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535 results for “DUST”
VEGA2 DUST PARTICLE COUNTER MASS ANALYSER DATA V1.0
Encounter data for Vega-2 consisted of two files: DSFAST27 and Dvg2CLN1. The data were submitted by the Univ of Chicago group along with hard copy versions of the operating manual and a preprint of the results.
STARDUST DUST COLLECTOR GEOMETRY V1.0
Data set describing the geometry and orientations of the spacecraft and the collector plate during the two interstellar dust collection phases and the Wild 2 encounter.
STARDUST C/E/L DUST FLUX MONITOR INSTRUMENT-2-EDR-V1.0
Data collected by the Dust Flux Monitor Instrument (DFMI) of the Stardust satellite, taken during the early cruise phase of the mission. These data were determined by peer review to be of no scientific use.
GALILEO DUST DETECTION SYSTEM V4.0
This data set contains the data from the Galileo dust detector system (GDDS) from start of mission through the end of mission. Included are the dust impact data, noise data, laboratory calibration data, and location and orientation of the spacecraft and instrument.
VEGA2 PUMA DUST MASS SPECTROMETER DATA V1.0
The data from IKI for this dataset were received as two binary files containing data taken in all instrument modes. These files were split into separate files for each mode, preserving the original ordering of the spectra within the table. Spectra in each mode table are arranged chronologically, using TIME of the spectrum on the BLISI clock, in sec.
GIOTTO EXTENDED MISSION DUST IMPACT DETECTOR V1.0
This dataset contains the results obtained from the Dust Impact Detection System (DIDSY) flown aboard the GIOTTO spacecraft during its extended mission to Comet P/Grigg-Skjellerup in 1992. The measurements and analysis of the three impacts detected during close approach are contained in text files. Calibration tables for the sensors are included in this dataset. These data have not been reviewed or formally archived with the PDS.
ULYSSES DUST DETECTION SYSTEM V3.1
This data set contains the data from the Ulysses dust detector system (UDDS) from start of mission through the end of mission, 1990-2007. (As the dust detector was turned off after Nov. 30, 2007, this is the last date for which UDDS data is recorded.) Included are the dust impact data, noise data, laboratory calibration data, and location and orientation of the spacecraft and instrument.
ROSETTA-ORBITER DUST MIDAS 3 PRL SAMPLES V1.0
The Micro-Imaging Dust Analysis System (MIDAS) is an instrument on the ROSETTA Orbiter that will provide 3D images and statistical parameters of pristine cometary particles hitting the detector. This data set includes all data from the PRELANDING mission phase.
VEGA1 DUST MASS SPECTROMETER MODAL DATA V1.0
The data from MPI for this dataset were received as text files each containing spectra of a single instrument mode (there were several files for most modes). These spectra were reformatted into binary tables, and all spectra from each mode were combined into a single file. The original order of the spectra has been preserved. Spacecraft time, relative to switch-on of the instrument is specified as 1 clock tick = 0.11852 seconds. The exact equation is:
VEGA1 DUST PARTICLE COUNTER MASS ANALYSER DATA V1.0
Encounter Data for Vega-1 included two files: DSFAST17 and Dvega101. These files were submitted by the Univ of Chicago group with hard copy versions of the operating manual and a preprint of results. The following explanation of the contents of the two files is below.
VEGA2 PUMA DUST MASS SPECTROMETER MODAL DATA V1.0
The data from MPI for this dataset were received as text files each containing spectra of a single instrument mode (there were several files for most modes). These spectra were reformatted into binary tables, and all spectra from each mode were combined into a single file. The original order of the spectra has been preserved. Spacecraft time, relative to switch-on of the instrument is specified as 1 clock tick = 0.11852 seconds. The exact equation is:
ULYSSES DUST DETECTION SYSTEM V2.0
Dataset Overview ================ This data set contains information on dust the dust environment in interplanetary space within the inner solar system, between Jupiter and the Sun, and at high polar latitudes of the Sun. Both interplanetary and interstellar dust particles have been detected. This information is collected with a dust impact experiment, from which may be inferred direction of motion, mass, velocity and charge (see ULYDINST.CAT). The data presented in this dataset include instrumental readouts, inferred metadata, calibration information and a calendar of events. Specifically:
Experimental study on the variation of atmospheric magnetic field intensity in dust evets, haze events, rainy days, snowy days and thunderstorms
<p>The simultaneous measurement of vertical magnetic field intensity (<em>B<sub>z</sub></em>), three-dimensional electric field (<em>E<sub>x</sub></em>, <em>E<sub>y</sub></em>, <em>E<sub>z</sub></em>), ambient temperature (<em>T</em>), ambient relative humidity (<em>RH</em>), mass concentration (<em>PM</em><sub>2.5</sub> and <em>PM</em><sub>10</sub>) and three-dimensional wind speed (<em>U<sub>x</sub></em>, <em>U<sub>y</sub></em>, <em>U<sub>z</sub></em>) were conducted at Lanzhou, China and Xi'an, China during haze events, dust events, snowfall events, rainfall events and thunderstorms. The hourly mean value and hourly standard deviation of d<em>B<sub>z</sub>/</em>d<em>t</em> were used to evaluate the disturbance level of atmospheric magnetic field (AMF) during these weather. The hourly mean value of d<em>B<sub>z</sub></em>/d<em>t</em> in dusty days, rainy days, snowy days and thunderstorms varies evidently compared to that in fair weather, which implies that these weather conditions will effectively affect the variation of AMF. Analysis of <em>E<sub>z</sub></em> and <em>U</em><em><sub>xy</sub></em> suggests that the movement of charged particles under the action of horizontal wind will change the average currents in atmosphere and induce a magnetic field, and this induced magnetic field will disturb the variation of AMF. Hence, the induced magnetic fields generated by the movement of charged particles should not be ignored in these complex weather conditions. The analysis of d<em>E<sub>xy</sub></em>/d<em>t</em> shows that the induced magnetic field generated by the change of the electric field can disturb the AMF as well. In addition, hourly standard deviations of d<em>B<sub>z</sub></em>/d<em>t</em> in haze event, snowfall event and thunderstorms are larger than that in fair weather, which means that these events can influence the fluctuation of AMF. The approximate circular motion of charged particles in the horizontal plane under turbulence was discussed to be the main reason for the intense fluctuation of AMF in haze and snowfall events, but the large fluctuation of AMF in thunderstorms maybe attributed to the transient changes of space electric field under lightning.</p>
Supplementary Material for Munaretto et al. Multiband photometry of Martian Recurring Slope Lineae (RSL) and dust-removed features at Horowitz crater, Mars from TGO/CaSSIS color observations
<p>Supplementary Material for Munaretto et al. Multiband photometry of Martian Recurring Slope Lineae (RSL) and dust-removed features at Horowitz crater, Mars from TGO/CaSSIS color observations. </p> <p>See the included README file for further information.</p>
Ruff PDART 2014 Mini-TES Mirror-dust-corrected Emissivity Bundle
Mars Exploration Rover Mini-TES Mirror-dust-corrected Emissivity by Steve Ruff, PDART 2014
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