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1. Diurnal variation of dust and gas production in comet 67P/Churyumov-Gerasimenko at the inbound equinox as seen by OSIRIS and VIRTIS-M on board Rosetta

Author

Tubiana, C., Rinaldi, G., Güttler, C., Snodgrass, C., Shi, X., Hu, X., Marschall, R., Fulle, M., Bockelée-Morvan, D., Naletto, G., Capaccioni, F., Sierks, H., Arnold, G., Barucci, M. A., Bertaux, J. -L., Bertini, I., Bodewits, D., Capria, M. T., Ciarniello, M., Cremonese, G., Crovisier, J., Da Deppo, V., Debei, S., De Cecco, M., Deller, J., De Sanctis, M. C., Davidsson, B., Doose, L., Erard, S., Filacchione, G., Fink, U., Formisano, M., Fornasier, S., Gutiérrez, P. J., Ip, W. -H., Ivanovski, S., Kappel, D., Keller, H. U., Kolokolova, L., Koschny, D., Krueger, H., La Forgia, F., Lamy, P. L., Lara, L. M., Lazzarin, M., Levasseur-Regourd, A. C., Lin, Z. -Y., Longobardo, A., López-Moreno, J. J., Marzari, F., Migliorini, A., Mottola, S., Rodrigo, R., Taylor, F., Toth, I., and Zakharov, V.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

On 27 Apr 2015, when 67P/C-G was at 1.76 au from the Sun and moving towards perihelion, the OSIRIS and VIRTIS-M instruments on Rosetta observed the evolving dust and gas coma during a complete rotation of the comet. We aim to characterize the dust, H2O and CO2 gas spatial distribution in the inner coma. To do this we performed a quantitative analysis of the release of dust and gas and compared the observed H2O production rate with the one calculated using a thermo-physical model. For this study we selected OSIRIS WAC images at 612 nm (dust) and VIRTIS-M image cubes at 612 nm, 2700 nm (H2O) and 4200 nm (CO2). We measured the average signal in a circular annulus, to study spatial variation around the comet, and in a sector of the annulus, to study temporal variation in the sunward direction with comet rotation, both at a fixed distance of 3.1 km from the comet centre. The spatial correlation between dust and water, both coming from the sun-lit side of the comet, shows that water is the main driver of dust activity in this time period. The spatial distribution of CO2 is not correlated with water and dust. There is no strong temporal correlation between the dust brightness and water production rate as the comet rotates. The dust brightness shows a peak at 0deg sub-solar longitude, which is not pronounced in the water production. At the same epoch, there is also a maximum in CO2 production. An excess of measured water production, with respect to the value calculated using a simple thermo-physical model, is observed when the head lobe and regions of the Southern hemisphere with strong seasonal variations are illuminated. A drastic decrease in dust production, when the water production (both measured and from the model) displays a maximum, happens when typical Northern consolidated regions are illuminated and the Southern hemisphere regions with strong seasonal variations are instead in shadow., Comment: 15 pages, accepted for publication in A&A

Published
2019
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3. The Imaging Photopolarimeter Experiment on Pioneer 11

Author

Baker, A. L., Baker, L. R., Beshore, E., Blenman, C., Castillo, N. D., Doose, L. R., Elston, J. P., Fountain, J. W., Gehrels, T., Kendall, J. H., KenKnight, C. E., Norden, R. A., Swindell, W., Tomasko, M. G., and Coffeen, D. L.

Published
1975

7. Rain, winds and haze during the Huygens probe's descent to Titan's surface

Author

Tomasko, M. G., Archinal, B., Becker, T., Bezard, B., Bushroe, M., Combes, M., Cook, D., Coustenis, A., de Bergh, C., Dafoe, L. E., Doose, L., Doute, S., Eibl, A., Engel, S., Gliem, F., Grieger, B., Holso, K., Howington-Kraus, E., Karkoschka, E., Keller, H. U., Kirk, R., Kramm, R., Kuppers, M., Lanagan, P., Lellouch, E., Lemmon, M., Lunine, J., McFarlane, E., Moores, J., Prout, G. M., Rizk, B., Rosiek, M., Rueffer, P., Schroder, S. E., Schmitt, B., See, C., Smith, P., Soderblom, L., Thomas, N., and West, R.

Subjects
Environmental issues, Science and technology, Zoology and wildlife conservation
Abstract

Author(s): M. G. Tomasko [1]; B. Archinal [2]; T. Becker [2]; B. Bézard [3]; M. Bushroe [1]; M. Combes [3]; D. Cook [2]; A. Coustenis [3]; C. de Bergh [3]; [...]

Published
2005
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8. Analysis of night-side dust activity on comet 67P observed by VIRTIS-M: a new method to constrain the thermal inertia on the surface

Author

Rinaldi, G., Formisano, M., Kappel, D., Capaccioni, F., Bockelée-Morvan, D., Cheng, Y.-C., Vincent, J.-B., Deshapriya, P., Arnold, G., Capria, M., Ciarniello, M., D’Aversa, E., D'aversa, E, De Sanctis, M., Doose, L., Erard, S., Federico, C., Filacchione, G., Fink, U., Leyrat, C., Longobardo, A., Magni, G., Migliorini, A., Mottola, S., Naletto, G., Raponi, A., Taylor, F., Tosi, F., Tozzi, G., Salatti, M., IASI (IASI), Consiglio Nazionale delle Ricerche (CNR), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [Taiwan] (IANCU), National Central University [Taiwan] (NCU), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Mécanique Textiles (LPMT), ENSITM-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Matériaux et nanosciences d'Alsace (FMNGE), Institut de Chimie du CNRS (INC)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), IASF-Roma - Istituto di Astrofisica Spaziale e Fisica cosmica - Roma, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Instituto de Estudos Avançados (IEAV), Institut, DLR Institute of Planetary Research, German Aerospace Center (DLR), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto di Fisica dello Spazio Interplanetario (IFSI), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-ENSITM-Matériaux et Nanosciences Grand-Est (MNGE), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), and Bockelée-Morvan, Dominique

Subjects
Asteroiden und Kometen, 67P/Churyumov-Gerasimenko -infrared, 010504 meteorology & atmospheric sciences, Comet, Imaging spectrometer, Coma (optics), Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, general -comets, Mantle (geology), [SDU] Sciences of the Universe [physics], comet, 0103 physical sciences, Thermal, comets, individual, infrared: planetary systems, 010303 astronomy & astrophysics, planetary systems, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], Jet (fluid), Range (particle radiation), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], comets: general, Leitungsbereich PF, comets: individual: 67P/Churyumov-Gerasimenko, Astronomy and Astrophysics, Plume, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

On 2015 July 18, near perihelion at a heliocentric distance of 1.28 au, the Visible InfraRed Thermal Imaging Spectrometer (VIRTIS-M) on board the Rosetta spacecraft had the opportunity of observing dust activity in the inner coma with a view of the night side (shadowed side) of comet 67P/Churyumov-Gerasimenko. At the time of the measurements we present here, we observe a dust plume that originates on the far side of the nucleus. We are able to identify the approximate location of its source at the boundary between the Hapi and Anuket regions, and we find that it has been in darkness for some hours before the observation. Assuming that this time span is equal to the conductive time scale, we obtain a thermal inertia in the range 25–36 W K−1 m−2 s−1/2. These thermal inertia values can be used to verify with a 3D finite-element method (FEM) numerical code whether the surface and subsurface temperatures agree with the values found in the literature. We explored three different configurations: (1) a layer of water ice mixed with dust beneath a dust mantle of 5 mm with thermal inertia of 36 J m−2 K−1 s−0.5; (2) the same structure, but with thermal inertia of 100 J m−2 K−1 s−0.5; (3) an ice-dust mixture that is directly exposed. Of these three configurations, the first seems to be the most reasonable, both for the low thermal inertia and for the agreement with the surface and subsurface temperatures that have been found for the comet 67P/Churyumov-Gerasimenko. The spectral properties of the plume show that the visible dust color ranged from 16 ± 4.8%/100 nm to 13 ± 2.6%/100 nm, indicating that this plume has no detectable color gradient. The morphology of the plume can be classified as a narrow jet that has an estimated total ejected mass of between 6 and 19 tons when we assume size distribution indices between −2.5 and −3.

Published
2019

9. Analysis of night-side dust activity on comet 67P observed by VIRTIS-M

Author

Rinaldi, G., Formisano, M., Kappel, David, Capaccioni, F., Bockelee-Morvan, D., Cheng, Y-C, Vincent, J-B, Deshapriya, P., Arnold, G., Capria, M. T., Ciarniello, M., De Sanctis, M. C., Doose, L., Erard, S., Federico, C., Filacchione, G., Fink, U., Leyrat, C., Longobardo, A., Magni, G., Mighorini, A., Mottola, S., Naletto, G., Raponi, A., Taylor, F., Tosi, F., Tozzi, G. P., and Salatti, M.

Subjects
Institut für Physik und Astronomie, ddc:530
Abstract

On 2015 July 18, near perihelion at a heliocentric distance of 1.28 au, the Visible InfraRed Thermal Imaging Spectrometer (VIRTIS-M) on board the Rosetta spacecraft had the opportunity of observing dust activity in the inner coma with a view of the night side (shadowed side) of comet 67P/Churyumov-Gerasimenko. At the time of the measurements we present here, we observe a dust plume that originates on the far side of the nucleus. We are able to identify the approximate location of its source at the boundary between the Hapi and Anuket regions, and we find that it has been in darkness for some hours before the observation. Assuming that this time span is equal to the conductive time scale, we obtain a thermal inertia in the range 25-36 W K-1 m(-2) s(-1/2). These thermal inertia values can be used to verify with a 3D finite-element method (REM) numerical code whether the surface and subsurface temperatures agree with the values found in the literature. We explored three different configurations: (1) a layer of water ice mixed with dust beneath a dust mantle of 5 mm with thermal inertia of 36 J m(-2) K-1 S-0.5 ; (2) the same structure, but with thermal inertia of 100 J m(-2) K-1 S-0.5; (3) an ice-dust mixture that is directly exposed. Of these three configurations, the first seems to be the most reasonable, both for the low thermal inertia and for the agreement with the surface and subsurface temperatures that have been found for the comet 67P/Churyumov-Gerasimenko. The spectral properties of the plume show that the visible dust color ranged from 16 +/- 4.8%/100 nm to 13 +/- 2.6%/100 nm, indicating that this plume has no detectable color gradient. The morphology of the plume can be classified as a narrow jet that has an estimated total ejected mass of between 6 and 19 tons when we assume size distribution indices between -2.5 and -3.

Published
2019

10. Diurnal variation of dust and gas production in comet 67P/Churyumov-Gerasimenko at the inbound equinox as seen by OSIRIS and VIRTIS-M on board Rosetta

Author

Agenzia Spaziale Italiana, German Research Foundation, Centre National de la Recherche Scientifique (France), Ministerio de Economía y Competitividad (España), Government of Sweden, European Space Agency, l'Observatoire de Paris, Science and Technology Facilities Council (UK), Tubiana, C., Rinaldi, G., Güttler, C., Snodgrass, C, Shi, X., Hu, X., Marschall, R., Fulle, M., Bockelée-Morvan, D., Naletto, G., Capaccioni, F, Sierks, H., Arnold, G., Barucci, M.A., Bertaux, J.L., Bertini, I., Bodewits, D., Capria, MT, Ciarniello, M, Cremonese, G., Crovisier, J, Da Deppo, Vania, Debei, S., De Cecco, M., Deller, J., De Sanctis, MC, Davidsson, B., Doose, L, Erard, S, Filacchione, G., Fink, U, Formisano, M, Fornasier, S., Gutiérrez, Pedro J., Ip, W. H., Ivanovski, S., Kappel, D, Keller, H.U., Kolokolova, L., Koschny, D., Krueger, H, La Forgia, F., Lamy, P.L., Lara, Luisa María, Lazzarin, M., Levasseur-Regourd, A. C., Lin, Zhong-Yi, Longobardo, A, López-Moreno, José Juan, Marzari, F., Migliorini, A, Mottola, S., Rodrigo Montero, Rafael, Taylor, F, Toth, I., Zakharov, V, Agenzia Spaziale Italiana, German Research Foundation, Centre National de la Recherche Scientifique (France), Ministerio de Economía y Competitividad (España), Government of Sweden, European Space Agency, l'Observatoire de Paris, Science and Technology Facilities Council (UK), Tubiana, C., Rinaldi, G., Güttler, C., Snodgrass, C, Shi, X., Hu, X., Marschall, R., Fulle, M., Bockelée-Morvan, D., Naletto, G., Capaccioni, F, Sierks, H., Arnold, G., Barucci, M.A., Bertaux, J.L., Bertini, I., Bodewits, D., Capria, MT, Ciarniello, M, Cremonese, G., Crovisier, J, Da Deppo, Vania, Debei, S., De Cecco, M., Deller, J., De Sanctis, MC, Davidsson, B., Doose, L, Erard, S, Filacchione, G., Fink, U, Formisano, M, Fornasier, S., Gutiérrez, Pedro J., Ip, W. H., Ivanovski, S., Kappel, D, Keller, H.U., Kolokolova, L., Koschny, D., Krueger, H, La Forgia, F., Lamy, P.L., Lara, Luisa María, Lazzarin, M., Levasseur-Regourd, A. C., Lin, Zhong-Yi, Longobardo, A, López-Moreno, José Juan, Marzari, F., Migliorini, A, Mottola, S., Rodrigo Montero, Rafael, Taylor, F, Toth, I., and Zakharov, V

Abstract

On 27 April 2015, when comet 67P/Churyumov-Gerasimenko was at 1.76 au from the Sun and moving toward perihelion, the OSIRIS and VIRTIS-M instruments on board the Rosetta spacecraft simultaneously observed the evolving dust and gas coma during a complete rotation of the comet.© C. Tubiana et al. 2019

Published
2019

11. The Imaging Photopolarimeter Experiment on Pioneer 10

Author

Gehrels, T., Coffeen, D., Tomasko, M., Doose, L., Swindell, W., Castillo, N., Kendall, J., Clements, A., Hämeen-Anttila, J., Knight, C. Ken, Blenman, C., Baker, R., Best, G., and Baker, L.

Published
1974

14. First Results from the Descent Imager/Spectral Radiometer (DISR) Experiment on the Huygens Entry Probe of Titan

Author

Tomasko, M. G, Doose, L. R, Rizk, B, Smith, P, See, C, Bushroe, M, McFarlane, L, Engel, S, Eibl, A, and Karkoschka, E

Subjects
Lunar And Planetary Science And Exploration
Abstract

The Cassini-Huygens mission was launched on October 15, 1997, and arrived in Orbit around Saturn in July, 2004. The Huygens Probe was released from the Cassini Orbiter on December 24, 2004 and entered Titan s atmosphere on January 14, 2005. Here we give the first results from the Descent Imager/Spectral Radiometer (DISR) instrument aboard the Huygens Probe during its descent into the atmosphere of Titan. Measurements were made by several different optical systems and sensors.

Published
2005

15. Aerosol and Cloud Properties at the Huygens Entry Site as Derived from the Descent Imager/Spectral

Author

Doose, L. R, Engel, S, Tomasko, M. G, Dafoe, L. E, West, R, and Lemmon, M

Subjects
Lunar And Planetary Science And Exploration
Abstract

The Huygens Probe descended through Titan s atmosphere on January 14, 2005. The Descent Imager/Spectral Radiometer (DISR) instrument made optical measurements which constrain the nature and vertical distribution and of the aerosols in the atmosphere.

Published
2005

17. The dust coma environment of 67P/Churyumov-Gerasimenko as observed by VIRTIS

Author

Rinaldi, G., Bockelee-Morvan, D., Ciarniello, M., Tozzi, G., Fink, U., Doose, L., Capaccioni, F., Della Corte, Vincenzo, Fulle, M., Rotundi, A., Filacchione, G., Taylor, F.W., Kappel, David, Erard, S., Leyrat, C., Raponi, A., D'Aversa, E., Ivanovski, S., Capria, M. T., Longobardo, A, Palomba, E., Tosi, F., Migliorini, A., and Salatti, M.

Subjects
Comet 67P, Dust, Coma, VIRTIS
Published
2018

19. Diurnal variation of dust and gas production in comet 67P/Churyumov-Gerasimenko at the inbound equinox as seen by OSIRIS and VIRTIS-M on board Rosetta

Author

Tubiana, C., primary, Rinaldi, G., additional, Güttler, C., additional, Snodgrass, C., additional, Shi, X., additional, Hu, X., additional, Marschall, R., additional, Fulle, M., additional, Bockelée-Morvan, D., additional, Naletto, G., additional, Capaccioni, F., additional, Sierks, H., additional, Arnold, G., additional, Barucci, M. A., additional, Bertaux, J.-L., additional, Bertini, I., additional, Bodewits, D., additional, Capria, M. T., additional, Ciarniello, M., additional, Cremonese, G., additional, Crovisier, J., additional, Da Deppo, V., additional, Debei, S., additional, De Cecco, M., additional, Deller, J., additional, De Sanctis, M. C., additional, Davidsson, B., additional, Doose, L., additional, Erard, S., additional, Filacchione, G., additional, Fink, U., additional, Formisano, M., additional, Fornasier, S., additional, Gutiérrez, P. J., additional, Ip, W.-H., additional, Ivanovski, S., additional, Kappel, D., additional, Keller, H. U., additional, Kolokolova, L., additional, Koschny, D., additional, Krueger, H., additional, La Forgia, F., additional, Lamy, P. L., additional, Lara, L. M., additional, Lazzarin, M., additional, Levasseur-Regourd, A. C., additional, Lin, Z.-Y., additional, Longobardo, A., additional, López-Moreno, J. J., additional, Marzari, F., additional, Migliorini, A., additional, Mottola, S., additional, Rodrigo, R., additional, Taylor, F., additional, Toth, I., additional, and Zakharov, V., additional

Published
2019
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20. Laboratory Measurements of Mineral Dust Scatterring Phase Function and Linear Polarization

Author

West, R. A, Doose, L. R, Eibl, A. M, Tomasko, M. G, and Mischenko, M. I

Abstract

With the goal of improving our understanding of how small mineral dust particles scatter light at visible and near-infrared wafelengths we measured the scattering phase function and linear polarization of small mineral dust particles over the scattering angle range 15 to 170 at three wavelengths (0.47, 0.652,and 0.937 m).

Published
1996

22. Lunar maria and related deposits: Preliminary Galileo imaging results

Author

Greeley, R, Belton, M, Bolef, L, Carr, M, Chapman, C, Davies, M, Doose, L, Fanale, F, Gaddis, L, and Greenberg, R

Subjects
Lunar And Planetary Exploration
Abstract

During the Earth-Moon flyby the Galileo Solid State Imaging system obtained new information on lunar media. Imaging data in spectral bands from 0.4 to 1.0 micron wavelength provide color data for deposits on the western limb. General objectives were to determine the composition and stratigraphy of mare and related deposits for areas not previously seen well in color, and to compare the results with well-studied nearside maria. Initial results from images reduced with preliminary calibrations show that Galileo spectral reflectance data are consistent with previous earthbased observations.

Published
1991

23. Summer outbursts in the coma of comet 67P/Churyumov–Gerasimenko as observed by Rosetta–VIRTIS

Author

Rinaldi, G, primary, Bockelée-Morvan, D, additional, Ciarniello, M, additional, Tozzi, G P, additional, Capaccioni, F, additional, Ivanovski, S L, additional, Filacchione, G, additional, Fink, U, additional, Doose, L, additional, Taylor, F, additional, Kappel, D, additional, Erard, S, additional, Leyrat, C, additional, Raponi, A, additional, D’Aversa, E, additional, Capria, M T, additional, Longobardo, A, additional, Palomba, E, additional, Tosi, F, additional, Migliorini, A, additional, Rotundi, A, additional, Della Corte, V, additional, and Salatti, M, additional

Published
2018
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24. Properties of the dust in the coma of 67P/Churyumov-Gerasimenko observed with VIRTIS- M

Author

Rinaldi, G., primary, Fink, U., additional, Doose, L., additional, Tozzi, G.P., additional, Capaccioni, F., additional, Filacchione, G., additional, Bockelée-Morvan, D., additional, Leyrat, C., additional, Piccioni, G., additional, Erard, S., additional, Bieler, A., additional, Błęcka, M., additional, Ciarniello, M., additional, Combi, M., additional, Fougere, N., additional, Migliorini, A., additional, Palomba, E., additional, Raponi, A., additional, and Taylor, F., additional

Published
2016
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25. Correction for Dust Opacity of Martian Atmospheric Water Vapor Abundances

Author

Hunten, D. M., Sprague, A. L., and Doose, L. R.

Subjects
Mars (Planet) -- Atmosphere, Planets -- Atmosphere, Astronomy, Earth sciences
Abstract

A method is presented to correct for the effects of dust opacity on the derivation of water-vapor abundances from observed spectral absorption lines. We show that the dust opacity can be inferred by use of limb-to-limb measurements of a [CO.sub.2] band. Ideally, simultaneous [CO.sub.2] and water-vapor measurements at the same location should be obtained; in practice, we make these two measurements sequentially. The effects of the dust opacity are computed by a doubling-adding program that has been applied to many planetary atmospheric problems, one of which is obtaining the phase function and single-scattering albedo of the dust in Mars' atmosphere observed by the cameras on the Mars Pathfinder lander. Sample analyses of data from three nights in March 1999 are shown. For these results there does appear to be a real diurnal variation in the [H.sub.2]O abundance. [C] 2000 Academic Press Key Words: Mars, atmosphere; Mars; climate; radiative transfer.

Published
2000

26. Latitudinal variations in Titan's methane and haze from Cassini VIMS observations

Author

P.F., Penteado, C.A., Griffith, M.G., Tomasko, Engel, S., See, C., Doose, L., K.H., Baines, R.H., Brown, B.J., Buratti, Clark, R., Nicholson, P., Sotin, C., Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), and Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.STU]Sciences of the Universe [physics]/Earth Sciences, ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2010

27. First Results from the Descent Imager/Spectral Radiometer (DISR) Experiment on the Huygens Entry Probe of Titan

Author

Tomasko, Marty G., Doose, L. R., Rizk, Bashar, Smith, P. H., See, Chuck, Bushroe, M., Mcfarlane, L., Engel, S., Eibl, A., Karkoschka, E., Prout, M., Dafoe, L. E., West, R. A., Soderblom, Laurence A., Archinal, B. A., Keller, Horst Uwe, Schroeder, S., Küppers, Michael, Bézard, Bruno, Lellouch, Emmanuel, Coustenis, Athéna, de Bergh, Catherine, Combes, Michel, Schmitt, Bernard, Douté, Sylvain, Thomas, Nicholas, Gliem, Fritz, Lemmon, Mark T., Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience

Published
2005

28. Observations of Titan's Surface and Atmosphere from the Descent Imager/Spectral Radiometer (DISR) on the Huygens Probe

Author

Soderblom, L., Tomasko, M., Archinal, B., Becker, T., Bézard, B., Bushroe, M., Combes, M., Cook, D., Coustenis, A., De Bergh, C., Dafoe, L. E., Doose, L., Douté, Sylvain, Eibl, A., Engel, S., Gliem, F., Grieger, B., Hare, T., Holso, K., Howington-Kraus, E., Karkoschka, E., Keller, H., Kirk, R., Kramm, R., Kuppers, M., Lanagan, P., Lellouch, E., Lemmon, M., Lunine, J., Mcfarlane, L., Moores, J., Prout, M., Rizk, B., Rosiek, M., Rueffer, P., Schröder, S. E., Schmitt, Bernard, See, C., Smith, P., Thomas, N., West, R., Pibaret-Bourdon, Béatrice, Astrogeology Science Center [Flagstaff], United States Geological Survey [Reston] (USGS), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie de Grenoble (LPG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut fur Datenverarbeitung, Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Department of Physics, Texas A&M University [College Station], Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Max Planck Institute for Solar System Research (MPS), and Universität Bern [Bern]

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; DISR characterized atmospheric radiation (350-1600 nm) and returned images and spectra of the surface of Titan. Linear polarization of the aerosol haze extending to the surface is i ˜50% at visible wavelengths. Monomers making up the aerosol particles are modeled at ˜0.1 microns, several 100 monomers making up a haze particle. The extinction optical depth at the surface is ˜4.5 at 531 nm, ˜2 at 939 nm and ˜0.5 at 1500 nm. The near-surface methane mole fraction is ˜5% (relative humidity ˜50%); methane fog or rain at the landing site is currently unlikely. Below ˜8 km the eastward zonal wind dropped to

Published
2005

29. Titan Surface Composition at the Huygens Landing Site from DISR Spectra

Author

Schmitt, Bernard, Douté, Sylvain, Bézard, B., Lellouch, E., Tomasko, M., Bernard, J., Quirico, Eric, Doose, L., Engel, S., See, C., Team, Disr, Laboratoire de Planétologie de Grenoble (LPG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, and Pibaret-Bourdon, Béatrice

Abstract

P44A-06; The Descent Imager/Spectral Radiometer (DISR) aboard the Huygens probe recorded complete visible and near infrared spectra (480-1600 nm) of the surface of Titan near the landing site during the last tens of meters of the descent and from a few tens of centimetres after landing. The surface spectrum has a relatively low albedo, peaking around 0.18 at 830 nm, a red slope in the visible range, a quasi-linear decrease of the reflectivity from 830 to 1420 nm, and displays a broad absorption near 1540 nm. The featureless blue slope of this spectrum above 830 nm is very unusual and has no known equivalent on any other object in the Solar System. In addition no published laboratory data of ices or organic materials displays such a spectral behaviour. Laboratory studies and numerical simulations of the DISR spectrum have been performed to try to understand the nature and composition of the materials constituting the surface of Titan. In particular reflectance spectra over the solar spectrum (300-4000 nm) of several types of tholins and organics have been recorded with the LPG spectro-gonio radiometer. Numerical simulations of the surface reflectance spectrum have been performed in order to constrain the optical properties of the different components (ices, organics, etc) and to infer their composition. We will present the current state of analysis of this spectrum.

Published
2005

30. First Results from the Descent Imager/Spectral Radiometer (DISR) Experiment on the Huygens Entry Probe of Titan

Author

Tomasko, M., Doose, L., Rizk, B., Smith, P., See, C., Bushroe, M., Mcfarlane, L., Engel, S., Eibl, A., Karkoschka, E., Prout, M., Dafoe, L. E., Holso, K., West, R., Soderblom, L., Archinal, B., Keller, U., Schroeder, S., Kuppers, M., Bézard, B., Lellouch, E., Coustenis, A., De Bergh, C., Combes, M., Schmitt, Bernard, Douté, Sylvain, Thomas, N., Gliem, F., Lemmon, M., Pibaret-Bourdon, Béatrice, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Astrogeology Science Center [Flagstaff], United States Geological Survey [Reston] (USGS), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie de Grenoble (LPG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Physikalisches Institut [Bern], Universität Bern [Bern], Institut fur Datenverarbeitung, Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Department of Atmospheric Sciences [College Station], Texas A&M University [College Station], Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), and Universität Bern [Bern] (UNIBE)

Abstract

International audience; We will present the first results of the Descent Imager/Spectral Radiometer (DISR) experiment on the Huygens Entry Probe of Titan

Published
2005

32. Analysis of Raman scattered Ly-alpha emissions from the atmosphere of Uranus

Author

Yelle, R. V, Doose, L. R, Tomasko, M. G, and Strobel, D. F

Subjects
Lunar And Planetary Exploration
Abstract

A line at 1280 A, due to Raman scattering of solar Lyman alpha (Ly-alpha) in the atmosphere of Uranus, has been detected by the Voyager Ultraviolet Spectrometer. The measured intensity of 40 + or - 20 R implies that 200 R to 500 R of the measured 1500 R Ly-alpha intensity at the subsolar point is due to Rayleigh scattering of the solar line. The presence of Rayleigh and Raman scattering at 1216 A suggests that the Uranian atmosphere is largely devoid of absorbing hydrocarbons above the 0.5 mbar level. The most natural explanation of this depletion is very weak vertical mixing equivalent to an eddy coefficient on the order of 200 sq cm/sec between 0.5 mbar and 100 mbar.

Published
1987

33. The single scattering phase functions of Jupiter's clouds

Author

Doose, L. R, Tomasko, M. G, and Castillo, N. D

Subjects
Lunar And Planetary Exploration
Abstract

The determination of the single scattering phase functions of Jupiter's clouds and a thin upper haze by Tomasko et al. was refined and extended to seven latitudes in blue and red light. The phase function is well-constrained by the Pioneer 10 and 11 photometric data sets. Multiple scattering models were computed to match the limb darkening at each latitude at up to 15 phase angles from 12 deg to 151 deg. Ground-based observations were used for absolute calibration and to extend the data to lower phase angles. The phase functions were parameterized using the double Henyey-Greenstein function. The three Henyey-Greenstein parameters and the single scattering albedo were determined using a non-linear least squares method for the haze and the clouds below. The phase functions derived for the northen zone and belt are remarkably similar to the phase functions of the corresponding regions in the south, with most of the differences in brightness of the northern and southern features resulting from minor differences in single scattering albedo. Analysis of the Equatorial Region is complicated by the presence of numerous small features, but the phase function required is generally similar to that seen in the more homogeneous regions. Details of the phase functions of the haze and clouds are presented, and the differences between the cloud phase functions at low and high latitudes in red and blue light are discussed.

Published
1986

35. Absorption of sunlight in the atmosphere of Venus

Author

Tomasko, M. G and Doose, L. R

Subjects
Lunar And Planetary Exploration
Abstract

The profiles of upward, downward and net solar flux on Venus were measured at altitudes from about 62 km to the surface in three spectral bands at a vertical resolution of a few hundred meters. These data measured the penetration and absorption of solar energy in Venus' lower atmosphere quantities that are essential in evaluating the role of the greenhouse mechanism in supporting Venus' remarkably high surface temperature. In addition, the data constrained the vertical structure and optical properties of the Venus clouds.

Published
1982

36. Spatially resolved methane band photometry of Saturn. I - Absolute reflectivity and center-to-limb variations in the 6190-, 7250-, and 8900-A bands

Author

West, R. A, Tomasko, M. G, Smith, B. A, Wijesinghe, M. P, Doose, L. R, Reitsema, H. J, and Larson, S. M

Subjects
Lunar And Planetary Exploration
Abstract

Spatially resolved measurements of Saturn's absolute reflectivity in methane bands at 6190, 7250, and 8900 A and in nearby continuum regions are presented. Images were obtained through narrow-band interference filters with a 500 x 500-pixel charge-coupled device. Band/continuum ratios were measured to high accuracy by referencing to the ring brightness in each image. Several data processing techniques enhanced the quality of the observations. These are the use of the ring symmetry to find center position and orientation, accurate subtraction of ring light, and constrained image deconvolution. Uncertainty in the continuum absolute reflectivity is within 10%. Uncertainties in band/continuum ratios are from one to several percent. The Equatorial Zone was much brighter than any other latitude in the strong 8900 band image. Northern midlatitudes were brighter than southern midlatitudes. The latter observation indicates fewer high-altitude aerosols in the south, a possible result of atmospheric dynamics or seasonal sublimation of NH3 crystals. The data are tabulated and presented in a form suitable for quantitative scattering model analyses.

Published
1982
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37. Photometry of Saturn at large phase angles

Author

Tomasko, M. G, Mcmillan, R. S, Doose, L. R, Castillo, N. D, and Dilley, J. P

Subjects
Lunar And Planetary Exploration
Abstract

In the present paper, the single-scattering phase function of Saturn's aerosols is determined from the vertical structure of Saturn's atmosphere, derived in a previous analysis, and Pioneer's imaging photometry of bright and dark zones on Saturn in red and blue light. The single-scattering phase function is well represented by a combination of two Henyey-Greenstein functions. Moderately forward scattering functions fit well both in red and blue light, although a definite difference between the two colors is found.

Published
1980

38. The imaging experiment on Pioneer 10

Author

Swindell, W and Doose, L. Y

Subjects
Space Sciences
Abstract

In the period plus or minus 4 days from Jovian pericenter, Pioneer 10 returned data from 153 imaging sequences. Data were obtained with the imaging photopolarimeter, a 2.54-cm-diam and 8.6-cm-focal-length steerable telescope configured as a narrow beam (0.5-mrad) photometer in a spin scan mode of operation. Images were obtained in two spectral bands (390 to 500 nm and 595 to 720 nm), and seven of the most interesting pictures are shown and discussed.

Published
1974

39. Pioneer Venus Sounder Probe Solar Flux Radiometer

Author

Tomasko, M. G, Doose, L. R, Palmer, J. M, Holmes, A, Wolfe, W. L, Debell, A. G, Brod, L. G, and Sholes, R. R

Subjects
Spacecraft Instrumentation
Abstract

The Solar Flux Radiometer aboard the Pioneer Venus Sounder Probe operated successfully during its descent through the atmosphere of Venus. The instrument measured atmospheric radiance over the spectral range from 400 to 1800 nm as a function of altitude. Elevation and azimuthal measurements on the radiation field were made with five optical channels. Twelve filtered Si and Ge photovoltaic detectors were maintained near 30 C with a phase-change material. The detector output currents were processed with logarithmic transimpedance converters and digitized with an 11-bit A/D converter. Atmospheric sampling in both elevation and azimuth was done according to a Gaussian integration scheme. The serial output data averaged 20 bits/sec, including housekeeping (sync, spin period, sample timing and mode). The data were used to determine the deposition of solar energy in the atmosphere of Venus between 67 km and the surface along with upward and downward fluxes and radiances with an altitude resolution of several hundred meters. The results allow for more accurate modeling of the radiation balance of the atmosphere than previously possible.

Published
1980

40. Imaging photopolarimeter on Pioneer Saturn

Author

Gehrels, T, Baker, L. R, Beshore, E, Blenman, C, Burke, J. J, Castillo, N. D, Dacosta, B, Degewij, J, Doose, L. R, and Coffeen, D. L

Subjects
Lunar And Planetary Exploration
Abstract

Results of Pioneer 11 imaging photopolarimeter observations of Saturn, its rings, and Titan are presented. The imaging photopolarimeter is a pointable telescope with an aperture of 2.5 cm and passbands of 390 to 500 to 720 nm which uses the spin of the spacecraft to scan across an object. Images of the Saturn system and of the rings are presented, and the absence of a D ring, structures in the C, B and A rings and the Cassini division and the discoveries of the F ring and the provisionally named Pioneer division separating it from the A ring are reported. A mean particle size less than 15 meters is estimated from estimates of total ring mass and the optical depth of the B ring. The discovery of the satellite 1979 S 1 at 2.53 Saturn radii is also noted. Models of the vertical aerosol structure of Saturn's atmosphere are compared with the polarization data, and it is indicated that the density of cloud particles decreases with altitude with a scale height about one fourth that of the gas, and that an optical depth of one is to be found at 750 mbar.

Published
1980

41. Lunar Maria and related deposits

Author

Greeley, R.(1), Belton, M.(2), Bolef, L.(1), Carr, M.(3), Chapman, C.(4), Davie s, M.(5), Doose, L.(6), Fanale, F.(7), Gaddis, L.(1), Greenberg, R.(6), Head, J. (8), Hoffmann,H, Jaumann,R, Johnson,T(9),Klaasen,K(9), Koloord, R(6), McEwe n, A(10), Murchie, S(8), Neukum,G, Oberst,J, Pieters, C(8), Pilcher, C.(11), Pl utchak, J(8), Robinson, M(6), Sullivan, R(1), Sunshine, J(8), and Veverka, J(12)

Published
1991

46. A CCD System to Detect Fast-Moving Asteroids

Author

Gehrels, T., primary, Boesgaard, H., additional, Doose, L. R., additional, Frecker, J. E., additional, McMillan, R. S., additional, Perry, M. L., additional, Scotti, J. V., additional, Shoemaker, E. M., additional, and Tholen, D., additional

Published
1983
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49. Possible tropical lakes on Titan from observations of dark terrain.

Author

Griffith CA, Lora JM, Turner J, Penteado PF, Brown RH, Tomasko MG, Doose L, and See C

Abstract

Titan has clouds, rain and lakes--like Earth--but composed of methane rather than water. Unlike Earth, most of the condensable methane (the equivalent of 5 m depth globally averaged) lies in the atmosphere. Liquid detected on the surface (about 2 m deep) has been found by radar images only poleward of 50° latitude, while dune fields pervade the tropics. General circulation models explain this dichotomy, predicting that methane efficiently migrates to the poles from these lower latitudes. Here we report an analysis of near-infrared spectral images of the region between 20° N and 20° S latitude. The data reveal that the lowest fluxes in seven wavelength bands that probe Titan's surface occur in an oval region of about 60 × 40 km(2), which has been observed repeatedly since 2004. Radiative transfer analyses demonstrate that the resulting spectrum is consistent with a black surface, indicative of liquid methane on the surface. Enduring low-latitude lakes are best explained as supplied by subterranean sources (within the last 10,000 years), which may be responsible for Titan's methane, the continual photochemical depletion of which furnishes Titan's organic chemistry.

Published
2012
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50. Absorption of sunlight in the atmosphere of venus.

Author

Tomasko MG, Doose LR, and Smith PH

Abstract

In this report the fluxes measured by the solar flux radiometer (LSFR) of the Pioneer Venus large probe are compared with calculations for model atmospheres. If the large particles of the middle and lower clouds are assumed to be sulfur, strong, short-wavelength absorption results in a net flux profile significantly different from the LSFR net flux measurements. Models in which the smallest particles are assumed to be sulfur gave flux profiles consistent with the measurements if an additional source of absorption is included in the upper cloud. The narrowband data from 0.590 to 0.665 micrometer indicate an absorption optical depth of about 0.05 below the cloud bottom. The broadband data imply that either this absorption extends over a considerable wavelength interval (as might be the case for dust) or that a very strong absorption band lies on one side of the narrowband filter (as suggested by early Venera 11 and Venera 12 reports). Thermal balance calculations based on the measured visible fluxes indicate high surface temperature for reasonable assumptions of cloud opacity and water vapor abundance. The lapse rate becomes convective within the middle cloud. For water mixing ratios of 2.0 x 10(-4) below the clouds we find a subadiabatic region extending from the cloud bottom to altitudes near 35 kilometers.

Published
1979
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