HMI/AIA  Science Teams Meeting 2006

HMI_Logo    Session Information     AIA_Logo
Version: 8 February, 2006

Detailed session schedules are available only in the: Final Announcement

Session Description
Plenary Sessions
P1Mon@ 8:30 Introduction and Status - HQ, Program, Project, Hardware - Points Ballroom
Title & Scherrer
P2Mon@ 10 Introduction and Status - Processing & Software - Points Ballroom
Scherrer & Title
P3Mon@ 5 Contributing Your Code and Using SDO Data - Points Ballroom
This session gives an introduction to the AIA/HMI JSOC software environment, application programming interface (API) and data export facilities. A tutorial will be given illustrating how to integrate existing analysis code into the pipeline, accessing SDO data via the JSOC API. Discuss data export methods necessary to access data outside the pipeline.
P4Tue@ 5 Collaborative Science: Solar-B, STEREO, SXI, PICARD, and others - Points Ballroom
Title & Scherrer

How can we make sure SDO best complements the science of other solar observatories?
P5Thu@ 5 Technical Needs, New Technical Groups, Plans, Schedules - Points Ballroom
Larsen & Schrijver

This session will be used to announce and discuss any newly formed technical working groups (from sessions H6, H7, M3, C8) and discuss their plans, schedules and technical needs, such as: How do the working groups coordinate data product definitions and formats to make them useful outside their specific domain? Can some code/algorithm development be shared in some areas?
P6Fri@ 12 Future Schedule and Wrap-up - Points Ballroom
Title & Scherrer

Summary of meeting results, plans and schedules for future team activities and for science activities.
Tutorial Introductions
T1Mon@ 1:15 Complexity and Non-Potentiality of Solar Corona: Observation and Modeling - Points Ballroom
G. Aulanier
Understanding the magnetic field and its energy content in the solar corona lies at the core of AIA/HMI science. The key challenges are the understanding of how and where is the energy injected, stored and released in the low corona. Even though potential and linear force-free fields can be used to qualitatively address these issues, they are inadequate to provide the quantitative answers. Both full MHD and non-linear force-free field modeling in 3D are clearly required. But they are very challenging to calculate and they are yet hardly constrained by, or applicable to actual observations. This tutorial will review current knowledge on these issues, identify problem areas that currently hamper our advances, and look forward to the contributions expected in the coming years. The review will discuss how the future unprecedented observations of both photospheric vector magnetic fields and coronal loops, with the new generation instruments of SOLIS, SOLAR-B and SDO, can be exploited to make critical breakthroughs.
T2Mon@ 2 Helioseismology with HMI - Points Ballroom
M. Thompson
The key HMI observational objective is to provide continuous monitoring of the structure and dynamics of the solar interior in a wide range of spatial and temporal scales, from imaging of supergranular cells and individual sunspots to the global circulation and solar-cycle changes. HMI challenges include developing sufficiently robust and efficient techniques, algorithms, and codes for global and local helioseismology measurements and inversions; forming strategies for data analyses to address specific science objectives; implementing analysis codes in the data processing pipeline; and preparing visualization and analysis tools. This turorial will review the current status of global and local helioseismology, and discuss the HMI tasks, approaches, unsolved problems, and plans.
T3Tue@ 8:30 Understanding the Photospheric and Near-Photospheric Magnetic Field and Solar Activity. - Points Ballroom
G. Fisher
Understanding the photospheric and near-photospheric magnetic field is one of the major science objectives of HMI. How do the sunspots and active regions form and evolve? How and why are the magnetic complexes of activity generated? How are the sheared magnetic field formed? What mechanisms cause the different classifications of configuration and topology of magnetic field of the sunspots and active regions? How/why are such magnetic classifications linked to solar activity? How does the dynamic of the photospheric magnetic field characterize solar transients? And how are the magnetic features related with solar irradiance variation? This tutorial will review the current status and progress on this objective, illustrate the challenges in answering these questions, identify potential contributions for addressing these issues from SDO, and discuss the techniques for magnetic and velocity field measurement.
T4Tue@ 9:15 Heating the Corona and Driving the Solar Wind - Points Ballroom
A. Van Ballegooijen
Global observations of the solar corona by SDO's AIA at a range of coronal temperatures, together with detailed spectroscopic observations from Solar-B of small regions of interest promise major advances in our understanding of the micro-scale physics of the solar corona. What determines how much heating is available for a specific volume within the solar corona? How does that energy deposition evolve in time? How important are field topology and strength? Can coronal seismology be a useful tool to understand subresolutoin properties of the coronal field? Are there common processes in open and closed fields and, if so, how can these be recognized and used to advance our understanding? How can SDO best be used to enhance our understanding of the open-field regions and of the solar wind that feeds the heliosphere?
T5Wed@ 8:30 Convection Zone Dynamics & Dynamos - Points Ballroom
M. Miesch
Three-dimensional dynamical simulations of the convection zone and tachocline and two-dimensional mean-field models of the solar activity cycle exhibit many features and processes which may be investigated using HMI and AIA data. I'll review the nature of these models and the testable predictions they make. The resolution and scope of global solar convection simulations is now sufficient to make meaningful contact with solar subsurface weather (SSW) maps on scales larger than supergranulation. Furthermore, all such simulations exhibit spatial and temporal variations in the differential rotation (DR) and meridional circulation (MC) which may be compared with helioseismic inversions. Helioseismic bounds on the structure and evolution of the DR and MC is also of crucial importance to mean-field solar dynamo models. Theoretical and numerical models of tachocline dynamics also provide testable predictions, including zonal jets and latitudinal entropy variations. In some cases, targeted helioseimic investigations may help distinguish between different models. Examples include the spatial structure of the MC and "nests" of recurring activity.
T6Wed@ 9:15 Space Weather: Needs & Users - Points Ballroom
D. Biesecker
This tutorial is intended to provide an opportunity to hear directly from a representative of the NOAA Space Environment Center (SEC) about the specific needs of SEC and its customers which might be met by SDO. The forecast center of SEC is looking forward to SDO with great expectations. Current missions such as ACE and SOHO, have been used with great success, and show how non-operational missions can be integrated into routine forecasting operations. Lessons learned from having integrated these existing missions into the forecast center will be one focus of this talk. We will also focus on the basic requirements which must be met for data to be useful to forecasters. This talk will also focus on the unmet needs currently identified by SEC which AIA and HMI might be able to address. This tutorial provides the AIA and HMI Teams an opportunity to hear directly from a representative of the space weather user community how SDO will contribute to future needs.
T7Thu@ 8:30 Solar Spectral Irradiance: From Sun to Earth, the Calibration Connection - Points Ballroom
F. Eparvier
The link between solar irradiance and Earth's upper atmosphere on all time scales is one of the most important areas of study of the SDO mission. This tutorial will give an overview of the coupling mechanisms between solar irradiance and terrestrial response. It will then focus on how measurements in the visible (with HMI) and in the EUV (with AIA) can be used, along with irradiance measurements (with EVE), to understand the solar sources of spectral irradiance variations. The review will identify where the main uncertainties are, and how they may be alleviated. It will also point out how results may depend on spectral models, abundances, potential non-LTE effects. It will also begin to prioritize some of the data products needed from the EVE/HMI/AIA science teams to advance understanding of Sun-Earth coupling through irradiance, as well as discuss the rationale for requirements on relative and absolute calibrations between past, current, and future instrumentation.
T8Thu@ 9:15 Coupling in the Sun-Heliosphere-Earth System - Points Ballroom
J. Kozyra
The Sun, heliosphere, and Earth are coupled by magnetic fields and the plasma that carries it. This tutorial reviews the coupling mechanisms between Sun and heliosphere at the top of the corona, and between heliosphere and the geomagnetic field, focusing on magnetic processes and on energetic particles. It will evaluate the advances is our understanding that are anticipated in the next few years, in particular from the STEREO mission. The review will discuss the role that SDO can play in deepening our understanding of these interface regions, with particular emphasis on what information is most critically needed about the lower boundary of the heliosphere and how the SDO science teams can develop the tools to extract that information.
Coronal Sessions: The coronal topics primarily reflect the Objectives in the AIA science plan (
Session participants are charged with completing an outline of science priorities and their rationale, required science data products, and the development of an implementation plan for the science and software needed to produce those data products.


Mon@ 3:15

Fri@ 10:30

Transients I, II: Drivers, Release, Consequences [AIA: Objective 3] - Point Alones
How does field destabilize, how does it then evolve? Where, how, how much energy is deposited, and in what form? Topics for these two sessions include: unstable field configurations and initiation of transients, evolution of transients, early evolution of CMEs, and energetic particles. Session C1 will focus on knowledge (and lack thereof) of drivers and destabilazation. C10 will focus on energy conversion, particle acceleration and propagation.
C2Tue@ 10:30 Coronal Structure Modeling -- Techniques. - Point Alones
This session will focus on disucssion of methodology for modeling coronal structures from observational data, including vector magnetic field, temperature and density. The methods include coronal field extrapolation from the vector magnetic field on the solar surface based on the NLFFF model, the coronal structures rendered from the observed coronal loops/features, and MHD simulations. Also discussed here is modeling of dynamics of coronal structure driven by observational data. Derivation of photospheric velocity fields using various techniques and the topology structure of the magnetic field will also be discussed. We will also discuss how to use these to help implement the science objectives.
C3Tue@ 10:30 Thermal Studies: Techniques - Bayview
This discussion section will address a variety of topics related to AIA science, differential emission measure (DEM) estimation, and temperature (thermal) maps. Some time will be allocated for participants to make brief presentations on the topics listed below, with ample time allocated for followup discussion. An emphasis will be given to issues which bear upon the scientific, operational, and technical aspects of DEM analysis with AIA. The principal goals for this discussion are (a) to generate commentary on issues of DEM analysis for AIA science; and (b) to promote the scientific value of DEM products in the new era of "very multi"-channel imagers.
  • Atomic and Plasma Physics Models.
  • DEM Algorithms and Techniques.
  • Data and IT Resources.
  • DEM Science.


Tue@ 1:15

Wed@ 10:30

Coronal Energy Inputs I, II [AIA: Objective 1] - Point Alones
How do magnetic field, electrical currents, and plasma enter the outer atmosphere? In what forms is energy available? Topics: 3D configurations of the corona; measuring and mapping free energy; the evolution of the field towards unstable configurations; the life cycle of the magnetic field. Session C4 will focus on theory, modeling, measurables. C6 will focus on practical application and development of metrics (and their software).
C5Tue@ 3:15 Coronal Seismology [AIA: Objective 5] - Point Alones
De Pontieu/DeLuca
What can coronal seismology, in the broadest sense of the term, teach us about the micro-physics and sub-resolution structure of the corona? Topics: wave excitation, transport and decay, probing coronal physics with waves, wave phenomena and topology.
C6Wed@ 2:30 Coronal Energy Input II: Continuation of C4. - Point Alones
C7Thu@ 10:30 Connections to Geospace [AIA: Objective 4] - Point Alones
What data can SDO provide to the user community for improved modeling and forecasting of geomagnetic events? We are interested in getting input from the coronal, heliosphere, magnetosphere, thermosphere, and ionosphere communities. In particular
  • What data would the user community like to get from SDO?
  • What observing programs, data products, cadence, resolution, etc., are needed?
  • What models and capabilities are essential to use this data in an effective way?
  • C8Thu@ 1:15 Coronal Data Products - Point Alones
    The purpose of this session is to identify the list of coronal data products needed to accomplish the five objectives of the AIA science investigation as outlined in the AIA concept study report, and categorize the associated software algorithms in one of the following categories: (1) algorithms ready to be incorporated in the JSOC pipelines today, (2) algorithms expected to be incorporated in the JSOC pipelines, but are not ready yet, (3) unclear whether algorithms will be incorporated in the JSOC pipelines, either because the algorithms are still in the nascent stages of development or because the computational demand is too high.
    C9Fri@ 8:30 Coronal Heating and Irradiance [AIA: Objective 2] - Point Alones
    What determines where and how heat is deposited into the quiescent solar atmosphere? How does plasma respond to heating? Topics: identification of features that drive irradiance variations, characterization of physical properties of coronal structures, development of loop atmosphere models, and predictive physical models for irradiance variability.
    C10Fri@ 10:30 Transients II: Continuation of C1. - Point Alones
    Helioseismology Sessions
    H1Mon@ 3:15 Local Helioseismology I: Current Issues - Point Cabrillo
    Local helioseismology already provides unprecedented views of the Sun's interior 3D structures and flows, sunspots, active regions, and even the far-side activity. These all remain critical areas for achieving the HMI science objectives. Some key questions for discussion at this session are: what are the primary targets and most critical issues of these investigations? How can we extend the local helioseismology measurements through the convection zone? What is needed to understand small-scale magnetic fields, sunspots, and active region? How best can we image the tachocline and 3D structures? What is needed to adequately measure the meridional and other 3D flows? How do we link the heliseismic measurements on different scales to the SDO photospheric, coronal and irradiance data? And how can we develop the predictive capabilities of local helioseismology.
    H2Tue@ 10:30 Magnetic Activity, Sunspots, and Active Regions - Point Cabrillo
    Incorporated in Session M1.
    H3Tue@ 1:15 Global Helioseismology: Current Issues and Collaboration with PICARD and Ground-Based Networks - Point Cabrillo
    This session will discuss global helioseismology science (e.g. chemical composition, EOS, differential rotation, the tachocline, asphericity, global magnetism, changes in stratification, radius changes, torsional oscillations irradiance variations etc), requirements for global helioseismology analyses, and also collaborations with the ground-based networks and the PICARD space mission.
    H4Tue@ 3:15 Local Helioseismology II: Techniques - Point Cabrillo
    What problems do we face in making local helioseismology techniques more reliable in time for HMI?
    As a way of kick starting the discussion, please take a look at the list below and see if any of these problems are ones that affect your research and if there are any tests you can perform that will further our understanding of how to address them in time for HMI. Which do you feel are most important? What modelling might need to be carried out, or artificial data produced to help us address these issues? What problems are missing from this list?
    Possible problems for Ring and Time-Distance Analysis, but with possible broader implications:
    • Foreshortening • Background noise • Spatially varying MTF effects (Instrumental FOV sensitivity) • Image distortions • Magnetic effects • Leaks (e.g., apodization effects on FFT) • Projection deficiencies (All projections are imperfect) • LOS effects (phase changes, distortion from center-to-limb effective height variations) • Carrington element errors • Tracking choice • Spectral line profile changes • Crosstalk between observables • Mode Asymmetry • Temporal and Spatial filter sensitivity • Why are there spatially varying frequencies or travel times across the disk? • How should time-distance data cubes be filtered before analysis?
    H5Wed@ 10:30 Numerical Simulations of Solar Oscillations and Artificial Data for Helioseismology - Point Cabrillo
    Numerical simulations are important for evaluating the accuracy of both global and local helioseismology measurements and inversions. This session will discuss various approaches to numerical modeling of solar oscillations, current results, and how these simulations can be used for validating helioseismology approximations and techniques. Special attention will be given to requirements and plans for generating artificial data sets needed for testing HMI helioseismology data products.
    H6Thu@ 10:30 Global Helioseismology Techniques & Data Products - Point Cabrillo
    While global seismology is a well established area, significant systematic errors are still present and many possibilities for improvements have not yet been investigated. In this session we will first discuss some of these issues, both regarding mode parameter estimation and inversions and try to identify the improvements we would like to have implemented in time for HMI.
    The second purpose of this session is to identify the list of global helioseismology data products be produced by the JSOC pipeline. The codes to produce these products should be selected and a working group charged with implementing the algorithms and integrating them in the JSOC pipeline should be formed.
    H7Thu@ 1:15 Local Helioseismology Data Products - Point Cabrillo
    The purpose of this session is to identify the list of local seismology data products be produced by the JSOC pipeline. The codes to produce these products should be selected and a working group charged with implementing the algorithms and integrating them in the JSOC pipeline should be formed.
    H8Wed@ 3:15 Solar Subsurface Flows - Point Cabrillo
    Hindman/J Zhao
    This session plans to addresses the following topics.
    What progress has been made in this research field and what is planned for future HMI observations?
    How can these HMI SSW maps be utilized? 3) What can they tell us about supergranular and giant-cell dynamics?
    What are the connections to active regions and coronal magnetic fields?
    What type of synoptic and predictive information can be obtained from these maps?
    What physical parameters can be deduced from the SSW data (e.g., vorticity, divergence, Reynolds stresses, kinetic helicity, etc.)?
    Where do you think we should concentrate our future efforts?
    What problems (distinct from technique issues) need to be accomplished before launch?
    What code development if any needs to be performed before launch?
    Should we organize special meetings or working groups for this topic?
    H9Fri@ 8:30 Near-Surface Seismology Effects - Point Cabrillo
    Lindsey/J Zhao
    Near-surface turbulence and magnetic fields play a critical role for global and local helioseismology measurements, causing systematic changes of oscillation power, mode frequencies, ingression and egression phases, travel times etc. Investigation of these effects is important for understanding the complex physics of the near-surface turbulent layer, magnetic field dynamics, interaction among waves, magnetic fields and turbulence, and also for improving helioseismology observations of the interior. This session will discuss key issues of the the near-surface effects, recent results obtained by data analyses and computer simulations, and plans for HMI investigations.
    H10Fri@ 10:30 Solar Cycle, Dynamo - Point Cabrillo - Point Cabrillo
    One of the most important SDO objective is investigation of the mechanisms of the solar cycle and dynamo. In this session we will discuss the critical issues and measurements for this objective, such as: does the solar dynamo work in the tachocline or in the whole convection zone, what is the origin of torsional oscillations, how are the interior changes related to the magnetic field patterns and evolution, what is the role of the meridional flow, and what are the critical measurements and data analyses that should be made by the SDO instruments for this investigations. To start the discussion on results, challenges and opportunities, we will have three short presentations on global and local helioseismology and dynamo theory (about 15 min each). The confirmed speakers are: Rachel Howe, Tom Duvall, and Mark Miesch. The other half of the session is reserved for open discussion. Participants are welcome to present one slide to advance the discussion.
    Magnetic Field Sessions
    Tue@ 10:30 Magnetic Activity, Sunspots and Active Regions - Point Cabrillo
    This session brings together theorists, modelers, and observers who use techniques of magnetism and helioseismology to study the origin and development of solar magnetic activity in order to foster collaboration, to identify scientific challenges, and to determine how HMI and AIA data products can be best used to address these challenges. What properties can be determined for specific regions and sunspots - magnetic, dynamic, helioseismic? How can AR development be forecast before or after emergence?
    M2Tue@ 3:15 Vector Magnetic Field Techniques - Bayview
    This session will cover techniques on measurement, calibration and processing of the vector magnetic field on the solar surface. We will focus on the measurement of the vector field using the filter-type magnetograph with limited wavelength samples, calibration of the instrumentation, inversion codes (progress and challenge), and techniques for resolving the 180 degree ambiguity in the measured transverse magentic field. Discussion needs also to be made on the accuracy and precision of the final calibrated products, and science requirements.
    M3Thu@ 3:15 Magnetic Field Data Products (including coronal field extrapolations) - Point Alones
    The purpose of this session is to identify the list of magnetic field data products to be produced by the JSOC pipeline. The codes to produce these products should be selected and a working group charged with implementing the algorithms and integrating them in the JSOC pipeline should be formed. Extrapolations of the coronal field are included here.
    M4Wed@ 10:30 The Large-Scale Magnetic Field - Bayview
    Incorporated in Session S3.
    M5Thu@ 10:30 Linking the Photospheric Magnetic Field with Geospace Consequences - Point Alones
    Incorporated in Session C7.
    Which quantities link the photospheric magnetic field with the geospace consequences? Can any relationships be established between the magnetic configuration and the topology of the solar origins and the magnetic clouds in the interplanetary space?
    M6Wed@ 10:30 Dynamics of Small-Scale Magnetic Field - Point Alones - Bayview
    Incorporated in Sessions C9 and S3.
    What are the significant unique contributions from HMI/AIA (high cadence, high spatial resolution, and full disk) to characterize the dynamics of the small scale magnetic field elements and to examine/modify/develop coronal heating models?
    M7Tue@ 10:30 Solar Boundary Conditions for MHD Simulations - Point Alones
    Incorporated in Session C2.
    M8Mon@ 3:15
    Tue@ 1:15
    Energy and Instability of the Coronal Magnetic Field - Point Alones
    Incorporated in Sessions C1 and C4.
    How is the non-potential (sheared/twisted) field generated? How can we estimate the energy (and energy injection into the corona)? How will we examine instability of magnetic field from the photospheric vector magnetic field?
    Other Science Sessions
    S1Mon@ 3:15 Long-term Data Bases, Operations, Intercalibration - Bayview
    SDO continues observational sequences begun with TRACE, SOHO, and several other observatories. This session addresses issues of intercalibration, overlapping operations and observations, and ensuring access to useful long-term solar data bases.
    S2Thu@ 10:30 Irradiance and EUV Calibrations - Bayview
    This session addresses calibration needs and procedures, primarily for AIA-EVE, but also for Solar-B/EIS and TRACE. How well do we need to know the relative and absolute calibrations? Where are the main uncertainties: ionization balances, abundances, spectral codes, ...? What types of overlapping observations are needed with other missions? How often does EVE science require AIA data, with what time lags in 'near-real time'?
    Wed@ 10:30 Solar Wind Prediction - Bayview
    This session focuses on modeling and eventual prediction of the state of the background (quiescent) solar wind. We will identify which parameters are needed for such models (e.g., line-of-sight and vector magnetic field data, expansion factors, densities, temperatures, etc.), and further discuss which models could/will be run, what temporal and spatial resolution is required for these models, which solar wind parameters will be predicted, what data are required to make these predictions, and how these models will be developed, validated, and run. TOPICS: There are two main types of models: the potential-field-based wind models, and MHD wind models. The session is therefore partitioned into about equal parts discussing each type of model. We have invited four speakers, who will each talk for 10 minutes. Each will be followed by a short (10-min) moderated discussion. In the remaining 10 minutes, we will wrap up and (hopefully) come to a consensus on the above points of discussion.
    S4Thu@ 3:15 Feature Recognition: Needs and Techniques - Bayview
    Aschwanden/De Pontieu/Bush
    Primary question: Who is the user community for a feature data base? Distilled from that: What do we need to recognize automatically? Which features require, or benefit from, observer assistance? Who develops software? What is needed to test and validate the software? How is the data integrated into the event logs and search engines? What external data are required (SDO, other space missions, NOAA, NSO, ...)
    S5Fri@ 8:30 The Sun Today, Events, Logs, Real-Time Data - Bayview
    This session addres the needs and plans for daily summary data products, event recognition and logs, near real-time and quick-look data products.
    S6Fri@ 10:30 Data Access: VSO, CoSEC, eSDO ... - Bayview
    The large data volume of HMI and AIA places special demands on tools and interfaces for locating, extracting, processing and delivering data to users. What products and services from AIA and HMI will be most useful to external users? How will these products and services be integrated into the larger space science community? What lessons can be learned from previous projects? Are there any emerging standards or practices that should be adopted? This session will discuss these questions to refine the design for HMI and AIA data access.
    PostersWed@ 1 Poster Session - Point Pinos
    Science Organizing Committee
    Participants are encouraged to bring posters describing work they think they need to do in order to accomplish the scientific goals of the AIA and HMI projects. This can include current work related to AIA & HMI science, development work that needs to be completed, analysis tools that require additional work, and methods that need to be evaluated. Poster presentations should also be provided in a standard electronic format for posting on the post-conference web site.
    SDO Science Working Group
    SWGWed@ 2:30

    Thu@ 8

    Science Working Group Meeting - Points Ballroom
    SWG Topics include instrument papers (book), E/PO and PAO plans, workshops, conferences, etc.