1. 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 Archiv e Offline Archiv e 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 Astrophysics Laboratory in Palo Alto. The Michelson Doppler Imager instrument of the Stanford Solar Oscillations Investigation onboard the ESA/NASA Solar and Heliospheric Observatory has been operating since December 1995 MDI Optics Electronics Sound speed beneath a sunspot Internal rotation Far-side of the Sun magnetic fields WSO is dedicated to long-term daily observations of the large scale magnetic fields. Data are used for analyses and correlative studies worldwide. All WSO data is freely available. We are interested in developing collaborations for studies of the Sun and Space Weather using WSO, MDI, and shortly HMI observations. All data from these projects is freely available via the web. There are more interesting studies to do with this data than can be accomplished by the just teams at Stanford and our Co-Investigators and other collaborators. Problems that need significant data volumes can be pre-processed at Stanford so the computing requirements for leading-edge helioseismology need not be a deterrent to new investigations. The HMI team includes researchers from 23 institutions. Additional collaborations are welcome. The Helioseismic and Magnetic Imager for the Solar Dynamics Observatory of the Living With a Star program of the Sun Earth Connection Division of the NASA Office of Space Science The primary goal of HMI is to study the origin of solar variability and to characterize and understand the Sun’s interior and the various components of magnetic activity. Launch in April 2008 HMI SDO LWS SEC NASA Observational Solar Physics Group at Hansen Experimental Physics Laboratory at Stanford University Faculty: Philip Scherrer Physics & HEPL Administrative: Romeo DurscherAdmin Assistant (financial) Margaret StehleAdmin. Assistant (documents) MDI Data and Operations: Jim AloiseSystem Software Keh-Cheng ChuScientific Software Sarah GregoryAt GSFC, MDI Observer Jeneen SommersScience & Engineering Assoc. Hao ThaiScience & Engineering Assoc. Brian RobertsComputer Operations HMI Development, VSO Development Rock BushSr. Research Scientist Rasmus Munk LarsenResearch Scientist Karen TianResearch Scientist SOI (MDI Helioseismology and motions) Analysis: Tom Duvall, Jr.NASA visiting scientist Alexander KosovichevSr. Research Scientist Jesper Schou Sr. Research Scientist Sebastian CouvidatResearch Scientist Laurent GizonResearch Scientist Junwei ZhaoResearch Scientist Rick Bogart Sr. Research Scientist John BeckResearch Scientist Shravan Mukunda Graduate Student – EE Shalini KrishnamurthyGraduate Student – SCCM Christina GreenGraduate Student – SCCM Majid ModarresiGraduate Student – SCCM WSO, Space Weather, Corona, MDI magnetic field: J. Todd HoeksemaSr. Research Scientist Taeil Bai Sr. Research Scientist Xue Pu Zhao Sr. Research Scientist Yang LiuSr. Research Scientist Elena BenevolenskayaResearch Scientist Keiji HayashiResearch Scientist Bala PoduvalResearch Scientist Paul BoernerGraduate Student - Physics Education and Public Outreach: Deborah ScherrerE/PO Coordinator Paul MortfieldConsultant OP Structure Telescope Front Window Front Door Vents Support Legs (6) Polarization Selector Focus/Calibration Wheels Active Mirror Limb B/S Alignment Mech Oven Structure Michelson Interf. Lyot Filter Shutters Connector Panel CEBs Detector (Vector) Fold Mirror Focal Plane B/S Detector (Doppler) Limb Sensor Overview of the Helioseismic and Magnetic Imager Investigation The primary scientific objectives of the Helioseismic and Magnetic Imager (HMI) investigation are to improve understanding of the interior sources and mechanisms of solar variability and the relationship of these internal physical processes to surface magnetic field structure and activity. The HMI instrument will make measurements of the dynamic motion of the solar photosphere on global and local solar scales to study solar surface oscillations and will make similarly scaled measurements of the polarization in a spectral line to study all three components of the photospheric magnetic field. HMI observations will help to establish the relationships between the internal solar dynamics and related magnetic activity. Specific scientific objectives of the HMI investigation are to measure and study: 1.Convection-zone dynamics and the solar dynamo; 2.Origin and evolution of sunspots, active regions and complexes of activity; 3.Sources and drivers of solar magnetic activity and disturbances; 4.Links between the internal processes and dynamics of the corona and heliosphere; 5.Precursors of solar disturbances for space-weather forecasts. The HMI instrument will produce measurements in the form of filtergrams in a set of polarizations and spectral line positions at a regular cadence for the duration of the mission that meet these basic requirements: Full-disk velocity and line-of-sight magnetic flux images with 1 arc-sec resolution every 50 seconds. Full-disk vector magnetic images of the solar magnetic field with 1 arc-sec resolution every 10 minutes. The HMI investigation will provide sufficient computing capability to convert these raw filtergram measurements into a set of observables and derived data products required for the HMI science objectives. The primary observables (Dopplergrams, longitudinal and vector magnetograms, and continuum intensity images) will be constructed from the raw filtergrams and will be made available at full resolution and cadence. Other derived products such as subsurface flow maps, far-side activity maps, and coronal and solar wind models that require longer sequences of observations will be produced and made available. All HMI data products will be made available to all interested investigators. SDO will carry The Atmospheric Imaging Array provided by Lockheed Martin Solar and Astrophysics Lab and the EUV Variability Experiment provided by the University of Colorado in addition to HMI. HMI Optics Package The web provides access to many of our E/PO activities. See also the poster by John Beck WSO Magnetic Field Synoptic maps of observed photospheric field have been made since 1976. Inferred coronal field maps are available for each Carrington rotation. These predict the polarity structure in the heliosphere. Solar polar field strength vs. time