Publications by Fred Taylor


First observations of H2O and CO2 vapor in comet 67P/Churyumov-Gerasimenko made by VIRTIS onboard Rosetta

ASTRONOMY & ASTROPHYSICS 583 (2015) ARTN A6

D Bockelee-Morvan, V Debout, S Erard, C Leyrat, F Capaccioni, G Filacchione, N Fougere, P Drossart, G Arnold, M Combi, B Schmitt, J Crovisier, M-C de Sanctis, T Encrenaz, E Kuehrt, E Palomba, FW Taylor, F Tosi, G Piccioni, U Fink, G Tozzi, A Barucci, N Biver, M-T Capria, M Combes, W Ip, M Blecka, F Henry, S Jacquinod, J-M Reess, A Semery, D Tiphene


Models of the global cloud structure on Venus derived from Venus Express observations

Icarus (2011)

JK Barstow, CCC Tsang, CF Wilson, PGJ Irwin, FW Taylor, K McGouldrick, P Drossart, G Piccioni, S Tellmann


Models of the global cloud structure on Venus derived from Venus Express observations

Icarus 217 (2012) 542-560

JK Barstow, CCC Tsang, CF Wilson, PGJ Irwin, FW Taylor, K McGouldrick, P Drossart, G Piccioni, S Tellmann

Spatially-resolved near-infrared spectra from the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) on Venus Express have been used to derive improved models of the vertical structure and global distribution of cloud properties in the southern hemisphere of Venus. VIRTIS achieved the first systematic, global mapping of Venus at wavelengths within transparency windows in the 1.6-2.6. μm range, which are sensitive on the nightside to absorption by the lower and middle cloud layers of thermally-emitted radiation from the hot lower atmosphere (Taylor, F.W., Crisp, D., Bézard, B. [1997]. Venus II: Geology, Geophysics, Atmosphere, and Solar Wind Environment, pp. 325-351). The cloud model used to interpret the spectra is based on previous work by Pollack et al. (Pollack, J., Dalton, J., Grinspoon, D., Wattson, R., Freedman, R., Crisp, D., Allen, D., Bézard, B., de Bergh, C., Giver, L. [1993] . Icarus 103, 1-42), Grinspoon et al. (Grinspoon, D.H., Pollack, J.B., Sitton, B.R., Carlson, R.W., Kamp, L.W., Baines, K.H., Encrenaz, T., Taylor, F.W. [1993]. Planet. Space Sci. 41, 515-542) and Crisp (Crisp, D. [1986] . Icarus 67, 484-514), and assumes a composition for the cloud particles of sulfuric acid and water, with acid concentration as a free parameter to be determined. Other retrieved parameters are the average size of the particles and the altitude of the cloud base in the model. Latitudinal variation in the atmospheric temperature structure was incorporated using data from the Venus Radio Science experiment (VeRa). Values are estimated initially using wavelength pairs selected for their unique sensitivity to each parameter, and then validated by comparing measured to calculated spectra over the entire wavelength range, the latter generated using the NEMESIS radiative transfer and retrieval code (Irwin, P.G.J., Teanby, N.A., de Kok, R., Fletcher, L.N., Howett, C.J.A., Tsang, C.C.C., Wilson, C.F., Calcutt, S.B., Nixon, C.A., Parrish, P.D. [2008]. J. Quant. Spectrosc. Radiat. Trans. 109, 1136-1150). The sulfuric acid concentration in the cloud particles is found to be higher in regions of optically thick cloud. The cloud base altitude shows a dependence on latitude, reaching a maximum height near -50°. The increased average particle size near the pole found by Wilson et al. (Wilson, C.F., Guerlet, S., Irwin, P.G.J., Tsang, C.C.C., Taylor, F.W., Carlson, R.W., Drossart, P., Piccioni, G. [2008] . J. Geophys. Res. (Planets) 113, E12) and the finding of spatially variable water vapor abundance at35-40. km altitude first reported by Tsang et al. (Tsang, C.C.C., Wilson, C.F., Barstow, J.K., Irwin, P.G.J., Taylor, F.W., McGouldrick, K., Piccioni, G., Drossart, P., Svedhem, H. [2010]. Geophys. Res. Lett. 37, L02202) are both confirmed. The implications of these improved descriptions of cloud structure and variability for the chemistry, meteorology, and radiative energy balance on Venus are briefly discussed. © 2011 Elsevier Inc.


Forty years of satellite meteorology at Oxford

QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY 137 (2011) 277-285

FW Taylor


Comparative planetology, climatology and biology of Venus, Earth and Mars

PLANETARY AND SPACE SCIENCE 59 (2011) 889-899

FW Taylor


Infrared limb sounding of Titan with the cassini composite infrared spectrometer: Effects of the mid-IR detector spatial responses: Errata

Applied Optics 49 (2010) 5575-5576

CA Nixon, NA Teanby, SB Calcutt, S Aslam, DE Jennings, VG Kunde, FM Flasar, PGJ Irwin, FW Taylor, DA Glenar, MD Smith

We provide a revised Table 5 for the paper by Nixon et al. [Appl. Opt. 48, 1912 (2009)], in which the abundances of < sup > 13 < /sup > CO < inf > 2 < /inf > and C < sup > 18 < /sup > O were incorrect . © 2010 Optical Society of America.


Correlations between cloud thickness and sub-cloud water abundance on Venus

GEOPHYSICAL RESEARCH LETTERS 37 (2010) ARTN L02202

CCC Tsang, CF Wilson, JK Barstow, PGJ Irwin, FW Taylor, K McGouldrick, G Piccioni, P Drossart, H Svedhem


Martian atmosphere as observed by VIRTIS-M on Rosetta spacecraft

JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS 115 (2010) ARTN E04004

A Coradini, D Grassi, F Capaccioni, G Filacchione, F Tosi, E Ammannito, MC De Sanctis, V Formisano, P Wolkenberg, G Rinaldi, G Arnold, MA Barucci, G Bellucci, J Benkhoff, JP Bibring, A Blanco, D Bockelee-Morvan, MT Capria, R Carlson, U Carsenty, P Cerroni, L Colangeli, M Combes, M Combi, J Crovisier, P Drossart, T Encrenaz, S Erard, C Federico, U Fink, S Fonti, W-H Ip, PGJ Irwin, R Jaumann, E Kuehrt, Y Langevin, G Magni, T McCord, V Mennella, S Mottola, G Neukum, V Orofino, P Palumbo, G Piccioni, H Rauer, B Schmitt, D Tiphene, FW Taylor, GP Tozzi


Mars' south polar hood as observed by the Mars Climate Sounder

JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS 115 (2010) ARTN E12015

JL Benson, DM Kass, A Kleinboehl, DJ McCleese, JT Schofield, FW Taylor


Diviner lunar radiometer observations of cold traps in the moon's south polar region

Science 330 (2010) 479-482

DA Paige, MA Siegler, JA Zhang, PO Hayne, EJ Foote, KA Bennett, AR Vasavada, BT Greenhagen, JT Schofield, DJ McCleese, MC Foote, E DeJong, BG Bills, W Hartford, BC Murray, CC Allen, K Snook, LA Soderblom, S Calcutt, FW Taylor, NE Bowles, JL Bandfield, R Elphic, R Ghent, TD Glotch, MB Wyatt, PG Lucey

Diviner Lunar Radiometer Experiment surface-temperature maps reveal the existence of widespread surface and near-surface cryogenic regions that extend beyond the boundaries of persistent shadow. The Lunar Crater Observation and Sensing Satellite (LCROSS) struck one of the coldest of these regions, where subsurface temperatures are estimated to be 38 kelvin. Large areas of the lunar polar regions are currently cold enough to cold-trap water ice as well as a range of both more volatile and less volatile species. The diverse mixture of water and high-volatility compounds detected in the LCROSS ejecta plume is strong evidence for the impact delivery and cold-trapping of volatiles derived from primitive outer solar system bodies.


Structure and dynamics of the Martian lower and middle atmosphere as observed by the Mars Climate Sounder: Seasonal variations in zonal mean temperature, dust, and water ice aerosols

JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS 115 (2010) ARTN E12016

DJ McCleese, NG Heavens, JT Schofield, WA Abdou, JL Bandfield, SB Calcutt, PGJ Irwin, DM Kass, A Kleinbohl, SR Lewis, DA Paige, PL Read, MI Richardson, JH Shirley, FW Taylor, N Teanby, RW Zurek


The Lunar Reconnaissance Orbiter Diviner Lunar Radiometer Experiment

SPACE SCIENCE REVIEWS 150 (2010) 125-160

DA Paige, MC Foote, BT Greenhagen, JT Schofield, S Calcutt, AR Vasavada, DJ Preston, FW Taylor, CC Allen, KJ Snook, BM Jakosky, BC Murray, LA Soderblom, B Jau, S Loring, J Bulharowski, NE Bowles, IR Thomas, MT Sullivan, C Avis, EM De Jong, W Hartford, DJ McCleese


Venus: Not evil, just a bit unfortunate

ASTRONOMY & GEOPHYSICS 51 (2010) 26-31

FW Taylor


Venus Cloud Properties from Venus Express VIRTIS Observations

AAS/Division for Planetary Sciences Meeting Abstracts #42 42 (2010) 994-994

J Barstow, FW Taylor, CCC Tsang, CF Wilson, PGJ Irwin, P Drossart, G Piccioni


The Scientific Exploration of Mars

Cambridge University Press, 2010

FW Taylor

What do we know about Mars? What remains to be understood? Is there evidence of life there? Will humans ever travel there? The dream of exploring Mars has ...


Planetary atmospheres

METEOROLOGICAL APPLICATIONS 17 (2010) 393-403

FW Taylor


Mars Climate Sounder limb profile retrieval of atmospheric temperature, pressure, and dust and water ice opacity

JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS 114 (2009) ARTN E10006

A Kleinboehl, JT Schofield, DM Kass, WA Abdou, CR Backus, B Sen, JH Shirley, WG Lawson, MI Richardson, FW Taylor, NA Teanby, DJ McCleese


Thermal tides in the Martian middle atmosphere as seen by the Mars Climate Sounder

JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS 114 (2009) ARTN E03005

C Lee, WG Lawson, MI Richardson, NG Heavens, A Kleinboehl, D Banfield, DJ McCleese, R Zurek, D Kass, JT Schofield, CB Leovy, FW Taylor, AD Toigo


Determining vertical cloud structure on Venus using near-infrared spectroscopy

European Planetary Science Congress 2009 (2009) 249-249

JK Barstow, FW Taylor, CCC Tsang, CF Wilson, PGJ Irwin, P Drossart, G Piccioni


Minor Species in the Deep Atmosphere of Venus: Dynamical Tracers seen by Venus Express

AAS/Division for Planetary Sciences Meeting Abstracts #41 41 (2009) #60.07-#60.07

C Tsang, CF Wilson, JK Barstow, B Bezard, PGJ Irwin, FW Taylor, G Piccioni, P Drossart, K McGouldrick, SB Calcutt

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