Persistent Identifier
|
hdl:2014/45295 |
Publication Date
|
2010-03-06 |
Title
| The U.S. Rosetta Project at its first science target: Asteroid (2867) Steins, 2008 |
Author
| Alexander, C. (Pasadena, CA : Jet Propulsion Laboratory, National Aeronautics and Space Administration, 2010)
Sweetnam, D. (Pasadena, CA : Jet Propulsion Laboratory, National Aeronautics and Space Administration, 2010)
Gulkis, S. (Pasadena, CA : Jet Propulsion Laboratory, National Aeronautics and Space Administration, 2010)
Weissman, P. (Pasadena, CA : Jet Propulsion Laboratory, National Aeronautics and Space Administration, 2010)
Holmes, D. (Pasadena, CA : Jet Propulsion Laboratory, National Aeronautics and Space Administration, 2010)
Parker, J. (Pasadena, CA : Jet Propulsion Laboratory, National Aeronautics and Space Administration, 2010)
Burch, J. (Pasadena, CA : Jet Propulsion Laboratory, National Aeronautics and Space Administration, 2010)
Goldstein, R. (Pasadena, CA : Jet Propulsion Laboratory, National Aeronautics and Space Administration, 2010)
Mokashi, P. (Pasadena, CA : Jet Propulsion Laboratory, National Aeronautics and Space Administration, 2010)
Fuselier, S. (Pasadena, CA : Jet Propulsion Laboratory, National Aeronautics and Space Administration, 2010)
McFadden, L. (Pasadena, CA : Jet Propulsion Laboratory, National Aeronautics and Space Administration, 2010) |
Point of Contact
|
Use email button above to contact.
Alexander, C. |
Description
| On September 5, 2008, the International Rosetta Mission encountered its first formal science target of the mission, asteroid (2867) Steins. We report preliminary results from the U.S. experiments. NASA’s contribution to the Rosetta mission consists of an ultraviolet (UV) spectrometer, a microwave spectrometer, a plasma instrument, and a portion of the electronics package for a mass spectrometer. The UV spectrometer (Alice) was used to obtain the first far-ultraviolet (FUV) spectrum of an asteroid. A ten-minute integration, surrounding the time of closest approach, averaging over a variety of geometries, showed very good signal from 850 Å to 2000 Å in the FUV. The microwave instrument (MIRO) obtained a high signal to noise measurement at both observing frequencies, enabling key thermal parameters to be derived. The plasma instrument (IES) obtained a brief measurement of the solar wind, and the Double Focusing Mass Spectrometer (DFMS) of the ROSINA instrument obtained a signal just at closest approach. Laboratory work with analogue materials was begun. |
Subject
| Other |
Production Date
| 2010-03-06 |