08__050610_SCIP/SEB_PSR_Delivery.1 SECCHI Data Processing, Analysis and Access Jeff Newmark Naval Research Laboratory 202-767-0244

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Presentation transcript:

08__050610_SCIP/SEB_PSR_Delivery.1 SECCHI Data Processing, Analysis and Access Jeff Newmark Naval Research Laboratory

08__050610_SCIP/SEB_PSR_Delivery.2 SECCHI Data Processing System

08__050610_SCIP/SEB_PSR_Delivery.3 Data Processing Level Definition LevelSourceDescription PacketsMOCCCSDS packets as transmitted by the spacecraft to the DSMS Level-0MOC/SSCCCSDS packet files sorted and duplicates removed; final after 30 days Level-0.5DPSFITS files containing uncompressed images oriented with ecliptic north “up”. Values are raw counts (DN) Level-1User workstation using Solarsoft FITS files with calibration applied by the user. Values are physical units (CORs, HI) or calibrated DN (EUVI) Level-2User workstation using Solarsoft Data products which are the result of combining two or more images (movies, polarized brightness images, Carrington maps etc). May or may not be calibrated in physical units Level-3User workstation using Solarsoft Derived quantities (electron density, emission measure etc)

08__050610_SCIP/SEB_PSR_Delivery.4 Data Products Science data will be processed to Level-0.5 at the SECCHI Data Processing Facility (DPF) at NRL –Uncalibrated FITS files: a binary data array preceded by a header –FITS files generated from real-time data are “Quick-Look” –FITS files generated from socket playback or Level-0 packet files are “Preliminary” –After 30 days, Level-0.5 FITS files are “Final” SECCHI images will be available as soon as the routine processing steps have been completed (within 30 minutes of receipt of all data necessary to form an image) Final Level-0.5 FITS files will be retrieved electronically by SSC and Co-I institutions from NRL as they are available Routine processing will generate additional products including movies (browse and high-resolution), Carrington maps, ancillary data (housekeeping tables and plots), and lists of events (CMEs, comets etc) Plots of long-term tracking of key parameters such as pointing, temperatures, voltages, currents, CCD offset bias and numbers of hot and dark pixels will be regularly updated

08__050610_SCIP/SEB_PSR_Delivery.5 Data and Analysis Tools Data and Analysis Tools – Will Be Distributed Freely in SOLARSOFT Library Available to Community Images, Movies, Synoptic Maps Movie Generation Tools Space Weather Information (e.g., Beacon Data) CME Lists (Automatic CME Recognition) Comet/Asteroid Lists Calibration Procedure (Photometric, Geometric) Removal of Energetic Particle Tracks Structure Measurements Potential B Field Calculation Tool Emission Measure Map Tool Image Visualization Tools (Single/Multiple Instrument) Three-Dimensional Image Reconstruction CME Propagation Modeling Tool Database/Web Interfaces (e.g. Virtual Solar Observatory Interface)

08__050610_SCIP/SEB_PSR_Delivery.6 Data Archive and Distribution 2 year mission at 46.2, 50.7, or 54.9 kbps  5 TB: –Stored on-line using Network Storage NRL Website provides interface to SECCHI data –Browser Interface (see following slide) –Subsets available through online query and/or DVD –Data Analysis tools and descriptions –Advanced Data Products – e.g. 3D reconstructions, Emission measure maps, CME lists, etc. Level 0.5 Final data product (FITS) routinely transferred electronically to SSC and other institutions (e.g. European Co-I institutes) Designed compatibility with Goddard VSO Beacon and display images/movies –Through website or FTP using query or by special collections Housekeeping plots –Through website or FTP

08__050610_SCIP/SEB_PSR_Delivery.7 Web Data Archive Access - Ideas Traditional – large lists –SOHO Data Archive –LASCO/EIT –Comments: Good for small number of images and/or well defined studies of particular time ranges or campaigns NRL SECCHI Data interface – Event or time/cadence driven, incorporate components of below options –SSW Latest Events (Freeland) - SolarsoftSolarsoft –HESSI – HESSI Data CenterHESSI Data Center –Comments: More of a near-real time tool, less prior knowledge of “event” necessary, more user “friendly.” SSC, VSO

08__050610_SCIP/SEB_PSR_Delivery.8 CME Reconstructions Currently pursuing two broad approaches for 3D reconstructions of CMEs and coronal structures (plumes, streamers, etc). –Parametric modeling (RayTrace) Thernisien, Howard, Vourlidas –Tomographic modeling (Pixon) Cook, Newmark, Antunes

08__050610_SCIP/SEB_PSR_Delivery.9 RayTrace Models the brightness (total and polarized) produced by Thomson electron scattering from an arbitrary electron density distribution. The input electron density distribution can be either a 3D data cube or an analytic description. The output is a 2D image that simulates the observation in a white light coronagraph (user-defined). The observer location, image spatial resolution, the orientation of the density model and the instrumental vignetting function are arbitrary.

08__050610_SCIP/SEB_PSR_Delivery.10 RayTrace Frontend From Thernisien et al. 2004

08__050610_SCIP/SEB_PSR_Delivery.11 3D CMEs Reconstruction ObservationsModeling Output

08__050610_SCIP/SEB_PSR_Delivery.12 Tomographic Modeling Strategy: –Apply 3D tomographic electron density reconstruction techniques to solar features (mainly CMEs). –Utilize B, pB, temporal evolution from 2/3 vantage points. –Construct (time dependent) 3D electron density distribution. Focus: –Use theoretical CME models and existing LASCO observations to identify the range of conditions and features where reconstruction techniques will be applicable. Goal: –Provide a practical tool that will achieve ~daily CME 3D electron density models during the STEREO mission.

08__050610_SCIP/SEB_PSR_Delivery.13 3D Reconstruction: CME model (J. Chen) Three Ecliptic Viewpoints: Image Visualization

08__050610_SCIP/SEB_PSR_Delivery.14 Optical Flow CME cadence 5-10 min MassOptical Flow

08__050610_SCIP/SEB_PSR_Delivery.15 MHD Modeling Essential to Interpret SECCHI Observations and to Connect Them to the in- Situ and Radio Wave Observations 3 Broad MHD Objectives: –Model the Quasi-Static Plasma Parameters –Investigate the Physics of the Initiation of CMEs –Propagate a Transient Structure Into the Heliosphere NRL –MHD CME initiation and propagation, Coronal loop structure, Coronal heating, Loop plasma evolution (incl. Prominences), Coronal hole evolution, Flux emergence, Active region structure –3D Visualization - Heliospace package, Developed with ARL (Tim Hall), Based on FAST (NASA/Ames) SAIC – Mikic, Linker, Riley, Lionello – coronal and Heliospheric time dependent MHD model = MAS Univ. Alabama – Wu – MHD models GSFC CCMC – Hesse - hosts models University of Michigan + JPL – 3D models of CMEs as seen from STEREO These Model Outputs Will Be Available As Boundary Values to New Codes for Predicting Solar Wind Properties, Energetic Particles, and Radio Emission