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Science 15 December 1989:
Vol. 246. no. 4936, pp. 1466 - 1473
DOI: 10.1126/science.246.4936.1466
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Articles

Voyager Radio Science Observations of Neptune and Triton

G. L. Tyler 1, D. N. Sweetnam 2, J. D. Anderson 2, S. E. Borutzki 2, J. K. Campbell 2, V. R. Eshleman 1, D. L. Gresh 1, E. M. Gurrola 1, D. P. Hinson 1, N. Kawashima 3, E. R. Kursinski 2, G. S. Levy 2, G. F. Lindal 2, J. R. Lyons 2, E. A. Marouf 1, P. A. Rosen 1, R. A. Simpson 1, and G. E. Wood 2

1 Stanford University, Stanford, CA 94305
2 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109
3 Institute of Space and Astronautical Science, Sagamihara, 229 Japan

The Voyager 2 encounter with the Neptune system included radio science investigations of the masses and densities of Neptune and Triton, the low-order gravitational harmonics of Neptune, the vertical structures of the atmospheres and ionospheres of Neptune and Triton, the composition of the atmosphere of Neptune, and characteristics of ring material. Demanding experimental requirements were met successfully, and study of the large store of collected data has begun. The initial search of the data revealed no detectable effects of ring material with optical depth tgr [unknown] 0.01. Preliminary representative results include the following: 1.0243 x 1026 and 2.141 x 1022 kilograms for the masses of Neptune and Triton; 1640 and 2054 kilograms per cubic meter for their respective densities; 1355 ± 7 kilometers, provisionally, for the radius of Triton; and J2 = 3411 ± 10(x 10-6) and J4 = -26+12-20(x10-6) for Neptune's gravity field (J>2 and J4 are harmonic coefficients of the gravity field). The equatorial and polar radii of Neptune are 24,764 ± 20 and 24,340 ± 30 kllometers, respectively, at the 105-pascal (1 bar) pressure level. Neptune's atmosphere was probed to a pressure level of about 5 x 105 pascals, and effects of a methane cloud region and probable ammonia absorption below the cloud are evident in the data. Results for the mixing ratios of helium and ammonia are still being investigated; the methane abundance below the clouds is at least 1 percent by volume. Derived temperature-pressure profiles to 1.2 x 105 pascals and 78 kelvins (K) show a lapse rate corresponding to "frozen" equilibrium of the para- and ortho-hydrogen states. Neptune's ionosphere exhibits an extended topside at a temperature of 950 ± 160 K if H+ is the dominant ion, and narrow ionization layers of the type previously seen at the other three giant planets. Triton has a dense ionosphere with a peak electron concentration of 46 x 109 per cubic meter at an altitude of 340 kilometers measured during occultation egress. Its topside plasma temperature is about 80 ± 16 K if N2+ is the principal ion. The tenuous neutral atmosphere of Triton produced distinct signatures in the occultation data; however, the accuracy of the measurements is limited by uncertainties in the frequency of the spacecraft reference oscillator. Preliminary values for the surface pressure of 1.6 ± 0.3 pascals and an equivalent isothermal temperature of 48 ± 5 K are suggested, on the assumption that molecular nitrogen dominates the atmosphere. The radio data may be showing the effects of a thermal inversion near the surface; this and other evidence imply that the Triton atmosphere is controlled by vapor-pressure equilibrium with surface ices, at a temperature of 38 K and a methane mixing ratio of about 10-4.


THIS ARTICLE HAS BEEN CITED BY OTHER ARTICLES:
Oxygen and Other Volatiles in the Giant Planets and their Satellites.
M. H. Wong, J. I. Lunine, S. K. Atreya, T. Johnson, P. R. Mahaffy, T. C. Owen, and T. Encrenaz (2008)
Reviews in Mineralogy and Geochemistry 68, 219-246
   Abstract »    Full Text »    PDF »
Metal ions in the atmosphere of Neptune.
Lyons JR (1995)
Science 267, 648-651
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Triton, Pluto, and the Origin of the Solar System.
J. I. Lunine and J. I. Lunine (1993)
Science 261, 697-698
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Ices on the Surface of Triton.
D. P. Cruikshank, D. P. Cruikshank, T. L. Roush, T. C. Owen, T. R. Geballe, C. de Bergh, B. Schmitt, R. H. Brown, and M. J. Bartholomew (1993)
Science 261, 742-745
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Surface Ices and the Atmospheric Composition of Pluto.
T. C. Owen, T. C. Owen, T. L. Roush, D. P. Cruikshank, J. L. Elliot, L. A. Young, C. de Bergh, B. Schmitt, T. R. Geballe, R. H. Brown, et al. (1993)
Science 261, 745-748
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Solar control of the upper atmosphere of Triton.
Lyons JR, Y. Yung, and M Allen (1992)
Science 256, 204-206
   Abstract »    PDF »
The Effect of Surface Roughness on Triton's Volatile Distribution.
R. V. Yelle and R. V. YELLE (1992)
Science 255, 1553-1555
   Abstract »    PDF »
Interior Structure of Neptune: Comparison with Uranus.
W. B. Hubbard, W. B. HUBBARD, W. J. NELLIS, A. C. MITCHELL, N. C. HOLMES, S. S. LIMAYE, and P. C. MCCANDLESS (1991)
Science 253, 648-651
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Triton's Global Heat Budget.
R. H. Brown, R. H. BROWN, T. V. JOHNSON, J. D. GOGUEN, G. SCHUBERT, and M. N. ROSS (1991)
Science 251, 1465-1467
   Abstract »    PDF »
Voyager at Triton.
J. I. Lunine and J. I. Lunine (1990)
Science 250, 386
   PDF »
Triton's Geyser-Like Plumes: Discovery and Basic Characterization.
L. A. Soderblom, L. A. Soderblom, S. W. Kieffer, T. L. Becker, R. H. Brown, A. F. Cook II, C. J. Hansen, T. V. Johnson, R. L. Kirk, and E. M. Shoemaker (1990)
Science 250, 410-415
   Abstract »    PDF »
Voyager Disk-Integrated Photometry of Triton.
J. Hillier, J. Hillier, P. Helfenstein, A. Verbiscer, J. Veverka, R. H. Brown, J. Goguen, and T. V. Johnson (1990)
Science 250, 419-421
   Abstract »    PDF »
Surface and Airborne Evidence for Plumes and Winds on Triton.
C. J. Hansen, C. J. Hansen, A. S. McEwen, A. P. Ingersoll, and R. J. Terrile (1990)
Science 250, 421-424
   Abstract »    PDF »
Temperature and Thermal Emissivity of the Surface of Neptune's Satellite Triton.
R. M. Nelson, R. M. Nelson, W. D. Smythe, B. D. Wallis, L. J. Horn, A. L. Lane, and M. J. Mayo (1990)
Science 250, 429-431
   Abstract »    PDF »
Energy Sources for Triton's Geyser-Like Plumes.
R. H. Brown, R. H. Brown, R. L. Kirk, T. V. Johnson, and L. A. Soderblom (1990)
Science 250, 431-435
   Abstract »    PDF »
Triton's Plumes: The Dust Devil Hypothesis.
A. P. Ingersoll, A. P. Ingersoll, and K. A. Tryka (1990)
Science 250, 435-437
   Abstract »    PDF »
Scatterers in Triton's Atmosphere: Implications for the Seasonal Volatile Cycle.
J. B. Pollack, J. B. Pollack, J. M. Schwartz, and K. Rages (1990)
Science 250, 440-443
   Abstract »    PDF »
Color and chemistry on Triton.
W. Thompson and C Sagan (1990)
Science 250, 415-418
   Abstract »    PDF »
Voyager 2 at Neptune: Imaging Science Results.
B. A. Smith, B. A. Smith, L. A. Soderblom, D. Banfield, c. Barnet, A. T. Basilevsky, R. F. Beebe, K. Bollinger, J. M. Boyce, A. Brahic, et al. (1989)
Science 246, 1422-1449
   Abstract »    PDF »
Photometry from Voyager 2: Initial Results from the Neptunian Atmosphere, Satellites, and Rings.
A. L. Lane, A. L. Lane, R. A. West, C. W. Hord, R. M. Nelson, K. E. Simmons, W. R. Pryor, L. W. Eposito, L. J. Horn, B. D. Wallis, et al. (1989)
Science 246, 1450-1454
   Abstract »    PDF »
Ultraviolet Spectrometer Observations of Neptune and Triton.
A. L. Broadfoot, S. K. Atreya, J. L. Bertaux, J. E. Blamont, A. J. Dessler, T. M. Donahue, W. T. Forrester, D. T. Hall, F. Herbert, J. B. Holberg, et al. (1989)
Science 246, 1459-1466
   Abstract »    PDF »
Magnetic Fields at Neptune.
N. F. Ness, M. H. Acuna, L. F. Burlaga, J. E. P. Connerney, R. P. Lepping, and F. M. Neubauer (1989)
Science 246, 1473-1478
   Abstract »    PDF »
Plasma Observations Near Neptune: Initial Results from Voyager 2.
J. W. Belcher, H. S. Bridge, F. Bagenal, B. Coppi, O. Divers, A. Eviatar, G. S. Gordon Jr., A. J. Lazarus, R. L. McNutt Jr., K. W. Ogilvie, et al. (1989)
Science 246, 1478-1483
   Abstract »    PDF »


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