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1. A Distribution of Large Particles in the Coma of Comet 103P/Hartley 2

Author

Kelley, Michael S., Lindler, Don J., Bodewits, Dennis, A'Hearn, Michael F., Lisse, Carey M., Kolokolova, Ludmilla, Kissel, Jochen, and Hermalyn, Brendan

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The coma of comet 103P/Hartley 2 has a significant population of large particles observed as point sources in images taken by the Deep Impact spacecraft. We measure their spatial and flux distributions, and attempt to constrain their composition. The flux distribution of these particles implies a very steep size distribution with power-law slopes ranging from -6.6 to -4.7. The radii of the particles extend up to 20 cm, and perhaps up to 2 m, but their exact sizes depend on their unknown light scattering properties. We consider two cases: bright icy material, and dark dusty material. The icy case better describes the particles if water sublimation from the particles causes a significant rocket force, which we propose as the best method to account for the observed spatial distribution. Solar radiation is a plausible alternative, but only if the particles are very low density aggregates. If we treat the particles as mini-nuclei, we estimate they account for <16-80% of the comet's total water production rate (within 20.6 km). Dark dusty particles, however, are not favored based on mass arguments. The water production rate from bright icy particles is constrained with an upper limit of 0.1 to 0.5% of the total water production rate of the comet. If indeed icy with a high albedo, these particles do not appear to account for the comet's large water production rate. production rate. Erratum: We have corrected the radii and masses of the large particles of comet 103P/Hartley 2 and present revised conclusions in the attached erratum., Comment: Original article: 46 pages, 17 figures, 5 tables, published in Icarus. Erratum: 5 pages, 1 table, accepted for publication in Icarus

Published
2013
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2. Techniques for Galactic Dust Measurements in the Heliosphere

Author

Grün, Eberhard, Landgraf, Markus, Horány, Mihaly, Kissel, Jochen, Krüger, Harald, Srama, Ralf, Svedhem, Håkan, and Withnell, Peter

Subjects
Astrophysics
Abstract

Galactic interstellar dust (ISD) is the major ingredient in planetary formation. However, information on this important material has been extremely limited. Recently the Ulysses dust detector has identified and measured interstellar dust outside 1.8~AU from the Sun at ecliptic latitudes above $50^{\circ}$. Inside this distance it could not reliably distinguish interstellar from interplanetary dust. Modeling the Ulysses data suggests that up to 30 % of dust flux with masses above $10^{-16}\rm kg$ at 1~AU is of interstellar origin. From the Hiten satellite in high eccentric orbit about the Earth there are indications that ISD indeed reaches the Earth's orbit. Two new missions carrying dust detectors, Cassini and Stardust, will greatly increase our observational knowledge. In this paper we briefly review instruments used on these missions and compare their capabilities. The Stardust mission [{\em Brownlee et al.}, 1996] will analyze the local interstellar dust population by an in-situ chemical analyzer and collect ISD between 2 and 3~AU from the Sun. The dust analyzer on the Cassini mission will determine the interstellar dust flux outside Venus' orbit and will provide also some compositional information. Techniques to identify the ISD flux levels at 1~AU are described that can quantify the interstellar dust flux in high-Earth orbit (outside the debris belts) and provide chemical composition information of galactic dust., Comment: Accepted for Journal of Geophysical Research, 6 figures, Latex

Published
1999
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4. EPOXI at Comet Hartley 2

Author

A'Hearn, Michael F., Belton, Michael J. S., Delamere, W. Alan, Feaga, Lori M., Hampton, Donald, Kissel, Jochen, Klaasen, Kenneth P., McFadden, Lucy A., Meech, Karen J., Melosh, H. Jay, Schultz, Peter H., Sunshine, Jessica M., Thomas, Peter C., Veverka, Joseph, Wellnitz, Dennis D., Yeomans, Donald K., Besse, Sebastien, Bodewits, Dennis, Bowling, Timothy J., Carcich, Brian T., Collins, Steven M., Farnham, Tony L., Groussin, Olivier, Hermalyn, Brendan, Kelley, Michael S., Li, Jian-Yang, Lindler, Don J., Lisse, Carey M., McLaughlin, Stephanie A., Merlin, Frédéric, Protopapa, Silvia, Richardson, James E., and Williams, Jade L.

Published
2011
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5. Impact Features on Stardust: Implications for Comet 81p/Wild 2 Dust

Author

Hörz, Friedrich, Bastien, Ron, Borg, Janet, Bradley, John P., Bridges, John C., Brownlee, Donald E., Burchell, Mark J., Chi, Miaofang, Cintala, Mark J., Dai, Zu Rong, Djouadi, Zahia, Dominguez, Gerardo, Economou, Thanasis E., Fairey, Sam A. J., Floss, Christine, Franchi, Ian A., Graham, Giles A., Green, Simon F., Heck, Philipp, Hoppe, Peter, Huth, Joachim, Ishii, Hope, Kearsley, Anton T., Kissel, Jochen, Leitner, Jan, Leroux, Hugues, Marhas, Kuljeet, Messenger, Keiko, Schwandt, Craig S., See, Thomas H., Snead, Christopher, Stadermann, Frank J., Stephan, Thomas, Stroud, Rhonda, Teslich, Nick, Trigo-Rodríguez, Josep M., Tuzzolino, A. J., Troadec, David, Tsou, Peter, Warren, Jack, Westphal, Andrew, Wozniakiewicz, Penelope, Wright, Ian, and Zinner, Ernst

Published
2006
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6. Comet 81p/Wild 2 under a Microscope

Author

Brownlee, Don, Tsou, Peter, Aléon, Jérôme, Alexander, Conel M. O'D., Araki, Tohru, Bajt, Sasa, Baratta, Giuseppe A., Bastien, Ron, Bland, Phil, Bleuet, Pierre, Borg, Janet, Bradley, John P., Brearley, Adrian, Brenker, F., Brennan, Sean, Bridges, John C., Browning, Nigel D., Brucato, John R., Bullock, E., Burchell, Mark J., Busemann, Henner, Butterworth, Anna, Chaussidon, Marc, Cheuvront, Allan, Chi, Miaofang, Cintala, Mark J., Clark, B. C., Clemett, Simon J., Cody, George, Colangeli, Luigi, Cooper, George, Cordier, Patrick, Daghlian, C., Dai, Zurong, D'Hendecourt, Louis, Djouadi, Zahia, Dominguez, Gerardo, Duxbury, Tom, Dworkin, Jason P., Ebel, Denton S., Economou, Thanasis E., Fakra, Sirine, Fairey, Sam A. J., Fallon, Stewart, Ferrini, Gianluca, Ferroir, T., Fleckenstein, Holger, Floss, Christine, Flynn, George, Franchi, Ian A., Fries, Marc, Gainsforth, Z., Gallien, J.-P., Genge, Matt, Gilles, Mary K., Gillet, Philipe, Gilmour, Jamie, Glavin, Daniel P., Gounelle, Matthieu, Grady, Monica M., Graham, Giles A., Grant, P. G., Green, Simon F., Grossemy, Faustine, Grossman, Lawrence, Grossman, Jeffrey N., Guan, Yunbin, Hagiya, Kenji, Harvey, Ralph, Heck, Philipp, Herzog, Gregory F., Hoppe, Peter, Hörz, Friedrich, Huth, Joachim, Hutcheon, Ian D., Ignatyev, Konstantin, Ishii, Hope, Ito, Motoo, Jacob, Damien, Jacobsen, Chris, Jacobsen, Stein, Jones, Steven, Joswiak, David, Jurewicz, Amy, Kearsley, Anton T., Keller, Lindsay P., Khodja, H., Kilcoyne, A. L. David, Kissel, Jochen, Krot, Alexander, Langenhorst, Falko, Lanzirotti, Antonio, Le, Loan, Leshin, Laurie A., Leitner, J., Lemelle, L., Leroux, Hugues, Liu, Ming-Chang, Leuning, K., Lyon, Ian, MacPherson, Glen, Marcus, Matthew A., Marhas, Kuljeet, Marty, Bernard, Matrajt, Graciela, McKeegan, Kevin, Meibom, Anders, Mennella, Vito, Messenger, Keiko, Messenger, Scott, Mikouchi, Takeshi, Mostefaoui, Smail, Nakamura, Tomoki, Nakano, T., Newville, M., Nittler, Larry R., Ohnishi, Ichiro, Ohsumi, Kazumasa, Okudaira, Kyoko, Papanastassiou, Dimitri A., Palma, Russ, Palumbo, Maria E., Pepin, Robert O., Perkins, David, Perronnet, Murielle, Pianetta, P., Rao, William, Rietmeijer, Frans J. M., Robert, François, Rost, D., Rotundi, Alessandra, Ryan, Robert, Sandford, Scott A., Schwandt, Craig S., See, Thomas H., Schlutter, Dennis, Sheffield-Parker, J., Simionovici, Alexandre, Simon, Steven, Sitnitsky, I., Snead, Christopher J., Spencer, Maegan K., Stadermann, Frank J., Steele, Andrew, Stephan, Thomas, Stroud, Rhonda, Susini, Jean, Sutton, S. R., Suzuki, Y., Taheri, Mitra, Taylor, Susan, Teslich, Nick, Tomeoka, Kazu, Tomioka, Naotaka, Toppani, Alice, Trigo-Rodríguez, Josep M., Troadec, David, Tsuchiyama, Akira, Tuzzolino, Anthony J., Tyliszczak, Tolek, Uesugi, K., Velbel, Michael, Vellenga, Joe, Vicenzi, E., Vincze, L., Warren, Jack, Weber, Iris, Weisberg, Mike, Westphal, Andrew J., Wirick, Sue, Wooden, Diane, Wopenka, Brigitte, Wozniakiewicz, Penelope, Wright, Ian, Yabuta, Hikaru, Yano, Hajime, Young, Edward D., Zare, Richard N., Zega, Thomas, Ziegler, Karen, Zimmerman, Laurent, Zinner, Ernst, and Zolensky, Michael

Published
2006
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7. Comet 67P/Churyumov-Gerasimenko sheds dust coat accumulated over the past four years

Author

Schulz, Rita, Hilchenbach, Martin, Langevin, Yves, Kissel, Jochen, Silen, Johan, Briois, Christelle, Engrand, Cecile, Hornung, Klaus, Baklouti, Donia, Bardyn, Anaïs, Cottin, Hervé, Fischer, Henning, Fray, Nicolas, Godard, Marie, Lehto, Harry, Le Roy, Léna, Merouane, Sihane, Orthous-Daunay, François-Régis, Paquette, John, Rynö, Jouni, Siljeström, Sandra, Stenzel, Oliver, Thirkell, Laurent, Varmuza, Kurt, and Zaprudin, Boris

Published
2015
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8. Surface of young Jupiter family Comet 81 P/Wild 2: view from the Stardust spacecraft

Author

Brownlee, Donald E., Horz, Friedrich, Newburn, Ray L., Zolensky, Michael, Duxbury, Thomas C., Sandford, Scott, Sekanina, Zdenek, Tsou, Peter, Hanner, Martha S., Clark, Benton C., Green, Simon F., and Kissel, Jochen

Subjects
Stardust (Space probe) -- Equipment and supplies, Comets -- Research -- Measurement -- Properties -- Equipment and supplies, Science and technology, Research, Measurement, Properties, Equipment and supplies
Abstract

Images taken by the Stardust mission during its flyby of 81P/Wild 2 show the comet to be a 5-kilometer oblate body covered with remarkable topographic features, including unusual circular features that appear to be impact craters. The presence of high-angle slopes shows that the surface is cohesive and self-supporting. The comet does not appear to be a rubble pile, and its rounded shape is not directly consistent with the comet being a fragment of a larger body. The surface is active and yet it retains ancient terrain. Wild 2 appears to be in the early stages of its degradation phase as a small volatile-rich body in the inner solar system., Jupiter family comets (JFCs) such as 81 P/Wild 2 typically range from the orbit of Jupiter to inner regions of the solar system. These subliming-disintegrating bodies have inner solar system [...]

Published
2004

9. Shape, Density, and Geology of the Nucleus of Comet 103P/Hartley 2

Author

Thomas, P.C, A'hearn, Michael F, Veverka, Joseph, Belton, Michael J. S, Kissel, Jochen, Klaasen, Kenneth P, McFadden, Lucy A, Melosh, H. Jay, Schultz, Peter H, Besse, Sebastien, Carcich, Brian T, Farnham, Tony L, Groussin, Olivier, Hermalyn, Brendan, Li, Jian-Yang, Lindler, Don J, Lisse, Carey M, Meech, Karen, and Richardson, James E

Subjects
Lunar And Planetary Science And Exploration
Abstract

Data from the Extrasolar Planet Observation and Deep Impact Extended Investigation (EPOXI) mission show Comet 103P/Hartley 2 is a bi-lobed, elongated, nearly axially symmetric comet 2.33 km in length. Surface features are primarily small mounds <40 m across, irregularly-shaped smooth areas on the two lobes, and a smooth but variegated region forming a “waist” between the two lobes. Assuming parts of the comet body approach the shape of an equipotential surface, the mean density of Hartley 2 is modeled to be 200–400 kg /cubic m.. Such a mean density suggests mass loss per orbit of >1%. The shape may be the evolutionary product of insolation, sublimation, and temporary deposition of materials controlled by the object’s complex rotation.

Published
2013
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10. EPOXI at Comet Hartley 2

Author

AʼHearn, Michael F., Belton, Michael J.S., Delamere, W. Alan, Feaga, Lori M., Hampton, Donald, Kissel, Jochen, Klaasen, Kenneth P., McFadden, Lucy A., Meech, Karen J., Melosh, H. Jay, Schultz, Peter H., Sunshine, Jessica M., Thomas, Peter C., Veverka, Joseph, Wellnitz, Dennis D., Yeomans, Donald K., Besse, Sebastien, Bodewits, Dennis, Bowling, Timothy J., Carcich, Brian T., Collins, Steven M., Farnham, Tony L., Groussin, Olivier, Hermalyn, Brendan, Kelley, Michael S., Li, Jian-Yang, Lindler, Don J., Lisse, Carey M., McLaughlin, Stephanie A., Merlin, Frédéric, Protopapa, Silvia, Richardson, James E., and Williams, Jade L.

Published
2011
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11. Cometary Volatiles and the Origin of Comets

Author

A'Hearn, Michael F, Feaga, Lori M, Keller, H. Uwe, Kawakita, Hideyo, Hampton, Donald L, Kissel, Jochen, Klaasen, Kenneth P, McFadden, Lucy A, Meech, Karen J, Schultz, Peter H, Sunshine, Jessica M, Thomas, Peter C, Veverka, Joseph, Yeomans, Donald K, Besse, Sebastien, Bodewits, Dennis, Farnham, Tony L, Groussin, Olivier, Kelley, Michael S, Lisse, Carey M, Merlin, Frederic, Protopapa, Silvia, and Wellnitz, Dennis D

Subjects
Lunar And Planetary Science And Exploration
Abstract

We describe recent results on the CO/C02/H2O composition of comets and compare these with models of the protoplanetary disk. We argue that the cometary observations require reactions on grain surfaces to convert CO to CO2 and also require formation between the CO and CO2 snow lines. This then requires very early mixing of cometesimals in the protoplanetary disk analogous to the mixing described for the asteroid belt by Walsh and Morbidelli. We suggest that most comets formed in the region of the giant planets. the traditional source of the Oort-cloud comets but not of the Jupiter-family comets

Published
2012

12. EPOXI at Comet Hartley 2

Author

A'Hearn, Michael F, Belton, Michael J. S, Delamere, W. Alan, Feaga, Lori M, Hampton, Donald, Kissel, Jochen, Klaasen, Kenneth P, McFadden, Jessica M, Meech, Karen J, Melosh, H. Jay, Schultz, Peter H, Sunshine, Jessica M, Thomas, Peter C, Veverka, Joseph, Wellnitz, Dennis D, Yeomans, Donald K, Besse, Sebastien, Bodewits, Dennis, Bowling, Timothy J, Carcish, Brian T, Collins, Steven M, Farnham, Tony F, Groussin, Oliver, Hermalyn, Brendan, and Kelley, Michael S

Subjects
Astronomy
Abstract

Understanding how comets work, i,e., what drives their activity, is crucial to using comets to study the early solar system. EPOXI flew past comet 103P/Hartley 2, one with an unusually small but very active nucleus. taking both images and spectra. Unlike large, relatively inactive nuclei, this nncleus is outgassing primarily due to CO2, which drags chnnks of ice out of the nnclens. It also shows significant differences in the relative abundance of volatiles from various parts of the nucleus.

Published
2011

13. High-molecular-weight organic matter in the particles of comet 67P/ChuryumovGerasimenko

Author

Fray, Nicolas, Bardyn, Anas, Cottin, Herv, Altwegg, Kathrin, Baklouti, Donia, Briois, Christelle, Colangeli, Luigi, Engrand, Ccile, Fischer, Henning, Glasmachers, Albrecht, Grn, Eberhard, Haerendel, Gerhard, Henkel, Hartmut, Hfner, Herwig, Hornung, Klaus, Jessberger, Elmar K., Koch, Andreas, Krger, Harald, Langevin, Yves, Lehto, Harry, Lehto, Kirsi, Le Roy, Lna, Merouane, Sihane, Modica, Paola, Orthous-Daunay, Franois-Rgis, Paquette, John, Raulin, Franois, Ryn, Jouni, Schulz, Rita, Siln, Johan, Siljestrm, Sandra, Steiger, Wolfgang, Stenzel, Oliver, Stephan, Thomas, Thirkell, Laurent, Thomas, Roger, Torkar, Klaus, Varmuza, Kurt, Wanczek, Karl-Peter, Zaprudin, Boris, Kissel, Jochen, and Hilchenbach, Martin

Subjects
Research, Properties, Natural history, Organic compounds -- Properties -- Natural history, Cosmochemistry -- Research, Chemical research, Molecular weights -- Research, Comets -- Properties -- Natural history
Abstract

Author(s): Nicolas Fray (corresponding author) [1]; Anas Bardyn [1, 2]; Herv Cottin [1]; Kathrin Altwegg [3]; Donia Baklouti [4]; Christelle Briois [2]; Luigi Colangeli [5]; Ccile Engrand [6]; Henning Fischer [...]

Published
2016
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14. Ulysses Dust Measurements Near Jupiter

Author

Grün, Eberhard, Zook, Herbert A., Baguhl, Michael, Fechtig, Hugo, Hanner, Martha S., Kissel, Jochen, Lindblad, Bertil A., Linkert, Dietmar, Linkert, Gudrun, Mann, Ingrid B., Morfill, Gregor E., Polanskey, Carol, Riemann, Reiner, Schwehm, Gerhard, and Siddique, Nadeem

Published
1992

15. Ulysses dust measurements near Jupiter

Author

Gruen, Eberhard, Zook, Herbert A, Baguhl, Michael, Fechtig, Hugo, Hanner, Martha S, Kissel, Jochen, Lindblad, Bertil A, Linkert, Dietmar, Linkert, Gudrun, and Mann, Ingrid B

Subjects
Lunar And Planetary Exploration
Abstract

Submicrometer- to micrometer-sized particles were recorded by the Ulysses dust detector within 40 days of the Jupiter flyby. Nine impacts were recorded within 50 Jupiter radii with most of them recorded after closest approach. Three of these impacts are consistent with particles on prograde orbits around Jupiter and the rest are believed to have resulted from gravitationally focused interplanetary dust. From the ratio of the impact rate before the Jupiter flyby to the impact rate after the Jupiter flyby it is concluded that interplanetary dust particles at the distance of Jupiter move on mostly retrograde orbits. On 10 March 1992, Ulysses passed through an intense dust stream. The dust detector recorded 126 impacts within 26 hours. The stream particles were moving on highly inclined and apparently hyperbolic orbits with perihelion distances of greater than 5 astronomical units. Interplanetary dust is lost rather quickly from the solar system through collisions and other mechanisms and must be almost continuously replenished to maintain observed abundances. Dust flux measurements, therefore, give evidence of the recent rates of production from sources such as comets, asteroids, and moons, as well as the possible presence of interstellar grains.

Published
1992

16. The Galileo Dust Detector

Author

Gruen, Eberhard, Fechtig, Hugo, Hanner, Martha S, Kissel, Jochen, Lindblad, Bertil-Anders, Linkert, Dietmar, Maas, Dieter, Morfill, Gregor E, and Zook, Herbert A

Subjects
Spacecraft Instrumentation
Abstract

The Galileo Dust Detector is intended to provide direct observations of dust grains with masses between 10 exp -19 and 10 exp -9 kg in interplanetary space and in the Jovian system, to investigate their physical and dynamical properties as functions of the distances to the sun, to Jupiter and to its satellites, and to study its interaction with the Galilean satellites and the Jovian magnetosphere. The investigation is performed with an instrument that measures the mass, speed, flight direction and electric charge of individual dust particles. It is a multicoincidence detector with a mass sensitivity 1 000 000 times higher than that of previous in situ experiments which measured dust in the outer solar system. The instrument weighs 4.2 kg, consumes 2.4 W, and has a normal data transmission rate of 24 bits/s in nominal spacecraft tracking mode. On December 29, 1989 the instrument was switched-on. After the instrument had been configured to flight conditions cruise science data collection started immediately. In the period to May 18, 1990 at least 168 dust impacts have been recorded. For 81 of these dust grains masses and impact speeds have been determined. First flux values are given.

Published
1992

17. Searching for calcium-aluminum-rich inclusions in cometary particles with Rosetta/COSIMA

Author

Paquette, John, ENGRAND, CECILE, Stenzel, Oliver, Hilchenbach, Martin, Kissel, Jochen, Cosima Team, The, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM AS), Université Paris-Saclay-Univ. Paris-Sud-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), COSIMA was built by a consortium led by the Max-Planck-Institut f € ur Extraterrestrische Physik, Garching, Germany in collaboration with Laboratoire de Physique et Chimie de l’Environnement et 8 de l’Espace, Orl eans, France, Institut d’Astrophysique Spatiale, CNRS/Universit e Paris Sud, Orsay, France, Finnish Meteorological Institute, Helsinki, Finland, Universit € at Wuppertal, Wuppertal, Germany, von Hoerner und Sulger GmbH, Schwetzingen, Germany, Universit € at der Bundeswehr, Neubiberg, Germany, Institut f € ur Physik, Forschungszentrum Seibersdorf, Seibersdorf, Austria, Institut f € ur Weltraumforschung, € Osterreichische Akademie der Wissenschaften, Graz,Austria, and and is led by the Max-Planck-Institut f € ur Sonnensystemforschung, G € ottingen, Germany

Subjects
Physics, Nebula, Solar System, ta115, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Comet, Astronomical unit, Astrophysics, 010502 geochemistry & geophysics, 01 natural sciences, Astrobiology, Secondary ion mass spectrometry, Geophysics, 13. Climate action, Space and Planetary Science, Chondrite, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Particle, Formation and evolution of the Solar System, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

International audience; The calcium-aluminum-rich inclusions (CAIs) found in chondritic meteorites are probably the oldest solar system solids, dating back to 4567.30 ± 0.16 million years ago. They are thought to have formed in the protosolar nebula within a few astronomical units of the Sun, and at a temperature of around 1300 K. The Stardust mission found evidence of CAI-like material in samples recovered from comet Wild 2. The appearance of CAIs in comets, which are thought to be formed at lower temperatures and larger distances from the Sun, is only explicable if some mechanism allows the efficient transfer of such objects from the inner solar nebula to the outer solar nebula. Such mechanisms have been proposed such as an X-wind or turbulence. In this work, particles collected from within the coma of comet 67P/Churyumov–Gerasimenko are examined for compositional evidence of the presence of CAIs. COSIMA (the Cometary Secondary Ion Mass Analyzer) uses secondary ion mass spectrometry to analyze the composition of cometary dust captured on metal targets. While CAIs can have a radius of centimeters, they are more typically a few hundred microns in size, and can be smaller than 1 μm, so it is conceivable that particles visible on COSIMA targets (ranging in size from about 10 μm to hundreds of microns) could contain CAIs. Using a peak fitting technique, the composition of a set of 13 particles was studied, looking for material rich in both calcium and aluminum. One such particle was found.

Published
2016
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18. Evolution of the physical properties of dust and cometary dust activity from 67P/Churyumov–Gerasimenko measured in situ by Rosetta/COSIMA

Author

Merouane, Sihane, primary, Stenzel, Oliver, additional, Hilchenbach, Martin, additional, Schulz, Rita, additional, Altobelli, Nicolas, additional, Fischer, Henning, additional, Hornung, Klaus, additional, Kissel, Jochen, additional, Langevin, Yves, additional, Mellado, Eva, additional, Rynö, Jouni, additional, and Zaprudin, Boris, additional

Published
2017
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19. Carbon-rich dust in comet 67P/Churyumov-Gerasimenko measured by COSIMA/Rosetta

Author

Bardyn, Anaïs, primary, Baklouti, Donia, additional, Cottin, Hervé, additional, Fray, Nicolas, additional, Briois, Christelle, additional, Paquette, John, additional, Stenzel, Oliver, additional, Engrand, Cécile, additional, Fischer, Henning, additional, Hornung, Klaus, additional, Isnard, Robin, additional, Langevin, Yves, additional, Lehto, Harry, additional, Le Roy, Léna, additional, Ligier, Nicolas, additional, Merouane, Sihane, additional, Modica, Paola, additional, Orthous-Daunay, François-Régis, additional, Rynö, Jouni, additional, Schulz, Rita, additional, Silén, Johan, additional, Thirkell, Laurent, additional, Varmuza, Kurt, additional, Zaprudin, Boris, additional, Kissel, Jochen, additional, and Hilchenbach, Martin, additional

Published
2017
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20. Nitrogen-to-carbon atomic ratio measured by COSIMA in the particles of comet 67P/Churyumov–Gerasimenko

Author

Fray, Nicolas, primary, Bardyn, Anaïs, additional, Cottin, Hervé, additional, Baklouti, Donia, additional, Briois, Christelle, additional, Engrand, Cécile, additional, Fischer, Henning, additional, Hornung, Klaus, additional, Isnard, Robin, additional, Langevin, Yves, additional, Lehto, Harry, additional, Le Roy, Léna, additional, Mellado, Eva Maria, additional, Merouane, Sihane, additional, Modica, Paola, additional, Orthous-Daunay, François-Régis, additional, Paquette, John, additional, Rynö, Jouni, additional, Schulz, Rita, additional, Silén, Johan, additional, Siljeström, Sandra, additional, Stenzel, Oliver, additional, Thirkell, Laurent, additional, Varmuza, Kurt, additional, Zaprudin, Boris, additional, Kissel, Jochen, additional, and Hilchenbach, Martin, additional

Published
2017
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23. Comet 81P/Wild 2 Under a Microscope

Author

Brownlee, Don, Tsou, Peter, Aleon, Jerome, Alexander, Conel M. O'D., Araki, Tohru, Bajt, Sasa, Baratta, Giuseppe A., Bastien, Ron, Bland, Phil, Bleuet, Pierre, Borg, Janet, Bradley, John P., Brearley, Adrian, Brenker, F., Brennan, Sean, Bridges, John C., Browning, Nigel D., Brucato, John R., Bullock, E., Burchell, Mark J., Busemann, Henner, Butterworth, Anna, Chaussidon, Marc, Cheuvront, Allan, Chi, Miaofang, Cintala, Mark J., Clark, B. C., Clemett, Simon J., Cody, George, Colangeli, Luigi, Cooper, George, Cordier, Patrick, Daghlian, C., Dai, Zurong, D'Hendecourt, Louis, Djouadi, Zahia, Dominguez, Gerardo, Duxbury, Tom, Dworkin, Jason P., Ebel, Denton S., Economou, Thanasis E., Fakra, Sirine, Fairey, Sam A. J., Fallon, Stewart, Ferrini, Gianluca, Ferroir, T., Fleckenstein, Holger, Floss, Christine, Flynn, George, Franchi, Ian A., Fries, Marc, Gainsforth, Z., Gallien, J.-P., Genge, Matt, Gilles, Mary K., Gillet, Philipe, Gilmour, Jamie, Glavin, Daniel P., Gounelle, Matthieu, Grady, Monica M., Graham, Giles A., Grant, P. G., Green, Simon F., Grossemy, Faustine, Grossman, Lawrence, Grossman, Jeffrey N., Guan, Yunbin, Hagiya, Kenji, Harvey, Ralph, Heck, Philipp, Herzog, Gregory F., Hoppe, Peter, Horz, Friedrich, Huth, Joachim, Hutcheon, Ian D., Ignatyev, Konstantin, Ishii, Hope, Ito, Motoo, Jacob, Damien, Jacobsen, Chris, Jacobsen, Stein, Jones, Steven, Joswiak, David, Jurewicz, Amy, Kearsley, Anton T., Keller, Lindsay P., Khodja, H., Kilcoyne, A. L. David, Kissel, Jochen, Krot, Alexander, Langenhorst, Falko, Lanzirotti, Antonio, Le, Loan, Leshin, Laurie A., Leitner, J., Lemelle, L., Leroux, Hugues, Liu, Ming-Chang, Luening, K., Lyon, Ian, MacPherson, Glen, Marcus, Matthew A., Marhas, Kuljeet, Marty, Bernard, Matrajt, Graciela, McKeegan, Kevin, Meibom, Anders, Mennella, Vito, Messenger, Keiko, Messenger, Scott, Mikouchi, Takashi, Mostefaoui, Smail, Nakamura, Tomoki, Nakano, T., Newville, M., ittler, Larry R., Ohnishi, Ichiro, Ohsumi, Kazumasa, 奥平, 恭子, Papanastassiou, Dimitri A., Palma, Russ, Palumbo, Maria E., Pepin, Robert O., Perkins, David, Perronnet, Murielle, Pianetta, P., Rao, William, Rietmeijer, Frans J. M., Robert, Francois, Rost, D., Rotundi, Alessandra, Ryan, Robert, Sandford, Scott A., Schwandt, Craig S., See, Thomas H., Schlutter, Dennis, Sheffield-Parker, J., Simionovici, Alexandre, Simon, Steven, Sitnitsky, I., Snead, Christopher J., Spencer, Maegan K., Stadermann, Frank J., Steele, Andrew, Stephan, Thomas, Stroud, Rhonda, Susini, Jean, Sutton, S. R., Suzuki, Y., Taheri, Mitra, Taylor, Susan, Teslich, Nick, Tomeoka, Kazu, Tomioka, Naotaka, Toppani, Alice, Trigo-Rodriguez, Josep M., Troadec, David, Tsuchiyama, Akira, Tuzzolino, Anthony J., Tyliszczak, Tolek, Uesugi, K., Velbel, Michael, Vellenga, Joe, Vicenzi, E., Vincze, L., Warren, Jack, Weber, Iris, Weisberg, Mike, Westphal, Andrew J., Wirick, Sue, Wooden, Diane, Wopenka, Brigitte, Wozniakiewicz, Penelope, Wright, Ian, Yabuta, Hikaru, 矢野, 創, Young, Edward D., Zare, Richard N., Zega, Thomas, Ziegler, Karen, Zimmerman, Laurent, Zinner, Ernst, Zolensky, Michael, Okudaira, Kyoko, Yano, Hajime, Brownlee, Don, Tsou, Peter, Aleon, Jerome, Alexander, Conel M. O'D., Araki, Tohru, Bajt, Sasa, Baratta, Giuseppe A., Bastien, Ron, Bland, Phil, Bleuet, Pierre, Borg, Janet, Bradley, John P., Brearley, Adrian, Brenker, F., Brennan, Sean, Bridges, John C., Browning, Nigel D., Brucato, John R., Bullock, E., Burchell, Mark J., Busemann, Henner, Butterworth, Anna, Chaussidon, Marc, Cheuvront, Allan, Chi, Miaofang, Cintala, Mark J., Clark, B. C., Clemett, Simon J., Cody, George, Colangeli, Luigi, Cooper, George, Cordier, Patrick, Daghlian, C., Dai, Zurong, D'Hendecourt, Louis, Djouadi, Zahia, Dominguez, Gerardo, Duxbury, Tom, Dworkin, Jason P., Ebel, Denton S., Economou, Thanasis E., Fakra, Sirine, Fairey, Sam A. J., Fallon, Stewart, Ferrini, Gianluca, Ferroir, T., Fleckenstein, Holger, Floss, Christine, Flynn, George, Franchi, Ian A., Fries, Marc, Gainsforth, Z., Gallien, J.-P., Genge, Matt, Gilles, Mary K., Gillet, Philipe, Gilmour, Jamie, Glavin, Daniel P., Gounelle, Matthieu, Grady, Monica M., Graham, Giles A., Grant, P. G., Green, Simon F., Grossemy, Faustine, Grossman, Lawrence, Grossman, Jeffrey N., Guan, Yunbin, Hagiya, Kenji, Harvey, Ralph, Heck, Philipp, Herzog, Gregory F., Hoppe, Peter, Horz, Friedrich, Huth, Joachim, Hutcheon, Ian D., Ignatyev, Konstantin, Ishii, Hope, Ito, Motoo, Jacob, Damien, Jacobsen, Chris, Jacobsen, Stein, Jones, Steven, Joswiak, David, Jurewicz, Amy, Kearsley, Anton T., Keller, Lindsay P., Khodja, H., Kilcoyne, A. L. David, Kissel, Jochen, Krot, Alexander, Langenhorst, Falko, Lanzirotti, Antonio, Le, Loan, Leshin, Laurie A., Leitner, J., Lemelle, L., Leroux, Hugues, Liu, Ming-Chang, Luening, K., Lyon, Ian, MacPherson, Glen, Marcus, Matthew A., Marhas, Kuljeet, Marty, Bernard, Matrajt, Graciela, McKeegan, Kevin, Meibom, Anders, Mennella, Vito, Messenger, Keiko, Messenger, Scott, Mikouchi, Takashi, Mostefaoui, Smail, Nakamura, Tomoki, Nakano, T., Newville, M., ittler, Larry R., Ohnishi, Ichiro, Ohsumi, Kazumasa, 奥平, 恭子, Papanastassiou, Dimitri A., Palma, Russ, Palumbo, Maria E., Pepin, Robert O., Perkins, David, Perronnet, Murielle, Pianetta, P., Rao, William, Rietmeijer, Frans J. M., Robert, Francois, Rost, D., Rotundi, Alessandra, Ryan, Robert, Sandford, Scott A., Schwandt, Craig S., See, Thomas H., Schlutter, Dennis, Sheffield-Parker, J., Simionovici, Alexandre, Simon, Steven, Sitnitsky, I., Snead, Christopher J., Spencer, Maegan K., Stadermann, Frank J., Steele, Andrew, Stephan, Thomas, Stroud, Rhonda, Susini, Jean, Sutton, S. R., Suzuki, Y., Taheri, Mitra, Taylor, Susan, Teslich, Nick, Tomeoka, Kazu, Tomioka, Naotaka, Toppani, Alice, Trigo-Rodriguez, Josep M., Troadec, David, Tsuchiyama, Akira, Tuzzolino, Anthony J., Tyliszczak, Tolek, Uesugi, K., Velbel, Michael, Vellenga, Joe, Vicenzi, E., Vincze, L., Warren, Jack, Weber, Iris, Weisberg, Mike, Westphal, Andrew J., Wirick, Sue, Wooden, Diane, Wopenka, Brigitte, Wozniakiewicz, Penelope, Wright, Ian, Yabuta, Hikaru, 矢野, 創, Young, Edward D., Zare, Richard N., Zega, Thomas, Ziegler, Karen, Zimmerman, Laurent, Zinner, Ernst, Zolensky, Michael, Okudaira, Kyoko, and Yano, Hajime

Abstract

著者人数: 183名

Published
2015

24. Aspects of the major element composition of Halley's dust

Author

Jessberger, Elmar K., Christoforidis, Alexander, and Kissel, Jochen

Subjects
Halley's comet -- Composition, Astronomical research -- Analysis, Comets -- Research, Cosmic dust -- Research, Environmental issues, Science and technology, Zoology and wildlife conservation
Published
1988

25. SARIM PLUS—sample return of comet 67P/CG and of interstellar matter

Author

Srama, Ralf, Krüger, Harald, Yamaguchi, T., Stephan, Thomas, Burchell, Mark J., Kearsley, Anton T., Sterken, V., Postberg, Frank, Kempf, Sascha, Grün, Eberhard, Altobelli, Nicolas, Ehrenfreund, Pascale, Dikarev, V., Horanyi, Mihaly, Sternovsky, Zoltan, Carpenter, James D., Westphal, Andrew J., Gainsforth, Zack, Krabbe, A., Agarwal, J., Yano, Hajime, Blum, J., Henkel, Hartmut, Hillier, Jon K., Hoppe, Peter, Trieloff, Mario, Hsu, S., Mocker, A., Fiege, K., Green, Simon F., Bischoff, A., Esposito, Francesca, Laufer, Rene, Hyde, T. W., Herdrich, G., Fasoulas, S., Jäckel, Annette, Jones, G., Jenniskens, P., Khalisi, E., Moragas-Klostermeyer, Georg, Spahn, F., Keller, H.U., Frisch, P., Levasseur-Regourd, A.C., Pailer, Norbert, Altwegg, Kathrin, Engrand, C., Auer, Siegfried, Silen, J., Sasaki, S., Kobayashi, M., Schmidt, Jürgen M., Kissel, Jochen, Marty, Bernard, Michell, Paul C.N., Palumbo, Pasquale, Vaisberg, O., Baggaley, Jack, Rotundi, Alessandra, Röser, Hans-Peter, Srama, Ralf, Krüger, Harald, Yamaguchi, T., Stephan, Thomas, Burchell, Mark J., Kearsley, Anton T., Sterken, V., Postberg, Frank, Kempf, Sascha, Grün, Eberhard, Altobelli, Nicolas, Ehrenfreund, Pascale, Dikarev, V., Horanyi, Mihaly, Sternovsky, Zoltan, Carpenter, James D., Westphal, Andrew J., Gainsforth, Zack, Krabbe, A., Agarwal, J., Yano, Hajime, Blum, J., Henkel, Hartmut, Hillier, Jon K., Hoppe, Peter, Trieloff, Mario, Hsu, S., Mocker, A., Fiege, K., Green, Simon F., Bischoff, A., Esposito, Francesca, Laufer, Rene, Hyde, T. W., Herdrich, G., Fasoulas, S., Jäckel, Annette, Jones, G., Jenniskens, P., Khalisi, E., Moragas-Klostermeyer, Georg, Spahn, F., Keller, H.U., Frisch, P., Levasseur-Regourd, A.C., Pailer, Norbert, Altwegg, Kathrin, Engrand, C., Auer, Siegfried, Silen, J., Sasaki, S., Kobayashi, M., Schmidt, Jürgen M., Kissel, Jochen, Marty, Bernard, Michell, Paul C.N., Palumbo, Pasquale, Vaisberg, O., Baggaley, Jack, Rotundi, Alessandra, and Röser, Hans-Peter

Abstract

The Stardust mission returned cometary, interplanetary and (probably) interstellar dust in 2006 to Earth that have been analysed in Earth laboratories worldwide. Results of this mission have changed our view and knowledge on the early solar nebula. The Rosetta mission is on its way to land on comet 67P/Churyumov-Gerasimenko and will investigate for the first time in great detail the comet nucleus and its environment starting in 2014. Additional astronomy and planetary space missions will further contribute to our understanding of dust generation, evolution and destruction in interstellar and interplanetary space and provide constraints on solar system formation and processes that led to the origin of life on Earth. One of these missions, SARIM-PLUS, will provide a unique perspective by measuring interplanetary and interstellar dust with high accuracy and sensitivity in our inner solar system between 1 and 2 AU. SARIM-PLUS employs latest in-situ techniques for a full characterisation of individual micrometeoroids (flux, mass, charge, trajectory, composition) and collects and returns these samples to Earth for a detailed analysis. The opportunity to visit again the target comet of the Rosetta mission 67P/Churyumov-Gerasimeenternko, and to investigate its dusty environment six years after Rosetta with complementary methods is unique and strongly enhances and supports the scientific exploration of this target and the entire Rosetta mission. Launch opportunities are in 2020 with a backup window starting early 2026. The comet encounter occurs in September 2021 and the reentry takes place in early 2024. An encounter speed of 6 km/s ensures comparable results to the Stardust mission.

Published
2012

26. Dust measurements during Ulysses' 2nd Jupiter encounter

Author

Grun, E., Zook, Harald, Baguhl, M., Fechtig, H., Hanner, M.S., Kissel, Jochen, Lindblad, B.A., Linkert, D., Linkert, G., Mann, I., McDonnell, J.A.M., Morfill, G.E., Polanskey, C., Riemann, R., Schwehm, G., Siddique, N., Grun, E., Zook, Harald, Baguhl, M., Fechtig, H., Hanner, M.S., Kissel, Jochen, Lindblad, B.A., Linkert, D., Linkert, G., Mann, I., McDonnell, J.A.M., Morfill, G.E., Polanskey, C., Riemann, R., Schwehm, G., and Siddique, N.

Abstract

In 2004 the Ulysses spacecraft had its second flyby at Jupiter at 0.8 AU from the planet. 28 dust streams emanating from the jovian system were identified over a 26-month period while the spacecraft was within 4 AU of the planet, and the dust instrument was operating, scanning jovigraphic latitudes from +75 degrees to -25 degrees. From late 2002 until mid 2005, jovian dust stream particles dominated the overall impact rate, reaching a maximum of about 2000 per day in mid 2004. The dust stream data imply strong coupling of the grains to the interplanetary magnetic field. Ulysses also continuously monitored the interstellar dust stream in the heliosphere.

Published
2007

27. COMETARY VOLATILES AND THE ORIGIN OF COMETS

Author

A'Hearn, Michael F., primary, Feaga, Lori M., additional, Keller, H. Uwe, additional, Kawakita, Hideyo, additional, Hampton, Donald L., additional, Kissel, Jochen, additional, Klaasen, Kenneth P., additional, McFadden, Lucy A., additional, Meech, Karen J., additional, Schultz, Peter H., additional, Sunshine, Jessica M., additional, Thomas, Peter C., additional, Veverka, Joseph, additional, Yeomans, Donald K., additional, Besse, Sebastien, additional, Bodewits, Dennis, additional, Farnham, Tony L., additional, Groussin, Olivier, additional, Kelley, Michael S., additional, Lisse, Carey M., additional, Merlin, Frederic, additional, Protopapa, Silvia, additional, and Wellnitz, Dennis D., additional

Published
2012
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28. Systematics of the CHON and other light-element particle populations in Comet Halley

Author

Clark, Benton, Mason, Larry W, and Kissel, Jochen

Subjects
Astrophysics
Abstract

Based on chemical signatures measured by the PIA experiment during the Giotto flyby of comet Halley, particle classifications were designated. In addition to silicate-like grains and particles of mixed (cosmic) composition, there appear to be several light-element rich populations, including the CHON, (H,C), (H,C,O), and (H,C,N) particle types. These compositional classes are further distinguished by differences in mass distributions, a density indicator, and variations in relative abundance within the coma. These particle populations are evidence for chemical heterogeneity in the surface of the cometary nucleus. Particles found mainly in the inner coma may be volatile icy grains. Most of the N of the comet may be found in up to three different populations of grains; one or more of these may be responsible for the observation of cyanojets.

Published
1986

29. South-North and radial traverses through the interplanetary dust cloud

Author

Grun, E., Staubach, P., Baguhl, M., Hamilton, D.P., Zook, Harald, Dermott, S., Gustafson, B.A., Fechtig, H., Kissel, Jochen, Linkert, D., Linkert, G., Srama, Ralf, Hanner, M.S., Polanskey, C., Horanyi, M., Lindblad, B.A., Mann, I., McDonnell, J.A.M., Morfill, G.E., Schwehm, G., Grun, E., Staubach, P., Baguhl, M., Hamilton, D.P., Zook, Harald, Dermott, S., Gustafson, B.A., Fechtig, H., Kissel, Jochen, Linkert, D., Linkert, G., Srama, Ralf, Hanner, M.S., Polanskey, C., Horanyi, M., Lindblad, B.A., Mann, I., McDonnell, J.A.M., Morfill, G.E., and Schwehm, G.

Abstract

Identical in situ dust detectors are flown on board the Galileo and Ulysses spacecraft. They record impacts of micrometeoroids in the ecliptic plane at heliocentric distances from 0.7 to 5.4 AU and in a plane almost perpendicular to the ecliptic from -79 degrees to +79 degrees ecliptic latitude. The combination of both Ulysses and Galileo measurements yields information about the radial and latitudinal distributions of micron- and submicron-sized dust in the Solar System. Two types of dust particles were found to dominate the dust flux in interplanetary space. Interplanetary micrometeoroids covering a wide mass range from 10(-16) to 10(-6) g are recorded mostly inside 3 AU and at latitudes below 30 degrees. Interstellar grains with masses between 10(-14) and 10(-12) g have been positively identified outside 3 AU near the ecliptic plane and outside 1.8 AU at high ecliptic latitudes (>50 degrees). Interstellar grains move on hyperbolic trajectories through the planetary system and constitute the dominant dust flux (1.5 X 10(-4) m(-2) sec(-1)) in the outer Solar System and at high ecliptic latitudes. To compare and analyze the Galileo and Ulysses data sets, a new model is developed based on J. Geophys. Res. 98, 17029-17048, Divine's (1993, ''five populations of interplanetary meteoroids'' model. Both models describe the interplanetary meteoroid environment in terms of dust populations on distinct orbits. Taking into account the measured velocities and the effect of radiation pressure on small particles (described by the ratio of radiation pressure force to gravity, beta), we define four populations of meteoroids on elliptical orbits and one population on hyperbolic orbit that can fit the micrometeoroid flux observed by Galileo and Ulysses. Micrometeoroids with masses greater than 10(-10) g and negligible radiation pressure (beta = 0) orbit the Sun on low to moderately eccentric orbits and with low inclinations (less than or equal to 30 degrees). Populations of smaller

Published
1997

30. Dust measurements in the Jovian magnetosphere

Author

Grun, E., Kruger, H., Dermott, S., Fechtig, H., Graps, A.L., Zook, Harald, Gustafson, B.A., Hamilton, D.P., Hanner, M.S., Heck, A., Horanyi, M., Kissel, Jochen, Lindblad, B.A., Linkert, D., Linkert, G., Mann, I., McDonnell, J.A.M., Morfill, G.E., Polanskey, C., Schwehm, G., Srama, Ralf, Grun, E., Kruger, H., Dermott, S., Fechtig, H., Graps, A.L., Zook, Harald, Gustafson, B.A., Hamilton, D.P., Hanner, M.S., Heck, A., Horanyi, M., Kissel, Jochen, Lindblad, B.A., Linkert, D., Linkert, G., Mann, I., McDonnell, J.A.M., Morfill, G.E., Polanskey, C., Schwehm, G., and Srama, Ralf

Abstract

Dust measurements have been obtained with the dust detector onboard the Galileo spacecraft inside a distance of about 60R(J) from Jupiter (Jupiter radius, R-J = 71, 492 km) during two periods of about 8 days around Galileo's closest approaches to Ganymede on 27 June and on 6 Sept 1996. The impact rate of submicrometer-sized particles fluctuated by a factor of several hundred with a period of about 10 hours, implying that their trajectories are strongly affected by the interaction with the Jovian magnetic field. Concentrations of small dust impacts were detected at the times of Ganymede closest approaches that could be secondary ejecta particles generated upon impact of other particles onto Ganymede's surface. Micrometer-sized dust particles, which could be on bound orbits about Jupiter, are concentrated in the inner Jovian system inside about 20R(J) from Jupiter.

Published
1997

31. 2 Years of Ulysses Dust Data

Author

Grun, E., Baguhl, M., Divine, N., Fechtig, H., Hamilton, D.P., Hanner, M.S., Kissel, Jochen, Lindblad, B.A., Linkert, D., Linkert, G., Manners, Ian, McDonnell, J.A.M., Morfill, G.E., Polanskey, C., Riemann, R., Schwehm, G., Siddique, N., Staubach, P., Zook, Harald, Grun, E., Baguhl, M., Divine, N., Fechtig, H., Hamilton, D.P., Hanner, M.S., Kissel, Jochen, Lindblad, B.A., Linkert, D., Linkert, G., Manners, Ian, McDonnell, J.A.M., Morfill, G.E., Polanskey, C., Riemann, R., Schwehm, G., Siddique, N., Staubach, P., and Zook, Harald

Abstract

From October 18, 1990 to February 8, 1992 the Ulysses spacecraft traversed interplanetary space between the Earth and Jupiter; at Jupiter the spacecraft was deflected below the ecliptic onto a highly-inclined orbit (i similar to 80 degrees). Here, we report on dust impact data obtained from launch until the end of 1992, nearly a year after the Jupiter flyby. During that time (792 days), the Ulysses dust detector recorded 968 impacts of dust particles with masses ranging from 10(-16) g to 10(-8) g. The impact rate varied from as low as one impact per week during quiet times to more than one per minute during the dust stream of March 10-11, 1992. In this paper, we present and describe the complete data set including both raw and reduced data. The performance of the sensor, which has been very satisfactory so far, is discussed in detail together with the noise discrimination scheme employed. The instrument's detection threshold is given as a function of both the particle's mass and its speed relative to Ulysses. The derived impact rates and the distribution of particle masses, speeds and impact directions are compared to a model of the meteoroid complex.

Published
1995

32. 3 Years of Galileo Dust Data

Author

Grun, E., Baguhl, M., Divine, N., Fechtig, H., Hamilton, D.P., Hanner, M.S., Kissel, Jochen, Lindblad, B.A., Linkert, D., Linkert, G., Manners, Ian, McDonnell, J.A.M., Morfill, G.E., Polanskey, C., Riemann, R., Schwehm, G., Siddique, N., Staubach, P., Zook, Harald, Grun, E., Baguhl, M., Divine, N., Fechtig, H., Hamilton, D.P., Hanner, M.S., Kissel, Jochen, Lindblad, B.A., Linkert, D., Linkert, G., Manners, Ian, McDonnell, J.A.M., Morfill, G.E., Polanskey, C., Riemann, R., Schwehm, G., Siddique, N., Staubach, P., and Zook, Harald

Abstract

From its launch in October 1989 until the end of 1992, the Galileo spacecraft traversed interplanetary space from Venus to the asteroid belt and successfully executed close flybys of Venus, the Earth, and the asteroid Gaspra. The dust instrument has been operating most of the time since it was switched on in December 1989. Except for short time intervals near Earth, data from the instrument were received via occasional(once per week to once per month) memory read outs containing 282-818 bytes of data. All events (impacts or noise events) were classified by an onboard program into 24 categories. Over the three-year time span, the dust detector recorded 469 ''big'' dust impacts. These were counted in 21 of the 24 event categories. The three remaining categories of very low amplitude events contain mostly noise events. The impact rate varied from 0.2 to 2 impacts per day depending on heliocentric distance and direction of spacecraft motion with respect to the interplanetary dust cloud. Because the average data transmission rate was very low, some data were not received on the ground. Complete data sets for 358 ''big'' impacts were received, but the other 111 ''big'' impacts were only counted. The observed impact rates are compared with a model of the meteoroid complex.

Published
1995

33. Dust Measurements at high Ecliptic Latitudes

Author

Baguhl, M., Hamilton, D.P., Grun, E., Dermott, S., Fechtig, H., Hanner, M.S., Kissel, Jochen, Lindblad, B.A., Linkert, D., Linkert, G., Manners, Ian, McDonnell, J.A.M., Morfill, G.E., Polanskey, C., Riemann, R., Schwehm, G., Staubach, P., Zook, Harald, Baguhl, M., Hamilton, D.P., Grun, E., Dermott, S., Fechtig, H., Hanner, M.S., Kissel, Jochen, Lindblad, B.A., Linkert, D., Linkert, G., Manners, Ian, McDonnell, J.A.M., Morfill, G.E., Polanskey, C., Riemann, R., Schwehm, G., Staubach, P., and Zook, Harald

Abstract

Along Ulysses' path from Jupiter to the south ecliptic pole, the onboard dust detector measured a dust impact rate that varied slowly from 0.2, to 0.5 impacts per day. The dominant component of the dust flux arrived from an ecliptic latitude and longitude of 10 degrees +/- 10 degrees and 280 degrees +/- 30 degrees which indicates an interstellar origin. An additional flux of small particles, which do not come from the interstellar direction and are unlikely to be zodiacal dust grains, appeared south of -45 degrees latitude. One explanation is that these particles are beta-meteoroids accelerated away from the sun by radiation pressure and electromagnetic forces.

Published
1995

34. Discovery of Jovian Dust Streams and Interstellar Grains by the Ulysses Spacecraft

Author

Grun, E., Zook, Harald, Baguhl, M., Balogh, A., Bame, S.J., Fechtig, H., Forsyth, R., Hanner, M.S., Horanyi, M., Kissel, Jochen, Lindblad, B.A., Linkert, D., Linkert, G., Mann, I., McDonnell, J.A.M., Morfill, G.E., Phillips, J.L., Polanskey, C., Schwehm, G., Siddique, N., Staubach, P., Svestka, J., Taylor, A., Grun, E., Zook, Harald, Baguhl, M., Balogh, A., Bame, S.J., Fechtig, H., Forsyth, R., Hanner, M.S., Horanyi, M., Kissel, Jochen, Lindblad, B.A., Linkert, D., Linkert, G., Mann, I., McDonnell, J.A.M., Morfill, G.E., Phillips, J.L., Polanskey, C., Schwehm, G., Siddique, N., Staubach, P., Svestka, J., and Taylor, A.

Abstract

On 8 February 1992, the Ulysses spacecraft flew by Jupiter at a distance of 5.4 AU from the Sun. During the encounter, the spacecraft was deflected into a new orbit, inclined at about 80-degrees to the ecliptic plane, which will ultimately lead Ulysses over the polar regions of the Sun1. Within 1 AU from Jupiter, the onboard dust detector2 recorded periodic bursts of submicrometre dust particles, with durations ranging from several hours to two days, and occurring at approximately monthly intervals (28 +/- 3 days). These particles arrived at Ulysses in collimated streams radiating from close to the line-of-sight direction to Jupiter, suggesting a jovian origin for the periodic bursts. Ulysses also detected a flux of micrometre-sized dust particles moving in high-velocity (greater-than-or-equal-to 26 km s-1) retrograde orbits (opposite to the motion of the planets); we identify these grains as being of interstellar origin.

Published
1993

35. The Ulysses Dust Experiment

Author

Grun, E., Fechtig, H., Giese, R.H, Kissel, Jochen, Linkert, D., Maas, C., McDonnell, J.A.M., Morfill, G.E., Schwehm, G., Zook, Harald, Grun, E., Fechtig, H., Giese, R.H, Kissel, Jochen, Linkert, D., Maas, C., McDonnell, J.A.M., Morfill, G.E., Schwehm, G., and Zook, Harald

Abstract

The Ulysses dust experiment is intended to provide direct observations of dust grains with masses between 10(-16) g and 10(-6) g in interplanetary space, to investigate their physical and dynamical properties as functions of heliocentric distance and ecliptic latitude. Of special interest is the question of what portion is provided by comets, asteroids and interstellar particles. The investigation is performed with an instrument that measures the mass, speed, flight direction and electric charge of individual dust particles. It is a multicoincidence detector with a mass sensitivity 10(6) times higher than that of previous in-situ experiments which measured dust in the outer solar system. The instrument weighs 3.8 kg, consumes 2.2 W, and has a normal data transmission rate of 8 bits/s in nominal spacecraft tracking mode. On 27th October 1990 the instrument was switched-on. The instrument was configured to flight conditions and science data collection started immediately. In the period to 13th January 1991 at least 44 dust impacts have been recorded. Flux values are given covering the heliocentric distance range from 1.04 to 1.7 AU.

Published
1992

36. Galileo and Ulysses Dust Measurements - from Venus to Jupiter

Author

Grun, E., Baguhl, M., Fechtig, H., Hanner, M.S., Kissel, Jochen, Lindblad, B.A., Linkert, D., Linkert, G., Manners, Ian, McDonnell, J.A.M., Morfill, G.E., Polanskey, C., Riemann, R., Schwehm, G., Siddique, N., Zook, Harald, Grun, E., Baguhl, M., Fechtig, H., Hanner, M.S., Kissel, Jochen, Lindblad, B.A., Linkert, D., Linkert, G., Manners, Ian, McDonnell, J.A.M., Morfill, G.E., Polanskey, C., Riemann, R., Schwehm, G., Siddique, N., and Zook, Harald

Abstract

The Galileo and Ulysses spaceprobes carry two similar dust detectors through interplanetary space from Venus to Jupiter. We report here on impacts which correspond to dust particles above a mass threshold of about 10(-13)g for which we have complete records. Between December 1989 and January 1992 Galileo repeatedly traversed interplanetary space between 0.7 and 2.26 AU and recorded 374 impacts. The observed impact rates ranged from 0.1 to about 3 impacts per day strongly dependent on whether the spacecraft moved towards or away from the Sun. From October 1990 to January 1992 the Ulysses spacecraft had reached a distance of 5.17 AU from the Sun and had recorded 72 impacts at rates between 0.1 and 0.5 per day. Inside about 2 AU the observed fluxes are compatible with a population of interplanetary dust particles moving on low to moderately eccentric (e = 0.1 to 0.5) and low inclination (i = 0 deg. to 30 deg.) orbits. Outside this distance a dust particle population on different orbits is required in order to explain the Ulysses data.

Published
1992

37. Surface of Young Jupiter Family Comet 81 P/Wild 2: Viewfrom the Stardust Spacecraft.

Author

Browntee, Donald E., Horz, Friedrich, Newburn, Ray L., Zolensky, Michael, Duxbury, Thomas C., Sandford, Scott, Sekanina, Zdenek, Tsou, Peter, Hanner, Martha S., Clark, Benton C., Green, Simon F., and Kissel, Jochen

Subjects
*SPACE vehicles, *COMETS, *RUBBLE, *PHOTOGRAPHS, *SOLAR system, *ASTRONAUTICS
Abstract

Images taken by the Stardust mission during its flyby of 81P/Wild 2 show the comet to be a 5-kilometer oblate body covered with remarkable topographic features, including unusual circular features that appear to be impact craters. The presence of high-angle slopes shows that the surface is cohesive and self-supporting. The comet does not appear to be a rubble pile, and its rounded shape is not directly consistent with the comet being a fragment of a larger body. The surface is active and yet it retains ancient terrain. Wild 2 appears to be in the early stages of its degradation phase as a small volatile-rich body in the inner solar system. [ABSTRACT FROM AUTHOR]

Published
2004

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