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Results for “CORPUSCULAR RADIATION”

Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.

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At least 19 records
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NASA NTRS1989

Energy deposition of corpuscular radiation in the middle atmosphere

Main components of corpuscular radiation contributing to energy deposition (ED in eV/cu cm/s) in the atmosphere (10 to 100 km) are cosmic ray nuclei (CR - galactic and solar) and high energy electrons (HEE), mainly of magnetospheric origin. Galactic CR depending on solar cycle phase and latitude are dominant source of ED by corpuscular radiation below 50 to 60 km. Below 20 km secondaries must be assumed. More accurate treatment need assuming of individual HE solar flare particles, cut off rigidities in geomagnetic field and their changes during magnetospheric disturbances. Electrons E sub e greater than 30 keV of magnetospheric origin penetrating to atmosphere contribute to production rate below 100 km especially on night side. High temporal variability, local time dependence and complicated energy spectra lead to complicated structure of electron ED rate. Electrons of MeV energy found at geostationary orbit, pronouncing relation to solar and geomagnetic activity, cause maximum ED at 40 to 60 km. Monitoring the global distribution of ED by corpuscular radiation in middle atmosphere need continuing low altitude satellite measurements of both HEE and x ray BS from atmosphere as well as measurements of energy spectra and charge composition of HE solar flare particles.

Kudela, K.↗
NASA NTRS1989

Effects of corpuscular radiation on weather and climate

There is no doubt that the antropogenic effect play an important role in the effects of corpuscular radiation on weather and climate. The task, however, is to distinguish between antropogenic effect in the atmosphere due to human activities and natural climatic fluctuations influencing biological systems. The increase in global temperature during the past 100 years is in relatively good coincidence with the increase in geomagnetic (corpuscular) activity. It is concluded that it could have been the increase in temperature on the Northern Hemisphere, due to the processes occurring in the auroral oval under enhanced corpuscular radiation which led to an increased atmospheric concentration of CO2 in the past. Both processes, i.e., antropogenic and solar activity effects, should be therefore intensively studied due to their important role for elucidating the past and present global change mainly in temperature, climate and biological systems.

Bucha, V.↗
NASA NTRS1993

A long-term change of the AR/KR/XE fractionation in the solar corpuscular radiation

Solar noble gases in an ilmenite separate from breccia 79035 (antiquity greater than 1 Ga) were analyzed by closed system stepped etching (CSSE). All five gases show the familiar two-component structure: first solar-wind (SW) gases are released, followed by gases from solar energetic particles (SEP). Element patterns in 79035 are similar to those of 71501 ilmenite. SW-He-Ne were partly lost, but SEP-He-Ne-Ar are retained (nearly) unfractionated. Constant Ar/Kr/Xe ratios indicate that ilmenites contain an unfractionated sample of the heavy SW-SEP noble gases. Ar/Kr/Xe ratios in the solar corpuscular radiation are, however, different from 'solar system' values, whereby the Kr/Xe difference in 79035 is about twice as large as in 71501. We propose that Xe is less fractionated than Kr and Ar, though its first ionization potential (FIP) is higher than the 'cutoff' at approximately 11.5 eV, above which all elements in SEP are usually assumed to be depleted by a roughly constant factor. SW-Ne may be isotopically slightly heavier in the ancient SW trapped by 79035, as proposed earlier. In this work we extend our previous CSSE studies of solar noble gases including Kr and Xe to a lunar sample irradiated at least 1 Ga ago (breccia 79035, ilmenite separate, 42-64 microns). This sample was particularly gently etched in the first steps. Surprisingly, the first three steps, each releasing less than or equal to 0.5% of the total 36-Ar, showed an SEP-like trapped component plus relatively large concentrations of cosmogenic gases. Steps 4ff contain much less cosmogenic and more solar gas with a SW-like isotope pattern. Thus, a very minor easily etchable phase that has completely lost its SW-gases must be responsible for steps 1-3. We will not discuss these steps here and refer to the actual step 4 as the 'initial' etching step.

Wieler, R.↗
NASA NTRS1980

A search for correlation between geomagnetic activity and stratospheric ozone

The total ozone column content (TOZ) measured from the Nimbus 4 BUV experiment is analyzed in geomagnetic coordinates to study a possible link between the solar corpuscular radiation and the lower stratosphere. Using planetary magnetic index Ap as a measure of the solar corpuscular radiation, it is shown that the correlation between TOZ and Ap, if any, occurs predominantly at high latitudes during winter seasons. This is typical of most of the claimed correlations between sun and weather and may be the result of the winter increase of planetary wave activity which by coincidence have periods comparable to magnetic activity. The fact that even major magnetic storms have no detectable effect on the stratospheric ozone during summer does not support a direct cause and effect relation between solar and stratospheric perturbations.

Chandra, S.↗
NASA NTRS1982

Mapping of auroral X-rays from rocket overflights

Remote sensing of energetic auroral X-rays from above the emission region can provide both local and global information regarding X ray and energetic electron deposition within the middle atmosphere. However, contamination of X ray detectors by local corpuscular radiation can severely affect the scope and accuracy of the detector measurements. It is, therefore, necessary to employ techniques designed to observe X rays while rejecting the far more intense corpuscular radiation component. A suitable approach for the mapping of auroral X rays involves the employment of rockets for flights above the emission region. A description is presented of the results obtained from two rocket flights launched from Poker Flat Research Range, Alaska, during aurorally active periods in March 1978. The data were measured with the aid of scanning detectors protected from particles by broom magnet techniques.

Goldberg, R. A.↗