Bochsler, P. — Page 2

NASA NTRS1984

Interpretation of He-3 abundance variations in the solar wind

The ion composition instrument (ICI) on ISEE-3 observed the isotopes of helium of mass 3 and 4 in the solar wind almost continuously between August 1978 and July 1982. This period included the increase towards the maximum of solar activity cycle 21, the maximum period, and the beginning of the descent towards solar minimum. Observations were made when the solar wind speed was between 300 and 620 km/s. For part of the period evidence for regular interplanetary magnetic sector structure was clear and a number of He-3 flares occurred during this time.

Coplan, M. A.↗

NASA NTRS1983

The relative abundance of 3He(++) in the solar wind

Continuous measurements of solar wind 3He(++) and 4He(++) were made covering a full range of solar wind conditions. The average flux ratio derived from these data is 2310 + or - 50, in excellent agreement with the Apollo foil measurements. A probable correlation between average flux ratio and solar activity was found; however, an examination of the data during periods of 3He(++)-rich solar flares shows no detectable increase in 3He(++) in the solar wind.

Coplan, M. A.↗

NASA NTRS1983

Mixed solar wind originating from coronal regions of different temperatures

Ionization states of elements in the solar wind are often used to determine thermal gradients in the lower corona. This method is based on the assumption, that in the beginning, solar wind material has a homogeneous temperature determining the original charge state of elements. Features in M/Q-spectra which might appear if the above assumption is violated are investigated and compared with observational evidence.

Bochsler, P.↗

NASA NTRS1983

Determination of solar wind elemental abundances from M/Q observations during three periods in 1980

Mass spectra in the M/Q range from 2 to 3, provided by a high-resolution mode of the ISEE-3 Plasma Composition Experiment, were evaluated for three selected periods during early 1980. The observed Ne/O ratios are compatible with estimated solar abundance ratios. In two of the three periods, the He/Ne-ratios agree with the Apollo foil results. Freezing-in temperatures for oxygen are similar to those obtained by other groups. Possible reasons for an unexpectedly high flux at M/Q = 2.4 are discussed.

Kunz, S.↗

NASA NTRS1983

Interpretation of 3He variations in the solar wind

The ion composition instrument (ICI) on ISEE-3 observed the isotopes of helium of mass 3 and 4 in the solar wind almost continuously between August 1978 and July 1982. This period included the increase towards the maximum of solar activity cycle 21, the maximum period, and the beginning of the descent towards solar minimum. Observations were made when the solar wind speed was between 300 and 620 km/s. For part of the period evidence for regular interplanetary magnetic sector structure was clear and a number of 3He flares occurred during this time.

Coplan, M. A.↗

NASA NTRS1980

Abundance ratios of He-4/2+//He-3/2+/ in the solar wind

The ion composition experiment aboard the Isee 3 spacecraft has been used to measure the He-4(2+)/He-3(2+) ratio in the solar wind. Using 4334 observations made between Aug. 18 and Nov. 24, 1978, and March 24 and Aug. 25, 1979, the average ratio He-4(2+)/He-3(2+) was 2.1 + or - 0.2 x 1000, in agreement with previous foil measurements. Individual observations vary widely from the average and the low He-4(2+)/He-3(2+) ratios occur at times of low He-4(2+) flux.

Ogilvie, K. W.↗

NASA NTRS1980

Observations of the velocity distribution of solar wind ions

Measurements made by the Isee 3 ion composition experiment have been used to determine the kinetic temperatures of 3He(++), 4He(++), 16O(6+), and 16O(7+) in the solar wind. It is found that these temperatures generally obey the relation that T(i)/m(i) equals const, but fluctuations, some of which are caused by dynamical effects in the flow, are observed. The temperature of oxygen sometimes rises above 10 K, which is very strong evidence for heating outside the collisional region of the corona. The tendency toward equal temperatures per nucleon occurs everywhere where collisions are unimportant, suggesting that the temperatures are set up close to the sun rather than elsewhere in the interplanetary medium. The velocity distribution function of helium is observed to be non-Maxwellian, with a pronounced high velocity tail.

Ogilvie, K. W.↗