%% This BibTeX bibliography file was created using BibDesk. %% http://bibdesk.sourceforge.net/ %% Created for Amara Graps at 2007-06-12 16:52:25 +0200 %% Saved with string encoding Western (ASCII) @inproceedings{Kehoe:2007, Abstract = {We investigate the dynamical and collisional evolution of dust particles in the zodiacal cloud from asteroidal sources using numerical simulations that incorporate the effects of radiation pressure, Poynting-Robertson drag, solar-wind drag, planetary perturbations, and also account for particle fragmentation. We note the size dependent behaviour of the particles as a result of interparticle collisions, secular gravitational perturbations, and passage through secular resonances and jovian mean motion resonances. This implies the need to adopt a realistic size-frequency distribution that includes particles greater than 100 microns in diameter in models of the zodiacal cloud. We find that the orientation of the mean plane of symmetry of the zodiacal cloud outside 2AU is dominated by the effect of Jupiter and evolves with the jovian secular cycle. It is for this reason that we are able to distinguish the solar system dust bands from the background zodiacal cloud, although dynamical and collisional effects act to disperse the orbits of the dust band particles. The inner edge to the dust bands at about 2AU is a result of the significant effect of the nu_16 secular resonance on the dust band particle orbits. These results provide an essential basis for developing detailed models of the zodiacal cloud that reproduce its observed global asymmetries and fine structure, including the dust bands.}, Author = {Kehoe, {Thomas J. J.} and Dermott, {Stanley F.} and Mahoney-Hopping, {Lauren M.}}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-12 13:07:24 +0200}, Date-Modified = {2007-06-12 13:12:27 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {81-85}, Publisher = {ESA Publications}, Title = {The Effect of Inter-Particle Collisions on the Dynamical Evolution of Asteroidal Dust and the Structure of the Zodiacal Cloud}, Year = {2007}} @inproceedings{Gruen:2007b, Abstract = {A dust astronomy mission aims at the simultaneous measurement of the origin and the chemical composition of individual dust grains in space. By distinguishing interstellar from interplanetary dust of cometary or asteroidal origin based on their trajectories and comparing their composition important clues on processes in the early solar system can be obtained. The dust observatory mission "Cosmic DUNE" has been defined to reach this goal with newly developed dust instrumentation. A dust trajectory sensor has been developed which is capable of obtaining precision trajectories of sub-micron sized particles in space. A new high mass resolution dust analyzer of 0.1 m^2 impact area can cope with the low fluxes expected in interplanetary space. With these instruments both novel dust measurements in low-Earth orbit and improved dust collection and sample return schemes are achievable.}, Author = {Gruen, E. and Srama, R. and Helfert, S. and Kempf, S. and Moragas-Klostermeyer, G. and Krueger, H. and Altobelli, N. and Auer, S. and Dikarev, V. and Harris, D. and Horanyi, M. and Rachev, M. and Srowig, A. and Sternovsky, Z.}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 12:08:58 +0200}, Date-Modified = {2007-06-10 12:14:05 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {245-249}, Publisher = {ESA Publications}, Title = {Prospects of Dust Astronomy Missions}, Year = {2007}} @inproceedings{Stubbs:2007c, Abstract = {All astronauts who walked on the Moon reported difficulties with lunar dust. These problems were likely worsened by the fact that the dust was electrically charged, which enhanced its adhesive properties. In order to develop strategies to tackle these issues it will be necessary to advance our theoretical understanding of the lunar dust-plasma environment, as well as comprehensively characterize it with in-situ measurements. Summarized here are the relevant properties of lunar dust and its impact on astronauts, together with a discussion of the three main problem areas: (1) Dust Adhesion and Abrasion, (2) Surface Electric Fields and (3) Dust Transport. Also discussed are recent calculations relating to some of the Apolloera observations, together with necessary future in-situ measurements and suggested mission strategies.}, Author = {Stubbs, {Timothy J. } and Vondrak, {Richard R. } and Farrell, { William M. }}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 12:05:34 +0200}, Date-Modified = {2007-06-12 16:50:53 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {239-243}, Publisher = {ESA Publications}, Title = {Impact of Dust on {Lunar} Exploration}, Year = {2007}} @inproceedings{Corsaro:2007, Abstract = {The characterization of dust populations between 100 microns and 1 cm is a key component to improving our understanding of the ongoing physical processes of asteroids, comets, Kuiper Belt objects, planetary rings and planetary satellites. It is also critical for satellite impact risk assessments in the near Earth environment, and future explorations to the Moon, Mars, Jupiter, Saturn, etc. There is a lack of data in this critical size regime, with present in situ detection capability limited to particles 10 microns or smaller. The instrument described here is capable of continuously measuring the flux of orbital debris in the near Earth environment, and micrometeoroids present in interplanetary space or on planetary surfaces for future solar system exploration missions. It uses a fiber optic displacement sensor suite installed on the framework supporting the thin fabric film. This sensor suite monitors fabric motion generated by particle impacts, while also providing a record of fabric tension and integrity. Such an instrument is particularly well suited for use on large area structures, such as inflatable structures and solar sails (Fig. 1).}, Author = {Corsaro, R. and Liou, {J. C. } and Giovane, F. and Tsou, P.}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 12:02:09 +0200}, Date-Modified = {2007-06-10 12:05:20 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {235-238}, Publisher = {ESA Publications}, Title = {Continuous Large-Area Micrometeoroid Flux Measuring Instrument}, Year = {2007}} @inproceedings{Auer:2007b, Abstract = {Solar UV radiation and solar wind, which give cosmic dust grains their charges, can also interfere with the in-situ measurement of those dust charges. They can generate small currents, equivalent to detector leakage currents, which are collected on the sensing electrodes of a dust charge detector. They increase the noise of the detector and can drive it into saturation. In order to safely discharge the currents, a new charge-sensitive amplifier (CSA) has been developed using a double-gate junction field-effect transistor (JFET), a low-leakage input protection diode, and a second feedback loop. Positive currents are safely discharged via the JFET's first gate(G1)-to-source junction, while negative currents are discharged via the protection diode. The currents generate a low-amplitude, low-frequency bias voltage at G1, which would drive a conventional JFET into saturation. To compensate for the bias voltage at G1, a low-frequency baseline-restorer-type feedback loop generates another bias voltage, one that controls the JFET's second gate, G2, in such a way that the JFET is always operating in its optimum range. This CSA does not require an input capacitor or a feedback resistor, which would generate their own noise and thereby increase the overall noise of the CSA. A CSA lab model with these features has been built and tested. Its noise is <100 electrons (rms) in a frequency band from 10 kHz to greater than 10 MHz at room temperature and at a detector capacitance of 5 pF.}, Author = {Auer, Siegfried}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 11:58:21 +0200}, Date-Modified = {2007-06-12 16:48:39 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {231-233}, Publisher = {ESA Publications}, Title = {Low-Noise Amplifier for Measuring Dust Charges in the Presence of Plasma and {UV} Radiation}, Year = {2007}} @inproceedings{Liou:2007, Abstract = {A 10 m^2 aerogel and acoustic sensor system has been under development by the U.S. Naval Research Laboratory (NRL) with main collaboration from the NASA Orbital Debris Program Office at Johnson Space Center. This Large Area Debris Collector (LAD-C) is tentatively scheduled to be deployed by the U.S. Department of Defense Space Test Program (STP) on the International Space Station (ISS) in late 2007. The system will be retrieved, after one to two years of data and sample collection, for post-flight analysis. In addition to cosmic dust and orbital debris sample return, the acoustic sensors will record impact characteristics for potential orbit determination of some of the collected samples. Source identification based on their dynamical signatures may be possible. The LAD-C science return will benefit orbital debris, cosmic dust, and satellite safety communities. This paper presents an overview of the mission objectives, basic configuration, deployment consideration, and science return of the experiment. }, Author = {Liou, {J.-C. } and Giovane, F. and Corsaro, R. and Stansbery, E.}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 11:54:11 +0200}, Date-Modified = {2007-06-12 16:47:45 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {227-230}, Publisher = {ESA Publications}, Title = {{LAD-C}: A {Large Area Cosmic Dust} and {Orbital Debris Collector} on the {International Space Station}}, Year = {2007}} @inproceedings{Tsou:2007, Abstract = {The Large Area Dust Collection (LADC), greater than 10 m^2 of instrumented silica aerogel mounted externally on the International Space Station, will capture and return large dust particles intercepted in Earth orbit. The uniqueness of LADC is that it carries a self-contained acoustic impact recording and locationing system to offer the opportunity to determine the particles' trajectories nondestructively and, for the first time, an opportunity to ascertain the particles' parent sources. Another uniqueness of LADC is that the flight cost for space deployment, integration and Earth return will be provided by the Department of Defense (DoD) Space Test Program (STP). LAD-C flight will also provide statistical significant samples of ~thirty 100 microns large extraterrestrial particles and the retrieval of samples themselves for detailed Earth based laboratory analysis to determine the chemical and physical nature of the particles.}, Author = {Tsou, P. and Giovane, F. and Liou, {J-C.} and Corsaro, R.}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 11:49:35 +0200}, Date-Modified = {2007-06-12 16:46:09 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {219-226}, Publisher = {ESA Publications}, Title = {{Large Area Dust Collection} - On the {International Space Station}}, Year = {2007}} @inproceedings{Srama:2007b, Abstract = {Dust particles' trajectories are determined by the measurement of the electric signals that are induced when a charged grain flies through a position sensitive electrode system. The objective of the trajectory sensor is to measure dust charges in the range 10^{-16} to 10^{-13} C and dust speeds in the range 6 to 100 km/s. The trajectory sensor has four sensor planes consisting of about 16 wire electrodes each. Two adjacent planes have orthogonal wire direction. A charge sensitive amplifier ASIC has been developed with a RMS noise of about 1.5 times 10^{-17} C. The signals from 32 electrodes are digitized and sampled at 25 MHz rate by an transient recorder ASIC (Application Specific Integrated Circuit). First tests with a laboratory set-up have been performed and demonstrate the expected performance.}, Author = {Srama, R. and Srowig, A. and Auer, S. and Harris, D. and Helfert, S. and Kempf, S. and Moragas-Klostermeyer, G. and Gruen, E.}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 11:45:14 +0200}, Date-Modified = {2007-06-10 11:49:28 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {213-217}, Publisher = {ESA Publications}, Title = {A Trajectory Sensor for Sub-micron Sized Dust}, Year = {2007}} @inproceedings{Srama:2007a, Abstract = {The Large Area Mass Analyser (LAMA) discussed in this paper was developed by the Max Planck Institute Nuclear Physics in Heidelberg. This spectrometer is designed to perform elemental analysis of interplanetary dust, interstellar dust or space debris particles in the Earth environment. The instrument consists of a target with a sensitive area of 0.1 m^2 and performs time-of-flight measurements of the impact plasma ions from hypervelocity dust impacts. The device employs a reflectron for the improvement of the mass resolution which has values between 150 and 300. The mass resolution of this spectrometer is better than of any other known instrument with a comparatively large sensitive area. Here we report about the first laboratory tests at the Heidelberg dust accelerator facility using iron particles with speeds up to 35 kms^{-1}}, Author = {Srama, R. and Kempf, S. and Moragas-Klostermeyer, G. and Landgraf, M. and Helfert, S. and Sternovsky, Z. and Rachev, M. and and Gruen, E.}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 11:40:17 +0200}, Date-Modified = {2007-06-12 16:44:33 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {209-212}, Publisher = {ESA Publications}, Title = {Laboratory Tests of the {Large Area Mass Analyser}}, Year = {2007}} @inproceedings{Sternovsky:2007, Abstract = {An instrument to analyze the chemical composition of dust particles in space has been developed. The large target area (0.2 m^2) makes this instrument suitable for detecting rare interstellar dust grains. The device is a reflectron type time-of-flight mass spectrometer that measures the ions from the impact-generated plasma due to hypervelocity dust impacts on the target surface. The SIMION ion optics software package has been used to investigate different potential field configurations and optimize the mass resolution and focusing of the ions. The final cylindrical configuration uses a set of six ring electrodes on the side and six annular electrodes at the top, biased to different potentials, to create the potential distribution of the reflectron. The laboratory model of the instrument has been fabricated and is undergoing preliminary testing. Dust impacts are simulated by using a frequency-doubled (532 nm) Nd:YAG laser with ~8 ns pulse length. The mass resolution is m/delta_m greater-than-or-equal 125.}, Author = {Sternovsky, Zoltan and Amyx, Keegan and Bano, Gregor and Landgraf, Markus and Horanyi, Mihaly and Knappmiller, Scott and Robertson, Scott and Gruen, Eberhard and Srama, Ralf and Auer, Siegfried}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 11:33:44 +0200}, Date-Modified = {2007-06-10 11:40:01 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {205-208}, Publisher = {ESA Publications}, Title = {The Large Area Mass Analyzer (LAMA) for In-Situ Chemical Analysis of Interstellar Dust Particles}, Year = {2007}} @inproceedings{Carpenter:2007, Abstract = {Between 2002 and 2004, witness samples of 60 nm thick, aluminum films were exposed to the International Space Station's external environment. On retrieval these films were found to have been perforated extensively by impacting particles, whose inferred diameters are tens of nanometres. This size regime, whether natural dust or man made debris, is almost two orders of magnitude smaller than has previously been measured with conventional instrumentation. We report here on the ongoing characterization of the exposed films and work to develop future thin film experiments for the detection of interplanetary dust.}, Author = {Carpenter, {J.D. } and Stevenson, {T.J. } and Kearsley, {A. } and Fraser, {G.W. }}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 11:30:27 +0200}, Date-Modified = {2007-06-10 11:33:35 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {201-204}, Publisher = {ESA Publications}, Title = {Thin Films as Dust Detectors}, Year = {2007}} @inproceedings{Ueno:2007, Abstract = {We developed a new observation system "WIZARD"; Wide-field Imager of Zodiacal light with Array Detector. Since the zodiacal light is faint and very extended all over the sky, WIZARD employs a sensitive CCD with a wide field optics with sufficient spatial resolution to remove the contribution of integrated flux of individual stars. WIZARD is designed to measure the absolute brightness of the diffuse sky at visible wavelength and to have good stability of the instrumental zero-level and low noise feature. The first light of WIZARD was performed in 2001 at Mauna Kea, Hawaii, and the first scientific image of the gegenschein was taken in 2002 under collaboration with SUBARU observatory. We have been promoting extended observations of the zodiacal light along the ecliptic plane. The design and the performance of WIZARD system, and also the preliminary results of the zodiacal light observations are introduced in this paper. }, Author = {Ueno, Munetaka and Ishiguro, Masateru and Usui, Fumihiko and Nakamura, Ryosuke and Ootsubo, Takafumi and Miura, Naoya and Sarugaku, Yuki and Kwon, {Suk Minn } and Hong, {SeungSoo} and Mukai, Tadashi}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 11:16:39 +0200}, Date-Modified = {2007-06-12 13:33:35 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {197-200}, Publisher = {ESA Publications}, Title = {{WIZARD} - A New Observation System of the Zodiacal Light}, Year = {2007}} @inproceedings{Wurm:2007, Abstract = {There are two major sources of interplanetary dust in the Solar System: comets and asteroids. Since most of the short period comets are assumed to originate from the Kuiper belt, dust might eventually be traced back to two ring-like reservoirs -- the Kuiper belt and the asteroid belt. We have recently found that photophoresis in a late Solar Nebula might explain exactly that -- the formation of belts. Based on the only assumption that a transparent, yet gas rich protoplanetary disk existed, a concentration of solid matter in ring-like structures seems inevitable. In particular, the position of the ring(s) depends on the disk model and on the thermal, optical, and surface properties of the particles. While dust aggregates are concentrated several tens of A.U. away from the Sun, chondrules, which are found in primitive meteorites, are concentrated a few A.U. away from the Sun. This suggests that (primitive) asteroids and comets or Kuiper belt objects form rather late in protoplanetary disks by photophoretic concentration.}, Author = {Wurm, Gerhard and Krauss, Oliver}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 11:13:18 +0200}, Date-Modified = {2007-06-10 11:16:28 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {191-194}, Publisher = {ESA Publications}, Title = {The Fundamental Role of Photophoresis for Dust in Planetary Systems}, Year = {2007}} @inproceedings{Stubbs:2007b, Abstract = {From the Apollo era there is much evidence to show that the lunar ``horizon glow'' and ``streamers'' observed at the terminator are caused by sunlight scattered by dust grains originating from the Moon's surface. A simple dynamic dust ``fountain'' model has previously been proposed to explain observations of submicron dust ``lofted'' to altitudes of ~100 km. In this model charged dust grains follow ballistic trajectories, subsequent to being accelerated upwards through a narrow sheath region by the surface electric field. Described here are the effects of including a more realistic exponentially decaying electric field (consistent with Debye shielding of a charged surface in a plasma). Also discussed are the different mechanisms by which highly charged dust grains can be generated at the lunar surface; in particular, the possible effects of triboelectric charging are considered. Dust in the exosphere will affect the optical quality of the lunar environment for astronomical observations, as well as interfere with future robotic and human exploration activities.}, Author = {Stubbs, {Timothy J. } and Vondrak, {Richard R. } and Farrell, {William M. }}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 11:09:07 +0200}, Date-Modified = {2007-06-12 13:31:07 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {185-189}, Publisher = {ESA Publications}, Title = {A Dynamic Fountain Model for Dust in the {Lunar} Exosphere}, Year = {2007}} @inproceedings{Stubbs:2007a, Abstract = {The electrostatic charging of the lunar surface is caused by its interaction with the local plasma environment and solar UV and X-ray induced photoemission of electrons. Probe equations are used here to calculate electrostatic lunar surface potentials as a function of angle from the subsolar point, thus giving a global perspective on charging processes. Since the Moon is in the solar wind plasma flow for most of its orbit, surface potentials are first determined for typical fast and slow stream conditions. They are then calculated using data from the Electron Reflectometer aboard Lunar Prospector. The latter reveals how the hot tenuous plasma of the lunar wake drives large negative surface potentials (up to -200 V) on the nightside of the Moon. Lunar surface charging in the Earth's magnetosphere is also discussed, with initial predictions indicating that the nightside charges to ~ -600 V in the plasma sheet. The ability to predict surface potentials is vital for understanding the lunar environment; in particular, processes such as ion sputtering and electrically-driven dust transport. The latter is especially important since dust significantly interfered with Apollo exploration activities.}, Author = {Stubbs, {Timothy J. } and Halekas, {Jasper S. } and Farrell, {William M. } and Vondrak, {Richard R. }}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 11:05:19 +0200}, Date-Modified = {2007-06-12 13:30:09 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {181-184}, Publisher = {ESA Publications}, Title = {Lunar Surface Charging: A Global Perspective Using {Lunar Prospector} Data}, Year = {2007}} @inproceedings{Auer:2007a, Abstract = {The electric charges of highly irregular dust grains were computed. We find that, of all possible shapes, a sphere carries the lowest charge and "fluffy" grains, especially grains consisting of long rods, carry charges as high as kappa=30 times the charge of a spherical grain having the same volume and surface potential. We conclude that one tends to over-estimate a grain's size when deducing it from the grain's charge, unless the shape factor kappa is taken into account. }, Author = {Auer, Siegried and Kempf, Sascha and Gruen, Eberhard}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 11:01:40 +0200}, Date-Modified = {2007-06-10 11:05:09 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {177-180}, Publisher = {ESA Publications}, Title = {Computed Electric Charges of Grains with Highly Irregular Shapes}, Year = {2007}} @inproceedings{Colwell:2007, Abstract = {Dust particles in the regoliths of planetary satellites, asteroids, and ring particles can become charged due to photoemission from solar ultraviolet photons, solar wind currents, and, in some cases, magnetospheric electrons. A surface potential is created on the surface of airless bodies in the solar system, such as the Moon, due to these same currents. This leads to a plasma sheath over the nighttime surface and a photoelectron layer over the daytime surface. Charged dust particles injected into this near-surface plasma environment are affected by the electrostatic force as well as gravity. This can lead to transport of dust and levitation of particles above the surface. Lunar electrostatic dust dynamics have been proposed for several observed dust phenomena [1-6]. Similar phenomena may play a role in the spokes of Saturn's rings [7, 8] and in the formation of smooth deposits in the floors of some craters on the asteroid Eros as observed by the NEAR-Shoemaker spacecraft [9]. }, Author = {Colwell, {J. E. } and Horanyi, M. and Robertson, S. and Wang, X. and Haugsjaa, A. and Wheeler, P.}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 10:57:31 +0200}, Date-Modified = {2007-06-10 11:01:13 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {171-175}, Publisher = {ESA Publications}, Title = {Behavior of Charged Dust in Plasma and Photoelectron Sheaths}, Year = {2007}} @inproceedings{Abbas:2007, Abstract = {It is well known since the Apollo missions that just above the lunar regolith is a layer of levitated dust that is electrostatically charged by the incident solar UV radiation and by interaction with the solar wind. Photoelectric emissions induced by the UV radiation at photon energies higher than the work function of the grain materials, however, are recognized to be the dominant process for charging of the lunar dust in the sunlight. This requires measurement of the photoelectric yield of individual dust grains to determine their charge and equilibrium potentials. In this paper, we present the first laboratory measurements of the photoelectric yields of individual micron/sub-micron size dust grains selected from soil samples from the Soviet Luna-24 Mission. The experimental results on photoelectric emissions indicate that the yields are dust size dependent. The yields increase with the grain size by an order of magnitude from the sub-micron size to grains of several microns radii, at which they reach asymptotic values. The yields for large-size grains were determined to be more than an order of magnitude higher than the bulk measurements reported in the literature. }, Author = {Abbas, {M. M. } and Tankosic, D. and Craven, {P. D. } and Hoover, {R. B. } and Taylor, {L. A. } and Spann, {J. F. } and LeClair, {A. } and West, {E. A. }}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 10:50:32 +0200}, Date-Modified = {2007-06-10 10:57:21 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {165-170}, Publisher = {ESA Publications}, Title = {Measurements of Photoelectric Yields of Individual Lunar Dust Grains}, Year = {2007}} @inproceedings{Krauss:2007a, Abstract = {We report on the experimental determination of beta values, i.e. ratios of radiation pressure force to gravity, of graphite aggregates of several microns in size. The method used yields simultaneously values for the parallel and the transverse component of the radiation pressure force. For a graphite aggregate of size 6 times 17 microns, we find a variation of beta with values from 4.3 to 14.9 and a transverse component of the radiation pressure force that is about 55% of the component in the forward direction. The broad distribution of values measured for a single particle is due to the variation of the orientation of the highly irregularly shaped particle during the series of measurements. The unexpectedly high values can be explained by the characteristic structure of graphite aggregates. }, Author = {Krauss, Oliver and Wurm, Gerhard}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 10:45:45 +0200}, Date-Modified = {2007-06-12 13:27:04 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {161-164}, Publisher = {ESA Publications}, Title = {Radiation Pressure on Single Graphite Aggregates}, Year = {2007}} @inproceedings{Rotundi:2007, Abstract = {In preparation for the Stardust sample analyses, we performed combined micro-IR/micro-Raman measurements on five Interplanetary Dust Particles (IDPs) that were characterized by Field Emission Scanning Electron Microscope analyses. We demonstrate the synergy between these techniques to detect Fe-oxides and the degree of ordering in amorphous carbons, and IR-based classification of these IDPs collected in the lower stratosphere. We present IR spectra and micro-Raman data that offer new insight in the evolution of the amorphous carbon component in (1) three chondritic aggregate IDPs, (2) a sulfide IDP and (3) a Fe-rich IDP sphere with a vestige of sulfur remnant after ablation and melting of a sulfide IDP.}, Author = {Rotundi, A. and Ferrini, G. and Baratta, {G.A.} and Palumbo, {M.E.} and Palomba, E. and Colangeli, L.}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 10:42:05 +0200}, Date-Modified = {2007-06-10 10:45:33 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {149-153}, Publisher = {ESA Publications}, Title = {Combined Micro-Infrared (IR) and Micro-Raman Measurements on Stratospheric Interplanetery Dust Particles}, Year = {2007}} @inproceedings{Taylor:2007, Abstract = {Micrometeorites collected from the South Pole water well in 1995 and 2000 have terrestrial depositional ages of 1100-1500 AD and 800-1100 AD respectively. We measured a size distribution for micrometeorites collected in 2000. Compared to the size distribution measured in 1995 the tail slopes of the size distributions are the same. However the 2000 collection has twice as many micrometeorites and proportionally more large micrometeorites. We also tabulate the unmelted-to-melted ratio for micrometeorites in five size ranges and compare the results with previous collections. The unmelted-to-melted ratios obtained for this collection are similar to those from Greenland and an Antarctic collection of present-day micrometeorites. Collections from older Antarctic ice show larger and more variable ratios.}, Author = {Taylor, S. and Matrajt, G. and Lever, {J.H. } and Joswiak, {D. J. } and Brownlee, {D. E. }}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 10:32:20 +0200}, Date-Modified = {2007-06-12 13:24:31 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {145-148}, Publisher = {ESA Publications}, Title = {Size Distribution of Antarctic Micrometeorites}, Year = {2007}} @inproceedings{Joswiak:2007, Abstract = {Atmospheric entry velocities were estimated on 31 stratospheric IDPs (interplanetary dust particles) using measured atmospheric entry temperatures from stepped He-release release measurements [4] and the atmospheric entry model of Love and Brownlee [5]. Twelve IDPs with atmospheric entry velocities > 18 km/s are believed to have been derived from comets while 4 IDPs with atmospheric entry velocities < 14 km/s likely originated in asteroids. Significant differences in density, morphology and mineralogy exist between the cometary and asteroidal groups. The cometary IDPs have an average density of 1.0 g/cm^3 and are largely dominated by high internal porosities and anhydrous mineralogy. One cometary IDP, which is dissimiliar to the others, is principally composed of hydrated silicate minerals. The asteroidal IDPs have a much higher average density of 3.3 g/cm^3 compared to the cometary IDPs. Three of the four asteroidal IDPs are principally composed of hydrated minerals with low porosities arranged in compact structures. One asteroidal IDP, however, is similar to the majority of cometary IDPs; it contains anhydrous minerals with high internal porosity.}, Author = {Joswiak, {D. J. } and Brownlee, {D. E.} and Pepin, {R. O. } and and Schlutter, {D. J. }}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 10:27:02 +0200}, Date-Modified = {2007-06-12 13:22:47 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {141-144}, Publisher = {ESA Publications}, Title = {Densities and Mineralogy of Cometary and Asteroidal Interplanetary Dust Particles Collected in the Stratosphere}, Year = {2007}} @inproceedings{Caro:2007, Abstract = {A brief overview of astrobiologically relevant organic species detected in small solar system bodies, in particular meteorites, is provided. Such organic molecules, however, are only a minor component of the carbon in these objects. Many of them, like amino acids, probably the most interesting family of molecules for astrobiology, have not yet been detected in the interstellar medium. Most of the carbon is present as the so-called macromolecular organic material, both in meteorites and interplanetary dust particles. We show that material is analogous to hydrogenated amorphous carbon, a hydrocarbon widely studied by chemists. A form of hydrogenated amorphous carbon is also observed in grains toward the diffuse interstellar medium, and even in Seyfert 2 galaxies, although with different chemical properties. Therefore, in our attempt to trace the evolution of carbonaceous matter as the local interstellar cloud collapsed leading to the formation of the solar nebula, we focus on the study of an ubiquitous form of carbon, namely hydrogenated amorphous carbon.}, Author = {Caro, {G. M. Munoz} and Martinez-Frias, J.}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 10:23:23 +0200}, Date-Modified = {2007-06-10 10:26:33 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {133-138}, Publisher = {ESA Publications}, Title = {Carbonaceous Dust in Planetary Systems: Origin and Astrobiological Significance}, Year = {2007}} @inproceedings{Krivov:2007, Abstract = {In the last decade, hundreds of debris disks around main sequence stars have been detected through infrared excesses in the stellar spectra and some imaged directly. This review outlines essential forces and effects exerted on dust in debris disks and then summarizes key properties of the disks, as determined by these physics. Size and spatial distribution of dust, long- and short-term evolution of disks, as well as interrelations between dust, its parent bodies, and embedded planets are addressed.}, Author = {Krivov, {Alexander V. }}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 10:20:51 +0200}, Date-Modified = {2007-06-12 13:20:48 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {123-132}, Publisher = {ESA Publications}, Title = {Physics of Debris Disks}, Year = {2007}} @inproceedings{Moro:2007, Abstract = {Main sequence stars are commonly surrounded by debris disks, formed by cold far-IR-emitting dust that is thought to be continuously replenished by a reservoir of undetected dust-producing planetesimals. In a planetary system with a belt of planetesimals (like the Solar System's Kuiper Belt) and one or more interior giant planets, as the particles spiral inward due to Poynting-Robertson (PR) drag they can get trapped in the mean motion resonances (MMRs) with the planets. This process can create structure in the dust disk, as the particles accumulate at certain semimajor axes. Sufficiently massive planets may also scatter and eject dust particles out of a planetary system, creating a dust depleted region inside the orbit of the planet, a feature that is common in most of the spatially debris disks observed so far. We have studied the efficiency of particle ejection and the resulting dust density contrast inside and outside the orbit of the planet, as a function of the planet's mass and orbital elements and the particle size. Because the debris disk structure is sensitive to long period planets, complementing a parameter space not covered by radial velocity and transit surveys, its study can help us learn about the diversity of planetary systems. Presently, the Spitzer Space Telescope is carrying out observations of debris disks most of which are spatially unresolved. It is interesting therefore to study how the structure carved by planets affects the shape of the disk's Spectral Energy Distribution (SED), and consequently if the SED can be used to infer the presence of planets. We have numerically calculated the 3-D equilibrium spatial density distributions of dust disks originated by a belt of planetesimals similar to the Kuiper Belt (KB) in the presence of interior giant planets in different planetary configurations (with planet masses ranging from 1-10 MJup in circular orbits with semimajor axis between 1--30 AU). For each of these systems we calculate its SED for a representative sample of chemical compositions. We discuss what types of planetary systems can be distinguishable from one another and the main parameter degeneracies in the model SEDs. We find that the SEDs are degenerated, and therefore to unambiguously constrain the planet location we need to obtain high resolution images able to spatially resolve the disk. In the future, observatories like ALMA, LBT, SAFIR, TPF and JWST will be able to image the dust in planetary systems analogous to our own.}, Author = {Moro-Martin, Amaya and Malhotra, Renu and Wolf, Sebastian}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-10 10:16:54 +0200}, Date-Modified = {2007-06-10 10:20:34 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {113-122}, Publisher = {ESA Publications}, Title = {Signatures of Planets in Debris Disks}, Year = {2007}} @inproceedings{McBride:2007, Abstract = {We discuss issues involved with interpreting time-of-flight mass spectra (TOFMS) obtained by the Chemical Analyser subsystem of the Cassini Cosmic Dust Analyser (CDA). We use an in-house ion dynamics code specifically written for CDA which helps us to understand and constrain the initial impact plasma ion kinetic energy and angular distributions. We also present some typical results obtained from within the Saturnian system. We find that particles predominantly consist of water ice (manifesting itself in the TOFMS as hydronium ions, with varying numbers of water molecules attached) and minor silicate impurities. Some ammonia may also be present.}, Author = {McBride, N. and Hillier, {J.K.} and Green, {S.F.} and Srama, R. and Kempf, S. and Postberg, F. and Moragas-Klostermeyer, G. and McDonnell, {J.A.M.} and Gruen, E.}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-09 22:22:35 +0200}, Date-Modified = {2007-06-12 13:18:07 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {107-110}, Publisher = {ESA Publications}, Title = {Cassini Cosmic Dust Analyser: Composition of Dust at {Saturn}}, Year = {2007}} @inproceedings{Zeehand:2007, Abstract = {We investigate dust grains orbiting a planet and interacting with its satellite system. The grains are subject to the gravitational force of Jupiter and its four Galilean satellites, the electromagnetic force from the rotating planetary magnetic field, and solar radiation pressure. We generate clouds of 5-micron grains launched perpendicular to the surfaces of the Galilean satellites at each of their respective escape velocities. This collisional ejecta moves initially along planar, near-circular orbits but is often perturbed to orbits with high inclinations and eccentricities. Collisions with not only the satellite of origin but also with the other moons and even Jupiter can then occur. These perturbed grains suggest a possible circumjovian origin for the detections by the Pioneer 10 and 11 meteoroid experiments, which recorded dust well out of the Jovian equatorial plane.}, Author = {Zeehandelaar, {D. B. } and Hamilton, {D. P. }}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 18:26:00 +0200}, Date-Modified = {2007-06-12 13:16:46 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {103-106}, Publisher = {ESA Publications}, Title = {A Local Source for the {Pioneer} 10 and 11 Circumjovian Dust Detections}, Year = {2007}} @inproceedings{Graps:2007a, Abstract = {In September 1996, a dust/debris detector: GORID was launched into the geostationary (GEO) region as a piggyback instrument on the Russian Express-2 telecommunications spacecraft. The instrument began its normal operation in April 1997 and ended its mission in July 2002. The goal of this work was to use GORID's particle data to identify and separate the space debris to interplanetary dust particles (IDPs) in GEO, to more finely determine the instrument's measurement characteristics and to derive impact fluxes. While the physical characteristics of the GORID impacts alone are insufficient for a reliable distinction between debris and interplanetary dust, the temporal behavior of the impacts are strong enough indicators to separate the populations based on clustering. Non-cluster events are predominantly interplanetary, while cluster events are debris. The GORID mean flux distributions (at mass thresholds which are impact speed dependent) for IDPs, corrected for dead time, are 1.35 times 10^{-4} m^{-2} s^{-1} using a mean detection rate: 0.54 d^{-1}, and for space debris are 6.1 times 10^{-4} m^{-2}s^{-1} using a mean detection rate: 2.5 d^{-1}. Beta-meteoroids were not detected. Clusters could be a closely-packed debris cloud or a particle breaking up due to electrostatic fragmentation after high charging.}, Author = {Graps, {A. L. } and Green, {S.F.} and McBride, N. and McDonnell, {J.A.M.} and Bunte, K. and Svedhem, H. and Drolshagen, G.}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 18:23:24 +0200}, Date-Modified = {2007-06-12 13:15:35 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {97-102}, Publisher = {ESA Publications}, Title = {{GEO} Debris and Interplanetary Dust: Fluxes and Charging Behavior}, Year = {2007}} @inproceedings{Ipatov:2007, Abstract = {The orbital evolution of asteroidal, trans-Neptunian, and cometary dust particles under the gravitational influence of planets, the Poynting-Robertson drag, radiation pressure, and solar wind drag was integrated. Results of our runs were compared with the spacecraft observations of the number density of dust particles and with the WHAM observations of velocities of zodiacal particles. This comparison shows that the fraction of cometary dust particles of the overall dust population inside Saturn's orbit is significant and can be dominant. The probability of a collision of an asteroidal or cometary dust particle with the Earth during its dynamical lifetime is at a maximum at a particle diameter d~100 microns.}, Author = {Ipatov, {S. I. } and Mather, { J. C.}}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 18:20:57 +0200}, Date-Modified = {2007-06-07 18:23:17 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {91-94}, Publisher = {ESA Publications}, Title = {Migration of Dust Particles to the Terrestrial Planets}, Year = {2007}} @inproceedings{Flandes:2007, Abstract = {During late 2002 and mid 2005, the Ulysses spacecraft approached Jupiter (~0.8 AU at its closest distance) and detected 28 new Jovian dust particle streams. The tiny positively charged dust grains (~10 nm) in the streams are accelerated away from Jupiter by its corotational electric field to very high speeds (greater than 200 km s^{-1}). Data indicate that, once outside the Jovian magnetosphere, dust grains are under the influence of the interplanetary magnetic field (IMF) and some characteristics of this field are observed on the dust streams. On the whole, every detected dust stream is preceded by a high IMF event that in most cases corresponds to corotating interaction regions (CIRs) and in few cases to coronal mass ejections (CMEs). The dust stream duration matches roughly the duration of these previous events indicating a confinement of the dust stream particles in the compressed regions of the interplanetary plasma. Additionally, most dust stream peaks and the precedent high IMF events peaks seem to be separated by an interval roughly similar to the time needed by a dust particle to travel from the source to the spacecraft's detector.}, Author = {Flandes, A. and and Krueger, H.}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 18:17:15 +0200}, Date-Modified = {2007-06-12 13:13:30 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {87-90}, Publisher = {ESA Publications}, Title = {Solar Wind Modulation of {Jupiter} Dust Stream Detection}, Year = {2007}} @inproceedings{Mukai:2007, Abstract = {We present the light absorption cross-section of a mm-size aggregate consisting of large monomers computed by geometric optics using ray tracing. Referring to these cross-sections together with those derived from Mie theory associated with the Maxwell-Garnett mixing rule (MG-Mie), the temperature of such an aggregate at a solar distance of 1 AU is derived. It is found that a significantly lower temperature of 206 K, compared with 280 K for a blackbody, appears for a large silicate aggregate with the equivalent volume of a sphere of 2 mm in radius, while a silicate sphere larger than 1 mm in radius shows a blackbody temperature. Furthermore, the ratio, beta of radiation pressure to solar gravity on such a 2 mm-aggregate, derived by the MG-Mie method, shows a larger beta of 2 times 10^{-4} compared to 10^{-4} for a sphere with an equivalent volume.}, Author = {Mukai, T. and Okada, Y.}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 17:52:32 +0200}, Date-Modified = {2007-06-12 13:25:46 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {157-160}, Publisher = {ESA Publications}, Title = {Optical Properties of Large Aggregates}, Year = {2007}} @inproceedings{Durda:2007, Abstract = {We present mass-frequency data for fragments from the impact disruption of four chondritic meteorites, extending to masses several orders of magnitude smaller the mass-frequency data that are usually measured in similar impact experiments. Masses of mm- to cm-scale fragments were determined by directly weighing debris collected from the floor of the Ames Vertical Gun Range impact chamber. Masses of sub-mm to dust-size fragments were determined from analysis of foil penetration data. The mass-frequency distributions display a range of morphologies ranging from nearly linear power-law distributions to `broken' power laws with progressively shallower slopes at smaller fragment masses, apparently dependent on the magnitude of the impact specific energy.}, Author = {Durda, {Daniel D. } and Flynn, {George J.} and Sandel, {L. Erica } and Strait, {Melissa M.}}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 17:41:14 +0200}, Date-Modified = {2007-06-07 17:47:43 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {77-80}, Publisher = {ESA Publications}, Title = {Size-Frequency Distributions of Dust - Size Debris from the Impact Disruption of Chondritic Meteorites}, Year = {2007}} @inproceedings{Lasue:2007, Abstract = {Physical properties of the interplanetary dust such as the local polarization and temperature, together with their heliocentric variations, may be derived from scattered and emitted light observations. With a realistic size distribution typical of the interplanetary dust, a very good fit of the polarization phase curve near 1 AU is obtained for a mixture of silicate and more absorbing organic material (approx 40 % in mass). The decrease of P_{90 deg} values with the solar distance is interpreted as a decrease of the organic percentage towards the Sun. Finally the contribution of dust particles of cometary origin is at least 20% at ~1AU.}, Author = {Lasue, J. and Levasseur-Regourd, {A. C.}}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 17:39:08 +0200}, Date-Modified = {2007-06-07 17:44:19 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {73-76}, Publisher = {ESA Publications}, Title = {Approaching Interplanetary Dust Physical Properties from Light Scattering and Thermal Observations and Simulations}, Year = {2007}} @inproceedings{Krueger:2007b, 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.}, Author = {Krueger, H. and Gruen, E.}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 17:35:45 +0200}, Date-Modified = {2007-06-12 13:02:42 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {69-72}, Publisher = {ESA Publications}, Title = {Dust Measurements During {Ulysses'} 2nd {Jupiter} Encounter}, Year = {2007}} @inproceedings{Altobelli:2007, Abstract = {We present the Cosmic Dust Analyzer (CDA) data obtained by the Cassini spacecraft during the interplanetary cruise phase between the Jupiter fly-by and the Saturn orbit insertion (SOI). Prior to the Cassini mission, the only in-situ dust detectors ever flown between Jupiter and Saturn were the Pioneer 10 and Pioneer 11 dust experiments. However, owing to the sensitivity of these instruments, only big particles (larger than 10 microns for Pioneer 10 and larger than 25 microns for Pioneer 11) could be detected. In contrast, CDA allows the detection of smaller grains. In particular, hundreds of high-velocity tiny dust particles, so-called stream particles, originating from both the Jovian and Saturnian systems were detected even at great distances from their source. In addition, we identified 17 interplanetary dust particles (IDPs), most probably of cometary origin, on moderate to high eccentric orbits. Furthermore, an impact cluster was identified, relying on both directional and temporal criteria, suggesting an encounter with a cometary trail. The shape of the impact charge signals suggests porous material for those particles.}, Author = {Altobelli, N. and Kempf, S. and Roy, M. and Srama, R. and Helfert, S. and Moragas-Klostermeyer, G. and Gruen, E.}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 17:09:58 +0200}, Date-Modified = {2007-06-07 17:35:37 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {65-68}, Publisher = {ESA Publications}, Title = {Preliminary Results on Analysis of the {Cosmic Dust Analyzer} Data Between {Jupiter} and {Saturn}}, Year = {2007}} @inproceedings{Skorov:2007, Abstract = {The innermost cometary water atmosphere formed by sublimation under solar heating is simulated by Direct Simulation Monte Carlo (DSMC). The nucleus is modeled as a non-spherical rotational body. The corresponding surface boundary conditions for the sublimating gas are determined from a self-consistent thermophysical model of a cometary nucleus developed by the authors. Fields of macrocharacteristics both for gas and dust are calculated by parallel computer implementation of the kinetic model. We show that the innermost coma is sensitive to the nucleus shape as well as to the variations of local gas production rates. In general, spatial structures of the innermost coma are a result of interactions of gas flows sublimated from different surface regions.}, Author = {Skorov, {Yu. V. } and Markelov, {G. N.} and and Keller, {H. U.}}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 17:06:20 +0200}, Date-Modified = {2007-06-07 17:06:20 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {55-58}, Publisher = {ESA Publications}, Title = {Dust Production and Nucleus Evolution}, Year = {2007}} @inproceedings{Madsen:2007, Abstract = {We report on new observations of the motion of zodiacal dust using optical absorption line spectroscopy of zodiacal light. We have measured the change in the profile shape of the scattered solar Mg I 5184 line toward several lines of sight in the ecliptic plane as well as the ecliptic pole. The variation in line centroid and line width as a function of helio-ecliptic longitude show a clear prograde signature and suggest that significant fraction of the dust follows non-circular orbits that are not confined to the ecliptic plane. When combined with dynamical models, the data suggest that the zodiacal dust is largely cometary, rather than asteroidal, in origin.}, Author = {Madsen, {G.J. } and Reynolds, { R.J. } and Ipatov, {S.I.} and Kutyrev, {A.S.} and Mather, {J.C.} and and Moseley, {S.H.}}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 17:01:52 +0200}, Date-Modified = {2007-06-12 13:00:38 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {61-64}, Publisher = {ESA Publications}, Title = {New Oberservations and Models of the Kinematics of the Zodiacal Dust Cloud}, Year = {2007}} @inproceedings{Ootsubo:2007, Abstract = {We carried out mid-infrared observations (multi-band imaging and N-band spectroscopy) of the Deep Impact collision with a Jupiter family comet 9P/Tempel 1 using the Cooled Mid-Infrared Camera and Spectrometer (COMICS) on the 8.2 m Subaru Telescope. Imaging observations reveal that a large fan-shaped impact ejecta was extended to the south-west direction from the nucleus, which is close to the surface normal vector of the impact point of the comet. The N-band spectrum (8--13 microns; R approx. 250) of the dust ejecta from the comet nucleus 3.5 hours after the Deep Impact event shows a strong crystalline olivine feature. We also made spectroscopic observations 24 hours before and 28 hours after the impact. These spectra have no evident silicate feature in the 10 micron region. We present several spectra at the different positions from the comet nucleus, and report the preliminary result of our fitting analysis using a thermal emission model of cometary dust grains. The mass ratio of crystalline to amorphous silicate grains for the dust ejected from the subsurface of 9P/Tempel 1 is much larger than the dust in the coma of other Jupiter family comet, such as 78P/Gehrels 2, but similar to Oort cloud comets, such as Hale-Bopp.}, Author = {Ootsubo, Takafumi and Sugita, Seiji and Kadono, Toshihiko and Honda, Mitsuhiko and Sakon, Itsuki and Kawakita, Hideyo and Watanabe, Jun-ich and Subaru/COMICS team}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 16:58:36 +0200}, Date-Modified = {2007-06-12 12:57:24 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {45-49}, Publisher = {ESA Publications}, Title = {Mid-Infrared Observation of the Dust Plume from {Comet 9P/Tempel 1} Generated by the {Deep Impact} Collision Using {Subaru/Comics}}, Year = {2007}} @inproceedings{Green:2007, Abstract = {During its passage through the coma of comet 81P/Wild 2 in January 2004 to collect dust particles for return to the Earth, instruments on Stardust made extensive measurements of the dust coma environment. The inner coma was characterized by many narrow jets, imaged by the Navigation Camera. Dust fluxes measured by the Dust Flux Monitor Instrument (DFMI) revealed a highly non-uniform spatial distribution, with short duration bursts of impacts implying localized spatial density changes of orders of magnitude on scales of less than a km as well as a second period of high activity ~4000 km from the nucleus where almost 80% of the detected impacts occurred. The Cometary and Interstellar Dust Analyzer (CIDA) obtained 29 dust impact mass spectra near closest approach. The spacecraft Attitude Control System (ACS) detected one event attributable to a large particle impact.}, Author = {Green, {S.F.} and McBride, N. and Colwell, {M.T.S.H. } and McDonnell, {J.A.M. } and Tuzzolino, {A.J.} and Economou, {T.E. } and Clark, {B.C.} and Sekanina, Z. and Tsou, {P.} and Brownlee, {D.E.}}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 16:45:17 +0200}, Date-Modified = {2007-06-12 12:55:46 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {35-44}, Publisher = {ESA Publications}, Title = {Stardust {Wild 2} Dust Measurements}, Year = {2007}} @inproceedings{Agarwal:2007, Abstract = {We report on the results of nearly 10 hours of integration of the dust trail and neckline of comet 67P/Churyumov- Gerasimenko (67P henceforth) using the Wide Field Imager at the ESO/MPG 2.2m telescope in La Silla. The data was obtained in April 2004 when the comet was at a heliocentric distance of 4.7 AU outbound. 67P is the target of the Rosetta spacecraft of the European Space Agency. Studying the trail and neckline can contribute to the quantification of mm-sized dust grains released by the comet. We describe the data reduction and derive lower limits for the surface brightness. In the processed image, the angular separation of trail and neckline is resolved. We do not detect a coma of small, recently emitted grains.}, Author = {Agarwal, Jessica and Boehnhardt, Hermann and Gruen, Eberhard}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 16:25:20 +0200}, Date-Modified = {2007-06-12 12:59:02 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {51-54}, Publisher = {ESA Publications}, Title = {Imaging the Dust Trail and Neckline of {67P/Churyumov-Gerasimenko}}, Year = {2007}} @inproceedings{Miura:2007, Abstract = {21P/Giacobini-Zinner is known as the parent comet of the Draconids, which made spectacular showers in 1933 and 1946. Hence 21P/Giacobini-Zinner is likely to have a dense dust trail. We conducted survey observations of the faint scattered light of 21P/Giacobini-Zinner on 2004 May 23 using the 2.2 m telescope of the University of Hawaii at Mauna Kea, and using the 105 cm Schmidt telescope at Kiso during 2005 May 2--14. We confirm that the typical size of the particles is 10~100 microns for 21P/Giacobini-Zinner and that 21P/Giacobini-Zinner doesn't have a dust trail of particles with a size of >1mm, greater than the detection limit of these observations, a result which shows that there is a significant gap in number density between meteoric dust trails and visible-infrared dust trails.}, Author = {Miura, Naoya and Ishiguro, Masateru and Sarugaku, Yuki and Usui, Fumihiko and Ueno, Munetaka}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 16:22:25 +0200}, Date-Modified = {2007-06-12 12:51:41 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {23-26}, Publisher = {ESA Publications}, Title = {A {CCD} Search for the Dust Trail of the {Draconid} Parent Comet {21P/Giacobini-Zinner}}, Year = {2007}} @inproceedings{Baggaley:2007, Abstract = {Interstellar dust (ISD) particles larger than about 1 micron (4 times 10^{-12} g) can penetrate freely into the inner solar system where, in the event of Earth impact, they can be accessed by the detection of the plasma and excited species created when the particles ablate in the Earth's atmosphere. The ablation process and current experimental techniques available for plasma and excitation detection mean that the particle size regime accessible from ground-based sensing is much larger than can be sampled from space-craft. However, the much larger collecting area provided by the atmosphere in the meteor mode results in comparable detection statistics for the two techniques. The value of this Earth based probing of interstellar dust lies in the ability to provide quality dynamical characteristics: the velocity information allows the recovery of the ISD pre-solar system encounter trajectories. This paper provides an overview of experimental techniques and the attempts to map the galactic sources of interstellar dust.}, Author = {Baggaley, {W.J.} and Marsh, {S.H.} and Close, S.}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 16:16:24 +0200}, Date-Modified = {2007-06-12 12:55:01 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {27-32}, Publisher = {ESA Publications}, Title = {Interstellar Meteors}, Year = {2007}} @inproceedings{Jenn:2007b, Abstract = {The hypervelocity entry of a sample return capsule on its way back from interplanetary space acts as an artificial meteor, with flow conditions similar to natural m-sized meteoroids. Unlike natural fireballs, a sample return capsule arrives at a known time and its shock emissions and ablation can be studied without the confusion of fragmentation and the obscuring emissions from ablated meteoric metals. The entry of the Stardust Sample Return Capsule (SRC) on Sunday January 15, 2006, was also a real-life test of key risk drivers for future Thermal Protection System (TPS) design, by measuring the amount of radiative heat flux and the ablation response of the TPS. This paper presents results from the calculations made to predict the expected meteoric emissions for the Stardust SRC entry and re-evaluates the surface temperature measurements obtained during a prior mission that observed the Genesis sample return. }, Author = {Jenniskens, P. and Kontinos, D. and Jordan, D. and Wright, M. and Olejniczak, J. and Raiche, G. and Wercinski, P. and Desai, {P. N.} and Taylor, {M. J.}, Stenbaek-Nielsen, {H. C. } and McHarg, {M. G. } and Abe, S. and Rairden, {R.L.} and Albers, J. and Winter, M. and, Harms, F. and Wolf, J. and ReVelle, {D.O. } and Gural, P. and Dantowitz R. and Rietmeijer, F. and Hladiuk, D. and Hildebrand, {A.R.}}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 16:04:40 +0200}, Date-Modified = {2007-06-07 16:41:38 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {7-10}, Publisher = {ESA Publications}, Title = {Preparing for the Meteoritic Return of {Stardust}}, Year = {2007}} @inproceedings{Jenn:2007a, Abstract = {Even though comets have been observed to break, there was no strong evidence until now that the meteoroids generated in these discrete and relatively rare events accounted for meteoroid streams detected as meteor showers on Earth. That has changed now minor planet 2003 EH1 and other such inactive (dormant) and weakly active comet nuclei are found still intimately associated with known meteoroid streams. More and more of such minor bodies are now identified. The meteor showers that are likely from the fragmentation of comets rather than from Whipple-type ejection by water vapor drag now include the Quadrantids, Daytime Arietids, delta-Aquariids, Capricornids, Taurids, Andromedids, Phoenicids, and Geminids, representing most of our strongest annual showers. This makes the breakup of dormant comet nuclei an important mechanism to replenish the zodiacal cloud. }, Author = {Jenniskens, Peter}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 14:23:31 +0200}, Date-Modified = {2007-06-07 14:23:31 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {3-6}, Publisher = {ESA Publications}, Title = {Meteor Showers from Broken Comets}, Year = {2007}} @inproceedings{Campbell:2007, Abstract = {Interplanetary particles larger than 10^{13} kg (3 microns) create significant light and ionization when colliding with the atmosphere of the Earth. This provides a way to study the higher mass component of the interplanetary dust complex, since the collecting area of the Earth's atmosphere is large and the meteors resulting from these impacts are easily recorded with optical cameras and radars. Particles in this size range have too low a flux relative to the size scale of in-situ dust detectors to be captured in dust detectors, and are difficult to detect remotely. Meteoroids are generally divided into two broad categories: shower meteors, which appear to come from narrow radiants as seen from the surface of the Earth and occur over a limited range of the Earth's orbit every year, and sporadic meteors, which are always active and come from diffuse radiants. Recent advances in observing technology, particularly in automated data analysis, have produced great advances in the understanding of meteoroid distribution at 1 AU.}, Author = {Campbell-Brown, M.}, Booktitle = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Date-Added = {2007-06-07 14:02:40 +0200}, Date-Modified = {2007-06-12 12:47:47 +0200}, Editor = {Krueger, H. and Graps, A.}, Month = {January}, Number = {SP-643}, Organization = {European Space Agency}, Pages = {11-21}, Publisher = {ESA Publications}, Title = {The Meteoroid Environment: Shower and Sporadic Meteors}, Year = {2007}} @proceedings{dustbook07, Date-Added = {2007-05-31 15:28:22 +0200}, Date-Modified = {2007-05-31 15:32:54 +0200}, Editor = {Kr\"uger, H. and Graps, A.}, Month = {January}, Organization = {European Space Agency}, Publisher = {ESA Publications}, Title = {Dust in Planetary Systems (Workshop, September 26-30 2005, Kauai, Hawaii)}, Volume = {SP-643}, Year = {2007}}