John H. Hoffman

From Wikipedia, the free encyclopedia

This article may require cleanup to meet Wikipedia's quality standards. Please improve this article if you can. (June 2008)

This article or section may contain original research or unverified claims. Please improve the article by adding references. See the talk page for details. (June 2008)

Sections should be added to this article, to conform with Wikipedia's Manual of Style. Please discuss this issue on the talk page. This article has been tagged since June 2008.

This article does not cite any references or sources. (June 2008) Please help improve this article by adding citations to reliable sources. Unverifiable material may be challenged and removed.

This article or section needs to be wikified to meet Wikipedia's quality standards. Please help improve this article with relevant internal links. (June 2008)

John Hoffman is a space scientist who developed instruments for Apollo 15, Apollo 16, Apollo 17, Pioneer Venus project, and Giotto mission; also designed the mass spectrometer for the Phoenix Mars Lander mission in May 2008. He is currently a professor of physics at The University of Texas at Dallas.

History

John Hoffman received his bachelor's degree from St. Mary's College in Winona Minnesota and continued his education at the University of Minnesota under the mentorship of Professor A. O. C. Nier who pioneered the field of mass spectroscopy. His PhD dissertation was on the helium isotopic distribution in large iron meteorites.

He spent 7 years at the U. S. Naval Research Laboratory, Washington, D. C., developing miniaturized mass spectrometers for space flight. These were flown on Aerobee and Javelin rockets.

Dr. Hoffman joined the Graduate Research Center of the Southwest in 1966. His main interest was in the study of atmospheric/ionospheric composition and isotopic ratios for which he has developed instrument packages that have flown on many rockets and satellites.

He developed instruments for the Apollos 15, 16, and 17 lunar missions, the latter being part of the ALSEP surface package. The goal was to detect and determine the composition of the lunar atmosphere. There is an atmosphere on the moon composed mainly of noble gases and hydrogen, but the pressure is lower than that in the best vacuum systems on earth.

His instrument flew on the Pioneer Venus mission to Venus in 1978. Data was received throughout the descent of the probe to the surface. Carbon dioxide is the dominant gas in the atmosphere. A surprise discovery showed that for the two "sister" planets there is a two order of magnitude difference in the isotopic ratios (the ratio of the heavier to lighter forms of these gases) for hydrogen and argon than for those gases on earth. These isotopic ratio differences have had large implications on models of the nature of the solar nebula and the formation of the present (secondary) atmospheres of the terrestrial planets.

Hoffman was a member of the team who flew a mass spectrometer on the European Space Agency's Giotto mission to Halley's Comet in 1986. This instrument was developed by laboratories in four countries, three European and at UT Dallas. It measured both the neutral and ionized constituents of the comet's coma. The coma contains, besides water vapor and H30 ions, an extended source of carbon monoxide. The atmosphere forms around a comet as it comes near the sun and is heated by radiation from the sun.

Hoffman has also flown mass spectrometers on earth orbiting satellites, Explorer 31, ISIS-II, AE-C, D, and E, and Wake Shield, plus numerous sounding rockets and stratospheric balloon flights. The first observations of the polar wind, ions flowing out from the atmosphere, were made by his ion mass spectrometer flown on the ISIS spacecraft in 1971.

Dr. Hoffman is a co-investigator for the TEGA experiment that will fly on the Mars Scout Phoenix mission in 2007. The spacecraft will land in the far northern region of Mars, above the Arctic Circle in the area that the Mars Odyssey spacecraft has found evidence for water. An arm on the lander will dig a trench a meter deep in the surface of Mars to look for water ice and other water related substances (minerals). These will be scooped up and analyzed in a series of small furnaces. The effluents from the furnaces will be analyzed by the UT Dallas mass spectrometer to determine the presence of water and the mineralogical composition of soil samples. Isotopic ratios of the principal elements in the samples will be determined and compared to the isotopic ratios of the atmospheric gases that will be measured by the mass spectrometer when it is not analyzing samples from the TEGA furnaces.

This article is uncategorized. Please categorize this article to list it with similar articles. (June 2008)