure of Doppler scintillations.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research (ISSN 0148-0227); 90; 154-162
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