-
2
-
-
0000647286
-
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However, D in comets is enriched relative to Earth's value [P. Eberhardt, M. Reber, D. Krankovsky, R. R. Hodges, Astron. Astrophys. 302, 301 (1995)].
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0001185139
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0028505157
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Nair, H.1
Allen, M.2
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Yung, Y.L.4
Clancy, R.T.5
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9
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0001185139
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V. A. Krasnopolsky, Icarus 101, 313 (1993); H. Nair, M. Allen, A. D. Anbar, Y. L. Yung, R. T. Clancy, ibid. 111, 124 (1994); V. A. Krasnopolsky, J. Geophys. Res. 100, 3263 (1995).
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37049182906
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T. Owen, J. P. Maillard, C. de Bergh, B. L. Lutz, Science 240, 1767 (1988); V. A. Krasnopolsky, G. L. Bjoraker, M. J. Mumma, D. E. Jennings, J. Geophys. Res. 102, 6525 (1997). The abstract of G. L. Bjoraker, M. J. Mumma, and H. P. Larson [Bull. Am. Astron. Soc. 21, 991 (1989)] is under revision.
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Science
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Owen, T.1
Maillard, J.P.2
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Lutz, B.L.4
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15
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17044428646
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-
T. Owen, J. P. Maillard, C. de Bergh, B. L. Lutz, Science 240, 1767 (1988); V. A. Krasnopolsky, G. L. Bjoraker, M. J. Mumma, D. E. Jennings, J. Geophys. Res. 102, 6525 (1997). The abstract of G. L. Bjoraker, M. J. Mumma, and H. P. Larson [Bull. Am. Astron. Soc. 21, 991 (1989)] is under revision.
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Krasnopolsky, V.A.1
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Mumma, M.J.3
Jennings, D.E.4
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16
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-
37049182906
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-
T. Owen, J. P. Maillard, C. de Bergh, B. L. Lutz, Science 240, 1767 (1988); V. A. Krasnopolsky, G. L. Bjoraker, M. J. Mumma, D. E. Jennings, J. Geophys. Res. 102, 6525 (1997). The abstract of G. L. Bjoraker, M. J. Mumma, and H. P. Larson [Bull. Am. Astron. Soc. 21, 991 (1989)] is under revision.
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Bjoraker, G.L.1
Mumma, M.J.2
Larson, H.P.3
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17
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0028468978
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L. L. Watson, I. D. Hutcheon, S. Epstein, E. Stolper, Science 265, 86 (1994).
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Science
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Watson, L.L.1
Hutcheon, I.D.2
Epstein, S.3
Stolper, E.4
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19
-
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0024274906
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Y. L. Yung et al., Icarus 76, 146 (1988).
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(1988)
Icarus
, vol.76
, pp. 146
-
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Yung, Y.L.1
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20
-
-
2642687275
-
-
note
-
This line consists of two components at 1215.668 and 1215.674 Å, with the intensity ratio of 2:1. The weighted mean wavelength is 1215.670 Å.
-
-
-
-
21
-
-
2642606003
-
-
note
-
D are the masses of the electron, H, and D, respectively.
-
-
-
-
22
-
-
2642595675
-
-
note
-
GHRS was replaced with the Space Telescope imaging spectrograph (STIS) in February 1997. Although STIS has many advantages when compared with GHRS, its dark current per square arc second is higher than that of GHRS by a factor of 8, and exposures required to detect weak emissions from extended sources are longer by the same factor.
-
-
-
-
23
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-
0008509228
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-
P. Benvenuti and E. Schreier, Eds. European Southern Observatory, Garching, Germany
-
J. L. Bertaux, J. T. Clarke, M. Mumma, T. Owen, E. Quemerais, in Science with the Hubble Space Telescope, P. Benvenuti and E. Schreier, Eds. (European Southern Observatory, Garching, Germany, 1992), p. 459; J. T. Clarke, R. Lallement, J. L. Bertaux, E. Quemerais, Astrophys. J. 448, 893 (1995).
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(1992)
Science with the Hubble Space Telescope
, pp. 459
-
-
Bertaux, J.L.1
Clarke, J.T.2
Mumma, M.3
Owen, T.4
Quemerais, E.5
-
24
-
-
11944252980
-
-
J. L. Bertaux, J. T. Clarke, M. Mumma, T. Owen, E. Quemerais, in Science with the Hubble Space Telescope, P. Benvenuti and E. Schreier, Eds. (European Southern Observatory, Garching, Germany, 1992), p. 459; J. T. Clarke, R. Lallement, J. L. Bertaux, E. Quemerais, Astrophys. J. 448, 893 (1995).
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Astrophys. J.
, vol.448
, pp. 893
-
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Clarke, J.T.1
Lallement, R.2
Bertaux, J.L.3
Quemerais, E.4
-
25
-
-
2642595674
-
-
note
-
-1.
-
-
-
-
26
-
-
2642591607
-
-
note
-
10.7 cm = 70.
-
-
-
-
27
-
-
0011425955
-
-
The angle between the instrument direction and the velocity of the interstellar wind was 115°, therefore the line of interplanetary H was Doppler shifted by -0.052 Å and its Doppler width was 0.06 Å [F. M. Wu and D. L. Judge, Astrophys. J. 239, 389 (1980)]. The line intensity was 200 R for this direction at solar minimum [J. M. Ajello, A. I. Stewart, G. E. Thomas, A. Graps, ibid. 317, 964 (1987)]. Half of the field of view was screened by Mars, reducing the effective intensity to 100 R and modifying the wavelength shift to -0.026 Å.
-
(1980)
Astrophys. J.
, vol.239
, pp. 389
-
-
Wu, F.M.1
Judge, D.L.2
-
28
-
-
0001009213
-
-
The angle between the instrument direction and the velocity of the interstellar wind was 115°, therefore the line of interplanetary H was Doppler shifted by -0.052 Å and its Doppler width was 0.06 Å [F. M. Wu and D. L. Judge, Astrophys. J. 239, 389 (1980)]. The line intensity was 200 R for this direction at solar minimum [J. M. Ajello, A. I. Stewart, G. E. Thomas, A. Graps, ibid. 317, 964 (1987)]. Half of the field of view was screened by Mars, reducing the effective intensity to 100 R and modifying the wavelength shift to -0.026 Å.
-
(1987)
Astrophys. J.
, vol.317
, pp. 964
-
-
Ajello, J.M.1
Stewart, A.I.2
Thomas, G.E.3
Graps, A.4
-
29
-
-
2642636496
-
-
note
-
5 for an aperture of 0.22″ x 0.22″ and smaller by a factor of 6 for 1.74″ x 1.74″. The difference in sensitivities for these apertures was a factor of 64.
-
-
-
-
30
-
-
2642687274
-
-
note
-
Both D lines binned in 16 pixels result in signal-to-noise ratios of 5. The given uncertainty accounts for both statistical and baseline uncertainties.
-
-
-
-
32
-
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0028457349
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-
V. A. Krasnopolsky, S. Bowyer, S. Chakrabarti, G. R. Gladstone, J. S. McDonald, Icarus 109, 337 (1994); V. A. Krasnopolsky and G. R. Gladstone, J. Geophys. Res. 101, 15765 (1996).
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Icarus
, vol.109
, pp. 337
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Krasnopolsky, V.A.1
Bowyer, S.2
Chakrabarti, S.3
Gladstone, G.R.4
McDonald, J.S.5
-
33
-
-
0028457349
-
-
V. A. Krasnopolsky, S. Bowyer, S. Chakrabarti, G. R. Gladstone, J. S. McDonald, Icarus 109, 337 (1994); V. A. Krasnopolsky and G. R. Gladstone, J. Geophys. Res. 101, 15765 (1996).
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J. Geophys. Res.
, vol.101
, pp. 15765
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Krasnopolsky, V.A.1
Gladstone, G.R.2
-
36
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0027388285
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-
Densities and energies of electrons above Mars' ionopause are from M. H. G. Zhang, J. G. Luhmann, A. F. Nagy, J. P. Spreiter, and S. S. Stahara [J. Geophys. Res. 98, 3311 (1993)]. Cross sections are from L. J. Kieffer [At. Data 1, 19 (1969)].
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J. Geophys. Res.
, vol.98
, pp. 3311
-
-
Zhang, M.H.G.1
Luhmann, J.G.2
Nagy, A.F.3
Spreiter, J.P.4
Stahara, S.S.5
-
37
-
-
0002463812
-
-
Densities and energies of electrons above Mars' ionopause are from M. H. G. Zhang, J. G. Luhmann, A. F. Nagy, J. P. Spreiter, and S. S. Stahara [J. Geophys. Res. 98, 3311 (1993)]. Cross sections are from L. J. Kieffer [At. Data 1, 19 (1969)].
-
(1969)
At. Data
, vol.1
, pp. 19
-
-
Kieffer, L.J.1
-
38
-
-
0001478653
-
-
Solar photon fluxes are from P. G. Richards, J. A. Fennelly, and D. G. Torr [J. Geophys. Res. 99, 8981 (1994)]. Cross sections are from S. K. Atreya [Atmospheres and Ionospheres of the Outer Planets and Their Satellites (Springer, New York, 1986)].
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J. Geophys. Res.
, vol.99
, pp. 8981
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Richards, P.G.1
Fennelly, J.A.2
Torr, D.G.3
-
42
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-
2642666122
-
-
note
-
2O vapor in the lower atmosphere.
-
-
-
-
44
-
-
2642668107
-
-
note
-
2. Self-absorption by D atoms is only a few percent, confirming the validity of the single scattering approximation.
-
-
-
-
46
-
-
2642688253
-
-
note
-
2, which are similar to those of HD in (27) and taken from the same sources. As for HD, the model reflects the global mean conditions but for solar maximum. These differ from the daytime conditions of the model in (4). Temperature, ion density, and eddy diffusion profiles are taken from the solar maximum model in (6).
-
-
-
-
47
-
-
2642669099
-
-
note
-
2.
-
-
-
-
48
-
-
0003878179
-
-
Hemisphere Publishing, New York
-
This value and its uncertainty were calculated using data from L. V. Gurvich, I. V. Veyts, and C. B. Alcock [Thermodynamic Properties of Individual Substances, Hemisphere Publishing, New York, 1989)]. The uncertainties of the given temperature and the thermodynamic constants contribute equally to the final value.
-
(1989)
Thermodynamic Properties of Individual Substances
-
-
Gurvich, L.V.1
Veyts, I.V.2
Alcock, C.B.3
-
49
-
-
0028553804
-
-
HD+H2O is larger than that measured in the laboratory [C. Lecluse and F. Robert, Geochim. Cosmochim. Acta 58, 2927 (1994)]. See discussion in Y. L. Yung and D. M. Kass, Science 280, 1545 (1998).
-
(1994)
Geochim. Cosmochim. Acta
, vol.58
, pp. 2927
-
-
Lecluse, C.1
Robert, F.2
-
50
-
-
0032486185
-
-
HD+H2O is larger than that measured in the laboratory [C. Lecluse and F. Robert, Geochim. Cosmochim. Acta 58, 2927 (1994)]. See discussion in Y. L. Yung and D. M. Kass, Science 280, 1545 (1998).
-
(1998)
Science
, vol.280
, pp. 1545
-
-
Yung, Y.L.1
Kass, D.M.2
-
52
-
-
0001310345
-
-
This factor depends on temperature and is equal to 0.79 ± 0.05 for T = 220 ± 20 K [L. Merlivat and G. Nief, Tellus 19, 122 (1967)].
-
(1967)
Tellus
, vol.19
, pp. 122
-
-
Merlivat, L.1
Nief, G.2
-
53
-
-
2642635464
-
-
note
-
2O between them is slow and reservoirs do not completely disappear. This assumption is questionable.
-
-
-
-
54
-
-
2642659020
-
-
note
-
e = 30 m. Our model differs from the model (12) in which reservoir two is disconnected from reservoir one and gradually shrinks from 3.6 to 0.2 m.
-
-
-
-
55
-
-
0001055033
-
-
Reservoir two may be a part of the polar cap water, which is estimated at 15 m by B. M. Jakosky [J. Geophys. Res. 95, 1475 (1990)]. It should also include some crustal water.
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(1990)
J. Geophys. Res.
, vol.95
, pp. 1475
-
-
Jakosky, B.M.1
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56
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-
0010576241
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M. H. Acuna et al., Science 279, 1676 (1998).
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(1998)
Science
, vol.279
, pp. 1676
-
-
Acuna, M.H.1
-
59
-
-
2642636495
-
-
note
-
V.A.K. thanks T. Reyes for consulting in data processing. This work was supported by the HST Guest Observer Program.
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