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Hoffman, J. H.

Publications and source records attributed to Hoffman, J. H..

At least 73 records · Page 4
All sourcesNASA NTRSDOE OSTI
NASA NTRS1975

Implications of atmospheric Ar-40 escape on the interior structure of the moon

Radiogenic Ar-40 escapes from the lunar atmosphere at a rate of about 2 x 10 to the 21st atoms/sec. This amounts to 8% of the rate of argon production in the entire moon by potassium decay. A curious feature of the argon escape rate is a variability with time scale of several months. It is shown that the variation in argon loss correlates with high-frequency lunar teleseismic events. The only apparent region of the moon which could possibly supply the amount of argon needed for escape via a plausible temporal mechanism is a semimolten asthenosphere which may be entirely primitive unfractionated lunar material, or an Fe-FeS core that is enriched in potassium. A core that is devoid of potassium is not compatible with the atmospheric argon measurements.

Hodges, R. R., Jr.↗
NASA NTRS1974

Initial ion composition results from the Isis 2 satellite

Isis 2 satellite carried, among other ionospheric instruments an ion mass spectrometer designed to measure the composition of the ionosphere in the mass range from 1 to 64 amu. The satellite, in a nearly constant 1400-km orbit, was launched on April 1, 1971. Examples of data show a wide variation in ion composition from 99% H(+) at night near the equator to greater than 95% O(+) and N(+) in the daytime poleward of the plasmapause. Both H(+) and He(+) are observed to be streaming outward from the high-latitude regions with velocities of several kilometers per second (the polar wind), determined from phase shifts in roll modulation maximums between light and heavy ion species. During the August 1972 magnetic storm a unique ionosphere developed, consisting of N(+) as the dominant species between 55 and 80 deg invariant latitude (above the plasmapause) and N2(+), NO(+), and O2(+) at the 1000 per cu cm concentration level, whereas these molecular species are usually below the detection limit of 1 ion per cu cm in quiet times at this altitude.

Hoffman, J. H.↗
NASA NTRS1974

Mass spectrometric measurements of atmospheric composition

The development of a magnetic sector field analyzer for continuous sampling and measurement of outer planetary atmospheres is discussed. Special features of the analyzer include a dynamic range of 10 to the minus 7th power, a mass range from 1 to 48 AMU, two ion sensitivities, a special scan time of 35 sec at 14 BPS, and the use of ion counting techniques for analysis.

Hoffman, J. H.↗
NASA NTRS1974

Observation of a two-temperature ion energy distribution in regions of polar wind flow

Study of deviations from thermal equilibrium among the ions in the ionosphere by considering that the 'light' ions H(+) and He(+) may be at a different temperature from the 'heavy' ion O(+). In particular, the case in which thermal protons are observed to be flowing relative to the assumed static ambient oxygen ions is considered. The proton flow is assumed to be along the direction of the magnetic field. Of the cases tested, it is found that the measured proton temperature is from one to ten times the measured oxygen ion temperature. Such temperature enhancements may be expected both because of the energy transfer associated with the ion flow and as a consequence of the preferential energy coupling from the light-ion distribution in the exosphere.

Maier, E. J.↗
NASA NTRS1974

Measurements of solar wind helium in the lunar atmosphere

Measurements of lunar atmospheric helium during 1973 from the Apollo 17 surface mass spectrometer are presented. The average helium abundance is shown to be about 70% of the theoretical model value, suggesting that the solar wind helium flux in 1973, during sunspot minimum, was substantially less than the expected average flux. Large-amplitude transients in the helium data indicate rapid response of the lunar atmosphere to changes in solar wind. The atmospheric helium abundance is shown to be correlated with the geomagnetic index Kp.

Hodges, R. R., Jr.↗
NASA NTRS1974

The lunar atmosphere

In contrast to the earth's atmosphere, the atmosphere of the moon is exceedingly tenuous and appears to consist mainly of noble gases. The solar wind impinges on the lunar surface, supplying detectable amounts of helium, neon and Ar-36. Influxes of solar wind protons and carbon and nitrogen ions are significant, but atmospheric gases containing these elements have not been positively identified. Radiogenic Ar-40 and Rn-222 produced within the moon have been detected. The present rate of effusion of argon from the moon accounts for about 0.4% of the total production of Ar-40 due to decay of K-40 if the average abundance of potassium in the moon is 1000 ppm. Lack of weathering processes in the regolith suggests that most of the atmospheric Ar-40 originates deep in the lunar interior, perhaps in a partially molten core. If so, other gases may be vented along with the argon.

Hodges, R. R., Jr.↗
NASA NTRS1974

Episodic release of Ar-40 from the interior of the moon

Measurements of lunar atmosphere made by the mass spectrometer at the Apollo 17 landing site during the first 9 lunations of 1973 show an apparently cyclical variation of radiogenic Ar-40, with maximum to minimum abundance ratio of about 2. There seems to be a 6-7 month periodicity in the oscillation, but the limited data base makes a fixed oscillatory pattern uncertain. The significance of the variation of atmospheric argon lies in the implication that its source is episodic in nature, ranging in strength from about 1% of the total rate of production of Ar-40 in the moon to near zero. This requires a presently active mechanism for transient venting of gas from deep within the moon.

Hodges, R. R., Jr.↗
NASA NTRS1973

Composition and physics of the lunar atmosphere.

The existence in the lunar atmosphere of helium, neon, argon, and possibly molecular hydrogen has been confirmed by the Apollo 17 mass spectrometer. The observed helium concentrations and distribution agree closely with model predictions for a non-condensable gas based on a solar wind source, thermal escape and a Monte Carlo random walk calculated longitudinal distribution. Heavier gases are lost by photoionization and subsequent sweeping away by the solar wind electric field. The observed nighttime neon concentration of 80,000 molecules per cu cm is consistent with expected amounts. Argon, however, is adsorbed on the lunar surface late at night when the surface temperature is lowest. It shows the expected predawn enhancement exhibited by condensable gases released into the atmosphere at the sunrise terminator. Hydrogen appears to exist in the molecular rather than atomic state. Its observed concentration is less than a factor of 3 higher than that predicted by a model similar to that used for helium.

Hoffman, J. H.↗
NASA NTRS1973

The magnetic ion-mass spectrometer on Atmosphere Explorer.

The magnetic ion-mass spectrometer is designed to measure the abundances of the ambient positive ions in the ionosphere. It will be calibrated in flight against the retarding-potential analyzer and the cylindrical electrostatic probe to give absolute concentration data for the ion species detected. These parameters can be measured to approximately plus or minus 10% in well-behaved regions where concentrations are above 1000/cu cm. However, in highly structured polar regions, some degradation in accuracy may be expected. Three mass ranges, covered simultaneously by the scan of the instrument, 1 to 4, 4 to 16, and 16 to 64 amu, permit measurement of the entire mass range, 1 to 64 amu, in 1 sec in the main (peaks) mode. An alternate mode, analog-long, will extend the mass range to 90 amu with a 9-sec period.

Hoffman, J. H.↗
NASA NTRS1973

Absolute calibration of Apollo lunar orbital mass spectrometer.

Recent experiments were conducted in Langley Research Center's molecular beam system to perform an absolute calibration of the lunar orbital mass spectrometer which was flown on the Apollo 15 and 16 missions. Tests were performed with several models of the instrument using two test gases, argon and neon, in the 1 ntorr to .1 picotorr range. Sensitivity to argon at spacecraft orbital velocity was .00028 A/torr enabling partial pressures in the .01-picotorr range to be measured at the spacecraft altitude. Neon sensitivity was nearly a factor of 5 less. Test data support the feasibility of using the lunar orbital mass spectrometer as a tool to gather information about the lunar atmosphere.

Yeager, P. R.↗
NASA NTRS1973

Composition and dynamics of lunar atmosphere

The model of lunar atmosphere is updated to take into account new information on the dynamics and amounts of H2, He-4, Ne-20, Ar-36, and Ar-40. Helium and neon appear to be in close balance with the solar wind, although Ar-36 is depleted in the atmosphere, suggesting that surface materials are not saturated with argon. Atmospheric carbon compounds, which should result from the solar wind influx of carbon, remain undetected, as do nitrogen compounds. However, evidence of a volcanic gas release is presented, which suggests the transient presence of these elements.

Hodges, R. R., Jr.↗
NASA NTRS1972

Orbital search for lunar volcanism.

The total rate of volcanic release of gases into the lunar atmosphere is estimated to be less than 60 g/sec. One of the implications of this degassing is that, if it occurs as sporadic releases of large quantities of gas, these events can be detected by an orbiting mass spectrometer, such as that carried on the flight of Apollo 15 and one that will operate during the Apollo 16 mission. The nature of a volcanic perturbation of the lunar atmosphere is discussed, and a lower bound is derived for the expected time between detected events.

Hodges, R. R., Jr.↗
NASA NTRS1972

Lunar orbital mass spectrometer experiment

The experiment to measure the composition and distribution of the ambient lunar atmosphere by mass spectrometer is reported. The lunar orbital mass spectrometer is described along with the calibration procedures for the instrument. Preliminary results indicate that a large number of gas molecules were observed in the vicinity of the spacecraft in lunar orbit. Many of these molecules are considered to be of spacecraft origin.

Hoffman, J. H.↗
NASA NTRS1972

Lunar orbital mass spectrometer experiment

A lunar orbital mass spectrometer carried by the Apollo 16 command and service module was used to detect the lunar atmosphere and to search for active lunar volcanism. The experimental procedure and results are described.

Hodges, R. R.↗
NASA NTRS1972

Lunar orbital mass spectrometer experiment.

One of the Orbital Science experiments on Apollo 15 was a mass spectrometer designed to measure the composition and distribution of the lunar atmosphere. It operated for nearly 90 hours, producing spectra of an unexpectedly complex nature, indicating that many complex gas molecules exist in the vicinity of the spacecraft. The most plausible explanation is that there was continual vaporization of frozen or liquid drops of water, fuel, or other matter that had been ejected from the spacecraft with small relative velocity so that these particles remained in nearby orbits. The search for naturally occurring gases in these spectra involves a statistical analysis of the data which has not been completed to date. A theoretical prediction regarding the possibilities of detecting lunar volcanism from orbit is included.

Hoffman, J. H.↗