64 results on '"Daniel J. McCleese"'
Search Results
2. The Ensemble Mars Atmosphere Reanalysis System (EMARS) Version 1.0
- Author
-
Thomas Nehrkorn, Patrick M. Dudas, Steven J. Greybush, Takemasa Miyoshi, R. John Wilson, Mark Leidner, Timothy H. McConnochie, M. Wespetal, Janusz Eluszkiewicz, Armin Kleinböhl, Ross N. Hoffman, Matthew J. Hoffman, Yongjing Zhao, David M. Kass, Daniel J. McCleese, H. E. Gillespie, and Eugenia Kalnay
- Subjects
Data Papers ,Thermal Emission Spectrometer ,Meteorology ,reanalysis ,Physics::Geophysics ,Atmosphere ,Data assimilation ,Polar vortex ,Meteorology. Climatology ,Thermal ,mars ,Physics::Atmospheric and Oceanic Physics ,QE1-996.5 ,assimilation ,ensemble ,Storm ,Geology ,Mars Exploration Program ,Atmosphere of Mars ,Physics::Space Physics ,atmosphere ,General Earth and Planetary Sciences ,Environmental science ,Astrophysics::Earth and Planetary Astrophysics ,QC851-999 ,Data Paper - Abstract
The Ensemble Mars Atmosphere Reanalysis System (EMARS) dataset version 1.0 contains hourly gridded atmospheric variables for the planet Mars, spanning Mars Year (MY) 24 through 33 (1999 through 2017). A reanalysis represents the best estimate of the state of the atmosphere by combining observations that are sparse in space and time with a dynamical model and weighting them by their uncertainties. EMARS uses the Local Ensemble Transform Kalman Filter (LETKF) for data assimilation with the GFDL/NASA Mars Global Climate Model (MGCM). Observations that are assimilated include the Thermal Emission Spectrometer (TES) and Mars Climate Sounder (MCS) temperature retrievals. The dataset includes gridded fields of temperature, wind, surface pressure, as well as dust, water ice, CO2 surface ice and other atmospheric quantities. Reanalyses are useful for both science and engineering studies, including investigations of transient eddies, the polar vortex, thermal tides and dust storms, and during spacecraft operations.
- Published
- 2019
3. Solar-System-Wide Significance of Mars Polar Science
- Author
-
J. J. Plaut, Colman Gallagher, Stephen R. Lewis, J. Bapst, C. Andres, John F. Mustard, S. F. A. Cartwright, Lauren A. Edgar, Susan J. Conway, Alan D. Howard, Michael Mischna, Gareth A. Morgan, Maria E. Banks, S. Diniega, Mark L. Skidmore, A. Van Brenen, Carol R. Stoker, Ralf Jaumann, Charity M. Phillips-Lander, Ali M. Bramson, Jennifer L. Whitten, Michael Daly, Michael H. Hecht, Solmaz Adeli, Manish R. Patel, N. Oliveira, S. Mukherjee, Matthew Chojnacki, Kimberly D. Seelos, F. Foss, S. Nerozzi, John E. Moores, Patricio Becerra, Nathaniel E. Putzig, Michael T. Mellon, Vince Eke, Margaret E. Landis, P. B. James, U. Gayathri, F. Bernardini, John Wilson, J. M. Widmer, J. Chesal, Alexey A. Pankine, Klaus-Michael Aye, C. Stuurman, Andrea Coronato, Z. Yoldi, C. Rezza, L. E. McKeown, Edwin S. Kite, B. Hartmann, Ákos Kereszturi, Melinda A. Kahre, Kennda Lynch, M. M. Sori, Alain Khayat, A. Kleinboehl, Matteo Crismani, Scott D. Guzewich, L. R. Lozano, Daniel J. McCleese, Norbert Schorghofer, O. Karatekin, Cynthia L. Dinwiddie, Gordon R. Osinski, Lori K. Fenton, Luca Montabone, Andreas Johnsson, Roberto Orosei, Peter C. Thomas, J. P. Knightly, Matthew R. Balme, Claire E. Newman, Eldar Noe Dobrea, Joseph A. MacGregor, Ernst Hauber, A. C. Pascuzzo, Jennifer Hanley, Bryana L. Henderson, Oded Aharonson, German Martinez, Timothy N. Titus, M. R. Perry, Tanguy Bertrand, P. A. Johnson, Maurizio Pajola, Shane Byrne, Matthew A. Siegler, Anya Portyankina, Nicolas Thomas, R. Karimova, C. Orgel, Michelle Koutnik, Leslie K. Tamppari, Amy McAdam, James A. Whiteway, Briony Horgan, Frances E. G. Butcher, E. Vos, François Forget, Christine S. Hvidberg, Vincent Chevrier, Travis F. Hager, Roland M. B. Young, T. G. Cave, Peter L. Read, M. R. Elmaary, Shannon M. Hibbard, C. J. Hansen, Paul O. Hayne, David A. Crown, J. C. Stern, J. C. Echaurren, I. Mishev, P. Russell, Roger N. Clark, Hanna G. Sizemore, J. W. Holt, F. Chuang, Adrian J. Brown, Colin M. Dundas, S. Ulamsec, G. Luizzi, Isaac B. Smith, Anna Łosiak, Peter Fawdon, David L. Goldsby, Alfred S. McEwen, C. Amos, S. E. Wood, C. Cesar, David E. Stillman, R. W. Obbard, Ralph D. Lorenz, A. Svensson, Ryan C. Ewing, Aymeric Spiga, B. S. Tober, T. Meng, P. Acharya, S. M. Milkovich, Paul Streeter, Kris Zacny, P. Sinha, Joseph S. Levy, Don Banfield, Eric I. Petersen, K. E. Herkenhoff, J. L. Eigenbrode, S. Piqueux, Mackenzie Day, Renyu Hu, Gregory Michael, James W. Head, Alejandro Soto, Richard Massey, A. R. Khuller, P. B. Buhler, S. Clifford, Samuel P. Kounaves, Daniel C. Berman, K. E. Mesick, Bernard Schmitt, Wendy M. Calvin, J. C. Johnson, David A. Fisher, C. Neisch, Robert L. Staehle, C. Herny, D. E. Lalich, Edgard G. Rivera-Valentín, David E. Smith, Anshuman Bhardwaj, Jorge Rabassa, Anna Grau Galofre, Alice Lucchetti, Lydia Sam, A. M. Rutledge, and A. J. Cross
- Subjects
polar science ,geology ,Solar System ,Habitability ,water ,ice ,Mars ,Mars Exploration Program ,Astrobiology ,missions ,Planetary science ,Planet ,Polar ,Climate record ,climate ,Geology - Abstract
Mars Polar Science is an integrated, compelling system that serves as a nearby analogue to numerous other planets, supports human exploration, and habitability. Mars possesses the closest and most easily accessible layered ice deposits outside of Earth, and accessing those layers to read the climate record would be a triumph for planetary science.
- Published
- 2021
4. Mars Climate Sounder Observation of Mars' 2018 Global Dust Storm
- Author
-
Nicholas G. Heavens, John T. Schofield, L. J. Steele, James H. Shirley, Armin Kleinböhl, David M. Kass, and Daniel J. McCleese
- Subjects
Geophysics ,Dust storm ,General Earth and Planetary Sciences ,Environmental science ,Atmosphere of Mars ,Mars Exploration Program ,Astrobiology - Published
- 2020
5. Asymmetries in Snowfall, Emissivity, and Albedo of Mars' Seasonal Polar Caps: Mars Climate Sounder Observations
- Author
-
James H. Shirley, T. Horvath, John T. Schofield, C. E. Gary-Bicas, Armin Kleinböhl, Nicholas G. Heavens, Paul O. Hayne, David M. Kass, Sylvain Piqueux, and Daniel J. McCleese
- Subjects
Geophysics ,Space and Planetary Science ,Geochemistry and Petrology ,Infrared ,Earth and Planetary Sciences (miscellaneous) ,Emissivity ,Environmental science ,Polar ,Mars Exploration Program ,Albedo ,Snow ,Atmospheric sciences - Published
- 2020
6. Rapid Expansion and Evolution of a Regional Dust Storm in the Acidalia Corridor During the Initial Growth Phase of the Martian Global Dust Storm of 2018
- Author
-
Sylvain Piqueux, James H. Shirley, David M. Kass, Armin Kleinböhl, Nicholas G. Heavens, John T. Schofield, L. J. Steele, Daniel J. McCleese, and S. Suzuki
- Subjects
Martian ,Geophysics ,Dust storm ,Rapid expansion ,Growth phase ,General Earth and Planetary Sciences ,Environmental science ,Atmosphere of Mars ,Mars Exploration Program ,Atmospheric sciences - Published
- 2020
7. Impact of gravity waves on the middle atmosphere of Mars: a non-orographic gravity wave parameterization based on Global Climate modeling and MCS observations
- Author
-
John T. Schofield, David M. Kass, Thomas Navarro, Armin Kleinböhl, Daniel J. McCleese, Gabriella Gilli, Aymeric Spiga, François Forget, Ehouarn Millour, Luca Montabone, Observatório Astronómico de Lisboa, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Earth, Planetary and Space Sciences, University of California, Los Angeles, CA, USA, Space Science Institute [Boulder] (SSI), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), and California Institute of Technology (CALTECH)
- Subjects
Martian ,Earth and Planetary Astrophysics (astro-ph.EP) ,010504 meteorology & atmospheric sciences ,Atmospheric circulation ,Northern Hemisphere ,FOS: Physical sciences ,Mars Exploration Program ,Atmosphere of Mars ,[SDU.STU.ME]Sciences of the Universe [physics]/Earth Sciences/Meteorology ,Atmospheric sciences ,01 natural sciences ,Mesosphere ,Physics - Atmospheric and Oceanic Physics ,Geophysics ,13. Climate action ,Space and Planetary Science ,Geochemistry and Petrology ,Meridional flow ,Atmospheric and Oceanic Physics (physics.ao-ph) ,Earth and Planetary Sciences (miscellaneous) ,Gravity wave ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Geology ,0105 earth and related environmental sciences ,Astrophysics - Earth and Planetary Astrophysics - Abstract
The impact of gravity waves (GW) on diurnal tides and the global circulation in the middle/upper atmosphere of Mars is investigated using a General Circulation Model (GCM). We have implemented a stochastic parameterization of non-orographic GW into the Laboratoire de M\'et\'eorologie Dynamique (LMD) Mars GCM (LMD-MGCM) following an innovative approach. The source is assumed to be located above typical convective cells ($\sim$ 250 Pa) and the effect of GW on the circulation and predicted thermal structure above 1 Pa ($\sim$ 50 km) is analyzed. We focus on the comparison between model simulations and observations by the Mars Climate Sounder (MCS) on board Mars Reconnaissance Orbiter during Martian Year 29. MCS data provide the only systematic measurements of the Martian mesosphere up to 80 km to date. The primary effect of GW is to damp the thermal tides by reducing the diurnal oscillation of the meridional and zonal winds. The GW drag reaches magnitudes of the order of 1 m/s/sol above 10$^{-2}$ Pa in the northern hemisphere winter solstice and produces major changes in the zonal wind field (from tens to hundreds of m/s), while the impact on the temperature field is relatively moderate (10-20K). It suggests that GW induced alteration of the meridional flow is the main responsible for the simulated temperature variation. The results also show that with the GW scheme included, the maximum day-night temperature difference due to the diurnal tide is around 10K, and the peak of the tide is shifted toward lower altitudes, in better agreement with MCS observations., Comment: JGR (Planets), accepted
- Published
- 2020
8. MCS Observations of the Initiation and Development of Large Regional Dust Events on Mars
- Author
-
Daniel J. McCleese, Shigeru Suzuki, David M. Kass, John T. Schofield, J. H. Shirley, Nicholas Heavens, Armin Kleinboehl, and Liam Steele
- Subjects
Martian ,Environmental science ,Storm ,Mars Exploration Program ,Astrobiology - Abstract
Why do some Martian dust storms, in some Mars years, expand to reach planet-encircling status, while the majority do not? In what ways do the largest regional events differ from those that become g...
- Published
- 2019
9. Hydrogen escape from Mars enhanced by deep convection in dust storms
- Author
-
James H. Shirley, Nicholas G. Heavens, Armin Kleinböhl, Michael Chaffin, Sylvain Piqueux, Paul O. Hayne, Jasper Halekas, John T. Schofield, Daniel J. McCleese, and David M. Kass
- Subjects
Martian ,Water transport ,010504 meteorology & atmospheric sciences ,Astronomy and Astrophysics ,Storm ,Atmosphere of Mars ,Mars Exploration Program ,Atmospheric sciences ,01 natural sciences ,Atmosphere ,Atmospheric chemistry ,0103 physical sciences ,Environmental science ,010303 astronomy & astrophysics ,Water vapor ,0105 earth and related environmental sciences - Abstract
Present-day water loss from Mars provides insight into Mars’s past habitability1–3. Its main mechanism is thought to be Jeans escape of a steady hydrogen reservoir sourced from odd-oxygen reactions with near-surface water vapour2, 4,5. The observed escape rate, however, is strongly variable and correlates poorly with solar extreme-ultraviolet radiation flux6–8, which was predicted to modulate escape 9 . This variability has recently been attributed to hydrogen sourced from photolysed middle atmospheric water vapour 10 , whose vertical and seasonal distribution is only partly characterized and understood11–13. Here, we report multi-annual observational estimates of water content and dust and water transport to the middle atmosphere from Mars Climate Sounder data. We provide strong evidence that the transport of water vapour and ice to the middle atmosphere by deep convection in Martian dust storms can enhance hydrogen escape. Planet-encircling dust storms can raise the effective hygropause (where water content rapidly decreases to effectively zero) from 50 to 80 km above the areoid (the reference equipotential surface). Smaller dust storms contribute to an annual mode in water content at 40−50 km that may explain seasonal variability in escape. Our results imply that Martian atmospheric chemistry and evolution can be strongly affected by the meteorology of the lower and middle atmosphere of Mars. Mars Climate Sounder’s multi-annual observations of the vertical distribution of water and dust in the Martian atmosphere show that deep convection from dust storms transports water from the lower to the middle atmosphere, enhancing water loss to space.
- Published
- 2018
10. Discovery of a widespread low-latitude diurnal CO2 frost cycle on Mars
- Author
-
John T. Schofield, Armin Kleinböhl, David M. Kass, Paul O. Hayne, James H. Shirley, Daniel J. McCleese, Nicholas G. Heavens, and Sylvain Piqueux
- Subjects
Martian ,010504 meteorology & atmospheric sciences ,Water on Mars ,Ice crystals ,Martian soil ,Mars Exploration Program ,Atmosphere of Mars ,Atmospheric sciences ,01 natural sciences ,Astrobiology ,Geophysics ,Olympus Mons ,Space and Planetary Science ,Geochemistry and Petrology ,0103 physical sciences ,Earth and Planetary Sciences (miscellaneous) ,Martian polar ice caps ,010303 astronomy & astrophysics ,Geology ,0105 earth and related environmental sciences - Abstract
While the detection of CO2 ice has only been reported outside the Martian polar regions at very high elevation (i.e., Elysium, Olympus Mons, and the Tharsis Montes), nighttime surface observations by the Mars Climate Sounder on board the Mars Reconnaissance Orbiter document the widespread occurrence of atmospherically corrected ground temperatures consistent with the presence of extensive carbon dioxide frost deposits in the dusty low thermal inertia units at middle/low latitudes. Thermal infrared emissivities, interpreted in conjunction with mass balance modeling, suggest micrometer size CO2 ice crystals forming optically thin layers never exceeding a few hundreds of microns in thickness (i.e., 10−2 kg m−2) locally, which is insufficient to generate a measurable diurnal pressure cycle (<
- Published
- 2016
11. Interannual similarity in the Martian atmosphere during the dust storm season
- Author
-
Daniel J. McCleese, Armin Kleinböhl, John T. Schofield, M. D. Smith, and David M. Kass
- Subjects
Daytime ,010504 meteorology & atmospheric sciences ,Storm ,Mars Exploration Program ,Atmosphere of Mars ,Atmospheric sciences ,01 natural sciences ,Geophysics ,Planet ,Dust storm ,Climatology ,0103 physical sciences ,General Earth and Planetary Sciences ,Environmental science ,Solstice ,010303 astronomy & astrophysics ,Southern Hemisphere ,0105 earth and related environmental sciences - Abstract
We find that during the dusty season on Mars (southern spring and summer) of years without a global dust storm there are three large regional-scale dust storms. The storms are labeled A, B, and C in seasonal order. This classification is based on examining the zonal mean 50 Pa (approximately 25 km) daytime temperature retrievals from TES/MGS and MCS/MRO over 6 Mars Years. Regional-scale storms are defined as events where the temperature exceeds 200 K. Examining the MCS dust field at 50 Pa indicates that warming in the Southern Hemisphere is dominated by direct heating, while northern high latitude warming is a dynamical response. A storms are springtime planet encircling Southern Hemisphere events. B storms are southern polar events that begin near perihelion and last through the solstice. C storms are southern summertime events starting well after the end of the B storm. C storms show the most interannual variability.
- Published
- 2016
12. No widespread dust in the middle atmosphere of Mars from Mars Climate Sounder observations
- Author
-
Daniel J. McCleese, John T. Schofield, Armin Kleinböhl, David M. Kass, and W. A. Abdou
- Subjects
Atmosphere ,Daytime ,Altitude ,Water on Mars ,Space and Planetary Science ,Extinction (astronomy) ,Environmental science ,Astronomy and Astrophysics ,Storm ,Atmosphere of Mars ,Mars Exploration Program ,Atmospheric sciences - Abstract
It has been established that dust in the atmosphere of Mars is not distributed homogeneously in the vertical but exhibits layering in the lower atmosphere. Recently published results also suggest a dust maximum in the middle atmosphere that predominantly occurs at 50–60 km altitude on the daytime hemisphere. We use measurements from the Mars Climate Sounder to investigate the distribution of dust above ∼ 40 km altitude. Our results do not support the existence of widespread dust in the middle atmosphere of Mars inferred from earlier observations. The average dust extinction does not exceed 10 - 6 km−1 at 463 cm−1 above 50 km altitude in atmospheric conditions without large dust storms.
- Published
- 2015
13. Investigations of the Mars Upper Atmosphere with ExoMars Trace Gas Orbiter
- Author
-
Oleg Korablev, Alejandro Cardesin, David M. Kass, Colin Wilson, Nikolai Ignatiev, Ann Carine Vandaele, Daniel J. McCleese, Nicholas M. Schneider, Manish R. Patel, Armin Kleinböhl, J. E. Rodriguez, Jean-Claude Gérard, Maya García-Comas, Jose-Juan Lopez-Moreno, Sabrina Guilbon, Sergio Jiménez-Monferrer, Anna Fedorova, R. T. Clancy, Ian Thomas, Francisco Gonzalez-Galindo, Miguel Lopez-Valverde, Franck Montmessin, Michael Chaffin, Franck Lefèvre, Anni Määttänen, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), European Space Astronomy Centre (ESAC), European Space Agency (ESA), Department of Physics [Oxford], University of Oxford [Oxford], Space Science Institute [Boulder] (SSI), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], European Commission, Ministerio de Economía, Industria y Competitividad (España), Belgian Science Policy Office, UK Space Agency, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA), University of Oxford, and NASA-California Institute of Technology (CALTECH)
- Subjects
010504 meteorology & atmospheric sciences ,Mars ,01 natural sciences ,Astrobiology ,law.invention ,Aerobraking ,Atmosphere ,Orbiter ,law ,Remote sounding ,0103 physical sciences ,Upper atmosphere ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Martian ,Airglow ,Astronomy and Astrophysics ,Mars Exploration Program ,Atmosphere of Mars ,ACS ,ExoMars ,Trace gas ,[SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] ,13. Climate action ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,Environmental science ,NOMAD ,Thermosphere - Abstract
López-Valverde, M. A. et al., The Martian mesosphere and thermosphere, the region above about 60 km, is not the primary target of the ExoMars 2016 mission but its Trace Gas Orbiter (TGO) can explore it and address many interesting issues, either in-situ during the aerobraking period or remotely during the regular mission. In the aerobraking phase TGO peeks into thermospheric densities and temperatures, in a broad range of latitudes and during a long continuous period. TGO carries two instruments designed for the detection of trace species, NOMAD and ACS, which will use the solar occultation technique. Their regular sounding at the terminator up to very high altitudes in many different molecular bands will represent the first time that an extensive and precise dataset of densities and hopefully temperatures are obtained at those altitudes and local times on Mars. But there are additional capabilities in TGO for studying the upper atmosphere of Mars, and we review them briefly. Our simulations suggest that airglow emissions from the UV to the IR might be observed outside the terminator. If eventually confirmed from orbit, they would supply new information about atmospheric dynamics and variability. However, their optimal exploitation requires a special spacecraft pointing, currently not considered in the regular operations but feasible in our opinion. We discuss the synergy between the TGO instruments, specially the wide spectral range achieved by combining them. We also encourage coordinated operations with other Mars-observing missions capable of supplying simultaneous measurements of its upper atmosphere. © 2018, Springer Science+Business Media B.V., part of Springer Nature., The IAA/CSIC team has been supported by the European Union’s Horizon 2020 Programme (H2020-Compet-08-2014) under grant agreement UPWARDS-633127, by CSIC Proyecto Intramural 201450E022 and by the Plan Nacional del Espacio ESP2015-65064-C2-1-P (MINECO/FEDER). This research was partly supported by the SCOOP/BRAIN program of the Belgian Science Policy Office (BELSPO). We acknowledge the work of Sabrina Guilbon during her Master internship at LATMOS on the development of the technique to compare the slant profiles of SPICAM and the LMD GCM. M.R.P. thanks UKSA for support under grant ST/I003061/1 and ST/P001262/1. C.F.W. acknowledges funding support from the UK Space Agency. Work by A.K., D.J.MC. and D.M.K. at the Jet Propulsion Laboratory, California Institute of Technology was performed under a contract with the National Aeronautics and Space Administration. OK, NI and AF thanks funding from Roscosmos for the ACS operation support and science funding from The Federal Agency of scientific organization (Planeta No. 0028-2014-0004).
- Published
- 2018
- Full Text
- View/download PDF
14. Extreme detached dust layers near Martian volcanoes: Evidence for dust transport by mesoscale circulations forced by high topography
- Author
-
David M. Kass, John T. Schofield, Sylvain Piqueux, Daniel J. McCleese, Armin Kleinböhl, Paul O. Hayne, James H. Shirley, Nicholas G. Heavens, and Bruce A. Cantor
- Subjects
Martian ,Atmosphere ,Geophysics ,Olympus Mons ,Dust storm ,Tharsis Montes ,Mesoscale meteorology ,General Earth and Planetary Sciences ,Storm ,Mars Exploration Program ,Atmospheric sciences ,Geology - Abstract
Modeling suggests that thermal circulations over Mars's highest volcanoes transport water vapor and dust from the surface into the middle atmosphere, forming detached layers in these constituents. Intense vertical mixing also takes place in regional and global dust storms, which can generate detached layers that are extreme in both altitude and magnitude. Here we employ observations by the Mars Climate Sounder (MCS) on board Mars Reconnaissance Orbiter, taking advantage of improved vertical coverage in MCS's aerosol retrievals, to discover a new class of extreme detached dust layers (EDDLs). Observed during minimal dust storm activity and furthermore distinguished by their potentially large and measurable horizontal extent (>1000 km), these EDDLs cluster near Olympus Mons and the Tharsis Montes, from which they likely originate. The existence of these EDDLs suggests that vertical mixing by topographic circulations can be much stronger than previously modeled and more frequent than previously observed.
- Published
- 2015
15. Temperatures and aerosol opacities of the Mars atmosphere at aphelion: Validation and inter-comparison of limb sounding profiles from MRO/MCS and MGS/TES
- Author
-
Daniel J. McCleese, Jennifer Benson, John T. Schofield, Joshua L. Bandfield, J. H. Shirley, Timothy H. McConnochie, D. M. Kass, Nicholas G. Heavens, David P. Hinson, and A. Kleinböhl
- Subjects
Thermal Emission Spectrometer ,Astronomy and Astrophysics ,Atmosphere of Mars ,Mars Exploration Program ,Atmospheric sciences ,Aerosol ,law.invention ,Atmosphere ,Orbiter ,Depth sounding ,Space and Planetary Science ,law ,Environmental science ,Radio occultation - Abstract
We exploit the relative stability and repeatability of the Mars atmosphere at aphelion for an inter-comparison of Mars Global Surveyor/Thermal Emission Spectrometer (MGS/TES) and Mars Reconnaissance Orbiter/Mars Climate Sounder (MRO/MCS) nighttime temperature profiles and aerosol opacity profiles in Mars years 25, 26, 29, 30, and 31. Cross-calibration of these datasets is important, as they together provide an extended climatology for this planetary atmosphere. As a standard of comparison we employ temperature profiles obtained by radio occultation methods during the MGS mission in Mars years 24, 25, and 26. We first compare both zonal mean TES limb sounding profiles and zonal mean MCS limb sounding profiles with zonal means of radio occultation temperature profiles for the same season (Ls = 70–80°) and latitudes (55–70°N). We employ a statistical z test for quantifying the degree of agreement of temperature profiles by pressure level. For pressures less than 610 Pa (altitudes > 3 km), the ensemble mean temperature difference between the radio occultation and TES limb sounding profiles found in these comparisons was 1.7 ± 0.7 K. The ensemble mean temperature difference between radio occultation and MCS profiles was 1.4 ± 1.0 K. These differences fall within the formal error estimates for both TES and MCS, validating the accuracy of the instruments and their respective retrieval algorithms. In the second phase of our investigation, we compare aphelion season zonal mean TES limb sounding temperature, water ice opacity, and dust opacity profiles with those obtained at the same latitudes in different years by MCS. The ensemble mean temperature difference found for three comparisons between TES and MCS zonal mean temperature profiles was 2.8 ± 2.1 K. MCS and TES temperatures between 610 Pa and 5 Pa from 55 to 70°N are largely in agreement (with differences
- Published
- 2015
16. Variability of the martian seasonal CO2 cap extent over eight Mars Years
- Author
-
Sylvain Piqueux, David M. Kass, Daniel J. McCleese, John T. Schofield, Armin Kleinböhl, and Paul O. Hayne
- Subjects
Thermal Emission Spectrometer ,Polar night ,Space and Planetary Science ,Dust storm ,Diurnal temperature variation ,Equivalent latitude ,Environmental science ,Astronomy and Astrophysics ,Martian polar ice caps ,Mars Exploration Program ,Atmosphere of Mars ,Atmospheric sciences - Abstract
We present eight Mars Years of nearly continuous tracking of the CO2 seasonal cap edges from Mars Year (MY) 24 to 31 using Mars Global Surveyor (MGS) Thermal Emission Spectrometer (TES) and Mars Reconnaissance Orbiter (MRO) Mars Climate Sounder (MCS) thermal infrared data. Spatial and temporal resolutions are 1 pixel per degree and 10°Ls (aerocentric longitude of the Sun). The seasonal caps are defined as the regions where the diurnal radiometric temperature variations at ∼32 μm wavelength do not exceed 5 K. With this definition, terrains with small areal fraction of defrosted regolith able to experience measurable diurnal temperature cycles are not mapped as part of the cap. This technique is adequate to distinguish CO2 from H2O ices, and effective during the polar night or under low illumination conditions. The present analysis answers outstanding questions stemming from fragmented observations at visible wavelengths: (1) the previously sparsely documented growth of the North seasonal caps (160° < Ls < 270°) is shown to be repeatable within 1–2° equivalent latitude, and monotonic over the MY 24–31 time period; high repeatability is observed during the retreat of the caps in non-dusty years (∼1° or less equivalent latitude); (2) the MY 25 storm does not seem to have impacted the growth rate, maximal extents, or recession rate of the North seasonal caps, whereas the MY 28 dust storm clearly sped up the recession of the cap (∼2° smaller on average after the storm, during the recession, compared to other years); (3) during non-dusty years, the growth of the South seasonal cap (350° < Ls < 100°) presents noticeable variability (up to ∼4° equivalent latitude near Ls = 20°) with a maximum extent reached near Ls = 90°; (4) the retreat of the Southern seasonal cap (100° < Ls < 310°) exhibits large inter-annual variability, especially near 190° < Ls < 220°; (5) the recession of the MY 25 South seasonal cap is significantly accelerated during the equinox global dust storm, with surface temperatures suggesting increased patchiness or enhanced dust mantling on the CO2 ice. These results suggest that atmospheric temperatures and dust loading are the primary source of variability in an otherwise remarkably repeatable cycle of seasonal cap growth and recession.
- Published
- 2015
17. Seasonal and diurnal variability of detached dust layers in the tropical Martian atmosphere
- Author
-
James H. Shirley, R. John Wilson, W. A. Abdou, David M. Kass, Nicholas G. Heavens, Armin Kleinböhl, Daniel J. McCleese, and Morgan S. Johnson
- Subjects
Tharsis Montes ,Mars Exploration Program ,Atmospheric model ,Atmosphere of Mars ,Atmospheric sciences ,Atmosphere ,Geophysics ,Space and Planetary Science ,Geochemistry and Petrology ,Dust storm ,Climatology ,Earth and Planetary Sciences (miscellaneous) ,Environmental science ,Upwelling ,Hadley cell - Abstract
Evidence for widespread nonuniform vertical mixing of dust in Mars's tropical atmosphere (in the form of features called “detached dust layers” or DDLs) is a challenge for atmospheric modeling. We characterize the seasonal, diurnal, and geographic variability of DDL activity in retrievals from observations by the Mars Climate Sounder onboard Mars Reconnaissance Orbiter. We find that dust injection above the boundary layer, which forms DDLs, is a spatially ubiquitous phenomenon in the tropics during the daytime, implying that it has a significant nontopographic component. DDL formation is more intense in northern spring and summer than in southern spring and summer but is still common when the zonal average dust distribution appears uniformly mixed. DDLs do not appear to follow the upwelling associated with Mars's Hadley circulation or the extant climatology of local dust storm activity in the tropics. Geographic variability in the nightside vertical dust distribution does not always correlate with the dayside vertical dust distribution, implying that there is spatial and seasonal variability in the efficiency of dust deposition/removal processes. Nighttime dust removal is especially efficient over the Tharsis Montes during northern spring and summer, which suggests some association between water ice clouds and removal. Intense injection combined with efficient removal results in a high amplitude of diurnal variability in the dust distribution at 15–30 km above the surface of the tropics during much of the Martian year.
- Published
- 2014
18. JPL Innovation Foundry
- Author
-
Daniel J. McCleese and Brent Sherwood
- Subjects
Engineering ,Concurrent engineering ,business.industry ,media_common.quotation_subject ,Principal (computer security) ,Aerospace Engineering ,Context (language use) ,Maturity (finance) ,Domain (software engineering) ,Scarcity ,Engineering management ,Space Science ,Activity-based costing ,business ,media_common - Abstract
Space science missions are increasingly challenged today: in ambition, by increasingly sophisticated hypotheses tested; in development, by the increasing complexity of advanced technologies; in budgeting, by the decline of flagship-class mission opportunities; in management, by expectations for breakthrough science despite a risk-averse programmatic climate; and in planning, by increasing competition for scarce resources. How are the space-science missions of tomorrow being formulated? The paper describes the JPL Innovation Foundry, created in 2011, to respond to this evolving context. The Foundry integrates methods, tools, and experts that span the mission concept lifecycle. Grounded in JPL's heritage of missions, flight instruments, mission proposals, and concept innovation, the Foundry seeks to provide continuity of support and cost-effective, on-call access to the right domain experts at the right time, as science definition teams and Principal Investigators mature mission ideas from “cocktail napkin” to PDR. The Foundry blends JPL capabilities in proposal development and concurrent engineering, including Team X, with new approaches for open-ended concept exploration in earlier, cost-constrained phases, and with ongoing research and technology projects. It applies complexity and cost models, project-formulation lessons learned, and strategy analyses appropriate to each level of concept maturity. The Foundry is organizationally integrated with JPL formulation program offices; staffed by JPL's line organizations for engineering, science, and costing; and overseen by senior Laboratory leaders to assure experienced coordination and review. Incubation of each concept is tailored depending on its maturity and proposal history, and its highest-leverage modeling and analysis needs.
- Published
- 2013
19. Radiometric comparison of Mars Climate Sounder and Thermal Emission spectrometer measurements
- Author
-
Joshua L. Bandfield, John T. Schofield, Michael J. Wolff, Daniel J. McCleese, and Michael D. Smith
- Subjects
Martian ,Thermal Emission Spectrometer ,Space and Planetary Science ,Nadir ,Environmental science ,Astronomy and Astrophysics ,Mars Exploration Program ,Spectral bands ,Atmosphere of Mars ,Albedo ,Atmospheric temperature ,Atmospheric sciences ,Remote sensing - Abstract
Mars Climate Sounder (MCS) nadir oriented thermal infrared and solar channel measurements are com- pared with Thermal Emission Spectrometer (TES) measurements across multiple Mars years. Thermal infrared measurements were compared by convolving the TES data using the MCS spectral band passes. The MCS solar channel measurements were calibrated using Compact Reconnaissance Imaging Spectrom- eter for Mars observations to provide the proper gain factor (3.09 � 10 � 3 Ws r � 1 m � 2 lm � 1 ). The compar- isons of the datasets show that day and night surface and atmospheric temperatures are within 3 K over the course of 5 martian years, after accounting for the local time differences. Any potential interannual variations in global average temperature are masked by calibration and modeling uncertainties. Previous work attributed apparent interannual global surface and atmospheric temperature variations to major dust storm activity; however, this variation has since been attributed to a calibration error in the TES dataset that has been corrected. MCS derived Lambert albedos are slightly higher than TES measurements acquired over the same season and locations. Most of this difference can be attributed to the spectral response functions of MCS and TES. Consistent with previous work, global albedo is highly variable (� 6%) and this variability must be taken into account when determining long term global trends. Vertical aerosol distributions were also derived from the calibrated MCS visible channel limb measurements, demonstrating the utility of the MCS visible channel data for monitoring of aerosols.
- Published
- 2013
20. The semidiurnal tide in the middle atmosphere of Mars
- Author
-
Daniel J. McCleese, John T. Schofield, Armin Kleinböhl, David M. Kass, and R. John Wilson
- Subjects
Martian ,Atmospheric tide ,Atmosphere of Mars ,Mars Exploration Program ,Atmospheric sciences ,Physics::Geophysics ,Atmosphere ,Geophysics ,Dust storm ,Climatology ,Physics::Space Physics ,Thermal ,Astrophysics::Solar and Stellar Astrophysics ,General Earth and Planetary Sciences ,Environmental science ,Timekeeping on Mars ,Astrophysics::Earth and Planetary Astrophysics ,Physics::Atmospheric and Oceanic Physics - Abstract
[1] Atmospheric thermal tides are global oscillations in atmospheric fields that are subharmonics of a solar day. While atmospheric tides on Earth are mainly relevant in the upper atmosphere, on Mars, they dominate temperature variations and winds throughout the atmosphere. Observations and model simulations to date have suggested that the migrating diurnal tide is the predominant mode in the Martian atmosphere, and that the semidiurnal tide is only relevant in the tropical middle atmosphere during conditions of high dust loading. New comprehensive observations by the Mars Climate Sounder in a geometry that allows coverage of multiple local times show that the semidiurnal tide is a dominant response of the Martian atmosphere throughout the Martian year. The maximum semidiurnal amplitude of ~ 16 K is found at southern winter high latitudes, which makes it the largest tidal amplitude observed in the Martian middle atmosphere outside of dust storm conditions. The semidiurnal tide can be successfully modeled due to recent advances of Mars General Circulation Models (MGCMs) that include the radiatively active treatment of water ice clouds. Tidal forcing occurs through absorption of radiation by aerosols and points to the vertical structure of dust and clouds and their radiative effects as being essential for our understanding of the thermal structure and the general circulation of the Martian atmosphere. As with terrestrial GCMs trying to quantify mechanisms affecting climate, future Mars modeling efforts will require microphysical schemes to control aerosol distributions, and vertically and temporally resolved measurements of temperature and aerosols will be essential for their validation.
- Published
- 2013
21. Infrared remote sounding of the middle atmosphere of venus from the pioneer orbiter
- Author
-
Daniel J. McCleese, David J. Diner, John Theodore Houghton, L. S. Elson, S. E. Bradley, J. T. Schofield, Martha S. Hanner, J. V. Martonchik, Fredric W. Taylor, P. E. Reichley, Andrew P. Ingersoll, and J. Delderfield
- Subjects
Multidisciplinary ,biology ,Equator ,Venus ,Atmospheric temperature ,Atmospheric sciences ,biology.organism_classification ,law.invention ,Latitude ,Atmosphere ,Atmosphere of Venus ,Orbiter ,Altitude ,law ,Physics::Space Physics ,Astrophysics::Earth and Planetary Astrophysics ,Geology ,Physics::Atmospheric and Oceanic Physics - Abstract
Orbiter infrared measurements of the Venus atmosphere in the 60- to 140-kilometer region show very small diurnal temperature differences near the cloud tops, increasing somewhat at higher levels. The seasonal (that is, equator to pole) contrasts are an order of magnitude larger, and the temperatures unexpectedly increase with increasing latitude below 80 kilometers. An isothermal layer at least two scale heights in vertical extent is found near the 100-kilometer altitude, where the temperature is about 175 K. Structure is present in the cloud temperature maps on a range of spatial scales. The most striking is at high latitude, where contrasts of nearly 50 K are observed between a cold circumpolar band and the region near the pole itself.
- Published
- 2016
22. Remote sounding of the Martian atmosphere in the context of the InterMarsNet mission: General circulation and meteorology
- Author
-
S. B. Calcutt, Fredric W. Taylor, Conway B. Leovy, Daniel J. McCleese, Duane O. Muhleman, Patrick G. J. Irwin, R. T. Clancy, and John T. Schofield
- Subjects
Meteorology ,Astronomy and Astrophysics ,Context (language use) ,Atmosphere of Mars ,law.invention ,Orbiter ,Depth sounding ,Space and Planetary Science ,Planet ,law ,Remote sensing (archaeology) ,General Circulation Model ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Water cycle ,Physics::Atmospheric and Oceanic Physics ,Remote sensing - Abstract
A concept has been developed for a remote sensing experiment to investigate the physics of the Martian atmosphere from a spin-stabilized orbiter, like that planned for the InterMarsNet mission. Using coincident infrared and microwave channels and limb-to-limb scanning, it can map the planet much more extensively than previously in temperature, atmospheric dust loading, and humidity. When combined with one or more surface stations measuring the same variables, the sounder experiment can contribute to major progress in understanding the general circulation and dust and water cycles of the atmosphere of Mars, and the characterization of medium-scale meteorological systems. Copyright © 1996 Elsevier Science Ltd.
- Published
- 2016
23. THE GLOBAL DISTRIBUTION OF WATER-VAPOR IN THE MIDDLE ATMOSPHERE OF VENUS
- Author
-
Fredric W. Taylor, J. T. Schofield, and Daniel J. McCleese
- Subjects
biology ,Solar zenith angle ,Astronomy and Astrophysics ,Venus ,biology.organism_classification ,Atmospheric sciences ,Atmosphere of Venus ,Space and Planetary Science ,Brightness temperature ,Radiance ,Mixing ratio ,Environmental science ,Water vapor ,Optical depth - Abstract
Near-IR measurements are presented of the mean vertical and horizontal distribution of water vapor in the Venus clouds as measured by the Pioneer Venus Orbiter IR radiometer, and comparisons are made with previous data. Six thermal channels were used to generate several hundred thousand readings for determination of the mean mixing ratio. Averaging was performed as a function of the solar zenith angle, with profiles retrieved with a relaxation method applied to radiance data at 45 microns. Consideration was given to mean cloud models and temperature profiles obtained from the five temperature sounding channels scanning from 11.5-15 microns. Laboratory tests were effected to validate the transmission functions. The results included a maximum column abundances above the cloud optical depth in the early afternoon in the equatorial regions. Mixing ratio enhancement was highest on the dayside and at high altitudes, with a mean ratio of 0.0001 at a 40% uncertainty level. Day-to-day fluctuations in the pressure level at 11.5 microns was larger than 10%, far below the factors of 2-3 determined by other investigators.
- Published
- 2016
24. The lunar reconnaissance orbiter diviner lunar radiometer experiment
- Author
-
Neil Bowles, Benjamin T. Greenhagen, David A. Paige, J. Bulharowski, L. A. Soderblom, Ian Thomas, John T. Schofield, S. Loring, Bruce C. Murray, D. J. Preston, S. B. Calcutt, Fredric W. Taylor, K. J. Snook, Ashwin R. Vasavada, Marc C. Foote, Carlton C. Allen, E. M. de Jong, B. Jau, M. T. Sullivan, Daniel J. McCleese, Wayne Hartford, C. Avis, and Bruce M. Jakosky
- Subjects
Radiometer ,Infrared ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy and Astrophysics ,Silicate ,Physics::History of Physics ,Astrobiology ,law.invention ,Physics::Geophysics ,chemistry.chemical_compound ,Orbiter ,Planetary science ,chemistry ,law ,Space and Planetary Science ,Thermal ,Physics::Space Physics ,Environmental science ,Astrophysics::Earth and Planetary Astrophysics ,Lunar Laser Ranging experiment ,Diviner ,Remote sensing - Abstract
The Diviner Lunar Radiometer Experiment on NASA's Lunar Reconnaissance Orbiter will be the first instrument to systematically map the global thermal state of the Moon and its diurnal and seasonal variability. Diviner will measure reflected solar and emitted infrared radiation in nine spectral channels with wavelengths ranging from 0.3 to 400 microns. The resulting measurements will enable characterization of the lunar thermal environment, mapping surface properties such as thermal inertia, rock abundance and silicate mineralogy, and determination of the locations and temperatures of volatile cold traps in the lunar polar regions. © The author(s) 2009.
- Published
- 2016
25. Convective instability in the martian middle atmosphere
- Author
-
John T. Schofield, James H. Shirley, Nicholas G. Heavens, Mark I. Richardson, Christopher C. Lee, David M. Kass, W. G. Lawson, Armin Kleinböhl, Daniel J. McCleese, and W. A. Abdou
- Subjects
Martian ,Atmosphere ,Convective instability ,Space and Planetary Science ,Atmospheric instability ,Northern Hemisphere ,Astronomy and Astrophysics ,Atmosphere of Mars ,Gravity wave ,Atmospheric temperature ,Atmospheric sciences ,Geology - Abstract
Dry convective instabilities in Mars’s middle atmosphere are detected and mapped using temperature retrievals from Mars Climate Sounder observations spanning 1.5 martian years. The instabilities are moderately frequent in the winter extratropics. The frequency and strength of middle atmospheric convective instability in the northern extratropics is significantly higher in MY 28 than in MY 29. This may have coupled with changes to the northern hemisphere mid-latitude and tropical middle atmospheric temperatures and contributed to the development of the 2007 global dust storm. We interpret these instabilities to be the result of gravity waves saturating within regions of low stability created by the thermal tides. Gravity wave saturation in the winter extratropics has been proposed to provide the momentum lacking in general circulation models to produce the strong dynamically-maintained temperature maximum at 1–2 Pa over the winter pole, so these observations could be a partial control on modeling experiments.
- Published
- 2010
26. Intense polar temperature inversion in the middle atmosphere on Mars
- Author
-
Nicholas G. Heavens, S. B. Calcutt, Nicholas A Teanby, Stephen R. Lewis, Richard W. Zurek, Armin Kleinböhl, W. G. Lawson, Fredric W. Taylor, Don Banfield, Oded Aharonson, Patrick G. J. Irwin, John T. Schofield, Mark I. Richardson, Peter L. Read, Daniel J. McCleese, David M. Kass, W. A. Abdou, Conway B. Leovy, and David A. Paige
- Subjects
Martian ,Atmosphere ,Orbiter ,Atmospheric circulation ,law ,Downwelling ,General Earth and Planetary Sciences ,Environmental science ,Weather and climate ,Hadley cell ,Mars Exploration Program ,Atmospheric sciences ,law.invention - Abstract
Current understanding of weather, climate and global atmospheric circulation on Mars is incomplete, in particular at altitudes above about 30 km. General circulation models for Mars are similar to those developed for weather and climate forecasting on Earth and require more martian observations to allow testing and model improvements. However, the available measurements of martian atmospheric temperatures, winds, water vapour and airborne dust are generally restricted to the region close to the surface and lack the vertical resolution and global coverage that is necessary to shed light on the dynamics of Mars middle atmosphere at altitudes between 30 and 80 km (ref.7). Here we report high-resolution observations from the Mars Climate Sounder instrument on the Mars Reconnaissance Orbiter. These observations show an intense warming of the middle atmosphere over the south polar region in winter that is at least 10-20 K warmer than predicted by current model simulations. To explain this finding, we suggest that the atmospheric downwelling circulation over the pole, which is part of the equator-to-pole Hadley circulation, may be as much as 50 more vigorous than expected, with consequences for the cycles of water, dust and CO"2 that regulate the present-day climate on Mars. © 2008 Macmillan Publishers Limited.
- Published
- 2008
27. Atmospheric temperature sounding on Mars, and the climate sounder on the 2005 reconnaissance orbiter
- Author
-
John T. Schofield, Richard W. Zurek, Stephen R. Lewis, Daniel J. McCleese, Fredric W. Taylor, Peter L. Read, and S. B. Calcutt
- Subjects
Martian ,Atmospheric Science ,Aerospace Engineering ,Astronomy and Astrophysics ,Mars Exploration Program ,Atmosphere of Mars ,Atmospheric temperature ,law.invention ,Atmosphere ,Orbiter ,Depth sounding ,Geophysics ,Space and Planetary Science ,law ,General Earth and Planetary Sciences ,Environmental science ,Water vapor ,Remote sensing - Abstract
Detailed measurements of the vertical profiles of atmospheric temperature, water vapour, dust and condensates in the Martian atmosphere are needed to characterize the present-day Martian climate and to understand the intricately related processes upon which it depends. Among the most important of these are accurate and extensive temperature measurements. Progress to date, key problems still to be addressed and upcoming new approaches to the measurement task are briefly reviewed, and expectations for the Mars Climate Sounder experiment on the 2005 Mars Reconnaissance Orbiter are described. Some even more advanced methods for temperature, humidity and condensate sounding in the decade beyond MCS/MRO, and promising approaches to achieving these are also considered. (c) 2006 Published by Elsevier Ltd on behalf of COSPAR.
- Published
- 2006
28. The State and Future of Mars Polar Science and Exploration
- Author
-
Bruce C. Murray, François Forget, Stephen M. Clifford, Erik W. Blake, William D. Harrison, Dorthe Dahl-Jensen, David D. Wynn-Williams, Aaron P. Zent, S. E. Wood, John F. Nye, Kenneth Lepper, James W. Rice, Daniel J. McCleese, James A. Cutts, K. E. Herkenhoff, Andrew P. Ingersoll, Fraser P. Fanale, Bruce G. Bills, Robert M. Haberle, William B. Durham, Peter C. Thomas, Benton C. Clark, Suzanne E. Smrekar, Ralph P. Harvey, David E. Smith, Jack D. Farmer, Michael H. Carr, Ellen Mosley-Thompson, R. Grard, Kumiko Gotto-Azuma, Jonathan Cameron, Philip R. Christensen, Philip B. James, David A. Paige, Stephen R. Platt, Kenneth L. Tanaka, Hugh H. Kieffer, Jeffrey S. Kargel, H. Jay Zwally, Gary D. Clow, Wendy M. Calvin, David A. Fisher, Alan D. Howard, Carol R. Stoker, J. J. Plaut, Niels Reeh, David Crisp, Jeffrey R. Barnes, Thorsteinn Thorsteinsson, Maria T. Zuber, Janus Larsen, Richard W. Zurek, and Michael C. Malin
- Subjects
Extraterrestrial Environment ,010504 meteorology & atmospheric sciences ,Climate ,Solar luminosity ,Mars ,01 natural sciences ,Astrobiology ,Atmosphere ,Impact crater ,Planet ,Dust storm ,Exobiology ,0103 physical sciences ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Martian ,Ice ,Astronomy and Astrophysics ,Mars Exploration Program ,Atmosphere of Mars ,Carbon Dioxide ,Space Flight ,Cold Climate ,13. Climate action ,Space and Planetary Science ,Geology - Abstract
As the planet's principal cold traps, the martian polar regions have accumulated extensive mantles of ice and dust that cover individual areas of approximately 10(6) km2 and total as much as 3-4 km thick. From the scarcity of superposed craters on their surface, these layered deposits are thought to be comparatively young--preserving a record of the seasonal and climatic cycling of atmospheric CO2, H2O, and dust over the past approximately 10(5)-10(8) years. For this reason, the martian polar deposits may serve as a Rosetta Stone for understanding the geologic and climatic history of the planet--documenting variations in insolation (due to quasiperiodic oscillations in the planet's obliquity and orbital elements), volatile mass balance, atmospheric composition, dust storm activity, volcanic eruptions, large impacts, catastrophic floods, solar luminosity, supernovae, and perhaps even a record of microbial life. Beyond their scientific value, the polar regions may soon prove important for another reason--providing a valuable and accessible reservoir of water to support the long-term human exploration of Mars. In this paper we assess the current state of Mars polar research, identify the key questions that motivate the exploration of the polar regions, discuss the extent to which current missions will address these questions, and speculate about what additional capabilities and investigations may be required to address the issues that remain outstanding.
- Published
- 2000
29. Special issue of Planetary of Space Science Planet Mars II
- Author
-
Th. Encrenaz, Daniel J. McCleese, James W. Head, and Christophe Sotin
- Subjects
Space and Planetary Science ,Terrestrial planet ,Terraforming ,Astronomy and Astrophysics ,Desert planet ,Mars Exploration Program ,Planet V ,Exploration of Mars ,Geology ,Astrobiology ,Fifth planet ,Double planet - Published
- 2007
30. Initial Results of Radio Occultation Observations of Earth's Atmosphere Using the Global Positioning System
- Author
-
Stephen S. Leroy, E. R. Kursinski, T. P. Yunck, Larry Romans, John T. Schofield, Willy Bertiger, William G. Melbourne, T. K. Meehan, Daniel J. McCleese, J. R. Eyre, George A. Hajj, R. N. Nagatani, and Catherine L. Thornton
- Subjects
Atmospheric sounding ,Multidisciplinary ,GNSS radio occultation ,Meteorology ,Global Ozone Monitoring by Occultation of Stars ,Occultation ,law.invention ,Atmosphere of Earth ,law ,Radiosonde ,Satellite ,Radio occultation ,Astrophysics::Earth and Planetary Astrophysics ,Physics::Atmospheric and Oceanic Physics - Abstract
Recent radio occultation measurements using Global Positioning System satellite transmitters and an orbiting receiver have provided a globally distributed set of high-resolution atmospheric profiles, suggesting that the technique may make a significant contribution to global change and weather prediction programs. Biases in occultation temperatures relative to radiosonde and model data are about 1 kelvin or less in the tropics and are generally less than 0.5 kelvin at higher latitudes. Data quality is sufficient to quantify significant model errors in remote regions. Temperature profiles also reveal either an equatorial Rossby-gravity or an inertio-gravity wave. Such waves provide a fundamental source of momentum for the stratospheric circulation.
- Published
- 1996
31. Carbon dioxide snow clouds on Mars: South polar winter observations by the Mars Climate Sounder
- Author
-
Armin Kleinböhl, Nicholas G. Heavens, Paul O. Hayne, David M. Kass, John T. Schofield, Daniel J. McCleese, and David A. Paige
- Subjects
Atmospheric Science ,Soil Science ,Aquatic Science ,Oceanography ,Atmospheric sciences ,Atmosphere ,Geochemistry and Petrology ,Earth and Planetary Sciences (miscellaneous) ,Emissivity ,Astrophysics::Galaxy Astrophysics ,Physics::Atmospheric and Oceanic Physics ,Earth-Surface Processes ,Water Science and Technology ,Ecology ,Paleontology ,Forestry ,Mars Exploration Program ,Albedo ,Snow ,Geophysics ,Space and Planetary Science ,Mars Orbiter Laser Altimeter ,Environmental science ,Martian polar ice caps ,Astrophysics::Earth and Planetary Astrophysics ,Polar mesospheric clouds - Abstract
[1] We present south polar winter infrared observations from the Mars Climate Sounder (MCS) and test three hypotheses concerning the origins of “cold spots”: regions of anomalously low infrared brightness temperatures, which could be due to enrichment in non-condensable gases, low-emissivity surface frost, or optically thick CO2 clouds. Clouds and surface frosts have been historically difficult to distinguish, but the unique limb sounding capability of MCS reveals extensive tropospheric CO2clouds over the cold spots. We find that both clouds and surface deposits play a significant role in lowering the infrared emissivity of the seasonal ice cap, and the granular surface deposits are likely emplaced by snowfall. Surface temperatures indicate the polar winter atmosphere is enriched by a factor ∼5–7 in non-condensable gases relative to the annual average, consistent with earlier gamma ray spectrometer observations, but not enough to account for the low brightness temperatures. A large ∼500-km diameter cloud with visible optical depth ∼0.1–1.0 persists throughout winter over the south polar residual cap (SPRC). At latitudes 70–80°S, clouds and low emission regions are smaller and shorter-lived, probably corresponding to large-grained “channel 1” clouds observed by the Mars Orbiter Laser Altimeter. Snowfall over the SPRC imparts the lowest emissivity in the south polar region, which paradoxically tends to reduce net accumulation of seasonal CO2 by backscattering infrared radiation. This could be compensated by the observed anomalously high summertime albedo of the SPRC, which may be related to small grains preserved in a rapidly formed snow deposit.
- Published
- 2012
32. The vertical distribution of dust in the Martian atmosphere during northern spring and summer: Observations by the Mars Climate Sounder and analysis of zonal average vertical dust profiles
- Author
-
Armin Kleinböhl, Mark I. Richardson, W. A. Abdou, Daniel J. McCleese, P. M. Wolkenberg, Nicholas G. Heavens, David M. Kass, J. L. Benson, James H. Shirley, and John T. Schofield
- Subjects
Martian ,Atmospheric Science ,Ecology ,Opacity ,Paleontology ,Soil Science ,Tropics ,Forestry ,Mars Exploration Program ,Atmosphere of Mars ,Aquatic Science ,Radiative forcing ,Oceanography ,Atmospheric sciences ,Geophysics ,Space and Planetary Science ,Geochemistry and Petrology ,Dust storm ,Climatology ,Earth and Planetary Sciences (miscellaneous) ,Mixing ratio ,Environmental science ,Earth-Surface Processes ,Water Science and Technology - Abstract
[1] The vertical distribution of dust in Mars's atmosphere is a critical and poorly known input in atmospheric physical and chemical models and a source of insight into the lifting and transport of dust and general vertical mixing in the atmosphere. We investigate vertical profiles of dust opacity retrieved from limb observations by Mars Climate Sounder during the relatively dust-clear Martian northern summer of 2006–2007 (Ls = 111°–177°of Mars year (MY) 28) and Martian northern spring and summer of 2007–2008 (Ls = 0°–180° of MY 29). To represent local maxima in inferred mass mixing ratio in these profiles, we develop an empirical alternative to the classic “Conrath profile” for representing the vertical distribution of dust in the Martian atmosphere. We then assess the magnitude and variability of atmospheric dust loading, the depth of dust penetration during these seasons, and the impact of the observed vertical dust distribution on the radiative forcing of the circulation. During most of northern spring and summer, the dust mass mixing ratio in the tropics has a maximum at 15–25 km above the local surface (the high-altitude tropical dust maximum (HATDM)). The HATDM appears to have increased significantly in magnitude and altitude during middle to late northern summer of MY 29. The HATDM gradually decayed during late summer of MY 28. Interannual variability in the dust distribution during middle to late northern summer may be connected with known interannual variability in tropical dust storm activity.
- Published
- 2011
33. Vertical distribution of dust in the Martian atmosphere during northern spring and summer: High-altitude tropical dust maximum at northern summer solstice
- Author
-
P. M. Wolkenberg, David M. Kass, Nicholas G. Heavens, W. A. Abdou, James H. Shirley, Daniel J. McCleese, John T. Schofield, Armin Kleinböhl, Mark I. Richardson, and J. L. Benson
- Subjects
Atmospheric Science ,Ecology ,Paleontology ,Soil Science ,Forestry ,Storm ,Mars Exploration Program ,Atmosphere of Mars ,Aquatic Science ,Oceanography ,Atmospheric sciences ,Atmosphere ,Mars general circulation model ,Geophysics ,Altitude ,Space and Planetary Science ,Geochemistry and Petrology ,Dust storm ,Climatology ,Earth and Planetary Sciences (miscellaneous) ,Environmental science ,Outflow ,Earth-Surface Processes ,Water Science and Technology - Abstract
[1] The vertical distribution of dust in Mars' atmosphere is a critical unknown in the simulation of its general circulation and a source of insight into the lifting and transport of dust. Zonal average vertical profiles of dust opacity retrieved by Mars Climate Sounder show that the vertical dust distribution is mostly consistent with Mars general circulation model (GCM) simulations in southern spring and summer but not in northern spring and summer. Unlike the GCM simulations, the mass mixing ratio of dust has a maximum at 15–25 km over the tropics during much of northern spring and summer: the high-altitude tropical dust maximum (HATDM). The HATDM has significant and characteristic longitudinal variability, which it maintains for time scales on the order of or greater than those on which advection, sedimentation, and vertical eddy diffusion would act to eliminate both the longitudinal and vertical inhomogeneity of the distribution. While outflow from dust storms is able to produce enriched layers of dust at altitudes much greater than 25 km, tropical dust storm activity during the period in which the HATDM occurs is likely too rare to support the HATDM. Instead, the lifting of dust by mesoscale circulations over topography, pseudomoist convection due to the solar heating of dust, and scavenging of dust by water ice are all possible drivers of the HATDM.
- Published
- 2011
34. 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
- Author
-
Daniel J. McCleese, Armin Kleinböhl, Fredric W. Taylor, Richard W. Zurek, Pgj Irwin, Joshua L. Bandfield, S. B. Calcutt, Peter L. Read, John T. Schofield, James H. Shirley, David M. Kass, W. A. Abdou, Stephen R. Lewis, Nicholas G. Heavens, Mark I. Richardson, David A. Paige, and Nicholas A Teanby
- Subjects
Martian ,Atmospheric Science ,Ecology ,Paleontology ,Soil Science ,Forestry ,Atmosphere of Mars ,Mars Exploration Program ,Aquatic Science ,Oceanography ,Atmospheric sciences ,Aerosol ,Atmosphere ,Geophysics ,Space and Planetary Science ,Geochemistry and Petrology ,Polar vortex ,Earth and Planetary Sciences (miscellaneous) ,Mixing ratio ,Environmental science ,Martian polar ice caps ,Earth-Surface Processes ,Water Science and Technology - Abstract
The first Martian year and a half of observations by the Mars Climate Sounder aboard the Mars Reconnaissance Orbiter has revealed new details of the thermal structure and distributions of dust and water ice in the atmosphere. The Martian atmosphere is shown in the observations by the Mars Climate Sounder to vary seasonally between two modes: a symmetrical equinoctial structure with middle atmosphere polar warming and a solstitial structure with an intense middle atmosphere polar warming overlying a deep winter polar vortex. The dust distribution, in particular, is more complex than appreciated before the advent of these high (∼5 km) vertical resolution observations, which extend from near the surface to above 80 km and yield 13 dayside and 13 nightside pole-to-pole cross sections each day. Among the new features noted is a persistent maximum in dust mass mixing ratio at 15-25 km above the surface (at least on the nightside) during northern spring and summer. The water ice distribution is very sensitive to the diurnal and seasonal variation of temperature and is a good tracer of the vertically propagating tide. Copyright 2010 by the American Geophysical Union.
- Published
- 2010
35. Mars' south polar hood as observed by the Mars Climate Sounder
- Author
-
Daniel J. McCleese, Armin Kleinböhl, Fredric W. Taylor, David M. Kass, J. L. Benson, and John T. Schofield
- Subjects
Atmospheric Science ,Ice cloud ,Daytime ,Ecology ,Paleontology ,Soil Science ,Forestry ,Mars Exploration Program ,Aquatic Science ,Oceanography ,Atmospheric temperature ,Atmospheric sciences ,Latitude ,Geophysics ,Space and Planetary Science ,Geochemistry and Petrology ,Earth and Planetary Sciences (miscellaneous) ,Longitude ,Optical depth ,Geology ,Water vapor ,Earth-Surface Processes ,Water Science and Technology - Abstract
[1] We have used observations from the Mars Climate Sounder to investigate south polar hood water ice clouds (at 12 μm), including the first systematic examination of the vertical (5 km resolution) and nighttime structure. We find that the structure and evolution of the polar hood is controlled more strongly by atmospheric temperature variations than by intrinsic fluctuations in water vapor abundance. The clouds form as a belt during LS = 10°–70° (phase 1) and LS = 100°–200° (phase 2). During phase 1, the cloud belt extends over a wide latitude range, between 30°S and 75°S with a visible column optical depth between 0.075 and 0.15. The cloud belt then evaporates as temperatures warm. During phase 2, the cloud belt reappears due to an increase in water vapor as a partial band of low-opacity clouds south of the Tharsis region and eventually becomes continuous in longitude, with a visible column opacity between 0.125 and 0.25. As the southern spring equinox approaches, the cloud belt shifts southward, following the seasonal cap edge. From LS = 140° to LS = 200°, the daytime belt lies about 15° farther south than the nighttime belt, due to tidally driven diurnal temperature differences. The vertical structure of the cloud belt is consistent within and between the two seasonal phases and is characterized by a thick lower cloud deck and an upper layer whose altitude shifts between the nighttime and daytime because of thermal tidal control of the condensation altitudes. Overall, the southern polar hood is observed to rapidly form and dissipate as the temperature crosses the saturation point of water vapor.
- Published
- 2010
36. Diviner Lunar Radiometer observations of cold traps in the Moon's south polar region
- Author
-
Benjamin T. Greenhagen, Joshua L. Bandfield, Jo Ann Zhang, Timothy D. Glotch, Daniel J. McCleese, Laurence A. Soderblom, Wayne Hartford, Paul G. Lucey, John T. Schofield, Bruce C. Murray, Richard C. Elphic, Fredric W. Taylor, Paul O. Hayne, Kristen A. Bennett, Carlton Allen, S. B. Calcutt, Michael B. Wyatt, Marc C. Foote, David A. Paige, Neil Bowles, Kelly Snook, Bruce G. Bills, E. DeJong, E. J. Foote, Rebecca R. Ghent, Ashwin R. Vasavada, and Matthew A. Siegler
- Subjects
Lunar water ,Solar System ,Multidisciplinary ,Radiometer ,Impact crater ,Satellite ,Ejecta ,Geology ,Diviner ,Plume ,Astrobiology - Abstract
Watering the Moon About a year ago, a spent upper stage of an Atlas rocket was deliberately crashed into a crater at the south pole of the Moon, ejecting a plume of debris, dust, and vapor. The goal of this event, the Lunar Crater Observation and Sensing Satellite (LCROSS) experiment, was to search for water and other volatiles in the soil of one of the coldest places on the Moon: the permanently shadowed region within the Cabeus crater. Using ultraviolet, visible, and near-infrared spectroscopy data from accompanying craft, Colaprete et al. (p. 463 ; see the news story by Kerr ; see the cover) found evidence for the presence of water and other volatiles within the ejecta cloud. Schultz et al. (p. 468 ) monitored the different stages of the impact and the resulting plume. Gladstone et al. (p. 472 ), using an ultraviolet spectrograph onboard the Lunar Reconnaissance Orbiter (LRO), detected H 2 , CO, Ca, Hg, and Mg in the impact plume, and Hayne et al. (p. 477 ) measured the thermal signature of the impact and discovered that it had heated a 30 to 200 square-meter region from ∼40 kelvin to at least 950 kelvin. Paige et al. (p. 479) mapped cryogenic zones predictive of volatile entrapment, and Mitrofanov et al. (p. 483 ) used LRO instruments to confirm that surface temperatures in the south polar region persist even in sunlight. In all, about 155 kilograms of water vapor was emitted during the impact; meanwhile, the LRO continues to orbit the Moon, sending back a stream of data to help us understand the evolution of its complex surface structures.
- Published
- 2010
37. Water ice clouds over the Martian tropics during northern summer
- Author
-
Daniel J. McCleese, David M. Kass, W. A. Abdou, Armin Kleinböhl, James H. Shirley, Mark I. Richardson, P. M. Wolkenberg, Nicholas G. Heavens, J. L. Benson, and John T. Schofield
- Subjects
Martian ,Ice cloud ,Tropics ,Mars Exploration Program ,Atmospheric model ,Atmospheric sciences ,complex mixtures ,Atmosphere ,Geophysics ,Altitude ,General Earth and Planetary Sciences ,Environmental science ,Martian polar ice caps ,sense organs - Abstract
[1] Atmospheric models suggest that infrared heating due to water ice clouds over the tropics of Mars during early northern summer has a significant impact on the thermal structure of the tropics at cloud level and of the middle atmosphere near the south pole. Retrievals from limb observations by the Mars Climate Sounder on Mars Reconnaissance Orbiter during early northern summer show that water ice clouds over the northern tropics are thinner and higher than in published model results. Later in this season, the latitudinal extent, apparent mass mixing ratio (and infrared heating rate), and altitude of nighttime tropical clouds significantly increase, reaching a maximum just before northern fall equinox. Published model results do not show this transition. By underestimating the altitude at which water ice clouds form, models also may underestimate the intensity of the meridional circulation at higher altitudes in the tropics during northern summer.
- Published
- 2010
38. Electrooptic phase modulation gas correlation spectroscopy: a laboratory demonstration
- Author
-
David M. Rider, John T. Schofield, Daniel J. McCleese, and Jack S. Margolis
- Subjects
Materials science ,business.industry ,Materials Science (miscellaneous) ,Industrial and Manufacturing Engineering ,Spectral line ,Mesosphere ,symbols.namesake ,Optics ,Physics::Space Physics ,symbols ,Astrophysics::Solar and Stellar Astrophysics ,Business and International Management ,Spectroscopy ,business ,Doppler effect ,Refractive index ,Phase modulation ,Stratosphere ,Physics::Atmospheric and Oceanic Physics ,Atmospheric optics - Abstract
A new gas-correlation spectroscopy technique is described which uses electrooptic phase modulation (EOPM) of atmospheric emission spectra together with a reference cell to selectively detect radiatively active gases. Laboratory results demonstrate that the EOPM gas-correlation technique is a sensitive approach to species abundance measurements, and support the feasibility of an instrument for measurement of winds in the stratosphere and mesosphere using an EOPM. Through the measurement of wind-induced Doppler shifts in the spectra of atmospheric species, this instrument offers a means of monitoring the wind field in the 20-100 km altitude range from a satellite.
- Published
- 2010
39. Mars Climate Sounder limb profile retrieval of atmospheric temperature, pressure, and dust and water ice opacity
- Author
-
Armin Kleinböhl, Fredric W. Taylor, Nicholas A Teanby, C. Backus, Bhaswar Sen, W. A. Abdou, Mark I. Richardson, John T. Schofield, James H. Shirley, David M. Kass, W. Gregory Lawson, and Daniel J. McCleese
- Subjects
Martian ,Atmospheric Science ,Radiometer ,Ecology ,Opacity ,Paleontology ,Soil Science ,Forestry ,Atmosphere of Mars ,Mars Exploration Program ,Aquatic Science ,Oceanography ,Atmospheric sciences ,Atmospheric temperature ,Geophysics ,Space and Planetary Science ,Geochemistry and Petrology ,Earth and Planetary Sciences (miscellaneous) ,Radiative transfer ,Environmental science ,Water vapor ,Earth-Surface Processes ,Water Science and Technology ,Remote sensing - Abstract
The Mars Climate Sounder (MCS) onboard the Mars Reconnaissance Orbiter is the latest of a series of investigations devoted to improving the understanding of current Martian climate. MCS is a nine-channel passive midinfrared and far-infrared filter radiometer designed to measure thermal emission in limb and on-planet geometries from which vertical profiles of atmospheric temperature, water vapor, dust, and condensates can be retrieved. Here we describe the algorithm that is used to retrieve atmospheric profiles from MCS limb measurements for delivery to the Planetary Data System. The algorithm is based on a modified Chahine method and uses a fast radiative transfer scheme based on the Curtis-Godson approximation. It retrieves pressure and vertical profiles of atmospheric temperature, dust opacity, and water ice opacity. Water vapor retrievals involve a different approach and will be reported separately. Pressure can be retrieved to a precision of 1–2% and is used to establish the vertical coordinate. Temperature profiles are retrieved over a range from 5–10 to 80–90 km altitude with a typical altitude resolution of 4–6 km and a precision between 0.5 and 2 K over most of this altitude range. Dust and water ice opacity profiles also achieve vertical resolutions of about 5 km and typically have precisions of 10^(−4)–10^(−5) km^(−1) at 463 cm^(−1) and 843 cm^(−1), respectively. Examples of temperature profiles as well as dust and water ice opacity profiles from the first year of the MCS mission are presented, and atmospheric features observed during periods employing different MCS operational modes are described. An intercomparison with historical temperature measurements from the Mars Global Surveyor mission shows good agreement.
- Published
- 2009
40. Thermal tides in the Martian middle atmosphere as seen by the Mars Climate Sounder
- Author
-
Christopher C. Lee, Anthony D. Toigo, W. G. Lawson, Daniel J. McCleese, David M. Kass, John T. Schofield, Conway B. Leovy, Richard W. Zurek, Nicholas G. Heavens, Don Banfield, Mark I. Richardson, Armin Kleinböhl, and Fredric W. Taylor
- Subjects
Martian ,Atmospheric Science ,Mesoscale convective system ,Ecology ,Opacity ,Paleontology ,Soil Science ,Forestry ,Atmosphere of Mars ,Mars Exploration Program ,Aquatic Science ,Oceanography ,Atmospheric sciences ,Article ,Latitude ,Atmosphere ,Geophysics ,Space and Planetary Science ,Geochemistry and Petrology ,Climatology ,Thermal ,Earth and Planetary Sciences (miscellaneous) ,Environmental science ,Earth-Surface Processes ,Water Science and Technology - Abstract
The first systematic observations of the middle atmosphere of Mars (35–80km) with the Mars Climate Sounder (MCS) show dramatic patterns of diurnal thermal variation, evident in retrievals of temperature and water ice opacity. At the time of writing, the data set of MCS limb retrievals is sufficient for spectral analysis within a limited range of latitudes and seasons. This analysis shows that these thermal variations are almost exclusively associated with a diurnal thermal tide. Using a Martian general circulation model to extend our analysis, we show that the diurnal thermal tide dominates these patterns for all latitudes and all seasons.
- Published
- 2009
41. Mars Climate Sounder: An investigation of thermal and water vapor structure, dust and condensate distributions in the atmosphere, and energy balance of the polar regions
- Author
-
David M. Kass, Peter L. Read, Richard W. Zurek, Daniel J. McCleese, John T. Schofield, S. B. Calcutt, David A. Paige, Fredric W. Taylor, Marc C. Foote, and Conway B. Leovy
- Subjects
Atmospheric Science ,Meteorology ,Soil Science ,Aquatic Science ,Oceanography ,Atmospheric sciences ,law.invention ,Atmosphere ,Orbiter ,Geochemistry and Petrology ,law ,Martian surface ,Earth and Planetary Sciences (miscellaneous) ,Weather satellite ,Earth-Surface Processes ,Water Science and Technology ,Ecology ,Paleontology ,Forestry ,Mars Exploration Program ,Atmosphere of Mars ,Atmospheric temperature ,Geophysics ,Space and Planetary Science ,Environmental science ,Water vapor - Abstract
Against a backdrop of intensive exploration of the Martian surface environment, intehded to lead to human exploration, some aspects of the modern climate and the meteorology of Mars remain relatively unexplored. In particular, there is a need for detailed measurements of the vertical profiles of atmospheric temperature, water vapor, dust, and condensates to understand the intricately related processes upon which the surface conditions, and those encountered during descent by landers, depend. The most important of these missing data are accurate and extensive temperature measurements with high vertical resolution. The Mars Climate Sounder experiment on the 2005 Mars Reconnaissance Orbiter, described here, is the latest attempt to characterize the Martian atmosphere with the sort of coverage and precision achieved by terrestrial weather satellites. If successful, it is expected to lead to corresponding improvements in our understanding of meteorological phenomena and to enable improved general circulation models of the Martian atmosphere for climate studies on a range of timescales. Copyright 2007 by the American Geophysical Union.
- Published
- 2007
42. An Investigation Of The Dynamics And Transport In The Middle Atmosphere
- Author
-
Daniel J. McCleese, D.M. Rider, and L.S. Elson
- Subjects
Atmosphere ,business.industry ,Environmental science ,Aerospace engineering ,Propulsion ,business ,Simulation - Published
- 2005
43. Linear and 2-D thermopile detector arrays using high-Z thermoelectric materials
- Author
-
W. Hu, T. A. McCann, John T. Schofield, M. Kenyon, E. W. Jones, M. R. Dickie, Daniel J. McCleese, S. Gaalema, Marc C. Foote, T. R. Krueger, and S.L. Soll
- Subjects
Materials science ,Spacecraft ,business.industry ,Detector ,Electrical engineering ,Mars Exploration Program ,Thermoelectric materials ,Thermopile ,Jet propulsion ,law.invention ,Orbiter ,Surface micromachining ,law ,Optoelectronics ,business - Abstract
The Jet Propulsion Laboratory has, for several years now, maintained a thermopile detector array program to address NASA application niches. An established process exists for producing thermopile single detectors and linear arrays using Bi-Te and Bi-Sb-Te thermoelectric materials and bulk silicon micromachining techniques. The detectors and arrays typically have D* values of 1-2 /spl times/ 10/sup 9/ cmHz/sup 1/2//W in vacuum. Arrays are being fabricated for the Mars Climate Sounder instrument on NASA's Mars Reconnaissance Orbiter spacecraft, to launch in 2005. A second effort is seeking to develop high performance two-dimensional arrays of thermopile detectors using surface micromachining to fabricate pixels on a substrate containing readout electronics.
- Published
- 2003
44. Space science applications of thermopile detector arrays
- Author
-
John T. Schofield, T. R. Krueger, Marc C. Foote, M. R. Dickie, T. A. McCann, Daniel J. McCleese, and Eric W. Jones
- Subjects
Physics ,Physics::Instrumentation and Detectors ,Detector ,Satellite system ,NPOESS ,Mars Exploration Program ,Radiation ,Thermopile ,law.invention ,Orbiter ,law ,Physics::Space Physics ,Astrophysics::Earth and Planetary Astrophysics ,Space Science ,Remote sensing - Abstract
Thermal detectors, while typically less sensitive than quantum detectors, are useful when the combination of long wavelength signals and relatively high temperature operation makes quantum detectors unsuitable. Thermal detectors are also appropriate in applications requiring flat spectral response over a broad wavelength range. JPL produces thermopile detectors and linear arrays to meet space science requirements in these categories. Thermopile detectors and arrays are currently being fabricated for two space applications. The first is the Mars Climate Sounder (MCS) instrument, to fly on the Mars Reconnaissance Orbiter mission, scheduled to launch in 2005. MCS is an atmospheric limb sounder utilizing nine 21-element thermopile arrays. The second application is the Earth Radiation Budget Suite (ERBS), part of the National Polar Orbiting Environmental Satellite System (NPOESS). This instrument measures upwelling radiation from the earth in the spectral range 0.3-100 μm.
- Published
- 2003
45. On the orbital forcing of Martian water and CO2cycles: A general circulation model study with simplified volatile schemes
- Author
-
Michael Mischna, R. John Wilson, Daniel J. McCleese, and Mark I. Richardson
- Subjects
Atmospheric Science ,Soil Science ,Atmospheric model ,Aquatic Science ,Oceanography ,Surface pressure ,Atmospheric sciences ,Physics::Geophysics ,Atmosphere ,Mars general circulation model ,Geophysical fluid dynamics ,Geochemistry and Petrology ,Earth and Planetary Sciences (miscellaneous) ,Physics::Atmospheric and Oceanic Physics ,Earth-Surface Processes ,Water Science and Technology ,Martian ,Ecology ,Paleontology ,Forestry ,Mars Exploration Program ,Geophysics ,Space and Planetary Science ,Physics::Space Physics ,Astrophysics::Earth and Planetary Astrophysics ,Water vapor ,Geology - Abstract
[1] Variations in the Martian water and CO2 cycles with changes in orbital and rotational parameters are examined using the Geophysical Fluid Dynamics Laboratory Mars General Circulation Model. The model allows for arbitrary specification of obliquity, eccentricity, and argument of perihelion as well as the position and thickness of surface ice. Exchange of CO2 between the surface and atmosphere is modeled, generating seasonal cycles of surface ice and surface pressure. Water is allowed to exchange between the surface and atmosphere, cloud formation is treated, and both cloud and vapor are transported by modeled winds and diffusion. Exchange of water and CO2 with the subsurface is not allowed, and radiative effects of water vapor and clouds are not treated. The seasonal cycle of CO2 is found to become more extreme at high obliquity, as suggested by simple heat balance models. Maximum pressures remain largely the same, but the minima decrease substantially as more CO2 condenses in the more extensive polar night. Vapor and cloud abundances increase dramatically with obliquity. The stable location for surface ice moves equatorward with increasing obliquity, such that by 45° obliquity, water ice is stable in the tropics only. Ice is not spatially uniform, but rather found preferentially in regions of high thermal inertia or high topography. Eccentricity and argument of perihelion can provide a second-order modification to the distribution of surface ice by altering the temporal distribution of insolation at the poles. Further model simulations reveal the robustness of these distributions for a variety of initial conditions. Our findings shed light on the nature of near-surface, ice-rich deposits at midlatitudes and low-latitudes on Mars.
- Published
- 2003
46. Mars exploration program strategy - 1995-2020
- Author
-
Daniel J. McCleese and Donna L. Shirley
- Subjects
Mars landing ,Mars Exploration Program ,Exploration of Mars ,Geology ,Astrobiology - Published
- 1996
47. Stratospheric wind infrared limb sounder
- Author
-
David M. Rider and Daniel J. McCleese
- Subjects
Atmospheric sounding ,Physics ,Earth's orbit ,Meteorology ,Infrared ,Space operations ,Orbital mechanics ,Stratosphere ,Wind measurement ,Remote sensing - Abstract
The Stratospheric Wind Infrared Limb Sounder (SWIRLS), which measures wind, temperature, and the abundance of O3 and N2O in the stratosphere from earth orbit is selected as one of the complement of atmospheric sounders that will fly on the Earth Observing System B platform series. This paper outlines the SWIRLS investigation and describes laboratory experiments demonstrating SWIRLS wind measurement capabilities.
- Published
- 1991
48. The Study of Atmospheric Transport by the SWIRLS Instrument on Eos
- Author
-
Daniel J. McCleese and David M. Rider
- Abstract
The Stratospheric Wind Infrared Limb Sounder (SWIRLS) investigation which has been selected for the Earth Observing System (Eos) is an investigation of dynamics and transport in the stratosphere that brings together the key measurements needed to develop an understanding of the coupling between chemistry and dynamics in the stratosphere. The investigation focuses on developing a description of the dynamical climatology of the stratosphere with emphasis on winds and temperature, and their variation on time scales ranging from diurnal to interannual. In addition, the the investigation will quantify the physical mechanisms responsible for structure and variations of the stratospheric circulation and temperature fields, including the transport of heat and momentum and will directly investigate the transport of ozone and and other trace atmospheric constituents. Existing measurements lack the combination of accuracy, global and temporal coverage, spatial resolution and simultaneity required to distinguish between dynamics and photochemical processes. Improved instruments are needed to understand why ozone and other trace constituents have their current distribution and how they are evolving.
- Published
- 1990
49. NASA's Mars surveyor program: 1996–2005
- Author
-
Daniel J. McCleese
- Subjects
Atmospheric Science ,business.industry ,Mars landing ,Aerospace Engineering ,Astronomy and Astrophysics ,Mars Exploration Program ,Surveyor ,Exploration of Mars ,Astrobiology ,Geophysics ,Space and Planetary Science ,General Earth and Planetary Sciences ,Mars global surveyor ,business ,Voyager program (Mars) ,Geology ,Remote sensing - Published
- 1997
50. Atmosphere and climate studies of Mars using the Mars Observer pressure modulator infrared radiometer
- Author
-
John T. Schofield, Daniel J. McCleese, Conway B. Leovy, Richard W. Zurek, R. D. Haskins, David A. Paige, and Fredric W. Taylor
- Subjects
Earth's energy budget ,Atmospheric Science ,Soil Science ,Aquatic Science ,Oceanography ,Atmospheric sciences ,Atmosphere ,Geochemistry and Petrology ,Earth and Planetary Sciences (miscellaneous) ,Physics::Atmospheric and Oceanic Physics ,Earth-Surface Processes ,Water Science and Technology ,Remote sensing ,Atmospheric sounding ,Ecology ,Paleontology ,Forestry ,Mars Exploration Program ,Atmosphere of Mars ,Atmospheric temperature ,Geophysics ,Space and Planetary Science ,Mars Orbiter Laser Altimeter ,Physics::Space Physics ,Environmental science ,Timekeeping on Mars ,Astrophysics::Earth and Planetary Astrophysics - Abstract
Studies of the climate and atmosphere of Mars are limited at present by a lack of meteorological data having systematic global coverage with good horizontal and vertical resolution. The Mars Observer spacecraft in a low, nearly circular, polar orbit will provide an excellent platform for acquiring the data needed to advance significantly our understanding of the Martian atmosphere and its remarkable variability. The Mars Observer pressure modulator infrared radiometer (PMIRR) is a nine-channel limb and nadir scanning atmospheric sounder which will observe the atmosphere of Mars globally from 0 to 80 km for a full Martian year. PMIRR employs narrow-band radiometric channels and two pressure modulation cells to measure atmospheric and surface emission in the thermal infrared. PMIRR infrared and visible measurements will be combined to determine the radiative balance of the polar regions, where a sizeable fraction of the global atmospheric mass annually condenses onto and sublimes from the surface. Derived meteorological fields, including diabatic heating and cooling and the vertical variation of horizontal winds, are computed from the globally mapped fields retrieved from PMIRR data.
- Published
- 1992
Catalog
Discovery Service for Jio Institute Digital Library
For full access to our library's resources, please sign in.