Characteristics of the Interstellar Helium by the He I 58.4-nm Optical Observation

Details Characteristics of the Interstellar Helium by the He I 58.4-nm Optical Observation Characteristics of the Interstellar Helium by the He I 58.4-nm Optical Observation

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh22d03y&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH22D-03

Physics

2144 Interstellar Gas, 2194 Instruments And Techniques

Scientific paper

There is a region with high-density helium gas in shape of a corn in the solar system, which is called the helium cone. The helium atoms originate from the local interstellar medium (LISM), and are injected into the heliosphere with the interstellar wind. The solar gravity force and radiation pressure decide the helium density distribution in the helium cone. Therefore the velocity, the density, and the temperature of the interstellar helium is estimated from the helium density distribution in the helium cone. An eXtreme Ultra-Violet (XUV) scanner has been built for Japanese first Mars Explorer, Planet-B. The scanner has detected the He I 58.4-nm emission resonantly scattered by the helium atoms in the helium cone on the Planet-B's cruise orbit to Mars. The He I emission rate is estimated from the helium cone formation model under the condition that the velocity vector of the interstellar wind and the loss rate (ionization rate) of helium atom in the interplanetary space are constant. The best agreement between the observation and the model gives the LISM parameters.

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