-
4
-
-
85130075664
-
-
C. C. Reese, V. S. Solomatov, C. P. Orth, J. Geophys, Res. 112, E04S04 (2007).
-
(2007)
J. Geophys, Res.
, vol.112
-
-
Reese, C.C.1
Solomatov, V.S.2
Orth, C.P.3
-
5
-
-
18844450315
-
-
G. R. Foulger, J. H. Natland, D. C. Presnall, D. L. Anderson, Eds. Special Volume388, Geological Society of America, Denver, CO
-
E. R. Stofan, S. E. Smrekar, in Plates, Plumes, and Paradigms, G. R. Foulger, J. H. Natland, D. C. Presnall, D. L. Anderson, Eds. (Special Volume388, Geological Society of America, Denver, CO, 2005), pp. 861-885.
-
(2005)
Plates, Plumes, and Paradigms
, pp. 861-885
-
-
Stofan, E.R.1
Smrekar, S.E.2
-
6
-
-
0000218841
-
-
J. Lecacheux, P. Drossart, P. Laques, F. Deladerriere, F. Colas, Planet. Space Sci. 41, 543 (1993).
-
(1993)
Planet. Space Sci.
, vol.41
, pp. 543
-
-
Lecacheux, J.1
Drossart, P.2
Laques, P.3
Deladerriere, F.4
Colas, F.5
-
9
-
-
0002805036
-
-
N. J. Rappaport, A. S. Konopliv, A. B. Kucinskas, P. G. Ford, Icarus 139, 19 (1999).
-
(1999)
Icarus
, vol.139
, pp. 19
-
-
Rappaport, N.J.1
Konopliv, A.S.2
Kucinskas, A.B.3
Ford, P.G.4
-
10
-
-
77951813934
-
-
We reduced the surface emissivity using the improved version of the Global Topography Data Record developed by (9) from updated ephemeris data. The Magellan data are referenced to the cartographic system given by (50) and are transformed into the system used by VIRTIS data (51), taking January 1991 as an approximate time of the Magellan observations. However, the best correlation of the topography implied by temperature derived from VIRTIS infrared images and Magellan altimetry is found when the Magellan coordinates are shifted another 0.15° in longitude. Estimates of Venus angular velocity 102, 53 and references therein disagree by amounts that, over the approximately 16-year separation between Magellan and Venus Express, can accommodate this deviation
-
We reduced the surface emissivity using the improved version of the Global Topography Data Record developed by (9) from updated ephemeris data. The Magellan data are referenced to the cartographic system given by (50) and are transformed into the system used by VIRTIS data (51), taking January 1991 as an approximate time of the Magellan observations. However, the best correlation of the topography implied by temperature derived from VIRTIS infrared images and Magellan altimetry is found when the Magellan coordinates are shifted another 0.15° in longitude. Estimates of Venus angular velocity 102, 53) and references therein] disagree by amounts that, over the approximately 16-year separation between Magellan and Venus Express, can accommodate this deviation.
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-
-
-
11
-
-
77951793901
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-
To calculate emissivity values employing a two-stream approximation of radiative transfer (12), we assumed an atmospheric reflectivity of 0.82 and a nonabsorbing atmosphere (54), which is appropriate for the 1.02-μm window 40 We assumed that the average plains are basaltic and that weathering has lowered the emissivity. Using an average emissivity of 0.58 produced an emissivity range in this area of 0.5 to 0.91, a range consistent with expected mineralogy
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To calculate emissivity values employing a two-stream approximation of radiative transfer (12), we assumed an atmospheric reflectivity of 0.82 and a nonabsorbing atmosphere (54), which is appropriate for the 1.02-μm window (40). We assumed that the average plains are basaltic and that weathering has lowered the emissivity. Using an average emissivity of 0.58 produced an emissivity range in this area of 0.5 to 0.91, a range consistent with expected mineralogy.
-
-
-
-
13
-
-
77951809410
-
-
(Lunar and Planetary Institute, Houston, TX, 2009), abstr
-
J. Helbert, A. Maturilli, N. Mueller, in Venus Geochemistry: Progress, Prospects, and New Missions (Lunar and Planetary Institute, Houston, TX, 2009), abstr. 2010.
-
(2010)
Venus Geochemistry: Progress, Prospects, and New Missions
-
-
Helbert, J.1
Maturilli, A.2
Mueller, N.3
-
15
-
-
77951875021
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-
Coronae are circular volcano-tectonic features that are unique to Venus and have an average diameter of -250 km 5 They are defined by their circular and often radial fractures and always produce some form of volcanism
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Coronae are circular volcano-tectonic features that are unique to Venus and have an average diameter of -250 km (5). They are defined by their circular and often radial fractures and always produce some form of volcanism.
-
-
-
-
16
-
-
0001639376
-
-
G. E. McGiIl, S. J. Steenstrup, C. Barton, P. G. Ford, Geophys. Res. Lett. 8, 737 (1981).
-
(1981)
Geophys. Res. Lett.
, vol.8
, pp. 737
-
-
McGiil, G.E.1
Steenstrup, S.J.2
Barton, C.3
Ford, P.G.4
-
18
-
-
75449110489
-
-
E. R. Stofan, S. E. Smrekar, D. L. Bindschadler, D. Senske, J. Geophys. Res. 23, 317 (1995).
-
(1995)
J. Geophys. Res.
, vol.23
, pp. 317
-
-
Stofan, E.R.1
Smrekar, S.E.2
Bindschadler, D.L.3
Senske, D.4
-
19
-
-
77951787472
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Estimated elastic thickness values at Themis Regio are typically 10 to 20 km 20, 21 The authors of (22) conducted a global admittance study and found values of elastic thickness of 0 to 50 km at both Dione and Themis Regiones. Their analysis also shows regions of large elastic thickness, up to 100 km, in the northern portion of Dione Regio covering Ushas Mons. Estimates of average apparent depth of compensation (ADC) for Dione and Themis Regiones are 130 km and 100 km (21), respectively. The elastic thickness at lmdr Regio cannot be reliably estimated due to the low resolution of the gravity field in that region 53 Stofan et al. (18) estimated an ADC of 260 km, which is consistent with a deep plume
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Estimated elastic thickness values at Themis Regio are typically 10 to 20 km (20, 21). The authors of (22) conducted a global admittance study and found values of elastic thickness of 0 to 50 km at both Dione and Themis Regiones. Their analysis also shows regions of large elastic thickness, up to 100 km, in the northern portion of Dione Regio covering Ushas Mons. Estimates of average apparent depth of compensation (ADC) for Dione and Themis Regiones are 130 km and 100 km (21), respectively. The elastic thickness at lmdr Regio cannot be reliably estimated due to the low resolution of the gravity field in that region (53). Stofan et al. (18) estimated an ADC of 260 km, which is consistent with a deep plume.
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-
-
-
24
-
-
77951861788
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-
Mapping of V-28 and V-53, T. K. P. Gregg, K. L. Tanaka, R. S. Saunders, Eds. U.S. Geological Society Open-File Report 20051271, Washington, DC
-
E. R. Stofan, J. E. Guest, A. W. Brian, Mapping of V-28 and V-53, T. K. P. Gregg, K. L. Tanaka, R. S. Saunders, Eds. (U.S. Geological Society Open-File Report 20051271, Abstracts of the Annual Meeting of Planetary Geologic Mappers, Washington, DC, 2005), pp. 20-21.
-
(2005)
Abstracts of the Annual Meeting of Planetary Geologic Mappers
, pp. 20-21
-
-
Stofan, E.R.1
Guest, J.E.2
Brian, A.W.3
-
25
-
-
77951824755
-
-
XXXIX, abstr.
-
E. R. Stofan, S. E. Smrekar, J. Helbert, P. Martin, N. Mueller, Lunar Planet. Sci. XXXIX, abstr. 1033 (2009).
-
(2009)
Lunar Planet. Sci.
, vol.1033
-
-
Stofan, E.R.1
Smrekar, S.E.2
Helbert, J.3
Martin, P.4
Mueller, N.5
-
28
-
-
0000118694
-
-
C. M. Pieters et al., Science 234, 1379 (1986).
-
(1986)
Science
, vol.234
, pp. 1379
-
-
Pieters, C.M.1
-
31
-
-
0026474421
-
-
Univ. of Arizona Press, Tucson, AZ
-
M. I. Zolotov, V. P. Volkov, in Venus Geology, Geochemistry, Geophysics-Research Results from the USSR (Univ. of Arizona Press, Tucson, AZ, 1992), pp. 177-199.
-
(1992)
Venus Geology, Geochemistry, Geophysics-Research Results from the USSR
, pp. 177-199
-
-
Zolotov, M.I.1
Volkov, V.P.2
-
33
-
-
0000941091
-
-
B. Fegley, K. Lodders, A. H. Treiman, G. Klingelhöfer, Icarus 115, 159 (1995a).
-
(1995)
Icarus
, vol.115
, pp. 159
-
-
Fegley, B.1
Lodders, K.2
Treiman, A.H.3
Klingelhöfer, G.4
-
34
-
-
0001566539
-
-
B. Fegley et al., Icarus 118, 373 (1995b).
-
(1995)
Icarus
, vol.118
, pp. 373
-
-
Fegley, B.1
-
35
-
-
60749136493
-
-
A. M. Baldridge, S. J. Hook, C. I. Grove, G. Rivera, Remote Sens. Environ. 113, 711 (2009).
-
(2009)
Remote Sens. Environ.
, vol.113
, pp. 711
-
-
Baldridge, A.M.1
Hook, S.J.2
Grove, C.I.3
Rivera, G.4
-
39
-
-
77951857228
-
-
New Scientist 23, 52 (2009)
-
New Scientist 23, 52 (2009) ( www.newscientist.com/article/dn17534).
-
-
-
-
41
-
-
0031206109
-
-
B. Fegley, Icarus 128, 474 (1997).
-
(1997)
Icarus
, vol.128
, pp. 474
-
-
Fegley, B.1
-
43
-
-
0001946464
-
-
J. J. Mahoney, M. F. Coffin, Eds. Monograph 100, American Geophysical Union, Washington, DC
-
P. R. Hooper, in Large Igneous Provinces: Continental, Oceanic and Planetary Flood Volcanism, J. J. Mahoney, M. F. Coffin, Eds. (Monograph 100, American Geophysical Union, Washington, DC, 1997), pp. 1-28.
-
(1997)
Large Igneous Provinces: Continental, Oceanic and Planetary Flood Volcanism
, pp. 1-28
-
-
Hooper, P.R.1
-
45
-
-
77951864451
-
-
R. G. Strom, G. G. Schaber, D. D. Dawson, J. Geophys. Res. 99, 10, 899 (1994).
-
(1994)
J. Geophys. Res.
, vol.99
, Issue.10
, pp. 899
-
-
Strom, R.G.1
Schaber, G.G.2
Dawson, D.D.3
-
46
-
-
77951871656
-
-
K. M. Roberts, J. E. Guest, J. W. Head, M. G. Lancaster, J. Geophys. Res. 97, 15, 991 (1992).
-
(1992)
J. Geophys. Res.
, vol.97
, Issue.15
, pp. 991
-
-
Roberts, K.M.1
Guest, J.E.2
Head, J.W.3
Lancaster, M.G.4
-
47
-
-
0003063098
-
-
H. Sigurdsson, Ed. Academic Press, San Diego, CA
-
C. R. K. Kilburn, in Encyclopedia of Volcanoes, H. Sigurdsson, Ed. (Academic Press, San Diego, CA, 2000), pp. 291-306.
-
(2000)
Encyclopedia of Volcanoes
, pp. 291-306
-
-
Kilburn, C.R.K.1
-
48
-
-
77951873330
-
-
We have rounded these numbers in recognition that the age estimates have higher uncertainties than the volume estimates
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We have rounded these numbers in recognition that the age estimates have higher uncertainties than the volume estimates.
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55
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77951826630
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This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, and was sponsored by the Planetary Geology and Geophysics Program and NASA. We gratefully acknowledge the work of the entire Venus Express and VIRTIS teams. We thank the European Space Agency, Agenzia Spaziale Italiana, Centre National des Etudes Spatiales, CNRS/Institut National des Sciences de l'Univers, and the other national space agencies that have supported this research. VIRTIS is led by INAF-IASF, Rome, Italy, and LESIA, Observatoire de Paris, France
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This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, and was sponsored by the Planetary Geology and Geophysics Program and NASA. We gratefully acknowledge the work of the entire Venus Express and VIRTIS teams. We thank the European Space Agency, Agenzia Spaziale Italiana, Centre National des Etudes Spatiales, CNRS/Institut National des Sciences de l'Univers, and the other national space agencies that have supported this research. VIRTIS is led by INAF-IASF, Rome, Italy, and LESIA, Observatoire de Paris, France.
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