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Buratti BJ, Orton GS, Roman MT, Momary T, Bauer JM. Astronomical Observations in Support of Planetary Entry-Probes to the Outer Planets. SPACE SCIENCE REVIEWS 2024; 220:46. [PMID: 38873000 PMCID: PMC11166823 DOI: 10.1007/s11214-024-01080-3] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 11/06/2023] [Accepted: 05/14/2024] [Indexed: 06/15/2024]
Abstract
A team of Earth-based astronomical observers supporting a giant planet entry-probe event substantially enhances the scientific return of the mission. An observers' team provides spatial and temporal context, additional spectral coverage and resolution, viewing geometries that are not available from the probe or the main spacecraft, tracking, supporting data in case of a failure, calibration benchmarks, and additional opportunities for education and outreach. The capabilities of the support program can be extended by utilizing archived data. The existence of a standing group of observers facilitates the path towards acquiring Director's Discretionary Time at major telescopes, if, for example, the probe's entry date moves. The benefits of a team convened for a probe release provides enhanced scientific return throughout the mission. Finally, the types of observations and the organization of the teams described in this paper could serve as a model for flight projects in general.
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Affiliation(s)
- Bonnie J. Buratti
- Jet Propulsion Laboratory California Institute of Technology, Pasadena, CA USA
| | - Glenn S. Orton
- Jet Propulsion Laboratory California Institute of Technology, Pasadena, CA USA
| | | | - Thomas Momary
- Jet Propulsion Laboratory California Institute of Technology, Pasadena, CA USA
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Assessment of the Impact of Ionizing Radiation Absorption on the Structural, Mechanical and Biophysical Properties of Textiles Used in Multilayer Space Suit. MATERIALS 2022; 15:ma15144992. [PMID: 35888459 PMCID: PMC9320627 DOI: 10.3390/ma15144992] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 05/09/2022] [Revised: 06/30/2022] [Accepted: 07/14/2022] [Indexed: 12/10/2022]
Abstract
The article presents research on ergonomics, biophysical comfort and safety of protective clothing. The resistance of the structural, thermal and mechanical properties of five fabrics (CBXS400, GG200T, Twaron CT736, Dyneema HB26 and T1790C), differing in geometry and raw material composition used in space suits, to dangerous ionizing radiation (β and γ) occurring in space was tested. For both types of radiation, four identical one-time doses in the range of 25–100 kGy were used. The effect of the applied absorbed doses of β and γ radiation on the parameters of textiles influencing ergonomics and safety of the cosmonaut’s work was verified by structural tests (micro-computed tomography and optical microcopy), thermal resistance tests (sweating guarded-hotplate) and strength tests (tensile testing machine). Experimental studies of thermal properties are supplemented with heat transport simulations using the finite volume method performed with 3D models of real textiles. The greatest reduction of thermal resistance for Twaron CT736 (−0.0667 m2·°C·W−1 for 100 kGy of β-radiation) and Dyneema HB26 (−0.0347 m2·°C·W−1 for 50 kGy of β-radiation) is observed. Strength tests have shown that all tested textiles are resistant to both types of radiation. Three textiles were selected to create a three-layer assembly with potential application in a cosmonaut’s glove (Extravehicular Activity—EVA).
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Mandt K, Mousis O, Marty B, Cavalié T, Harris W, Hartogh P, Willacy K. Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites. SPACE SCIENCE REVIEWS 2015; 197:297-342. [PMID: 31105346 PMCID: PMC6525011 DOI: 10.1007/s11214-015-0161-z] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
Comets play a dual role in understanding the formation and evolution of the solar system. First, the composition of comets provides information about the origin of the giant planets and their moons because comets formed early and their composition is not expected to have evolved significantly since formation. They, therefore serve as a record of conditions during the early stages of solar system formation. Once comets had formed, their orbits were perturbed allowing them to travel into the inner solar system and impact the planets. In this way they contributed to the volatile inventory of planetary atmospheres. We review here how knowledge of comet composition up to the time of the Rosetta mission has contributed to understanding the formation processes of the giant planets, their moons and small icy bodies in the solar system. We also discuss how comets contributed to the volatile inventories of the giant and terrestrial planets.
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Affiliation(s)
- K.E. Mandt
- Southwest Research Institute, San Antonio, TX, USA
| | - O. Mousis
- Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388, Marseille, France
| | - B. Marty
- CRPG-CNRS, Nancy-Université, Vandoeuvre-lès-Nancy, France
| | - T. Cavalié
- Max Planck Institute for Solar System Research, Göttingen, Germany
| | - W. Harris
- University of Arizona, Tucson, AZ, USA
| | - P. Hartogh
- Max Planck Institute for Solar System Research, Göttingen, Germany
| | - K. Willacy
- Jet Propulsion Laboratory, Pasadena, CA, USA
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Yurchenko SN, Barber RJ, Yachmenev A, Thiel W, Jensen P, Tennyson J. A Variationally Computed T = 300 K Line List for NH3. J Phys Chem A 2009; 113:11845-55. [DOI: 10.1021/jp9029425] [Citation(s) in RCA: 152] [Impact Index Per Article: 10.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/30/2022]
Affiliation(s)
- Sergei N. Yurchenko
- Institut für Physikalische Chemie und Elektrochemie, Technische Universität Dresden, D-01062 Dresden, Germany, Department of Physics and Astronomy, University College London, London WC1E 6BT, U.K., Max-Planck-Institut für Kohlenforschung, Kaiser-Wilhelm-Platz 1, D-45470 Mülheim an der Ruhr, Germany, and FBC, Theoretische Chemie, Bergische Universität, D-42097 Wuppertal, Germany
| | - Robert J. Barber
- Institut für Physikalische Chemie und Elektrochemie, Technische Universität Dresden, D-01062 Dresden, Germany, Department of Physics and Astronomy, University College London, London WC1E 6BT, U.K., Max-Planck-Institut für Kohlenforschung, Kaiser-Wilhelm-Platz 1, D-45470 Mülheim an der Ruhr, Germany, and FBC, Theoretische Chemie, Bergische Universität, D-42097 Wuppertal, Germany
| | - Andrey Yachmenev
- Institut für Physikalische Chemie und Elektrochemie, Technische Universität Dresden, D-01062 Dresden, Germany, Department of Physics and Astronomy, University College London, London WC1E 6BT, U.K., Max-Planck-Institut für Kohlenforschung, Kaiser-Wilhelm-Platz 1, D-45470 Mülheim an der Ruhr, Germany, and FBC, Theoretische Chemie, Bergische Universität, D-42097 Wuppertal, Germany
| | - Walter Thiel
- Institut für Physikalische Chemie und Elektrochemie, Technische Universität Dresden, D-01062 Dresden, Germany, Department of Physics and Astronomy, University College London, London WC1E 6BT, U.K., Max-Planck-Institut für Kohlenforschung, Kaiser-Wilhelm-Platz 1, D-45470 Mülheim an der Ruhr, Germany, and FBC, Theoretische Chemie, Bergische Universität, D-42097 Wuppertal, Germany
| | - Per Jensen
- Institut für Physikalische Chemie und Elektrochemie, Technische Universität Dresden, D-01062 Dresden, Germany, Department of Physics and Astronomy, University College London, London WC1E 6BT, U.K., Max-Planck-Institut für Kohlenforschung, Kaiser-Wilhelm-Platz 1, D-45470 Mülheim an der Ruhr, Germany, and FBC, Theoretische Chemie, Bergische Universität, D-42097 Wuppertal, Germany
| | - Jonathan Tennyson
- Institut für Physikalische Chemie und Elektrochemie, Technische Universität Dresden, D-01062 Dresden, Germany, Department of Physics and Astronomy, University College London, London WC1E 6BT, U.K., Max-Planck-Institut für Kohlenforschung, Kaiser-Wilhelm-Platz 1, D-45470 Mülheim an der Ruhr, Germany, and FBC, Theoretische Chemie, Bergische Universität, D-42097 Wuppertal, Germany
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Orton GS, Fisher BM, Baines KH, Stewart ST, Friedson AJ, Ortiz JL, Marinova M, Ressler M, Dayal A, Hoffmann W, Hora J, Hinkley S, Krishnan V, Masanovic M, Tesic J, Tziolas A, Parija KC. Characteristics of the Galileo probe entry site from Earth-based remote sensing observations. ACTA ACUST UNITED AC 1998. [DOI: 10.1029/98je02380] [Citation(s) in RCA: 75] [Impact Index Per Article: 2.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Spray JG, Kelley SP, Rowley DB. Evidence for a late Triassic multiple impact event on Earth. Nature 1998. [DOI: 10.1038/32397] [Citation(s) in RCA: 79] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Orton G, Ortiz JL, Baines K, Bjoraker G, Carsenty U, Colas F, Dayal A, Deming D, Drossart P, Frappa E, Friedson J, Goguen J, Golisch W, Griep D, Hernandez C, Hoffmann W, Jennings D, Kaminski C, Kuhn J, Laques P, Limaye S, Lin H, Lecacheux J, Martin T, McCabe G, Momary T, Parker D, Puetter R, Ressler M, Reyes G, Sada P, Spencer J, Spitale J, Stewart S, Varsik J, Warell J, Wild W, Yanamandra-Fisher P, Fazio G, Hora J, Deutsch L. Earth-Based Observations of the Galileo Probe Entry Site. Science 1996; 272:839-40. [PMID: 8662571 DOI: 10.1126/science.272.5263.839] [Citation(s) in RCA: 51] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/01/2023]
Abstract
Earth-based observations of Jupiter indicate that the Galileo probe probably entered Jupiter's atmosphere just inside a region that has less cloud cover and drier conditions than more than 99 percent of the rest of the planet. The visual appearance of the clouds at the site was generally dark at longer wavelengths. The tropospheric and stratospheric temperature fields have a strong longitudinal wave structure that is expected to manifest itself in the vertical temperature profile.
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Affiliation(s)
- G Orton
- G. Orton, J. Friedson, T. Martin, P. Yanamandra-Fisher, Mail Stop 169-237, Jet Propulsion Laboratory (JPL), California Institute of Technology, Pasadena, CA 91109; J. L. Ortiz, Mail Stop 169-237, JPL, and Instituto de Astrofisica de Andalucia, CSIC, P.O. Box 3004, 18080 Granada, Spain; K. Baines, Mail Stop 183-601, JPL; G. Bjoraker, D. Deming, D. Jennings, G. McCabe, P. Sada, Code 693, NASA Goddard Space Flight Center, Greenbelt, MD 20771; U. Carsenty, DLR Institute for Planetary Exploration, Rudower Chaussee 5, D-12489 Berlin, Germany; F. Colas, Bureau des Longitudes, 75015 Paris, France; A. Dayal and W. Hoffmann, Stewart Observatory, Univ. of Arizona, Tucson, AZ 85721; P. Drossart and J. Lecacheux, DESPA, Observatoire de Paris-Meudon, 92195 Meudon Cedex, France; E. Frappa and P. Laques, Observatoire Midi-Pyrenees, 65200 Bagneres de Bigorre, France; J. Goguen, Mail Stop 183-501, JPL; W. Golisch, D. Griep, C. Kaminski, J. Hora, Institute for Astronomy, Univ. of Hawaii, Honolulu, HI 96822; C. Hernandez, 9430 S.W. 29 Terrace, Miami, FL 33165; J. Kuhn, H. Lin, J. Varsik, National Solar Observatory, Sunspot, NM 88349; S. Limaye, Space Science and Engineering Center, Univ. of Wisconsin, Madison, WI 53706; T. Momary, 3806 Geology Building, Univ. of California, Los Angeles, CA 90024-1567; D. Parker, 12911 Lerida Street, Coral Gables, FL 33156; R. Puetter, CASS, Univ. of California at San Diego, La Jolla, CA 92093-0111; M. Ressler, Mail Stop 169-506, JPL; G. Reyes, Mail Stop 300-329, JPL; J. Spencer, Lowell Observatory, 1400 Mars Hill Road, Flagstaff, AZ 86001; J. Spitale and S. Stewart, Division of Geological and Planetary Sciences, 170-20, California Institute of Technology, Pasadena, CA 91125; J. Warell, Uppsala Astronomical Observatory, Box 515, S-75120 Uppsala, Sweden; W. Wild, Department of Astronomy and Astrophysics, Univ. of Chicago, Chicago, IL 60637; G. Fazio, Smithsonian Astrophysical Observatory, Cambridge, MA 02138; L. Deutsch, Five College Astronomy Department, Univ. of Massachusetts, Amherst, MA 01003
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Affiliation(s)
- Bernard Vonnegut
- Department of Atmospheric Science, State University of New York, Albany, NY 12222, USA
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West RA, Karkoschka E, Friedson AJ, Seymour M, Baines KH, Hammel HB. Impact debris particles in Jupiter's stratosphere. Science 1995; 267:1296-301. [PMID: 7871426 DOI: 10.1126/science.7871426] [Citation(s) in RCA: 77] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/27/2023]
Abstract
The aftermath of the impacts of periodic comet Shoemaker-Levy 9 on Jupiter was studied with the Wide Field Planetary Camera 2 on the Hubble Space Telescope. The impact debris particles may owe their dark brown color to organic material rich in sulfur and nitrogen. The total volume of aerosol 1 day after the last impact is equal to the volume of a sphere of radius 0.5 kilometer. In the optically thick core regions, the particle mean radius is between 0.15 and 0.3 micrometer, and the aerosol is spread over many scale heights, from approximately 1 millibar to 200 millibars of pressure or more. Particle coagulation can account for the evolution of particle radius and total optical depth during the month following the impacts.
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Affiliation(s)
- R A West
- Earth and Space Sciences Division, California Institute of Technology, Pasadena 91109
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Noll KS, McGrath MA, Trafton LM, Atreya SK, Caldwell JJ, Weaver HA, Yelle RV, Barnet C, Edgington S. HST spectroscopic observations of Jupiter after the collision of comet Shoemaker-Levy 9. Science 1995; 267:1307-13. [PMID: 7871428 DOI: 10.1126/science.7871428] [Citation(s) in RCA: 103] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/27/2023]
Abstract
Ultraviolet spectra obtained with the Hubble Space Telescope identified at least 10 molecules and atoms in the perturbed stratosphere near the G impact site, most never before observed in Jupiter. The large mass of sulfur-containing material, more than 10(14) grams in S2 alone, indicates that many of the sulfur-containing molecules S2, CS2, CS, H2S, and S+ may be derived from a sulfur-bearing parent molecule native to Jupiter. If so, the fragment must have penetrated at least as deep as the predicted NH4SH cloud at a pressure of approximately 1 to 2 bars. Stratospheric NH3 was also observed, which is consistent with fragment penetration below the cloud tops. Approximately 10(7) grams of neutral and ionized metals were observed in emission, including Mg II, Mg I, Si I, Fe I, and Fe II. Oxygen-containing molecules were conspicuous by their absence; upper limits for SO2, SO, CO, SiO, and H2O are derived.
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Affiliation(s)
- K S Noll
- Space Telescope Science Institute, Baltimore, MD 21218
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