Workflows for HELIOPhysics Dr. Gabriele Pierantoni Dr. David Perez Suarez
Workflows for Heliophysics • What advantages ? • Formal representation of a process • Allows to handle very complex programs • Allows sharing of knowledge through repositories.
Workflows for Heliophysics • What are they for ? • Propagation Models • Search metadata • Extract metadata
Workflows for Heliophysics • Where do they come from ? • Propagation Models • WS-PGRADE (TCD-SCSS & Others) • Search metadata • TAVERNA (HELIO) • Extract metadata • WS-PGRADE (TCD-PHY & TCD-SCSS)
Propagation Models A propagation model is used to help determine which observations, where and when may be of interest in order to satisfy the user's search criteria.
Advanced Propagation Model Origin Target t t P = Pmax ETA Range E P = POK Period of interest E P = Pmin E
LO-FAR • LOFAR is a real-time multiple sensor array. • Very different sensors can be placed along a common infrastructure and make use of it the same time. • Analysis of raw frequency data requires significant storage and computation resources. • We are developing a standardizes processing and storage workflow to the community to be easily configured
Processing Nodes • Data Staging • PreProcessing • Processing • PostProcessing • DataPublications
Java Standard Node PORTLET / PORTAL WORFLOWS NODES PROGRAMS
Java Standard Node Input Parameter Standard Java Node Input Data Output Data Input Status Output Status
Java Standard Node Check Status Input Data Load Files Failed Input Status Input Parameter Processing Output Data Completed Output Status
Java Standard Node AbstractGenericNode Defines the sequence of actions AbstractStringNode Defines how to read and write files ConcreteStringNode Defines the processing
ER-FLOW Web Services TAVERNA workflows WS-Pgrade Workflows Development of HELIO portal Access to DCIs
Events Count Counts the number of events for a period.
Fastest CMEs Propagation This workflow is used to investigate one of the most relevant events in HELIOphysics; Coronal Mass Ejections. The propagation of these events is studied throughout the Solar System by the means of the execution of the SHEBA propagation model on the HELIO Processing Service.
Fastest CMEs Propagation Find parameters for model Execute the model Validate the results
High Energy Flares Given a time range, this workflow looks for flares within the specified energy range and provides the observations for such time range for the list of instruments asked. It also provides the table of flares with its properties.