羟氨苄青霉素引起大疱性类天疱疮样疹

[1] The HiRISE camera features a 0.5 m diameter primary mirror, 12 m effective focal length, and a focal plane system that can acquire images containing up to 28 Gb (gigabits) of data in as little as 6 seconds. HiRISE will provide detailed images (0.25 to 1.3 m/pixel) covering ∼1% of the Martian surface during the 2-year Primary Science Phase (PSP) beginning November 2006. Most images will include color data covering 20% of the potential field of view. A top priority is to acquire ∼1000 stereo pairs and apply precision geometric corrections to enable topographic measurements to better than 25 cm vertical precision. We expect to return more than 12 Tb of HiRISE data during the 2-year PSP, and use pixel binning, conversion from 14 to 8 bit values, and a lossless compression system to increase coverage. HiRISE images are acquired via 14 CCD detectors, each with 2 output channels, and with multiple choices for pixel binning and number of Time Delay and Integration lines. HiRISE will support Mars exploration by locating and characterizing past, present, and future landing sites, unsuccessful landing sites, and past and potentially future rover traverses. We will investigate cratering, volcanism, tectonism, hydrology, sedimentary processes, stratigraphy, aeolian processes, mass wasting, landscape evolution, seasonal processes, climate change, spectrophotometry, glacial and periglacial processes, polar geology, and regolith properties. An Internet Web site (HiWeb) will enable anyone in the world to suggest HiRISE targets on Mars and to easily locate, view, and download HiRISE data products.

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Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment (HiRISE)

Global mineralogical mapping of Mars by the Observatoire pour la Mineralogie, l'Eau, les Glaces et l'Activite (OMEGA) instrument on the European Space Agency's Mars Express spacecraft provides new information on Mars' geological and climatic history. Phyllosilicates formed by aqueous alteration very early in the planet's history (the "phyllocian" era) are found in the oldest terrains; sulfates were formed in a second era (the "theiikian" era) in an acidic environment. Beginning about 3.5 billion years ago, the last era (the "siderikian") is dominated by the formation of anhydrous ferric oxides in a slow superficial weathering, without liquid water playing a major role across the planet.

https://science.sciencemag.org/content/sci/312/5772/400.full.pdf

Global Mineralogical and Aqueous Mars History Derived from OMEGA/Mars Express Data

The transport of sand and dust by wind is a potent erosional force, creates sand dunes and ripples, and loads the atmosphere with suspended dust aerosols This article presents an extensive review of the physics of wind-blown sand and dust on Earth and Mars Specifically, we review the physics of aeolian saltation, the formation and development of sand dunes and ripples, the physics of dust aerosol emission, the weather phenomena that trigger dust storms, and the lifting of dust by dust devils and other small-scale vortices We also discuss the physics of wind-blown sand and dune formation on Venus and Titan

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The physics of wind-blown sand and dust

[1] The Context Camera (CTX) on the Mars Reconnaissance Orbiter (MRO) is a Facility Instrument (i.e., government-furnished equipment operated by a science team not responsible for design and fabrication) designed, built, and operated by Malin Space Science Systems and the MRO Mars Color Imager team (MARCI). CTX will (1) provide context images for data acquired by other MRO instruments, (2) observe features of interest to NASA's Mars Exploration Program (e.g., candidate landing sites), and (3) conduct a scientific investigation, led by the MARCI team, of geologic, geomorphic, and meteorological processes on Mars. CTX consists of a digital electronics assembly; a 350 mm f/3.25 Schmidt-type telescope of catadioptric optical design with a 5.7° field of view, providing a ∼30-km-wide swath from ∼290 km altitude; and a 5000-element CCD with a band pass of 500–700 nm and 7 μm pixels, giving ∼6 m/pixel spatial resolution from MRO's nearly circular, nearly polar mapping orbit. Raw data are transferred to the MRO spacecraft flight computer for processing (e.g., data compression) before transmission to Earth. The ground data system and operations are based on 9 years of Mars Global Surveyor Mars Orbiter Camera on-orbit experience. CTX has been allocated 12% of the total MRO data return, or about ≥3 terabits for the nominal mission. This data volume would cover ∼9% of Mars at 6 m/pixel, but overlapping images (for stereo, mosaics, and observation of changes and meteorological events) will reduce this area. CTX acquired its first (instrument checkout) images of Mars on 24 March 2006.

https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2006JE002808

Context Camera Investigation on board the Mars Reconnaissance Orbiter

Grant 1 , R P Irwin, III 1 , J P Grotzinger 2 , R E Milliken 2 , L L Tornabene 3 , A S McEwen 3 , C M Weitz 4 , S W Squyres 5 , T D Glotch 6 , B J Thomson 6 , and the HiRISE Team 1 Smithsonian Institution, National Air and Space Museum, Center for Earth and Planetary Studies, 6 th at Independence SW, Washington, DC, 20013, grantj@siedu, 2 Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, 91125, 3 Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, 85721, 4 Planetary Science Institute, 1700 E Fort Lowell, Tucson, AZ, 85719, 5 Department of Astronomy, Space Sciences Building, Cornell University, Ithaca, NY 14853, 6 Jet Propulsion Lab, Caltech, 4800 Oak Grove Dr, Pasadena, CA 91109

/pdf/impact-and-aqueous-stratigraphy-in-holden-crater-as-revealed-18a4k9czu3.pdf

Impact and Aqueous Stratigraphy in Holden Crater as Revealed by HiRISE

Abstract Downward-looking spectra of the martian surface from the Miniature Thermal Emission spectrometer (Mini-TES), onboard each of the two Mars Exploration Rovers, are modeled in order to retrieve surface and near-surface atmospheric temperatures. By fitting the observed radiance in the vicinity of the 15-μm CO 2 absorption feature, the surface temperature and the near-surface atmospheric temperature, approximately 1.1 m above the surface, are determined. The temperatures from the first 180 sols (martian days) of each surface mission are used to characterize the diurnal dependence of temperatures. The near-surface atmospheric temperatures are consistently 20 K cooler than the surface temperatures in the warmest part of each sol, which is 1300–1400 LTST (local true solar time) depending on the location. Seasonal cooling trends are seen in the data by displaying the temperatures as a function of sol. Long ground stares, 8.5 min in duration, show as much as 8 K fluctuation in the near-surface atmospheric temperatures during the early afternoon hours when the near-surface atmosphere is unstable.

Surface and Near-Surface Atmospheric Temperatures for the Mars Exploration Rover Landing Sites

Searching for Active Dust Devils in Gusev Crater from Orbit by Mars Express and the Ground from Spirit

A Physical Interpretation of the SL-9 Impacts Observed from Palomar

In 1997, the COmet Nucleus TOUR (CONTOUR) was selected by NASA for a new start as part of the Discovery line. In this paper, we review the status of the mission, the mission timeline and the instruments to be flown. Detail is given of the science goals and how they are to be accomplished.

S. W. Squyres

Papers

Impact and Aqueous Stratigraphy in Holden Crater as Revealed by HiRISE

Surface and Near-Surface Atmospheric Temperatures for the Mars Exploration Rover Landing Sites

Searching for Active Dust Devils in Gusev Crater from Orbit by Mars Express and the Ground from Spirit

A Physical Interpretation of the SL-9 Impacts Observed from Palomar

The Comet Nucleus Tour (Contour)