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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 163 records · Page 9
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NASA NTRS1995

Ulysses observations of energetic ions over the south pole of the Sun

The Ulysses spacecraft began its journey out-of-the-ecliptic in February of 1992, when it encountered the planet Jupiter. In April of 1993, the spacecraft had reached 29 deg S, and from then on was completely immersed in the flow from the southern polar coronal hole. Accelerated ions were observed, recurring with a main peak once per solar rotation, with the intensity at the peak slowly decreasing with increasing latitude. This decrease continued to the end of 1993, when the spacecraft was at approximately 50 deg S. During the first three months of 1994 the intensity of the accelerated ions rose again, due either to an increase in magnetic activity on the sun or a reconfiguration of the heliospheric magnetic field. Recurrent accelerated ions were still being seen at the beginning of July 1994, when the spacecraft was at a latitude of 70 deg S, although with reduced intensity. The accelerated ions were no longer seen at latitudes higher than 70 deg S, the ion intensity staying constant at around the cosmic ray background level. This continued on until the highest latitude reached, 80.2 deg S, on 13 September 1994. The spacecraft then began its journey back towards lower latitudes, a small increase in the particle intensity being observed at the end of October whilst at approximately 72 deg S, and thereafter no more increases until the end of 1994, when the spacecraft was at approximately 45 deg S. We present interpretations for this asymmetry in latitude dependence.

Sanderson, T. R.↗
NASA NTRS1994

The CELSS Antarctic Analog Project: An Advanced Life Support Testbed at the Amundsen-Scott South Pole Station, Antarctica

CELSS Antarctic Analog Project (CAAP) represents a logical solution to the multiple objectives of both the NASA and the National Science Foundation (NSF). CAAP will result in direct transfer of proven technologies and systems, proven under the most rigorous of conditions, to the NSF and to society at large. This project goes beyond, as it must, the generally accepted scope of CELSS and life support systems including the issues of power generation, human dynamics, community systems, and training. CAAP provides a vivid and starkly realistic testbed of Controlled Ecological Life Support System (CELSS) and life support systems and methods. CAAP will also be critical in the development and validation of performance parameters for future advanced life support systems.

Straight, Christian L.↗
NASA NTRS2002

The Recent Mars Global Warming (MGW) and/or South Pole Advance (SPA) Hypothesis: Global Geological Evidence and Reasons Why Gullies Could Still be Forming Today

Hundreds of modern striped valleys, rock glaciers, debris-covered glaciers, and cryokarstic features localized in a strict latitude/altitude domain show a clear morphological and environmental continuum best explained by a recent climate change. Additional information is contained in the original extended abstract.

Cabrol, Nathalie A.↗
NASA NTRS1995

Ulysses above the sun's south pole: an introduction

Ulysses has explored the field and particle environment of the sun's polar region. The solar wind speed was fast and nearly constant above -50 degrees latitude. Compositional differences were observed in slow (low-latitude) solar wind and in fast (high-latitude) solar wind. The radial magnetic field did not change with latitude, implying that polar cap magnetic fields are transported toward the equator. The intensity of galactic cosmic rays was nearly independent of latitude. Their access to the polar region is opposed by outward-traveling, large amplitude waves in the magnetic field.

Solar System↗
NASA NTRS2010

South Pole Hydrogen Distribution for Present Lunar Conditions: Implications for Past Impacts

It has been known since the Lunar Prospector mission that the poles of the Moon evidently harbor enhanced concentrations of hydrogen [1,2]. The physical and chemical form of the hydrogen has been much debated. Using imagery from Clementine it was possible to roughly estimate permanently-shadowed regions (PSRs), and to perform image reconstructions of the Lunar Prospector epithermal neutron flux maps [3,4]. The hydrogen concentrations resulting from these reconstructions were consistent with a few weight percent water ice in selected locations. With the LCROSS impact, we now know that hydrogen in the form of ice does exist in lunar polar cold traps [5]. Armed with this information, and new data from LRO/Diviner, we can examine whether the pre-sent-day distribution of hydrogen in the form of water ice is consistent with a past large impact that delivered a large mass of volatiles to the lunar surface. These volatiles, mixed with solid impact ejecta, would then be lost from locations having high mean temperatures but would otherwise remain trapped in locations with sufficiently low mean annual temperatures [6]. The time scales for loss would depend on the location-dependent temperatures as well as impact history.

Elphic, R. C.↗
NASA NTRS2012

Mars Atmospheric CO2 Condensation Above the North and South Poles as Revealed by Radio Occultation, Climate Sounder, and Laser Ranging Observations

We study the condensation of CO2 in Mars atmosphere using temperature profilesretrieved from radio occultation measurements from Mars Global Surveyor (MGS) as wellas the climate sounding instrument onboard the Mars Reconnaissance Orbiter (MRO),and detection of reflective clouds by the MGS Mars Orbiter Laser Altimeter (MOLA). Wefind 11 events in 1999 where MGS temperature profiles indicate CO2 condensation andMOLA simultaneously detects reflective clouds. We thus provide causal evidence thatMOLA non-ground returns are associated with CO2 condensation, which strongly indicatestheir nature being CO2 clouds. The MGS and MRO temperature profiles together revealthe seasonal expansion and shrinking of the area and the vertical extent of atmosphericsaturation. The occurrence rate of atmospheric saturation is maximized at high latitudes inthe middle of winter. The atmospheric saturation in the northern polar region exhibits moreintense seasonal variation than in the southern polar region. In particular, a shrinking ofsaturation area and thickness from LS 270 to 300 in 2007 is found; this is probablyrelated to a planet-encircling dust storm. Furthermore, we integrate the condensation areaand the condensation occurrence rate to estimate cumulative masses of CO2 condensatesdeposited onto the northern and southern seasonal polar caps. The precipitation flux isapproximated by the particle settling flux which is estimated using the impulse responses ofMOLA filter channels. With our approach, the total atmospheric condensation mass canbe estimated from these observational data sets with average particle size as the onlyfree parameter. By comparison with the seasonal polar cap masses inferred from thetime-varying gravity of Mars, our estimates indicate that the average condensate particleradius is 822 mm in the northern hemisphere and 413 mm in the southern hemisphere.Our multi-instrument data analysis provides new constraints on modeling the global climateof Mars.

MOLA↗
NASA NTRSDate not supplied

Dust Mitigation: Impacts & Opportunities for Science on the Lunar South Pole

Lunar dust will be a feature of all lunar surface science investigations, whether welcome or not. While lunar dust may pose problems for some investigations, it is also the subject of many critical scientific discoveries made since the Apollo days. Dust mitigation, or learning how to work with and around the inevitable dust we will encounter on the surface, is not a new concept. However, new initiatives throughout NASA are underway in an effort to tackle dust mitigation strategically for the Artemis program. Dust mitigation efforts and technologies will enable successful lunar surface science investigations.

lunar dust↗
NASA NTRS2020

Lunar Lettuce Production During Artemis III Mission to the Moon's South Pole

The Artemis Science Plan identified that the infrastructure and resources associated during a human/robotic exploration mission can be used to conduct fundamental lunar science needed to mitigate the risks of human exploration of surface systems (i.e. Mars and the Moon). In particular, studying the response of life to the combination of fractional gravity and deep space radiation of the Moon is needed to mitigate the HEOMD risks to the crew that result from inadequate diets. Essential nutrients and vitamins available to astronauts have been shown to degrade within the stored food system during long duration missions. Other risks to exploration missions were isolation and confinement, distance from the Earth, radiation and partial gravity.

O. Monje↗
NASA NTRSDate not supplied

Dynamic Power Generation for Human and Scientific Exploration of the Lunar South Pole

Many NASA missions visit some of the harshest, darkest, coldest locations in the solar system and would not be possible, or would be extremely limited, without the use of nuclear power. Radioisotope Power Systems, or RPS, harness the heat of the natural decay of plutonium-238, to produce continuous electric power for operating spacecraft systems and science instruments. Radioisotope power has provided this “Power to Explore” for the past 60 years.

DRPS↗