Radio Science Results During the NEAR-Shoemaker Spacecraft Rendezvous with Eros-Reference-Cited by-同舟云学术

Radio Science Results During the NEAR-Shoemaker Spacecraft Rendezvous with Eros

Published:2000-09-22 Issue:5487 Volume:289 Page:2085-2088
ISSN:0036-8075
Container-title:Science
language:en
Short-container-title:Science

Author:

Yeomans D. K.¹,Antreasian P. G.¹,Barriot J.-P.²,Chesley S. R.¹,Dunham D. W.³,Farquhar R. W.³,Giorgini J. D.¹,Helfrich C. E.¹,Konopliv A. S.¹,McAdams J. V.³,Miller J. K.¹,Owen W. M.¹,Scheeres D. J.⁴,Thomas P. C.⁵,Veverka J.⁵,Williams B. G.¹

Affiliation:

1. Navigation and Mission Design Section, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.

2. Department of Terrestrial and Planetary Geodesy, Centre National d'Etudes Spatiales, Toulouse, France.

3. Applied Physics Laboratory, Johns Hopkins University, Laurel, MD 20723, USA.

4. Department of Aerospace Engineering, University of Michigan, Ann Arbor, MI 48109–2140, USA.

5. Cornell University, Ithaca, NY 14853, USA.

Abstract

We determined the mass of asteroid 433 Eros, its lower order gravitational harmonics, and rotation state, using ground-based Doppler and range tracking of the Near Earth Asteroid Rendezvous (NEAR)–Shoemaker spacecraft and images of the asteroid's surface landmarks. The mass of Eros is (6.687 ± 0.003) × 10 18 grams, which, coupled with our volume estimate, implies a bulk density of 2.67 ± 0.03 grams per cubic centimeter. The asteroid appears to have a uniform density distribution. The right ascension and declination of the rotation pole are 11.37 ± 0.05 and 17.22 ± 0.05 degrees, respectively, and at least over the short term, the rotation state of Eros is stable with no measurable free precession of the spin pole. Escape velocities on the surface vary from 3.1 to 17.2 meters per second. The dynamical environment of Eros suggests that it is covered with regolith and that one might expect material transport toward the deepest potential wells in the saddle and 5.5-kilometer crater regions.

Publisher

American Association for the Advancement of Science (AAAS)

Subject

Multidisciplinary

Reference16 articles.

1. Imaging of Asteroid 433 Eros During NEAR's Flyby Reconnaissance

2. Estimating the Mass of Asteroid 433 Eros During the NEAR Spacecraft Flyby

3. G. J. Bierman Factorization Methods for Discrete Sequential Estimation (Academic Press New York 1977).

4. W. M. Kaula Theory of Satellite Geodesy (Blaisdell Waltham MA 1966).

5. Traditional optical navigation requires images of reference stars to be in the same picture as images of the target body. However star images never appear in pictures of Eros' surface partly because the asteroid often fills the field of view partly because the camera is tracking the asteroid so that the stars would be trailed but mostly because the surface brightness of Eros is so great that the stars would be too dim to register. We therefore obtain the inertial attitude of the camera indirectly from the telemetered spacecraft attitude as obtained by the onboard star tracker. However the star tracker and the camera are not adjacent on the spacecraft and their relative orientation depends on the thermal characteristics of the spacecraft. We therefore take daily pictures of a star field compare the telemetered attitude to the camera's actual attitude as determined from the stars and apply the resulting small misalignment to all images taken on that day. Pixel-level changes in the misalignment are quite common and are probably the limiting error source for the optical landmark data.

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