Dec
6
Micron-Resolution Particle Image Velocimetry
December 6, 2005 | Comments Off
p class=”abstract”div class=”Abstract”During the past five years, significant progress has been made in the development and application of micron-resolution Particle
Image Velocimetry (µPIV). Developments of the technique have extended typical spatial resolutions of PIV from order 1-mm to
order 1-µm. These advances have been obtained as a result of novel improvements in instrument hardware and post processing
software.
div class=”AbstractPara”
div class=”"Theories describing the limits of in-plane and out-of-plane spatial resolution are presented. The basis of the theory for
in-plane spatial resolution extends the original work of Adrian Yao (1985). The theory for out-of-plane spatial resolution
closely follows the recent work of Olsen Adrian (2000).
/div
/div
div class=”AbstractPara”
div class=”"The desire for high spatial resolution dictates that the flow tracing particles typically range between 200 – 700 nm in diameter.
The effect of Brownian forces on particle motion is discussed in detail. Guidelines are given to determine optimal particle
size and to estimate particle flow following fidelity.
/div
/div
div class=”AbstractPara”
div class=”"Advances in post processing algorithms provide improvements in velocity accuracy and spatial resolution. The correlation-averaging
algorithm increases the effective particle concentration, while maintaining sufficiently low particle concentration in the
working fluid. Central difference interrogation provides second order accurate estimates of velocity, which becomes important
in regions containing high spatial variations in velocity. These post-processing techniques are particularly useful in challenging
micro length scales, and can also be extended to macroscopic flows.
/div
/div
div class=”AbstractPara”
div class=”"The utility of µPIV is demonstrated by applying it to flows in microchannels, micronozzles, BioMEMS, and flow around cells.
While the technique was initially developed for microscale velocity measurements, it has been extended to measure wall positions
with tens of nanometers resolution, the deformation of hydrogels, micro-particle thermometry, and infrared-PIV.
/div
/div
/div/pul
lispan class=”labelName”Content Type /spanspan class=”labelValue”Book Chapter/span/liliDOI 10.1007/3-540-26449-3_2/lilispan class=”labelName”Authors/spanul
liS.T. Wereley, Purdue University School of Mechanical Engineering West Lafayette IN 47907-1288/liliC.D. Meinhart, University of California, Santa Barbara Department of Mechanical and Environmental Engineering Santa Barbara CA 93106-5070/li
/ul/li
/ulul class=”parents”
ul class=”details”
lispan class=”header labelName”Book /spanspan class=”labelValue”a href=”http://www.springerlink.com/content/q65wu0/”Microscale Diagnostic Techniques/a/span/lilispan class=”labelName”DOI /spanspan class=”labelValue”10.1007/b137604/span/lilispan class=”labelName”Online ISBN /spanspan class=”labelValue”978-3-540-26449-1/span/lilispan class=”labelName”Print ISBN /spanspan class=”labelValue”978-3-540-23099-1/span/li
/ul
/ul
Dec
6
Linux Load Average—Take a Load Off!
December 6, 2005 | Comments Off
p class=”abstract”Linux Load Average—Take a Load Off!/pul
lispan class=”labelName”Content Type /spanspan class=”labelValue”Book Chapter/span/liliDOI 10.1007/3-540-26860-X_4/li
/ulul class=”parents”
ul class=”details”
lispan class=”header labelName”Book /spanspan class=”labelValue”a href=”http://www.springerlink.com/content/xv8666/”Analyzing Computer System Performance with Perl::PDQ/a/span/lilispan class=”labelName”DOI /spanspan class=”labelValue”10.1007/b94248/span/lilispan class=”labelName”Online ISBN /spanspan class=”labelValue”978-3-540-26860-4/span/lilispan class=”labelName”Print ISBN /spanspan class=”labelValue”978-3-540-20865-5/span/li
/ulul class=”details”
lispan class=”header labelName”Book Part /spanspan class=”labelValue”a href=”http://www.springerlink.com/content/u043420014m5/”Part I/a/span/li
/ul
/ul
Dec
6
Applications of System Design
December 6, 2005 | Comments Off
p class=”abstract”Applications of System Design/pul
lispan class=”labelName”Content Type /spanspan class=”labelValue”Book Chapter/span/liliDOI 10.1007/0-387-24162-0_6/li
/ulul class=”parents”
ul class=”details”
lispan class=”header labelName”Book /spanspan class=”labelValue”a href=”http://www.springerlink.com/content/pr40j1/”RF System Design of Transceivers for Wireless Communications/a/span/lilispan class=”labelName”DOI /spanspan class=”labelValue”10.1007/b104642/span/lilispan class=”labelName”Online ISBN /spanspan class=”labelValue”978-0-387-24162-3/span/lilispan class=”labelName”Print ISBN /spanspan class=”labelValue”978-0-387-24161-6/span/li
/ul
/ul
Dec
6
Access Services
December 6, 2005 | Comments Off
p class=”abstract”Access Services/pul
lispan class=”labelName”Content Type /spanspan class=”labelValue”Book Chapter/span/liliDOI 10.1007/3-540-27514-2_5/li
/ulul class=”parents”
ul class=”details”
lispan class=”header labelName”Book /spanspan class=”labelValue”a href=”http://www.springerlink.com/content/mgku52/”Enterprise Knowledge Infrastructures/a/span/lilispan class=”labelName”DOI /spanspan class=”labelValue”10.1007/3-540-27514-2/span/lilispan class=”labelName”Online ISBN /spanspan class=”labelValue”978-3-540-27514-5/span/lilispan class=”labelName”Print ISBN /spanspan class=”labelValue”978-3-540-23915-4/span/li
/ul
/ul
Dec
6
Conclusion
December 6, 2005 | Comments Off
p class=”abstract”Conclusion/pul
lispan class=”labelName”Content Type /spanspan class=”labelValue”Book Chapter/span/liliDOI 10.1007/3-540-27514-2_6/li
/ulul class=”parents”
ul class=”details”
lispan class=”header labelName”Book /spanspan class=”labelValue”a href=”http://www.springerlink.com/content/mgku52/”Enterprise Knowledge Infrastructures/a/span/lilispan class=”labelName”DOI /spanspan class=”labelValue”10.1007/3-540-27514-2/span/lilispan class=”labelName”Online ISBN /spanspan class=”labelValue”978-3-540-27514-5/span/lilispan class=”labelName”Print ISBN /spanspan class=”labelValue”978-3-540-23915-4/span/li
/ul
/ul
Dec
6
Knowledge Services
December 6, 2005 | Comments Off
p class=”abstract”Knowledge Services/pul
lispan class=”labelName”Content Type /spanspan class=”labelValue”Book Chapter/span/liliDOI 10.1007/3-540-27514-2_4/li
/ulul class=”parents”
ul class=”details”
lispan class=”header labelName”Book /spanspan class=”labelValue”a href=”http://www.springerlink.com/content/mgku52/”Enterprise Knowledge Infrastructures/a/span/lilispan class=”labelName”DOI /spanspan class=”labelValue”10.1007/3-540-27514-2/span/lilispan class=”labelName”Online ISBN /spanspan class=”labelValue”978-3-540-27514-5/span/lilispan class=”labelName”Print ISBN /spanspan class=”labelValue”978-3-540-23915-4/span/li
/ul
/ul
Dec
6
Reference samples for analysis of gas impurities in aluminium and titanium alloys: Features of production, certification and usage to ensure traceability of results
December 6, 2005 | Comments Off
p class=”abstract”ParaThe current state of production, certification and use of standard samples of aluminium- and titanium-based alloys with specified contents of gas impurities is described. A list of the certified standard samples with a specified gas impurity content which are available in Russia is presented./Para/pul
lispan class=”labelName”Content Type /spanspan class=”labelValue”Book Chapter/span/liliDOI 10.1007/3-540-27093-0_32/lilispan class=”labelName”Authors/spanul
liV.P. Antipin, All Russia Institute for Light Alloys Bldg. 2 Gorbunova Street 121596 Moscow Russia/liliA.A. Grigorieva, All Russia Institute for Light Alloys Bldg. 2 Gorbunova Street 121596 Moscow Russia/li
/ul/li
/ulul class=”parents”
ul class=”details”
lispan class=”header labelName”Book /spanspan class=”labelValue”a href=”http://www.springerlink.com/content/l7p91r/”Traceability in Chemical Measurement/a/span/lilispan class=”labelName”DOI /spanspan class=”labelValue”10.1007/b138593/span/lilispan class=”labelName”Online ISBN /spanspan class=”labelValue”978-3-540-27093-5/span/lilispan class=”labelName”Print ISBN /spanspan class=”labelValue”978-3-540-43989-9/span/li
/ul
/ul
Dec
6
Exploring the Saturn System in the Thermal Infrared: The Composite Infrared Spectrometer
December 6, 2005 | Comments Off
p class=”abstract”ParaThe Composite Infrared Spectrometer (CIRS) is a remote-sensing Fourier Transform Spectrometer (FTS) on the Cassini orbiter that measures thermal radiation over two decades in wavenumber, from 10 to 1400 cmsup−1/sup (1 mm to 7 iµ/im), with a spectral resolution that can be set from 0.5 to 15.5 cmsup−1/sup. The far infrared portion of the spectrum (10–600 cmsup−1/sup) is measured with a polarizing interferometer having thermopile detectors with a common 4-mrad field of view (FOV). The middle infrared portion is measured with a traditional Michelson interferometer having two focal planes (600–1100 cmsup−1/sup, 1100–1400 cmsup−1/sup). Each focal plane is composed of a 1 × 10 array of HgCdTe detectors, each detector having a 0.3-mrad FOV. CIRS observations will provide three-dimensional maps of temperature, gas composition, and aerosols/condensates of the atmospheres of Titan and Saturn with good vertical and horizontal resolution, from deep in their tropospheres to high in their mesospheres. CIRS’s ability to observe atmospheres in the limb-viewing mode (in addition to nadir) offers the opportunity to provide accurate and highly resolved vertical profiles of these atmospheric variables. The ability to observe with high-spectral resolution should facilitate the identification of new constituents. CIRS will also map the thermal and compositional properties of the surfaces of Saturn’s icy satellites. It will similarly map Saturn’s rings, characterizing their dynamical and spatial structure and constraining theories of their formation and evolution. The combination of broad spectral range, programmable spectral resolution, the small detector fields of view, and an orbiting spacecraft platform will allow CIRS to observe the Saturnian system in the thermal infrared at a level of detail not previously achieved./Para/pul
lispan class=”labelName”Content Type /spanspan class=”labelValue”Book Chapter/span/liliDOI 10.1007/1-4020-3874-7_4/lilispan class=”labelName”Authors/spanul
liF. Flasar, Goddard Space Flight Center Greenbelt MD 20771 USA/liliV. Kunde, University of Maryland College Park MD 20742 USA/liliM. Abbas, Marshall Space Flight Center Huntsville AL 35812 USA/liliR. Achterberg, Science Systems and Applications Inc. Lanham MD 20706 USA/liliP. Ade, University of Cardiff CF24 3YB UK/liliA. Barucci, Observatoire de Paris-Meudon F92195 Meudon Cedex France/liliB. Bézard, Oxford University OX1 3PU UK/liliG. Bjoraker, Goddard Space Flight Center Greenbelt MD 20771 USA/liliJ. Brasunas, Goddard Space Flight Center Greenbelt MD 20771 USA/liliS. Calcutt, Oxford University OX1 3PU UK/liliR. Carlson, Science Systems and Applications Inc. Lanham MD 20706 USA/liliC. Césarsky, European Southern Observatory 85748 Garching bei Muenchen Germany/liliB.J. Conrath, Cornell University Ithaca NY 14853 USA/liliA. Coradini, lstituto di Astrofisica Spaziale Rome I-00133 Italy/liliR. Courtin, Observatoire de Paris-Meudon F92195 Meudon Cedex France/liliA. Coustenis, Observatoire de Paris-Meudon F92195 Meudon Cedex France/liliS. Edberg, Jet Propulsion Laboratory Pasadena CA 91109 USA/liliS. Edgington, Jet Propulsion Laboratory Pasadena CA 91109 USA/liliC. Ferrari, CEA/Service d’Astrophysique 91191 Gif-sur-Yvette Cedex France/liliT. Fouchet, Observatoire de Paris-Meudon F92195 Meudon Cedex France/liliD. Gautier, Observatoire de Paris-Meudon F92195 Meudon Cedex France/liliP. Gierasch, Cornell University Ithaca NY 14853 USA/liliK. Grossman, Gesamthochschule Wuppertal 5600 Wuppertal 1 Germany/liliP. Irwin, Oxford University OX1 3PU UK/liliD. Jennings, Goddard Space Flight Center Greenbelt MD 20771 USA/liliE. Lellouch, Observatoire de Paris-Meudon F92195 Meudon Cedex France/liliA. Mamoutkine, Science Systems and Applications Inc. Lanham MD 20706 USA/liliA. Marten, Observatoire de Paris-Meudon F92195 Meudon Cedex France/liliJ. Meyer, CEA/Service d’Astrophysique 91191 Gif-sur-Yvette Cedex France/liliC. Nixon, University of Maryland College Park MD 20742 USA/liliG. Orton, Jet Propulsion Laboratory Pasadena CA 91109 USA/liliT. Owen, University of Hawaii Honolulu HI 96822 USA/liliJ. Pearl, Goddard Space Flight Center Greenbelt MD 20771 USA/liliR. Prangé, Observatoire de Paris-Meudon F92195 Meudon Cedex France/liliF. Raulin, Université de Paris 7 12 94010 Creteil Cedex France/liliP. Read, Oxford University OX1 3PU UK/liliP. Romani, Goddard Space Flight Center Greenbelt MD 20771 USA/liliR. Samuelson, University of Maryland College Park MD 20742 USA/liliM. Segura, QSS Group, Inc Lanham MD 20706 USA/liliM. Showalter, Stanford University Stanford CA 94305 USA/liliA. Simon-Miller, Goddard Space Flight Center Greenbelt MD 20771 USA/liliM. Smith, Goddard Space Flight Center Greenbelt MD 20771 USA/liliJ. Spencer, Southwest Research Institute Boulder CO 80302 USA/liliL. Spilker, Jet Propulsion Laboratory Pasadena CA 91109 USA/liliF. Taylor, Oxford University OX1 3PU UK/li
/ul/li
/ulul class=”parents”
ul class=”details”
lispan class=”header labelName”Book /spanspan class=”labelValue”a href=”http://www.springerlink.com/content/n482nr/”The Cassini-Huygens Mission/a/span/lilispan class=”labelName”DOI /spanspan class=”labelValue”10.1007/1-4020-3874-7/span/lilispan class=”labelName”Online ISBN /spanspan class=”labelValue”978-1-4020-3874-7/span/lilispan class=”labelName”Print ISBN /spanspan class=”labelValue”978-1-4020-3147-2/span/li
/ul
/ul
Dec
6
Cassini Imaging Science: Instrument Characteristics and Anticipated Scientific Investigations at Saturn
December 6, 2005 | Comments Off
p class=”abstract”The Cassini Imaging Science Subsystem (ISS) is the highest-resolution two-dimensional imaging device on the Cassini Orbiter and has been designed for investigations of the bodies and phenomena found within the Saturnian planetary system. It consists of two framing cameras: a narrow angle, reflecting telescope with a 2-m focal length and a square field of view (FOV) 0.35° across, and a wide-angle refractor with a 0.2-m focal length and a FOV 3.5° across. At the heart of each camera is a charged coupled device (CCD) detector consisting of a 1024 square array of pixels, each 12 iµ/i on a side. The data system allows many options for data collection, including choices for on-chip summing, rapid imaging and data compression. Each camera is outfitted with a large number of spectral filters which, taken together, span the electromagnetic spectrum from 200 to 1100 nm. These were chosen to address a multitude of Saturn-system scientific objectives: sounding the three-dimensional cloud structure and meteorology of the Saturn and Titan atmospheres, capturing lightning on both bodies, imaging the surfaces of Saturn’s many icy satellites, determining the structure of its enormous ring system, searching for previously undiscovered Saturnian moons (within and exterior to the rings), peering through the hazy Titan atmosphere to its yet-unexplored surface, and in general searching for temporal variability throughout the system on a variety of time scales. The ISS is also the optical navigation instrument for the Cassini mission. We describe here the capabilities and characteristics of the Cassini ISS, determined from both ground calibration data and in-flight data taken during cruise, and the Saturn-system investigations that will be conducted with it. At the time of writing, Cassini is approaching Saturn and the images returned to Earth thus far are both breathtaking and promising./pul
lispan class=”labelName”Content Type /spanspan class=”labelValue”Book Chapter/span/liliDOI 10.1007/1-4020-3874-7_6/lilispan class=”labelName”Authors/spanul
liCarolyn Porco/liliRobert West, CICLOPS/Space Science Institute Boulder CO USA/liliSteven Squyres, Jet Propulsion Laboratory Pasadena CA USA/liliAlfred McEwen, Cornell University Ithaca New York USA/liliPeter Thomas, Jet Propulsion Laboratory Pasadena CA USA/liliCarl Murray, University of Arizona Tucson AZ USA/liliAnthony Delgenio, Queen Mary, University of London London England/liliAndrew Ingersoll, NASA Goddard Institute for Space Studies New York New York USA/liliTorrence Johnson, CICLOPS/Space Science Institute Boulder CO USA/liliGerhard Neukum, California Institute of Technology Pasadena CA USA/liliJoseph Veverka, Jet Propulsion Laboratory Pasadena CA USA/liliLuke Dones, Freie Universität Berlin Germany/liliAndre Brahic, Southwest Research Institute Boulder CO USA/liliJoseph Burns, Jet Propulsion Laboratory Pasadena CA USA/liliVance Haemmerle, CICLOPS/Space Science Institute Boulder CO USA/liliBenjamin Knowles/liliDouglas Dawson, Cornell University Ithaca New York USA/liliThomas Roatsch, Université Paris 7-Denis Diderot Paris France/liliKevin Beurle, University of Arizona Tucson AZ USA/liliWilliam Owen, CICLOPS/Space Science Institute Boulder CO USA/li
/ul/li
/ulul class=”parents”
ul class=”details”
lispan class=”header labelName”Book /spanspan class=”labelValue”a href=”http://www.springerlink.com/content/n482nr/”The Cassini-Huygens Mission/a/span/lilispan class=”labelName”DOI /spanspan class=”labelValue”10.1007/1-4020-3874-7/span/lilispan class=”labelName”Online ISBN /spanspan class=”labelValue”978-1-4020-3874-7/span/lilispan class=”labelName”Print ISBN /spanspan class=”labelValue”978-1-4020-3147-2/span/li
/ul
/ul
Dec
6
Cassini Radio Science
December 6, 2005 | Comments Off
p class=”abstract”ParaCassini radio science investigations will be conducted both during the cruise (gravitational wave and conjunction experiments) and the Saturnian tour of the mission (atmospheric and ionospheric occultations, ring occultations, determinations of masses and gravity fields). New technologies in the construction of the instrument, which consists of a portion on-board the spacecraft and another portion on the ground, including the use of the Ka-band signal in addition to that of the S- and X-bands, open opportunities for important discoveries in each of the above scientific areas, due to increased accuracy, resolution, sensitivity, and dynamic range./Para/pul
lispan class=”labelName”Content Type /spanspan class=”labelValue”Book Chapter/span/liliDOI 10.1007/1-4020-3874-7_1/lilispan class=”labelName”Authors/spanul
liA. Kliore/liliJ. Anderson, California Institute of Technology Jet Propulsion Laboratory 4800 Oak Grove Drive Pasadena CA 91109 USA/liliJ. Armstrong, California Institute of Technology Jet Propulsion Laboratory 4800 Oak Grove Drive Pasadena CA 91109 USA/liliS. Asmar, California Institute of Technology Jet Propulsion Laboratory 4800 Oak Grove Drive Pasadena CA 91109 USA/liliC. Hamilton, California Institute of Technology Jet Propulsion Laboratory 4800 Oak Grove Drive Pasadena CA 91109 USA/liliN. Rappaport, California Institute of Technology Jet Propulsion Laboratory 4800 Oak Grove Drive Pasadena CA 91109 USA/liliH. Wahlquist, California Institute of Technology Jet Propulsion Laboratory 4800 Oak Grove Drive Pasadena CA 91109 USA/liliR. Ambrosini, Istituto di Radioastronomia CNR Via Gobetti 101 1-40129 Bologna Italy/liliF. Flasar, NASA-Goddard Space Flight Center Greenbelt MD 20771 USA/liliR. French, Wellesley College Wellesley MA 02481 USA/liliL. Iess, Università di Roma ‘La Sapienza’ Via Eudossiana 18 I-00184 Roma Italy/liliE. Marouf, San Jose State University One Washington Square San Jose CA 95192 USA/liliA. Nagy, University of Michigan 2455 Hayward Avenue Ann Arbor MI 48109 USA/li
/ul/li
/ulul class=”parents”
ul class=”details”
lispan class=”header labelName”Book /spanspan class=”labelValue”a href=”http://www.springerlink.com/content/n482nr/”The Cassini-Huygens Mission/a/span/lilispan class=”labelName”DOI /spanspan class=”labelValue”10.1007/1-4020-3874-7/span/lilispan class=”labelName”Online ISBN /spanspan class=”labelValue”978-1-4020-3874-7/span/lilispan class=”labelName”Print ISBN /spanspan class=”labelValue”978-1-4020-3147-2/span/li
/ul
/ul