SH51A-0246 

The Virtual Magnetospheric Observatory at UCLA

* Walker, R J (rwalker@igpp.ucla.edu), Institute of Geophysics and Planetary Physics and Department of Earth and Space Sciences, University of California, Los Angeles, Los Angeles, CA 90095-1567, United States King, T A (tking@igpp.ucla.edu), Institute of Geophysics and Planetary Physics, University of California, Los Angeles, Los Angeles, CA 90095-1567, United States Joy, S P (sjoy@igpp.ucla.edu), Institute of Geophysics and Planetary Physics, University of California, Los Angeles, Los Angeles, CA 90095-1567, United States Bargatze, L F (lfb@igpp.ucla.edu), Institute of Geophysics and Planetary Physics, University of California, Los Angeles, Los Angeles, CA 90095-1567, United States Chi, P (pchi@igpp.ucla.edu), Institute of Geophysics and Planetary Physics, University of California, Los Angeles, Los Angeles, CA 90095-1567, United States Weygand, J (jweygand@igpp.ucla.edu), Institute of Geophysics and Planetary Physics, University of California, Los Angeles, Los Angeles, CA 90095-1567, United States

The Virtual Magnetospheric Observatory (VMO) creates robust links to the world's relevant data bases and thereby provides one-stop shopping for the magnetospheric researcher seeking data. The VMO is a joint effort of scientists at the Goddard Space Flight Center (GSFC) and UCLA. The VMO supports two ways for a scientist to find the data and access the data needed for a given study. One is a structured interface developed at GSFC and the other is a word based interface (Google like) developed at UCLA. Both interfaces provide well organized views of the diverse scientific data holdings needed for magnetospheric research. The word based interface will be demonstrated at the poster. Since data are dynamic, the VMO portal design allows frequent and asynchronous updating. The VMO will only succeed in serving the needs of the magnetospheric science community if most of the world's data repositories are part of the system. Therefore we have worked to make it simple to participate in the VMO. The registries for both data and services are designed to make it easy for suppliers to make their resources available and update information. The basis for resource descriptions is the SPASE data model. We have created tools to enable data repositories to populate the registries and to communicate with the VMO even if they use other data models. Scientists trained in data management, called domain experts, are available to work with data suppliers to prepare the metadata and to create archival quality data products. We describe how the domain experts bring information into the VMO.

SH51A-0247 

Relational data searching for magnetospheric data using the Virtual Magnetosheric Observatory

* Merka, J (jan.merka@nasa.gov), GEST Center, University of Maryland, Baltimore County, 5523 Research Park Drive, Suite 320, Baltimore, MD 21228, * Merka, J (jan.merka@nasa.gov), Heliospheric Physics Laboratory, NASA/GSFC, Code 672, Greenbelt, MD 20771, Narock, T (Thomas.W.Narock@nasa.gov), GEST Center, University of Maryland, Baltimore County, 5523 Research Park Drive, Suite 320, Baltimore, MD 21228, Narock, T (Thomas.W.Narock@nasa.gov), Heliospheric Physics Laboratory, NASA/GSFC, Code 672, Greenbelt, MD 20771, Szabo, A (adam.szabo@nasa.gov), Heliospheric Physics Laboratory, NASA/GSFC, Code 672, Greenbelt, MD 20771,

The Virtual Magnetospheric Observatory (VMO) aims to provide a single unified search interface for magnetosperic data sets and already after only about a year of development it is sufficiently mature for scientific applications. The VMO is a multi-tiered environment composed of two peer observatories, one located at NASA/GSFC (VMO/G) and the other at UCLA (VMO/U), that divided up tasks in a complementary fashion similar to open source development methods. While the VMO/G is geared towards a relational search, the VMO/U is working on a Google-like word search. VMO/G co-develops the relational search with the Virtual Heliospheric Observatory (VHO) so users familiar with either of VMO or VHO query interfaces do not need to learn a new interface in order to work with the other VxO. This presentation will describe the VMO/G implementation of structured search and provide specific examples of scientific use cases demonstrating how the VMO enables new and faster research. http://vmo.nasa.gov

SH51A-0248 

The Global Magnetometer Initiative - SuperMAG: Supporting Virtual Observatories.

* Gjerloev, J), JHU-APL, Applied Physics Laboratory Johns Hopkins University 11100 Johns Hopkins Road, Laurel, MD 20723, United States Barnes, R), JHU-APL, Applied Physics Laboratory Johns Hopkins University 11100 Johns Hopkins Road, Laurel, MD 20723, United States

The development of the heliospheric virtual observatories (VxOs) has led to a great improvement in the ability to discover data resources. However these data resources are in a myriad of different file formats, they often require additional calibration or processing, and may require advanced technical knowledge of the instrument to be of any use. The aim of the VxOs is to enable interdisciplinary research and this will require in many cases, more than access to the raw data files. Researchers working in different disciplines will be using data sets that they are not necessarily familiar with. SuperMAG is an example of how to solve this problem. Using ground based magnetometer data has been complicated in the past by the fact that the various networks use different file formats, different coordinate systems, suffer from various inherent data errors and finally use different baseline techniques. SuperMAG provides derived magnetometer data products that correct for all of these problems and allows the user to focus on the science without requiring detailed knowledge of the data processing or technical details of the instrument. SuperMAG represents an interface layer between the VxOs and the raw data where the knowledge needed to work with the dataset is built into the system. In the future the VxOs can take advantage of systems like SuperMAG to act as a service that provides "value added", derived data products.

SH51A-0249 

Roles of Cluster Active Archive in heliophysics science research

McCaffrey, S (smccaffr@rssd.esa.int), ESA/ESTEC, Postbus 299, Noordwijk, 2200AG, Netherlands * Laakso, H (Harri.Laakso@esa.int), ESA/ESTEC, Postbus 299, Noordwijk, 2200AG, Netherlands Perry, C (C.H.Perry@rl.ac.uk), Rutherford Appleton laboratory, c/o Space Science and Technology Department, Didcot, OX11 0QX, United Kingdom Taylor, M (Matthew.Taylor@esa.int), ESA/ESTEC, Postbus 299, Noordwijk, 2200AG, Netherlands Escoubet, P (Philippe.Escoubet@esa.int), ESA/ESTEC, Postbus 299, Noordwijk, 2200AG, Netherlands Esson, S (Steve.Esson@esa.int), ESA/ESTEC, Postbus 299, Noordwijk, 2200AG, Netherlands Herment, D (dherment@rssd.esa.int), ESA/ESTEC, Postbus 299, Noordwijk, 2200AG, Netherlands

The four-satellite Cluster mission investigates small-scale structures (in three dimensions) of the Earth's plasma environment, such as those involved in the interaction between the solar wind and the magnetospheric plasma, in global magnetotail dynamics, in cross-tail currents, and in the formation and dynamics of the neutral line and of plasmoids. The Cluster Active Archive CAA (http://caa.estec.esa.int/) will contain the entire set of Cluster high resolution data and other allied products in a standard format and with a complete set of metadata in machine readable form. The data archived are (1) publicly accessible, (2) of the best quality achievable with the given resources, and (3) suitable for science use and publication by both the Cluster and broader scientific community. The CAA tends to provide user friendly services for searching and accessing these data, e.g., users can save their frequent data requests as profiles speeding up their future similar requests. The CAA is continuing to extend and improve the online capabilities of the system, e.g., the CAA products can be downloaded either via a web interface or a machine accessible interface.

SH51A-0250 

The Virtual Heliospheric Observatory (VHO)

* Szabo, A (Adam.Szabo@nasa.gov), NASA Goddard Space Flight Center, Code 672, Greenbelt, MD 20771, United States Narock, T (Tom.Narock@gsfc.nasa.gov), University of Maryland, Baltimore County, NASA/GSFC Code 672, Greenbelt, MD 20771, United States Merka, J (Jan.Merka@gsfc.nasa.gov), University of Maryland, Baltimore County, NASA/GSFC Code 672, Greenbelt, MD 20771, United States Roberts, A (Aaron.Roberts@nasa.gov), NASA Goddard Space Flight Center, Code 672, Greenbelt, MD 20771, United States Vandegriff, J (Jon.Vandegriff@jhuapl.edu), Johns Hopkins University, Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, United States Ho, G (George.Ho@jhuapl.edu), Johns Hopkins University, Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, United States Raines, J (jraines@umich.edu), University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, United States Schroeder, P (peters@ssl.berkeley.edu), University of California, Berkeley, Centennial Drive, Berkeley, CA 94720, United States Davis, A (ad@srl.caltech.edu), California Institute of Technology, 220-47, Pasadena, CA 91001, United States Kasper, J (jck@space.mit.edu), Massachusetts Institute of Technology, 77 Massachusetts Ave., Cambridge, MA 02139, United States

A fully functional version of the Virtual Heliospheric Observatory (VHO) will be demonstrated. Complex queries involving data from numerous spacecraft and various solar wind conditions allow rudimentary science data mining to be performed. VHO also features direct user access to parameter level metadata information that is essential for the correct scientific use and interpretation of the selected data products. Planned additional VHO related data services will also be detailed. http://vho.nasa.gov

SH51A-0251 

Virtual Energetic Particle Observatory for the Heliospheric Data Environment

* Cooper, J F (John.F.Cooper@nasa.gov), NASA Goddard Space Flight Center, Heliospheric Physics Laboratory, Code 672, Greenbelt, MD 20771, United States Armstrong, T P (armstrong@ftecs.com), Fundamental Technologies, LLC, 2411 Ponderosa Dr Suite A, Lawrence, KA 66046-5073, United States Hill, M E (matt.hill@jhuapl.edu), Applied Physics Laboratory, Johns Hopkins University, 11100 Johns Hopkins Rd MP3-E128, Laurel, MD 20723-6005, United States Lal, N (Nand.Lal@nasa.gov), NASA Goddard Space Flight Center, Heliospheric Physics Laboratory, Code 672, Greenbelt, MD 20771, United States McGuire, R E (Robert.E.McGuire@nasa.gov), NASA Goddard Space Flight Center, Heliospheric Physics Laboratory, Code 672, Greenbelt, MD 20771, United States McKibben, R B (bruce.mckibben@unh.edu), University of New Hampshire, 9 College Rd., Durham, NH 03824, United States Narock, T W (Thomas.W.Narock@nasa.gov), NASA Goddard Space Flight Center, Heliospheric Physics Laboratory, Code 672, Greenbelt, MD 20771, United States Szabo, A (Adam.Szabo@nasa.gov), NASA Goddard Space Flight Center, Heliospheric Physics Laboratory, Code 672, Greenbelt, MD 20771, United States Tranquille, C (cecil.tranquille@esa.int), European Space Agency - ESTEC, Research and Scientific Support Department of ESA, ESTEC P.O. Box 299, Noordwijk, Z-H 2200AG, Netherlands

The heliosphere is pervaded by interplanetary energetic particles, traditionally also called cosmic rays, from solar, internal heliospheric, and galactic sources. The particles species of interest to heliophysics extend from plasma energies to the GeV energies of galactic cosmic rays still measurably affected by heliospheric modulation and the still higher energies contributing to atmospheric ionization. The NASA and international Heliospheric Network of operational and legacy spacecraft measures interplanetary fluxes of these particles. Spatial coverage extends from the inner heliosphere and geospace to the heliosheath boundary region now being traversed by Voyager 1 and soon by Voyager 2. Science objectives include investigation of solar flare and coronal mass ejection events, acceleration and transport of interplanetary particles within the inner heliosphere, cosmic ray interactions with planetary surfaces and atmospheres, sources of suprathermal and anomalous cosmic ray ions in the outer heliosphere, and solar cycle modulation of galactic cosmic rays. The Virtual Energetic Particle Observatory (VEPO) will improve access and usability of selected spacecraft and sub-orbital NASA heliospheric energetic particle data sets as a newly approved effort within the evolving heliophysics virtual observatory environment. In this presentation, we will describe current VEPO science requirements, our initial priorities and an overview of our strategy to implement VEPO rapidly and at minimal cost by working within the high-level framework of the Virtual Heliospheric Observatory (VHO). VEPO will also leverage existing data services of NASA's Space Physics Data Facility and other existing capabilities of the U.S. and international heliospheric research communities.

SH51A-0252 

Real-time database for high resolution Neutron Monitor measurements

* Steigies, C T (steigies@physik.uni-kiel.de), Christian-Albrechts Universität zu Kiel, Olshausenstr. 40, Kiel, 24098, Germany Rother, O M (rother@physik.uni-kiel.de), Christian-Albrechts Universität zu Kiel, Olshausenstr. 40, Kiel, 24098, Germany Wimmer-Schweingruber, R F (wimmer@physik.uni-kiel.de), Christian-Albrechts Universität zu Kiel, Olshausenstr. 40, Kiel, 24098, Germany Heber, B (heber@physik.uni-kiel.de), Christian-Albrechts Universität zu Kiel, Olshausenstr. 40, Kiel, 24098, Germany

The worldwide network of standardised neutron monitors is, after 50 years, still the state-of-the-art instrumentation to measure spectral variations of the primary cosmic ray component. These measurements are an ideal complement to space based cosmic ray measurements. Data from the approximately 50 IGY and NM64 neutron monitors is stored locally but also available through data collections sites like the World Data Center (WDC) or the IZMIRAN ftp server. The data from the WDC is in a standard format, but only hourly values are available. IZMIRAN collects the data in the best available time resolution, but the data arrives on the ftp server only hours, sometimes days, after the measurements. Also, the high time-resolution measurements of the different stations do not have a common format, a conversion routine for each station is needed before they can be used for scientific analysis. Supported by the framework 7 program of the European Commission, we are setting up a real-time database where high resolution cosmic ray measurements will be stored and accessible immediately after the measurement. Stations that do not have 1-minute resolution measurements will be upgraded to 1-minute or better resolution with an affordable standard registration system, that will submit the measurements to the database via the internet in real-time. This resolves the problem of different data formats and for the first time allows to use real-time cosmic ray measurements for space weather predictions. Access to the NMDB database will be open to all users, and as a first step data from twelve participating groups will be collected in the database. The availability of the data from all European stations and stations from neighbouring countries from one real- time database will simplify the access of the Virtual Cosmic Ray Observatory (ViCRO) to measurements from a significant number of neutron monitors.

SH51A-0253 

Heliophysics Data and Modeling Research Using VSPO

Cornwell, C (carl.cornwell@aquilent.com), Aquilent, 1100 West St, Laurel, MD 20707, United States * Roberts, D A (aaron.roberts@nasa.gov), NASA GSFC, Code 672, Greenbelt, MD 20771, United States Hesse, M (michael.hesse@nasa.gov), NASA GSFC, Code 674, Greenbelt, MD 20771, United States

The primary advantage of Virtual Observatories in scientific research is efficiency: rapid searches for and access to data in convenient forms makes it possible to explore scientific questions without spending days or weeks on ancilary tasks. The Virtual Space Physics Observatory provides a general portal to Heliophysics data for this task. Here we will illustrate the advantages of the VO approach by examining specific geomagneticly active times and tracing the activity through the Sun-Earth system. In addition to previous and additional data sources, we will demonstrate an extension of the VSPO capabilities to allow searching for model run results from the range of CCMC models. This approach allows the user to quickly compare models and observations at a qualitative level; considerably more work will be needed to develop more seamless connections to data streams and the equivalent numerical output from simulations. http://vspo.gsfc.nasa.gov

SH51A-0254 

VESO: Virtual Earth-Sun Observatory

* Gonzalez-Esparza, A (americo@geofisica.unam.mx), Instituto de Geofisica, UNAM, Ciudad Universitaria Coyoacan, Mexico, DF 04510, Mexico Cifuentes-Nava, G (gercifue@geofisica.unam.mx), Instituto de Geofisica, UNAM, Ciudad Universitaria Coyoacan, Mexico, DF 04510, Mexico Hernandez-Quintero, E (estebanh@geofisica.unam.mx), Instituto de Geofisica, UNAM, Ciudad Universitaria Coyoacan, Mexico, DF 04510, Mexico Lara-Sanchez, A (alara@geofisica.unam.mx), Instituto de Geofisica, UNAM, Ciudad Universitaria Coyoacan, Mexico, DF 04510, Mexico Valdes-Galicia, J F (jfvaldes@geofisica.unam.mx), Instituto de Geofisica, UNAM, Ciudad Universitaria Coyoacan, Mexico, DF 04510, Mexico

We present the Virtual Earth-Sun Observatory (VESO) at the web site http://www.veso.unam.mx. This site shows a real time integrated database obtained from four instruments of the Instituto de Geofisica-UNAM studying Sun- Earth connection phenomena. (1) The Solar Radio Interferometer (RIS, Radio Interferómetro Solar) measures the lower solar atmosphere radiation at 7.5 GHz, revealing microwave bursts associated with solar activity. (2) The Mexican Array Radio Telescope (MEXART, Observatorio de Centelleo Interplanetario de Coeneo) will detect solar wind large-scale disturbances between Sun and Earth(e.g., Interplanetary counterparts of Coronal Mass Ejections (ICMES)and Stream Interaction Regions (SIR)) employing the interplanetary scintillation technique (IPS) operating at 140 MHz. (3) The Cosmic Ray Observatory (RC) detects high energy galactic and solar particles, whose flow is affected by magnetic disturbances in the solar wind, and (4) the Teoloyucan Geomagnetic Observatory (TEO) measures the variations in the Earth�s magnetic field. The VESO instruments provide data from four different points of the complex chain of the solar terrestrial relations and allow the study of intense solar events and in possible consequences in causing geomagnetic activity. The VESO project is part of the celebration of the International Heliophysical Year (IHY) and the Electronic Geophysical Year (EGY) in Mexico. http://www.veso.unam.mx/

SH51A-0255 

Lessons Learned in Heliophysics Data Description: Discussion of the Development and Use of the SPASE Data Model

* Thieman, J R (james.r.thieman@nasa.gov), NASA/GSFC, Code 690.1 NASA/GSFC, Greenbelt, MD 20771, United States Bell, E (Edwin.V.Bell@nasa.gov), NASA/GSFC, Code 690.1 NASA/GSFC, Greenbelt, MD 20771, United States Hourcle, J (Joseph.A.Hourcle@nasa.gov), NASA/GSFC, Code 671.1 NASA/GSFC, Greenbelt, MD 20771, United States King, J (Joseph.H.King@nasa.gov), NASA/GSFC, Code 690.1 NASA/GSFC, Greenbelt, MD 20771, United States King, T (tking@igpp.ucla.edu), UCLA, Institute of Geophys. and Planetary Phys. University of California 5881 Slichter Hall, Los Angeles, CA 90095-1567, United States Richards, P (P.J.Richards@rl.ac.uk), Rutherford Appleton Laboratory, RAL, Chilton, OXON, MD OX11, United Kingdom Walker, R (rwalker@igpp.ucla.edu), UCLA, Institute of Geophys. and Planetary Phys. University of California 5881 Slichter Hall, Los Angeles, CA 90095-1567, United States Weigel, R (rweigel@gmu.edu), George Mason University, Department of Physics and Astronomy GMU, Fairfax, VA 22030, United States Weiss, M (Michele.Weiss@jhuapl.edu), JHU/APL, The Johns Hopkins Univ./Applied Physics Laboratory, Laurel, MD 20723-6099, United States

The heliophysics community is presenting at this meeting the results of the development of a number of virtual observatories that have been funded by NASA to provide data access for various subdisciplines (magnetospheres. ionospheres, cosmic rays, radiation belts, etc.) within the realm of heliophysics. For users in one subdiscipline to determine what data might be available and useful in another subdiscipline it is necessary to do cross-subdiscipline searches. To enable such cross-subdiscipline searches to be done in an efficient and thorough manner it is important to have the data described according to a common set of metadata terms or data model. The Space Physics Archive Search and Extract (SPASE) Data Model was developed by representatives of the subdisciplines for this purpose. It is now being applied to describing the data sets in the virtual observatories and, as might be expected, there are a number of lessons that have been learned in this process. This presentation will make note of the lessons learned in the process of describing the data and what problems have yet to be solved. We intend to share this experience with representatives from other disciplines and learn from their experiences as well. We encourage those seeing the presentation to come prepared to relate their knowledge, even if it is only a brief interaction at that time. http://www.spase-group.org

SH51A-0256 

The Collaborative Heliophysics Observatory

* Hurlburt, N (hurlburt@lmsal.com), Lockheed Martin Advanced Technology Center, 3251 Hanover St, Palo Alto, CA 94304, United States Freeland, S (freeland@lmsal.com), Lockheed Martin Advanced Technology Center, 3251 Hanover St, Palo Alto, CA 94304, United States Cheung, M (cheung@lmsal.com), Lockheed Martin Advanced Technology Center, 3251 Hanover St, Palo Alto, CA 94304, United States Bose, P (prasanta.bose@lmco.com), Lockheed Martin Advanced Technology Center, 3251 Hanover St, Palo Alto, CA 94304, United States

The Collaborative Heliophysics Observatory (CHO) would provide a robust framework and enabling tools to fully utilize the VOs for scientific discovery and collaboration. Scientists across the realm of heliophysics would be able to create, use and share applications -- either as services using familiar tools or through intuitive workflows -- that orchestrate access to data across all virtual observatories. These applications can be shared freely knowing that proper recognition of data and processing components are acknowledged; that erroneous use of data is flagged; and that results from the analysis runs will in themselves be shared Ð all in a transparent and automatic fashion. In addition, the CHO would incorporate cross-VO models and tools to weave the various virtual observatories into a unified system. These provide starting points for interactions across the solar/heliospheric and heliospheric/magnetospheric boundaries. http://cosec.lmsal.com

SH51A-0257 

Data Unification and Analysis Services for VxO"s

* Vandegriff, J (jon.vandegriff@jhuapl.edu), Johns Hopkins University Applied Physics Lab, 11100 Johns Hopkins Rd., Laurel, MD 20723, United States Merka, J (jan.merka@gsfc.nasa.gov), University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, United States Narock, T (tom.narock@gsfc.nasa.gov), University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, United States Szabo, A (adam.szabo@nasa.gov), NASA/GSFC, Code 672, Greenbelt, MD 20771, United States

We present a prototype data unification mechanism for space physics data. The ultimate goal is to create a service that provides scientists with a simple yet scalable way to obtain immediately usable data from multiple, diverse, distributed data holdings. While emerging VxO's simplify the discovery of specific data products, the actual product files discovered are still in multiple formats and have widely varying layouts even with the same format. Thus when trying to make, for example, custom plots of data from different missions each of which uses a different format/layout, all the datasets must be first converted to a format and layout suitable for the researcher's own plotting tools, and this can be very time consuming and frustrating. Our service will read the data files from various online, remote locations and convert them into a standardized, internal representation. Once captured in a mission independent form, subsequent use of the data (display, analysis, output into other formats/layouts) can be completely ignorant of any dataset specific details. The prototype version of our service will be available as a set of IDL routines (i.e., a client side mechanism) that can be embedded into custom analysis programs, and eventually this functionality will be available through a REST style interface (i.e., a server side mechanism). The VxO's are an enabling piece of the unification process because VxOs provide uniform metadata that allows the creation of conversion routines to bring the data into a mission independent internal representation. Access to a sampling of magnetic field and plasma datasets available through the Virtual Heliophsyics Observatory (VHO) and the Virtual Magnetospheric Observatory (VMO) will be demonstrated. http://sd-www.jhuapl.edu/MIDL

SH51A-0258 

Scientific Uses and Directions of SPDF Data Services

McGuire, R (robert.e.mcguire@nasa.gov), NASA Goddard Space Flight Center, Code 672, Greenbelt, MD 20771, * Bilitza, D (Dieter.Bilitza-1@nasa.gov), George Mason University, Code 672 NASA Goddard Space Flight Center, Greenbelt, MD 20771, Candey, R (robert.m.candey@nasa.gov), NASA Goddard Space Flight Center, Code 672, Greenbelt, MD 20771, Chimiak, R (reine.a.chimiak@nasa.gov), NASA Goddard Space Flight Center, Code 583, Greenbelt, MD 20771, Cooper, J (john.f.cooper@nasa.gov), NASA Goddard Space Flight Center, Code 672, Greenbelt, MD 20771, Fung, S (shing.f.fung@nasa.gov), NASA Goddard Space Flight Center, Code 672, Greenbelt, MD 20771, Han, D (david.b.han@nasa.gov), NASA Goddard Space Flight Center, Code 583, Greenbelt, MD 20771, Harris, B (bernie.harris@nasa.gov), NASA Goddard Space Flight Center, Code 583, Greenbelt, MD 20771, Johnson, R (Rita.C.Johnson@nasa.gov), Perot Systems, Code 672 NASA Goddard Space Flight Center, Greenbelt, MD 20771, King, J (Joseph.H.King@nasa.gov), Perot Systems, Code 672 NASA Goddard Space Flight Center, Greenbelt, MD 20771, Kovalick, T (Tamara.J.Kovalick@nasa.gov), Perot Systems, Code 672 NASA Goddard Space Flight Center, Greenbelt, MD 20771, Leckner, H (Howard.A.Leckner@nasa.gov), Perot Systems, Code 672 NASA Goddard Space Flight Center, Greenbelt, MD 20771, Papitashvili, N (Natalia.E.Papitashvili@nasa.gov), Perot Systems, Code 672 NASA Goddard Space Flight Center, Greenbelt, MD 20771, Roberts, A (aaron.roberts@nasa.gov), NASA Goddard Space Flight Center, Code 672, Greenbelt, MD 20771,

From a science user's perspective, the multi-mission data and orbit services of NASA's Space Physics Data Facility (SPDF) project perform as a working and highly functional heliophysics virtual observatory. CDAWeb enables plots, listings and file downloads for current data across the boundaries of missions and instrument types (and now including data from THEMIS and STEREO), VSPO access to a wide range of distributed data sources. SSCWeb, Helioweb and our 3D Animated Orbit Viewer (TIPSOD) provide position data and query logic for most missions currently-important to heliophysics science. OMNIWeb with its new extension to 1- and 5- minute resolution provides interplanetary parameters at the Earth's bow shock as a unique value-added data product. To enable easier integrated use of our capabilities by developers and by the emerging heliophysics VxOs, our data and services are available through webservices-based APIs as well as through our direct user interfaces. SPDF has also now developed draft descriptions of its holdings in SPASE-compliant XML In addition to showcasing recent enhancements to SPDF capabilities, we will use these systems and our experience in developing them: to demonstrate a few typical science use cases; to discuss key scope and design issues among users, service providers and end data providers; and to identify key areas where existing capabilities and effective interface design are still inadequate to meet community needs. http://spdf.gsfc.nasa.gov

SH51A-0259 

Callable Virtual Observatory Functionality: Sample Use Cases

* Gurman, J B (gurman@gsfc.nasa.gov), NASA Goddard Space Flight Center, Code 671, Greenbelt, MD 20771, United States Hourclé, J A (Joseph.A.Hourcle.1@gsfc.nasa.gov), RSIS and NASA GSFC, Code 671.1, Greenbelt, MD 20771, United States Bogart, R S (rbogart@spd.aas.org), Stanford University, CSSA, Stanford, CA 94305, United States Tian, K (ktian@stanford.edu), Stanford University, CSSA, Stanford, CA 94305, United States Hill, F (fhill@noao.edu), National Solar Observatory, 950 N. Cherry Ave. P.O. Box 26732, Tucson, AZ 85726, United States Su�rez-Sol�, I (igor@noao.edu), National Solar Observatory, 950 N. Cherry Ave. P.O. Box 26732, Tucson, AZ 85726, United States Zarro, D M (Dominic.M.Zarro.1@gsfc.nasa.gov), ADNET and NASA GSFC, Code 671.1, Greenbelt, MD 20771, United States Davey, A R (ard@boulder.swri.edu), Smithsonian Astrophyscial Observatory, 60 Garden Street, Cambridge, MA 02138, United States Martens, P C (pmartens@spd.aas.org), Montana State University, Physics Department, Bozeman, MT 59717-3840, United States Yoshimura, K (yosimura@mithra.physics.montana.edu), Montana State University, Physics Department, Bozeman, MT 59717-3840, United States

A virtual observatory with an Application Programming Interface (API) can become a powerful tool in analysis and modeling. In particular, an API that integrates time selection on such criteria as "most recent" and closest to a given absolute time simplifies the user-end programming considerably. We examine three types of use cases (nowcasting, data assimilation input, and user-defined sampling rates) for such functionality in the Virtual Solar Observatory (VSO). http://virtualsolar.org/docs/AGU200712/

SH51A-0260 

Dealing with Large Dataset Queries in the Virtual Solar Observatory

* Suarez-Sola, F I (igor@nso.edu), National Solar Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719-4933, United States Bogart, R (RBogart@spd.aas.org), Stanford University, Center for Space Science and Astrophysics, Stanford, CA 94305-4085, United States Davey, A (ard@head.cfa.harvard.edu), Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138, United States Gurman, J B (gurman@gsfc.nasa.gov), NASA Goddard Space Flight Center, Code 671, Greenbelt, 20771, Hill, F (fhill@noao.edu), National Solar Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719-4933, United States Hourcle, J (oneiros@grace.nascom.nasa.gov), NASA Goddard Space Flight Center, Code 671, Greenbelt, 20771, Hourcle, J (oneiros@grace.nascom.nasa.gov), RSIS, 1651 Old Meadow Road, McLean, VA 22102, United States Martens, P C (martens@physics.montana.edu), Montana State University, PO BOX 173840, Bozeman, MT 59717-3840, United States Tian, K (ktian@stanford.edu), Stanford University, Center for Space Science and Astrophysics, Stanford, CA 94305-4085, United States Yoshimura, K (yosimura@physics.montana.edu), Montana State University, PO BOX 173840, Bozeman, MT 59717-3840, United States

The Virtual Solar Observatory (VSO) project presents a solution for dealing with large dataset queries. One of the main problems arising from the VSO user community has been managing queries that generate a large amount of metadata records spanning several providers. Until now the only way to do this was through painstakingly repeating the same query for smaller time periods and collecting the information at each pass. With the solution presented here we are making possible for users to access data over any arbitrary time period in one single query, minimizing the metadata generated, and yet allowing the user to sample either a small subset or the whole. http://virtualsolar.org

SH51A-0261 

Design Considerations for Data Catalogs

* Hourcle, J (joseph.a.hourcle@nasa.gov), NASA/GSFC (RSIS), Code 671.1, Greenbelt, MD 20771, United States Suarez-Sola, I (igor@noao.edu), National Solar Observatory, 950 N. Cherry Ave, Tucson, AZ 85719, United States Davey, A (ard@head.cfa.harvard.edu), Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, United States Tian, K (ktian@stanford.edu), Stanford University, Center for Space Science and Astrophysics, Stanford, CA 94305, United States Yoshimura, K (yosimura@mithra.physics.montana.edu), MSU-Bozeman, Physics Department PO Box 173840, Bozeman, MT 59717, United States Martens, P (martens@physics.montana.edu), MSU-Bozeman, Physics Department PO Box 173840, Bozeman, MT 59717, United States Gurman, J (joseph.b.gurman@nasa.gov), NASA/GSFC, Code 671.1, Greenbelt, MD 20771, United States Hill, F), National Solar Observatory, 950 N. Cherry Ave, Tucson, AZ 85719, United States Bogart, R (rick@sun.stanford.edu), Stanford University, Center for Space Science and Astrophysics, Stanford, CA 94305, United States

Mission data catalogs are typically built with the specific mission in mind. This can create challenges when trying to abstract the metadata to make it useful to other researchers. The deluge of data from new missions such as STEREO and Hinode have brought in not only issues in scale, but also complexities due to the difference in these new experiments in the context of existing norms. We will discuss issues and use cases to be considered in designing a mission's data systems in order to better serve the Heliospheric community.

SH51A-0262 

A Catalog of Halo Coronal Mass Ejections from SOHO

Gopalswamy, N (gopals@ssedmail.gsfc.nasa.gov), NASA Goddard Space Flight Center, Code 695.0, Greenbelt, MD 20771, United States Yashiro, S (yashiro@ssedmail.gsfc.nasa.gov), NASA Goddard Space Flight Center, Code 695.0, Greenbelt, MD 20771, United States Yashiro, S (yashiro@ssedmail.gsfc.nasa.gov), Catholic University of America, 620 Michigan Ave. NE, Washington, DC 20064, United States Michalek, G (michalek@ssedmail.gsfc.nasa.gov), NASA Goddard Space Flight Center, Code 695.0, Greenbelt, MD 20771, United States Michalek, G (michalek@ssedmail.gsfc.nasa.gov), Catholic University of America, 620 Michigan Ave. NE, Washington, DC 20064, United States Xie, H (hong.xie@ssedmail.gsfc.nasa.gov), NASA Goddard Space Flight Center, Code 695.0, Greenbelt, MD 20771, United States Xie, H (hong.xie@ssedmail.gsfc.nasa.gov), Catholic University of America, 620 Michigan Ave. NE, Washington, DC 20064, United States Vourlidas, A (vourlidas@nrl.navy.mil), Naval Research Lab, 4555 Overlook Avenue, SW, Washington, DC 20375, United States Howard, R A (russ.howard@nrl.navy.mil), Naval Research Lab, 4555 Overlook Avenue, SW, Washington, DC 20375, United States * Schmidt, J (jschmidt@ssedmail.gsfc.nasa.gov), NASA Goddard Space Flight Center, Code 695.0, Greenbelt, MD 20771, United States

Halo coronal mass ejections (CMEs) have become one of the important subsets of CMEs, thanks to the extensive data accumulated by the Solar and Heliospheric Observatory (SOHO) mission. Halo CMEs are inherently more energetic on the average, so they are important for producing geomagnetic storms and solar energetic particle events (Gopalswamy et al., 2007). One of the key aspects halo CMEs is their source location, which decides whether the halo is symmetric or not. When the source is closer to the solar limb, the CMEs tend to become asymmetric halos or partial halos. Halos with their sources nearer to the limb are also the fastest (because of projection effects), but are less geoeffective due to the glancing blow they deliver to Earth�fs magnetosphere. Thus, providing source information to all halo CMEs in a separate catalog is useful information in selecting candidate geoeffective CMEs. The second important quantity of CMEs is the space speed, which decides the arrival time of CMEs at Earth. Since CMEs change their width during their early evolution, it is not easy to correct for the projection effects from the geometry of eruption. One way of correcting for projection effects is to use a cone model for CMEs. There are at least 3 published cone models, all of them seem to remove the projection effects reasonably well. The geometric parameters of the cone are determined using different methods in each model. Here we use the model by Xie et al. (2004), which has generally less restrictions, and hence can be applied to more number of halos. This paper provides a brief description of the catalog of halo CMEs, which resides at the CDAW Data Center, NASA Goddard Space Flight Center, Greenbelt, MD. The catalog enhances the existing data services at the CDAW Data Center, which participates in the Virtual Solar Observatory. Work supported by NASA�fs Virtual Observatories for Solar and Space Physics Data Program. References Gopalswamy et al., JGR, 112, A06112, doi:10.1029/2006JA012149, 2007 Xie et al. JGR, 109, A03109, doi: 10.1029/2003JA010226, 2004 http://cdaw.gsfc.nasa.gov/CME_list/

SH51A-0263 

MEXICAN VIRTUAL SOLAR OBSERVATORY

Santillan, A (alfredo@astroscu.unam.mx), DGSCA, Universidad Nacional Autonoma de Mexico, Ciudad Universitaria, Coyoacan, Mexico, DF 04510, Mexico Hernandez-Cervantes, L (liliana@astroscu.unam.mx), Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, Ciudad Universitaria, Coyoacan, Mexico, DF 04510, Mexico Gonzalez-Ponce, A (alfredo@astroscu.unam.mx), Instituto de Ecologia, Universidad Nacional Autonoma de Mexico, Ciudad Universitaria, Coyoacan, Mexico, DF 04510, Mexico Hill, F (fhill@noao.edu), National Solar Observatory, PO Box 26732, Tucson, AZ 85726-6732, United States * Blanco-Cano, X (xbc@geofisica.unam.mx), Instituto de Geofisica, Universidad Nacional Autonoma de Mexico, Ciudad Universitaria, Coyoacan, Mexico, DF 04510, Mexico

The Virtual Solar Observatory (VSO) concept contains software tools for searching, manipulating, and analyzing data from archives of solar data at many different observatories around the world (Hill 2000). The VSO not only provides fast and reliable access to the existing solar data, but also represents a powerful and unique machinery to perform numerical simulations for the evolution of a variety of different phenomena associated with solar activity. Two Mexican Universities, Universidad Nacional Autónoma de México and the Universidad de Sonora, are working together to create the Mexican Virtual Solar Observatory (MVSO) that will be part of a wider National effort. In this work we present a general description of the MVSO project, as well as the advances obtained in the development of Graphical User Interfaces (GUI) to Remotely Perform Numerical Simulation of the Evolution of Coronal Mass Ejection in the Interplanetary Medium. http://mvso.astroscu.unam.mx

SH51A-0264 

Heliophysical Modeling at the CCMC - Community Modeling Activities to Compliment the VHGO.

* MacNeice, P (Peter.J.Macneice@nasa.gov), NASA, Goddard Sace Flight Center, CCMC, Greenbelt, MD 20771, United States Bakshi, S (Sarabjit.S.Bakshi@nasa.gov), NASA, Goddard Sace Flight Center, CCMC, Greenbelt, MD 20771, United States Berrios, D (David.H.Berrios@nasa.gov), NASA, Goddard Sace Flight Center, CCMC, Greenbelt, MD 20771, United States Chulaki, A (Anna.Chulaki-1@nasa.gov), NASA, Goddard Sace Flight Center, CCMC, Greenbelt, MD 20771, United States Goldfarb, M (Mary.R.Goldfarb@nasa.gov), NASA, Goddard Sace Flight Center, CCMC, Greenbelt, MD 20771, United States Hesse, M (Michael.Hesse@nasa.gov), NASA, Goddard Sace Flight Center, CCMC, Greenbelt, MD 20771, United States Kuznetsova, M (Maria.M.Kuznetsova@nasa.gov), NASA, Goddard Sace Flight Center, CCMC, Greenbelt, MD 20771, United States Maddox, M (Marlo.M.Maddox@nasa.gov), NASA, Goddard Sace Flight Center, CCMC, Greenbelt, MD 20771, United States Patel, K (Kiran.D.Patel@nasa.gov), NASA, Goddard Sace Flight Center, CCMC, Greenbelt, MD 20771, United States Pulkkinen, A (Antti.A.Pulkkinen@nasa.gov), NASA, Goddard Sace Flight Center, CCMC, Greenbelt, MD 20771, United States Rastaetter, L (Lutz.Rastaetter-1@nasa.gov), NASA, Goddard Sace Flight Center, CCMC, Greenbelt, MD 20771, United States Taktakishvili, A (staktak@helio.gsfc.nasa.gov), NASA, Goddard Sace Flight Center, CCMC, Greenbelt, MD 20771, United States

The Community Coordinated Modeling Center (CCMC) hosts an ever growing inventory of models to support the research activities of the Heliophysics community. In this poster we detail this model inventory. We describe the manner in which the CCMC provides access to these models to the community. This support includes model runs driven with archived data and 'realtime' runs which update as the latest data is ingested by the models. It includes runs for individual researchers and in support of observational planning and analysis for a number of flight missions. Our need to integrate the data streams into and out of numerous models and graphics packages has led to the development of a number of infra-structure component that are also highly relevant to the design of the VHGO. We discuss this issue and the natural and vital link that must develop between the VHGO and modeling centers such as the CCMC, if the usefulness of the VHGO is to be maximized. http://ccmc.gsfc.nasa.gov

Author(s) (2007), Title, Eos Trans. AGU, 88(52), Fall Meet. Suppl., Abstract #####-##.