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(The Leland Stanford Junior University)

The Leland Stanford Junior University, commonly referred to as Stanford University or Stanford, is a private research university located in Stanford, California, United States. The university is located on an 8,180-acre (3,310 ha) campus in northwestern Santa Clara Valley approximately 37 miles (60 km) southeast of San Francisco and approximately 20 miles (32 km) northwest of San Jose.

More information: http://en.wikipedia.org/wiki/Stanford_University

IDLE SPACE CODING FLOWCHART* yes Code based on idle activity... (1) (2b) Was the space Inactive or Temporarily Unassignable? (2a) Inactive: Function Code = E Under Renovation: Function Code = X no Was the space idle for more than 3 months? Inactive Temporarily Unassignable Was the space used prior to becoming inactive? (3a) Maintain room type and function codes same as before inactive period. Code room type and function codes based on projected use after inactive period. Code room type and function codes based on projected use after renovation. (3b) Space that was Under Alteration (Room Type code 082): Is the post-renovation use known? yes no no yes Maintain room type and function codes same as before inactive period. *New space (i.e. a new building) that was Unfinished is not considered Idle Space until it is completed. Code as Room Type 084 or 085 and Function Code ‘X’ until first available for use. Notes: Inactive: usable space voluntarily not used. Temporarily Unassignable: space not fit for use. This flowchart diagrams the information included in the Stanford University Space Inventory Instructions dated May 2000 on pages 5 and 29. Produced by GCRS, Stanford University 6/5/00.

An Overview of Smart Fields at Stanford University October 18, 2007 D. Echeverría Ciaurri Smart Fields Consortium Stanford University
CS 147: Intro to HCI Dan Maynes-Aminzade Before usability

CS 147: Intro to HCI Dan Maynes-Aminzade Before usability

After 1st Usability Review

11 October 2007 Prototyping Scott Klemmer tas: Marcello Bastea-Forte, Joel Brandt, Neil Patel, Leslie Wu, Mike Cammarano
Multimodal Interfaces Oviatt, S. Multimodal interfaces Mankoff, J., Hudson, S.E., & Abowd, G.D. Interaction techniques for ambiguity resolution in recognition-based interfaces

Multimodal Interfaces Oviatt, S. Multimodal interfaces Mankoff, J., Hudson, S.E., & Abowd, G.D. Interaction techniques for ambiguity resolution in recognition-based interfaces
HMI Science Analysis Plan

HMI Science Analysis Plan

Magnetic Shear Tachocline Differential Rotation Meridional Circulation Near-Surface Shear Layer Activity Complexes Active Regions Sunspots Irradiance Variations Flare Magnetic Configuration Flux Emergence Magnetic Carpet Coronal energetics Large-scale Coronal Fields Solar Wind Far-side Activity Evolution Predicting A-R Emergence IMF Bs Events Brightness Images Global Helioseismology Processing Local Helioseismology Processing Version 1.0w Filtergrams Line-of-sight Magnetograms Vector Magnetograms Doppler Velocity Continuum Brightness Line-of-Sight Magnetic Field Maps Coronal magnetic Field Extrapolations Coronal and Solar wind models Far-side activity index Deep-focus v and cs maps (0-200Mm) High-resolution v and cs maps (0-30Mm) Carrington synoptic v and cs maps (0-30Mm) Full-disk velocity, v(r,Θ,Φ), And sound speed, cs(r,Θ,Φ), Maps (0-30Mm) Internal sound speed, cs(r,Θ) (0

Mechanical Characteristics: Box: 0.84 × 0.55 × 0.16 m Over All: 1.19 × 0.83 × 0.30 m Mass: 44.0 kg First Mode: 73 Hz Z Y X Optical Characteristics: Effective Focal Length: 495 cm Telescope Clear Aperture: 14 cm Focal Plane Assembly ISS Beam-splitter Assembly Limb Sensor Assembly ISS Pre-Amp Electronics Box Camera Electronics Box Telescope Assembly Primary Lens Assembly Front Window Assembly Front Door Assembly Fold Mirror Assembly BDS Beam-splitter Assembly Michelson Interferometer Alignment Mechanism Filter Oven Assembly Lyot Filter Assembly Oven Controller E-Box Focus Mechanism ISS Mirror Assembly Hollow Core Motors Secondary Lens Assembly Structure HMI Principal Optics Package Components

The Solar Group is ~30 people working to better understand the Sun and the sources of its variability. There are several projects including one on the ground, one in space, and one in development for space. The Wilcox Solar Observatory at Stanford has been operating since 1975 HOP HEB HMI & AIA Joint Science Operations Center Architecture – The Stanford Solar Group will provide the ground data system for both HMI and Lockheed-Martin’s AIA instrument on SDO – Together these represent 95% of the SDO data, about 1.4TBytes/day Catalog Primary Archive HMI & AIA Operations House- keeping Database MOC DDS Redundant Data Capture System 30-Day Archive Offsite Archive Offline Archive HMI JSOC Pipeline Processing System Data Export & Web Service Stanford LMSAL High-Level Data Import AIA Analysis System LM-Local Archive Quicklook Viewing housekeeping GSFC White Sands World Science Team Forecast Centers EPO Public We use the web as a tool for ourselves as well as collaborators and the general public Our home page has links to our various projects: Observational Solar Physics at Stanford University Philip Scherrer MDI observations have enabled better understanding of the interior structure of the Sun. The techniques of local helioseismology have been developed with MDI data and led to plans for SDO/HMI. MDI was designed and build as part of an ongoing collaboration with the solar group at Lockheed-Martin Solar and Astrophys...

Active Region Science MSSL, University College London, UK Co-I J. Leonard Culhane Helioseismology * Local HS Inversion Code IoA, Cambridge University, UK Co-I Douglas O. Gough Active Region Science Rutherford Appleton Laboratories, UK Co-I Richard A. Harrison * Phase D only HMI Science Team Helioseismology Imperial College, UK Co-I Michael J. Thompson AR Science Max-Planck-Institut für Aeronomie, DE Co-I Sami K. Solanki Helioseismology University of Tokyo, JP Co-I Hiromoto Shibahashi Helioseismology National Astron. Obs. of Japan, JP Co-I Takashi Sekii Atmospheric Dynamics ILWS Coordination European Space Agency Co-I Bernhard Fleck Helioseismology * Solar Model Code TAC, Aarhus University, DK Co-I J. Christensen-Dalsgaard Convection Physics * Convection Zone MHD Model Code NASA Ames Research Center Co-I Alan Wray Solar Cycle * Magnetic Field Calibration Code University of California, Los Angeles Co-I Roger K. Ulrich Helioseismology * Sub-Surface-Weather Code JILA, Univ. of Colorado Co-I Juri Toomre Helioseismology * Helioseismic Analysis Code University of Southern California Co-I Edward J. Rhodes, Jr. Convection Physics * Convection Zone MHD Model Code NASA Ames Research Center Co-I N. Nicolas Mansour Coronal Physics * Coronal MHD Model Code Science Applications Intnl. Corp. Co-I Jon A. Linker Helioseismology * Farside Imaging Code Colorado Research Associates Co-I Charles A. Lindsey Irradiance and Shape * Limb and Irradiance Code University of Hawaii Co-I Jeffrey ...

HMI Data Analysis Pipeline Doppler Velocity Heliographic Doppler velocity maps Tracked Tiles Of Dopplergrams Stokes I,V Filtergrams Continuum Brightness Tracked full-disk 1-hour averaged Continuum maps Brightness feature maps Solar limb parameters Stokes I,Q,U,V Full-disk 10-min Averaged maps Tracked Tiles Line-of-sight Magnetograms Vector Magnetograms Fast algorithm Vector Magnetograms Inversion algorithm Egression and Ingression maps Time-distance Cross-covariance function Ring diagrams Wave phase shift maps Wave travel times Local wave frequency shifts Spherical Harmonic Time series To l=1000 Mode frequencies And splitting Version 1.2 Brightness Images Line-of-Sight Magnetic Field Maps Coronal magnetic Field Extrapolations Coronal and Solar wind models Far-side activity index Deep-focus v and cs maps (0-200Mm) High-resolution v and cs maps (0-30Mm) Carrington synoptic v and cs maps (0-30Mm) Full-disk velocity, v(r,Θ,Φ), And sound speed, cs(r,Θ,Φ), Maps (0-30Mm) Internal sound speed, cs(r,Θ) (0

A particularly obvious example of daily changing background noise level Constructing the BEST High-Resolution Synoptic Maps from MDI J.T. Hoeksema, Y. Liu, X.P. Zhao, A. Amezcua Stanford University Synoptic maps provide a global view of the solar magnetic field.  However, what constitutes the 'best' possible synoptic map depends on the application. Traditional charts are compiled from data observed close to central meridian from magnetograms observed over a 27-day solar rotation. But with higher resolution data, a whole new set of details must be addressed when assembling such maps.  Small-scale features move and evolve on the time scale over which the maps are constructed.  The fluctuating background noise level is comparable to the smallest features.  Projection effects and sensitivity variations of different sorts complicate the effort.  And what about the polar field? (See accompanying poster by Liu et al.)  Parts of the Sun cannot be seen.  We describe methods for assembling the best maps possible by accounting for image sensitivity, image scale, corrupt pixels, differential rotation, geometric field projection, zero offset, varying noise characteristics of MDI magnetograms, and polar field interpolation. Process for Constructing Synoptic Chart Announcing New Level 1.8 MDI Magnetograms For each 96-minute MDI magnetogram, we correct for Uniform Zero Offset due to Shutter Jitter (Existing) Bad Cosmic Ray Pixels (New, rare) MDI saturation (Not yet implement...

High-latitude activity and its relationship to the mid-latitude solar activity. Elena E. Benevolenskaya & J. Todd Hoeksema Stanford University Abstract. The high-latitude activity at photosphere and corona, and their relation to the mid-latitude activity in cycle 23 using the Extreme Ultraviolet (EUV) coronal observation have been explored using the MDI magnetic synoptic maps available on the SOHO web page with a new calibration and EIT synoptic maps. The EIT synoptic maps of EUV images in three lines Fe and in one line He II (171A, 195A, 284A and 304A) are obtained for period June 1996 - May 2006 (CR1911-CR2042) from the full disk EIT images. They are represented by values of the line intensity centered on the central meridian and can be directly compared with magnetic synoptic maps (MDI maps). It was found that the solar cycle dependence of the EUV polar corona occurs because of the large-scale topology of the solar corona and its relationship with the mid-latitude magnetic flux. It is seen more pronounced on the rising phase of the solar cycle due to the connectivity of the coronal structures extended from the mid-latitude to the high-latitude. But, after the solar cycle maximum the EUV polar corona shows a less dependence of the mid-latitude corona. In the polar regions the absent of the correlation of the unsigned magnetic flux and EUV corona occurs not only due to the effect of projection. But it tells about the numerous emerging bi-polar and unipolar regions in...

The “cone model” was originally developed by Zhao et al. ~10 (?) years ago in order to interpret the times of arrival of ICME ejecta following SOHO LASCO observations of halo CMEs- which were known to produce geoeffects more often than other CMEs. This poster provides an update on the approach that CISM is taking to develop a simplified model of a CME’s effects on the solar wind, namely the transient disturbances known as ICMEs that are the major cause of large geomagnetic storms. Case studies with the cone model include the halo CME in May 1997 that is also being simulated by CISM in a more detailed way starting at the Sun (see accompanying poster on the initiation of this event in the coronal model). Other potential case studies are described here, including cases involving multiple CME disturbances that interact in ways that modify their individual effects. Overall the cone model allows us to proceed in developing the heliospheric portions of the model, to explore the effects of interaction with the solar wind structure, and to develop model products necessary for SEP event simulations and geospace coupling. CISM Cone Model Approach to Interplanetary CME (ICME) Simulation D. Odstrcil3,4, X-P. Zhao5, Y. Liu5, T.J. Hoeksema5, C.N. Arge6, S. Ledvina1, P.Riley2, J. Linker2 1University of California, Berkeley, 2SAIC, 3University of Colorado, 4NOAA-SEC, 5Stanford, 6AFRL May 12, 1997 May 1, 1998 The ejecta has no magnetic structure and so best represents an IC...

Solar Astronomy: Science in Service to Education Kelly Beck (Haas Center for Public Service, Stanford), Deborah Scherrer (Stanford Solar Center, Stanford), Cherilynn Morrow (Space Science Institute) Science & Professional Issues What is science literacy and why is it important? How does one use solar science as a “hook” to generate enthusiasm? Science Fellows come from a broad range of subject fields, though require similar basic science communication skills Science faculty offer access to good, in-depth understanding of solar science. Science Fellows are provided with sufficient tools, skills, and resources to communicate the basics and appreciate the results of scientific research Education Issues Research-based methods for effective science communication Learning theories Science Standards How to identify previous knowledge and address misconceptions Inclusive learning environments and cultural issues Inquiry-based science teaching methods and hands-on learning Multiple intelligences Testing, pre- and post-assessment/evaluation Teaching approaches: “Guide on the Side” vs. “Sage on the stage” Our program uses solar science as a “hook” to intrigue students and the public as well as those who wish to reach them. Heliospheric Magnetic Imager Who? Our Stanford Science Fellows represent an extremely diverse group of potential leaders! Number of Science in Service Fellows: 11 Gender Split C...

Chabot Space & Science Center, in Oakland, CA, is an innovative teaching and learning center focusing on astronomy and the space sciences. Formed as a Joint Power Agency with the City of Oakland, the Oakland Unified School District, the East Bay Regional Park District, and in collaboration with the Eastbay Astronomical Society, Chabot addresses the critical issue of broad access to the specialized information and facilities needed to improve K-12 science education and public science literacy. Up to 2,000 K-12 teachers annually take part in Chabot’s professional development programs, in turn reaching up to 60,000 students each year. Through the Chabot/Stanford partnership, we are developing, testing, and evaluating classroom activities and laboratory research projects targeted to high school and community college-level classrooms. The outcome will be a 3-day Teacher Training Workshop which will eventually be provided as an online/DVD training course accessible to educators around the world. http://www.chabotspace.org/ Space Weather Monitors Preparing to Distribute Scientific Devices and Classroom Materials Worldwide for the IHY 2007 SID: The Low Cost Monitor Chabot Space & Science Center Curriculum Partners Chabot Space & Science Center Benjamin Burress Stanford Solar Center Deborah Scherrer Cal State University East Bay Ray Mitchell, Chief Engineer Deer Valley High School, Antioch, CA Jeff...

Earth's ionosphere reacts strongly to the intense x-ray and ultraviolet radiation released by the Sun during a solar event. By using a receiver to monitor the signal strength from distant VLF transmitters, and noting unusual changes as the waves bounce off the ionosphere, students around the world can directly monitor and track these Sudden Ionospheric Disturbances (SIDs). Stanford's Solar Center, in conjunction with the Electrical Engineering Department’s Very Low Frequency group and local educators, have developed inexpensive SID monitors that students can install and use at their local high schools. Students "buy in" to the project by building their own antenna, a simple structure costing less than $10 and taking a couple hours to assemble. Data collection and analysis is handled by a local PC, which need not be fast or elaborate. Stanford will be providing a centralized data repository and chat site where students can exchange and discuss data. Because there are VLF transmitters scattered around the world, the monitors can be placed virtually anywhere there is access to power. For more information, see solar-center.stanford.edu/SID List of Partners Stanford Solar Center Deborah Scherrer Hao Thai Sharad Khana Scott Winegarden Paul Mortfield Stanford Solar Observatories Group Philip Scherrer Sarah Gregory Stanford EE Department Umran Inan Morris Cohen Justin Tan Cal State University Hayward Ray Mitchell, Chief En...

Earth's ionosphere reacts strongly to the intense x-ray and ultraviolet radiation released by the Sun during a solar event. Students around the world can directly monitor and track these ionospheric disturbances by using a receiver to monitor the signal strength from distant VLF transmitters, and noting changes as the waves bounce off the ionosphere. Stanford's Solar Center, in conjunction with the Electrical Engineering Department’s Very Low Frequency group and local educators, have developed inexpensive ionospheric monitors that students can install and use at their local high schools. Students "buy in" to the project by building their own antenna, a simple structure costing about $10 and taking a couple hours to assemble. Data collection and analysis is handled by a local PC. Stanford will be providing a centralized data repository and chat site where students and researchers can exchange and discuss data. Two versions of the monitor exist – one low-cost (“SID”) and one research quality (“AWESOME”). Because there are VLF transmitters scattered around the world, the monitors can be placed virtually anywhere there is access to power. Our goal is to place one AWESOME and up to five SID monitors in each of the 191 UN countries. For more information, see solar-center.stanford.edu/SID List of Partners Stanford Solar Center Deborah Scherrer Hao Thai Sharad Khanal Scott Winegarden (now at UC Irvine) Stanford Solar Observatories Group ...

Earth's ionosphere reacts strongly to the intense x-ray and ultraviolet radiation released by the Sun during a solar event. By using a receiver to monitor the signal strength from distant VLF transmitters, and noting unusual changes as the waves bounce off the ionosphere, students around the world can directly monitor and track these Sudden Ionospheric Disturbances (SIDs). Stanford's Solar Center, in conjunction with Stanford’s Space, Telecommunications and Radioscience Laboratory and local educators, have developed inexpensive SID monitors that students can install and use at their local high schools. Students "buy in" to the project by building their own antenna, a simple structure costing less than $10 and taking a couple hours to assemble. Data collection and analysis is handled by a local PC, which need not be fast or elaborate. Stanford will be providing a centralized data repository and chat site where students can exchange and discuss data. Because there are VLF transmitters scattered around the world, the monitors can be placed virtually anywhere there is access to power. This project was inspired by the SID project of the American Association of Variable Star Observers (AAVSO) -- www.aavso.org/observing/programs/solar/sid.shtml For more information, see solar-center.stanford.edu/SID List of Partners Stanford Solar Center Deborah Scherrer Hao Thai Sharad Khanal Scott Winegarden Paul Mortfield Stanford Solar Observatories G...

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