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  • 1
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    Distribution of small volcanic cones on the surface of Venus by size and elevation: Implications for differential deposition of volcanic features (1993)
    In:  Other Sources
    Details
    Publication Date: 2019-01-25
    Description: It appears that volcanic features are not evenly distributed on the surface of Venus. Head et. al. theorizes that the sparcity of volcanic features in the lowlands may be due to an altitude dependent inhibition of volatile exsolution and the resulting products of neutral buoyancy zones sufficient to form magma reservoirs and favoring flood lavas at lower elevation. The astronomy research classes of Evergreen and Sahuaro High Schools surveyed a cross-section of different elevation topography to investigate size and distribution of small volcanic cones by elevation. The results from this survey are presented.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Twenty-Fourth Lunar and Planetary Science Conference. Part 3: N-Z; p 1231-1232
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  • 2
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    Neutron albedo measurements on rocket flights. (1966)
    In:  Other Sources
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    Publication Date: 2019-05-30
    Description: Rocket-borne neutron detector measurements of neutron albedo and intensities at various geomagnetic latitudes
    Keywords: SPACE RADIATION
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  • 3
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    Observations of the dynamics of the cosmic ray modulation (1984)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: New measurements of the outward propagation of the cosmic ray modulation and large transient decreases at a radial distance of 10-30 AU from the earth are reported. Also, new observations of the hysteresis effect in the 11-year modulation are presented for two solar cycles, and an attempt is made to reproduce the long-term modulation at earth from the observed transient or Forbush decreases. The results indicate that steady-state, spherically symmetric models of the heliosphere are not capable of explaining the 11-year variation. A time-dependent solution to the cosmic ray transport equation is required to describe the solar cosmic ray modulation.
    Keywords: SPACE RADIATION
    Type: Journal of Geophysical Research (ISSN 0148-0227); 89; 17-25
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  • 4
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    Cosmic ray gradients in the heliosphere and particle drifts (1981)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: K-coronameter, solar wind, and neutron monitor data are used to estimate the latitudinal gradient of protons of approximately 5 GeV in the heliosphere at 1 AU during 1965 and 1975. The reversal of sign of the gradient between 1965 and 1975 and the strong positive latitudinal gradient in 1975 predicted by models in which drifts are dominant are not observed.
    Keywords: SPACE RADIATION
    Type: Geophysical Research Letters; 8; June 198
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  • 5
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    The cosmic ray interplanetary radial gradient from 1972 - 1985 (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: It is now established that the solar modulation of cosmic rays is produced by turbulent magnetic fields propagated outward by the solar wind. Changes in cosmic ray intensity are not simultaneous throughout the modulation region, thus requiring time dependent theories for the cosmic ray modulation. Fundamental to an overall understanding of this observed time dependent cosmic ray modulation is the behavior of the radial intensity gradient with time and heliocentric distance over the course of a solar modulation cycle. The period from 1977 to 1985 when data are available from the cosmic ray telescopes on Pioneer (P) 10, Voyager (V) 1 and 2, and IMP 8 spacecraft is studied. Additional data from P10 and other IMP satellites for 1972 to 1977 can be used to determine the gradient at the minimum in the solar modulation cycle and as a function of heliocentric distance. All of these telescopes have thresholds for protons and helium nuclei of E 60 MeV/nucleon.
    Keywords: SPACE RADIATION
    Type: SH-4.7-1 , 19th Intern. Cosmic Ray Conf - Vol. 5; p 185-188; NASA-CP-2376-VOL-5
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  • 6
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    Latitudinal gradients of cosmic rays and the polarity reversal of the heliospheric magnetic field: A preliminary evaluation (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Within the statistical limits imposed by the currently available data and the noise inherent in the determination of the latitudinal gradient, no evidence for the expected change in the latitudinal gradient from pre-1980 to post-1980 epochs can be found. In addition, the rigidity dependence of the gradient appears to be the same in the two epochs. Thus, no evidence is found for a sensitivity of the latitudinal gradient to the polarity of the largescale heliospheric magnetic field such as has been predicted by models incorporating particle drifts.
    Keywords: SPACE RADIATION
    Type: SH-4.2-16 , 19th Intern. Cosmic Ray Conf - Vol. 4; p 469-472; NASA-CP-2376-VOL-4
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  • 7
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    The intensity recovery of Forbush-type decreases as a function of heliocentric distance and its relationship to the 11-year variation (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Recent data indicating that the solar modulation effects are propagated outward in the heliospheric cavity suggest that the 11-year cosmic ray modulation can best be described by a dynamic time dependent model. In this context an understanding of the recovery characteristics of large transient Forbush type decreases is important. This includes the typical recovery time at a fixed energy at 1 AU as well as at large heliocentric radial distances, the energy dependence of the recovery time at 1 Au, and the dependence of the time for the intensity to decrease to the minimum in the transient decreases as a function of distance. These transient decreases are characterized by their asymmetrical decrease and recovery times, generally 1 to 2 days and 3 to 10 days respectively at approx. 1 AU. Near earth these are referred to as Forbush decreases, associated witha shock or blast wave passage. At R equal to or greater than + or - 10 AU, these transient decreases may represent the combined effects of several shock waves that have merged together.
    Keywords: SOLAR PHYSICS
    Type: SH-4.1-9 , 19th Intern. Cosmic Ray Conf - Vol. 4; p 388-391; NASA-CP-2376-VOL-4
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  • 8
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    Energetic solar particle fluxes out to 3 AU during the 7 May 1978 flare event (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Simultaneous solar proton flux measurements on IMP 7 and by the world wide neutron monitor network during the May 7, 1978 flare event led to conclusions that in the energy range from 50 MeV to 10 GeV: (1) the propagation of the flare particles in the interplanetary magnetic field (IMF) between the Sun and the Earth was nearly scatter free; and (2) therefore, the intensity time (IT) profiles of the solar proton fluxes observed at Earth for about one hour after onset represent the solar injection profiles even to energies as low as 50 MeV. Observations of the IMF at Helios A indicate that the IMF was undisturbed between the Sun and Helios A at the time of the May 7, 1978 flare event; and, therefore, the solar particle propagation was also scatter free from the Sun to Helios A.
    Keywords: SOLAR PHYSICS
    Type: SH-3.2-6 , 19th Intern. Cosmic Ray Conf - Vol. 4; p 351-354; NASA-CP-2376-VOL-4
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  • 9
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    Some characteristics of the solar flare event of February 16, 1984 (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: In the morning of February 16, 1984 a solar cosmic ray event (GLE) was recorded by the world wide network of neutron monitors (NM). The counting rate vs. time profile of the Goose Bay NM (geog. lat. = 53.3 deg. N, deog. long. = 299.6 deg E) where the increase is expressed as percent of the counting rate of an equatorial sea level NM is presented. The Goose Bay NM was observed to have the maximum response to the solar particles. Its counting rate vs. time profile exhibits a rapid increase to maximum, has a large amplitude (approx. 170%) and decays rapidly to background in approx. 90 min. In Fig. 1 we also show the counting rate vs. time profile for the Tixie Bay NM (71.6 deg, 128.9 deg) which recorded an increase of only a few percent. Since the NMs at Goose Bay and Tixie Bay have asymptotic viewing directions approx. 180 deg apart in longitude, the anisotropy of the solar particle flux at Earth from these stations.
    Keywords: SOLAR PHYSICS
    Type: SH-3.1-7 , 19th Intern. Cosmic Ray Conf - Vol. 4; p 317-320; NASA-CP-2376-VOL-4
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  • 10
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    Solar activity and modulation of the cosmic ray intensity (1985)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: Since its discovery by Forbush (1954), the 11-year cycle modulation of the cosmic ray intensity has been studied extensively. Bowe and Hatton (1982) obtained a well-behaved transfer function F between the solar activity S and the cosmic ray intensity modulation Io-I. They suggested that the 11-year variation for sunspot cycle 20 can be attributed to the modulating effect of solar flare-induced shocks propagating through the heliosphere. The cosmic ray intensity in the absence of solar activity is denoted by Io, while I denotes the observed intensity. Bowe and Hatton infer that the boundary of the heliosphere is located at a distance of 70-90 AU. Since their conclusion is of great importance in understanding the mechanism of the 11-year modulation, the present investigation is concerned with a repetition of their study for two cycles, taking into account the use of a slightly modified method. The obtained results confirm the conclusions reached by Bowe and Hatton that there is a well-behaved transfer function for solar flares.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research (ISSN 0148-0227); 90; 4439-444
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