Author: J

SDO Teams Meeting

25-28 March 2008

Napa Valley MarriottNapa, California U.S.A.Purposes of the Meeting

With the launch of the Solar Dynamics Observatory, NASA's first LWS mission, only about one year away, the AIA, EVE, and HMI instrument teams of SDO are planning a 4-day joint meeting of the science teams at the Napa Valley Marriott from Tuesday, March 25 through Friday, March 28, 2008.

The meeting will bring together the co-investigator teams from the entire SDO mission and others beyond those core teams who are committed to actively participating in the science investigations.

This workshop provides an opportunity to help shape the infrastructure that enables scientists to easily find, access, and analyze data of interest in the enormous SDO archives.

Strong emphasis will be placed on planning those activities that need to be completed before launch and during the first two years of the mission.

The agenda will feature a series of (often parallel) scientific and technical working groups to discuss how the SDO data is best accessed, distributed, and analyzed, and what tools are needed to best stimulate scientific discoveries.

Posters are encouraged for science and techniques relevant to the goals of SDO.

Participation

The meeting is important for all co-I's and science team members. All EVE, AIA, and HMI science team members are invited and expected to attend. We also welcome all other members of the community who plan to significantly contribute to the science of SDO.

Tuesday @ 8:30 a.m.

SDO Project Status & Plans

Leader: Dean Pesnell

The opening session of the meeting will feature status reports from the SDO instrument teams the the SDO project.

· 8:30 SDO Project Status, Dean Pesnell

· 8:40 LWS Program Status, Lika Guhathakurta

· 8:50 SDO Program Update, Alex Pevtsov

· 9:00 Q&A, Moderated by Dean Pesnell

· 9:15 EVE Investigation Status, Tom Woods

· 9:30 HMI Investigation Status, Phil Scherrer

· 9:45 AIA Investigation Status, Alan Title

Tuesday @ 10:30 a.m.

Science & EPO Plenary

Leader: A. Kosovichev

· 10:30 Presentation of SDO Project E/PO Plans, Emilie Drobnes

10:45 Looking to the Future of Space Weather Specification and Geospace Forecasting, Dan BakerLooking to the Future of Space Weather Specification and Geospace Forecasting

Daniel N. Baker

Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO

· Recent international space science programs have made a concerted effort to study activity on the Sun, the propagation of energy bursts from the Sun to near-Earth space, energy coupling into the magnetosphere, and its redistribution and deposition in the upper and middle atmosphere. Extreme solar, geomagnetic and solar wind conditions can be observed by a large international array of satellites and ground-based sensors. We briefly discuss the types of space weather-related problems that have been identified in recent years and consider examples of space weather-induced spacecraft (and ground-based) anomalies and failures that affect both civilian and military systems. In this context, we discuss near-term plans to consolidate and integrate results from these many international programs and campaigns. An important component of this community effort is to propose technical and operational solutions to space weather problems that can be achieved in the next 5-10 years. This talk will focus on new scientific understanding that is needed for successful space weather programs and will describe actions that can help assure a good future integrated space weather program. We will particularly try to anticipate what observations and models will be needed within the geospace domain to enable successful forecasting capabilities.

11:25 Sources of Solar Irradiance Variability, Harry Warren NRL

· The physical conditions in the Earth's upper atmosphere, such as the particle density or the state of ionization, are largely determined by the magnitude and variability of the solar irradiance. As our presence in space has expanded, so has our need for timely and accurate information on the upper atmosphere. Atmospheric density measurements, for example, are needed to forecast satellite drag and predict the motion of space debris. Information on the ionosphere is needed to assess the accuracy of GPS measurements. One of the primary goals of the SDO mission is to understand the sources of irradiance variability using combined observations from EVE, AIA, and HMI. In this talk we will discuss the relationship between photospheric magnetic fields, solar features in the chromosphere, transition region, and corona, and changes in the solar radiative output at UV, EUV, and soft X-ray wavelengths. At the most basic level, changes in the solar irradiance can be understood in terms of changes in the total unsigned magnetic flux. Understanding irradiance variability in detail, however, requires determining how various solar features contribute to the radiative output of the Sun.

11:50 Recent Progress Toward Incorporating Observational Data into Theoretical Models of the Sun's Magnetic Field, Bill Abbett

· In recent years, significant progress has been made in our ability to model the Sun's magnetic field over a wide range of spatial and temporal scales, and over many physically-distinct regions of the solar atmosphere and interior. A wide range of numerical models of varying complexity are available to the Heliophysics research community, including magnetostatic models such as potential field and force-free extrapolations, and dynamic models such as radiative hydrodynamic solvers, and MHD codes. In addition, the quality and quantity of observational data continues to improve. These efforts do not proceed independently: synthetic data is routinely used to validate helioseismic and velocity inversion techniques, and observational data is used to validate, initiate, and in some cases drive numerical models. With an eye toward motivating discussion on how best the SDO data can be used to facilitate these investigations, I will briefly review recent progress toward assimilating data into models, and will describe some the theoretical challenges inherent to this process.

Tuesday @ 1:30 p.m.

Magnetic Field and Coronal Models I: Synoptic Maps and Potential Field Models

Leaders: Bill Abbett & Todd Hoeksema

In this opening session of the Magnetic Field/Coronal Modeling thread, we will begin by introducing the goals and objectives of the upcoming sessions from the perspective of the three teams HMI, AIA, and EVE. Once we have laid the groundwork for the upcoming discussions, we will then move on to a detailed discussion of how best to implement some of the more traditional models and data products into the software pipeline. In particular, we will focus on the generation of synoptic maps, farside maps, and PFSS/CSSS models.

· 1:30 - Introduction (Hoeksema)

· 1:35 - Instrument Team Needs & Plans

· HMI

· AIA

· EVE

· 2:00 - Synoptic Maps (Various)

· Synchronic & Synoptic Maps

· Synoptic Frames

· Far Side Simultations

· 2:40 - Potential and Current Sheet Models (Various)

Tuesday @ 1:30 p.m.

Thermal Structure: Recent Observations

Leader: Harry Warren

New observations from STEREO, XRT, and EIS have greatly expanded our ability to observe the thermal structure of the solar corona. These observations are likely to have important implications for the analysis of AIA observations.

Brief Talks on Recent Results (50 minutes)

· STEREO Observations of 1 MK Loops in 3D - Aschwanden (12 min)

· EIS Observations of Overdense 1 MK Loops - Warren (12 min)

· EIS Observations of Hot Lines - Patsourakos (12 min)

· XRT Observations of Active Regions - Reeves (12 min)

Discussion (40 minutes)

· What are the main observational questions that need to be pursued with AIA and how can they be achieved? For example, how can we best determine the physical parameters (e.g., density, temperature, pressure, and filling factor) of loops as a function of time with AIA? Will we need other observations (e.g., EIS density diagnostics or different vantage points from STEREO)? Are special codes needed (e.g., loop identification codes)?

Tuesday @ 1:30 p.m.

Helioseismology 1: HMI Initial Science Goals and Targets

Leaders: Juri Toomre & Sasha Kosovichev

Agenda (90 min)

· Large-scale and global MHD dynamics - Juri Toomre (15 min)

· Solar Magnetism and Dynamo - Jan Stenflo (15 min)

· Emerging Flux and Sunspots - Valentin Martinez Pillet (15 min)

· Links to coronal activity; flare and CME initiation - Brian Welsch (15 min)

· Solar shape and irradiance sources - Jeff Kuhn (15 min)

· General discussion (15 min)

Tuesday @ 1:30 p.m.

Education & Public Outreach

Leader: Emilie Drobnes & Deborah Scherrer

How do we make SDO memorable to the media and the public eye?

· Sun in 3D = STEREO

· Astronauts and pretty pictures = Hubble

· Moon = LRO

· ? = SDO

We need your help to fill in the blank!

During this break-out session we will brain storm possible media messages for SDO. These exciting and attention grabbing messages will become synonymous with our mission and help us reach out to the media and the public. This will allow us to not only share our excitement for the science being performed using SDO but help share its importance to our community and to our daily lives. We will also hold discussions on the mechanisms for getting our messages and press releases out and how best to take advantage of any and all opportunities to spread the word.

Tuesday @ 3:30 p.m.

Grand Ballroom: Cabernet & Zinfandel

Vector Field Production, HMI vs MDI intercalibration

Session Leader: Yang Liu

Vector B (3:30-5:00)

· 3:30 Intro. (Liu)

· 3:31 Update: Observing plan (J. Schou/J. Borrero)

· 3:41 Update: Calibration (J. Schou)

· 3:51 Intercalibration Discussion

· 4:01 Update: Inversion Technique (J. Borrero)

· 4:11 Update: 180-degree Disambiguation (TBD)

· 4:21 Overview: Data Processing and Products with SOLIS (C. Henney)

· 4:31 Summary of HMI Vector Field Products (T. Hoeksema)

· 4:36 Community discussion

HMI plans to provide vector field data in four categories: quick-look, standard, on-demand and on-request.

Basically, quick-look data products are mostly used for helping operating instruments and predicting space weather. Standard data products are served as monitor and reference to meet basic research needs.

On-demand data products are completed for a small fraction of data when interesting things happen or whenever requested. It is expected that this kind of data products will serve most research purposes.

On-request data products are completed when system resources allowed. The discussion is mainly focused on defining the four kinds of products.

Possible topics for discussion

· 1. Quick-look data products: Which products are needed for these purposes? Whatresolution and cadence of data are needed?

· 2. Requirements on the other three kinds of data products.

· 3. Since changes of the horizontal field could occur in fairly short time-scale, any strategies to make synoptic maps of vector magnetic field physically meaningful?

· 4. Plans for intercalibration of HMI line-of-sight fields with other instruments

1. Given the performance of these data-processing codes, what are the best cadence and resolution of the data production that fit both data processing capability and research goal?

2. Given the difference of the processing and requirement of the active regions and quiet Sun, what is the best strategy to process the full disk data?

3. What is the best way to present full disk vector field maps?

4. How to produce synoptic maps of vector magnetic field, and what kind of maps makes physics meaningful and technique doable?

Tuesday @ 3:30 p.m.

Thermal Structure: Theory

Leader: Harry Warren

This will be a session on the forward modeling of active region emission.

* Brief Talks on the Current status of Forward Modeling (30-45 minutes total)

· MHD modeling, Zoran Mikic

· Hydrodynamic Modeling, Robert Walsh

· Hydrostatic Modeling, Harry Warren

* Discussion (60-45 minutes total)

We will address several lines of questioning during the discussion:

· When will we be able to model the field, add atmospheres, compute emissions, and compare with observations?

· Is that likely to succeed in the coming few years as a routine procedure?

· Will it stay a research-grade and time-consuming thing for years to come?

· If we succeed, how do we go about learning from that?

We will also consider the various inputs to this modeling (such as magnetic field extrapolations or the instrumental temperature response functions) and consider if the MHD and hydrodynamic modeling has any special needs that need to be addressed before the data pipelines are completed. Finally, we will also discuss the status of various MHD and hydrodynamic codes.

Tuesday @ 3:30 p.m.

Local HS 2: Techniques & Comparisons, Simulations & Validations

Leaders: Deborah Haber & Tom Duvall (Part 1), Bob Stein & Konstantin Parchevsky (Part 2)

Part 1: Techniques and Intercomparison (45 minutes)

· 1. Systematic errors, Deborah Haber

· 2. Random error estimates - time-distance, Sebastien Couvidat

· 3. MDI ring diagram frequency variations, Rachel Howe)

· 4. Comparison of ring diagram and tine-distance results, Brad Hindman

· 5. Comparison of MDI, GONG with HMI, Tom Duvall

Part 2: Numerical Simulations and Validation of Local Helioseismology (45 minutes)

· 1. Realistic Non linear simulations

· Supergranulation Scale Solar Surface Convection Simulations, (8 min) Dali Georgobiani

· Realistic numerical simulations of solar magneto-convection, (8 min) Laetitia Jacoutot

· 2. Linear Wave Modeling

· Far Side Modeling (TBC), (8 min) Thomas Hartlep

· MHD simulations (TBC), (8 min) Shravan Hanasoge

· 3. General Discussion, Konstantin Parchevski

· What data are already available?

· What is being planned to be done?

· List of standard tests.

Tuesday @ 5:30 p.m.

Poster Session 1

Session Leader: Todd Hoeksema

This poster session will include a JSOC Demo and focus on Poster Group 1: SDO Science Topics

Wednesday @ 8:30 a.m.

Science Plenary + JSOC / Data Handling / Informatics

Leader: Phil Scherrer

8:30 Validating Time-Distance Helioseismology Results by Use of Numerical Simulations , Junwei Zhao, et al. Stanford University

· Authors: Junwei Zhao1, Alexander G. Kosovichev1, Robert F. Stein2, Dali Georgobiani2, Ake Nordlund3, Thomas Hartlep4, and Nagi N. Mansour4

· 1 W.W.Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA94305-4085

· 2 Department of Physics and Astronomy, Michigan State University, East Lansing, MI48824

· 3 Niels Bohr Institute, Copenhagen University, DK-2100 Copenhagen, Denmark

· 4 NASA Ames Research Center, Mailstop 230-2, Moffett Field, CA94035

· Because helioseismology is to derive solar properties that cannot be directly observed, to examine helioseismology techniques on numerically simulated data is essentially an effective way to validate these techniques. By use of realistic numerical simulation of solar convections in small scales, i.e., 96Mm in horizontal dimension and 20 Mm in vertical dimension, we have demonstrated that time-distance can satisfactorily invert flow fields up to 8 Mm or so into the interior. By use of numerical simulation of solar acoustic wavefields in global scales, we have validated the time-distance far-side imaging technique. We also demonstrate that with the help of numerical simulations, we are able to image acoustic structures in the solar tachocline area, a crucial area for solar dynamo operations.

9:00 Magnetic Fields on Multiple Scales , Sami Solanki MPI

· The part of the Sun's magnetic field accessible to observations is structured on a large variety of scales in space as well as in time. In space they reach from the highest spatial resolution currently achievable to nearly the entire solar surface. Timescales of magnetic field variation range from minutes to millenia. After a description of the current knowledge of magnetic field structuring on multiple scales some of the physical processes leading to such a structure are introduced.

· 10:00 The SDO Joint Science Operations Center, Phil Scherrer

Wednesday @ 10:30 a.m.

SDO Knowledge Base

Leader: Karel Schrijver

· 10:30 CCMC Capabilities and SDO, Peter MacNiece

· 10:45 SDO Knowledge Base - Introduction, Karel Schrijver

By about the end of 2008, SDO will give us over 2TB of data per day. That is too much for almost all of us to retrieve, store, or review on a routine basis. Finding data of interest within the vast archive of SDO data therefore requires a largely automated system to identify events, and an efficient system to find and retrieve the metadata on these events and, ultimately, link to the observations themselves.

As you hopefully know, we are developing a meta-data knowledge base (http://www.lmsal.com/helio-informatics/hpkb/) that contains information that describes what happened on the Sun. During the SDO teams meeting, we will demonstrate the developing system, and discuss with you, the user community, how the system should function, how it should present its findings in response to your queries, and what kinds of 'events' it should contain. And then, of course, we shall have to discuss which of the aspects that we would like to have are actually affordable and implementable within the coming year, and how we make optimal use with work done within the project and in the community.

Specifically:

· In the morning of Wednesday, March 26, we will present our thoughts on the system (including how our initial system focused on the Sun can grow into a broad-reaching Heliophysics system and how it complements the Virtual Observatories), demonstrate its first incarnation, discuss how features and events may be found by the analysis of the data flowing into the archive, and start a discussion on the fundamentals of the system.

Wednesday @ 2:30 p.m.

Knowledge Base Tools - Browse, Search & Output

Leader: K. Schrijver

· Visualization tools

· Interfacing with the knowledgebase

· Output: options, layout

Wednesday @ 2:30 p.m.

Space Weather - Plasmas

Leader: Frank Eparvier

This Session will focus on solar-driven particles and fields impacts on the geospace environment with the following guiding questions:

· What are the plasma forecasting/nowcasting needs of operational community?

· What's missing that SDO can provide?

· What tools need to be developed for SDO data to be used for space weather?

Tentative agenda (90 minutes total):

· Introduction - Eparvier (5 min)

· Currently Planned AIA SWx Products - (10 min)

· Currently Planned HMI SWx Products - (10 min)

· Potential EVE Plasma-related SWx Products - Eparvier (5 min)

· The NOAA/SWPC Perspective - Viereck/Onsager/Biesecker (10 min)

· The CCMC Perspective - Mac Neice/Hesse (10-15 min)

· CISM ?

· Others ?

· Discussion (30-35 min)

Confirmed participants:

· Eparvier, Woods, Chamberlin, Woodraska, & Hock from EVE instrument team Viereck, Tobiska, MacNeice or Hesse, Didkovsky, HMI SWx reps, AIA SWx reps, Others

Wednesday, 2:30 p.m.

Vector Magnetic Field Inversions - Technical Splinter

Leaders: Steve Tomczyk & Juan Borrero

Technical working session for small group involved in vector magnetic field inversions with HMI data.

· 2:30 How to choose the most adequate inversion technique for spectropolaimetric data, Basilio Ruiz

· 2:45 Community Spectro-polarimetric Analysis Center (CSAC), Bruce Lites

· 3:00 Quick-look vector field data products: emphasis on Space Weather forecasting, Steven Tomczyk

· 3:15 Standard vector field data products: HMI inversion algorithm, Juan M Borrero

· 3:30-4:00: Discussion

· Quick-look data products for space weather forecasting

· What are the important data products?

· To what accuracy are they needed?

Wednesday @ 4:15 p.m.

Knowledge Base Tools INPUT: Surface-to-Heliosphere Events

Leader: K. Schrijver

Focus on: surface-to-heliosphere events

Products: prioritized list, working groups, tasked co-Is

This session discusses events from the solar surface into the heliosphere.

· What kinds of events should be identified?

· What tools exist or need to be developed to identify the events and quantify their properties?

· What parameters should be derived/measured?

The outcome of the sessions should be a prioritized list of events that will be of most use for the community, plus plans on how to incorporate, find, and validate these.

· 10 min. Schrijver: Discussion: what types of events are needed, and what kinds of metrics/attributes should quantify them?

· 10 min. Nitta: Flares and CMEs

· 10 min. De Pontieu: Oscillation events

· 5 min. Ireland: The SIPWORK community: activities and tools

· 10 min. Berghmans: Feature finding and catalogs in Brussels

· 5 min. Eparvier: Feature needs from the irradiance perspective

· Remainder: open discussion

Wednesday -4:15 p.m.

Knowledge Base Tools - Model Events

Leader: Mark Cheung

As demonstrated in the Wednesday morning session for the Heliophysics Knowledge Base, we have laid down the infrastructure for a unified repository of features and events detected in solar and heliospheric observations. For the purposes of comparison between models and observations, and for forecasting applications, it is equally important that the Knowledge Base be able to support features and events from data-driven simulations.

In this session, we will

· Provide examples of how some `model events' can naturally be included into the current implementation of the Knowledge Base

· Explore possible improvements in design to accommodate further categories of model events and features

· Discuss how to link the Knowledge Base to existing and upcoming model repositories such as the CCMC.

Wednesday @ 4:15 p.m.

Local HS 3: Subsurface Flows; Near-surface and Magnetic Effects

Leaders: Brad Hindman, Charlie Lindsay, & Junwei Zhao

1. Helioseismic Signatures of Near-Surface Magnetic Fields (Doug Braun)

· What are the helioseismic signatures of near-surface anomalies?

· What are the effects of these on diagnostics of underlying thermal structure, flows, magnetic fields and other local physical anomalies in the solar interior?

· What are the effects of various filtering and other analytical techniques applied to seismic observations containing the signatures of near-surface anomalies?

· What can the above effects tell us about active region structure and dynamics (mode conversion, for example)?

· What can/should be done about prospective artifacts caused by near-surface anomalies?

2. Further Magnetic Effects in Helioseismic Signatures (Paul Rajaguru)

· What helioseismic signatures can be caused by variations in line profiles due to Zeeman splitting?

· What supporting research can/needs to be done to separate these signatures from those of flows, sound-speed anomalies and other objects of helioseismic diagnostics?

· What are the effects of phase-speed filtering on helioseismic diagnostics of thermal structure and flows beneath active regions?

· Can these be credibly accounted for? If so, by what means?

3. The Role of MHD Simulations in Helioseismic Diagnostics (Konstantin Parchevsky)

· What is the practicality of credible simulations of near-surface acoustics in the quiet Sun and active regions?

· What kinds of seismic environments can be simulated?

· What is the role of fully compressible simulations of convection with and without magnetic fields?

4. Large-Scale Flows (Rudi Komm)

· What is needed for diagnostics of large-scale flows in the HMI era?

· What are the effects of surface magnetic regions on seismic diagnostics of large scale flows, and how can we devise a realistic account for them?

· What resources do we need to understand what drives large-scale flows?

5. Testing Helioseismic Methods for HMI (Aaron Birch)

· What are the major control issues surrounding flows and near-surface and magnetic effects as presently understood?

· What can MHD simulations give us for testing helioseismic models of local solar interior anomalies?

· What is needed to derive realistic artificial data from simulations?

· What control facilities can be developed without recourse to detailed MHD simulations?

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A Closely Related Topic in Session on KB Tools - Helioseismic & Magnetic Events (Friday @ 10:30 a.m.)

· What can seismic emission from flares tell us about the mechanics of flares in the HMI era?

· What control facilities does seismic emission from flares offer for helioseismic diagnostics?

· What can seismic emission from flares tell us about the thermal structure and dynamics of the solar interior underlying magnetic regions?

· What supporting observations of acoustically active flares would be useful?

· What is the prospective utility of a white light flare alarm from the HMI pipeline in the solar and space-weather community at large?

· What is the practicality of such a flare alarm?

Thursday @ 8:30 a.m.

Science Plenary

Leader: Alexander Kosovichev

8:30 Links Between Internal Processes and the Dynamics of the Corona and Heliosphere , Rudi Komm

NSO

· Active regions (magnetic fields, in general) provide a point of contact between helioseismic studies of the upper convection zone and studies of the solar atmosphere. Helioseismic observations allow us to derive in detail subsurface flows and sound-speed structures associated with active regions. Recent helioseismic studies have shown, for example, that subsurface flows associated with active regions are very complex and highly twisted and that their twisted nature is related to the flare production of active regions. In this context, it is of interest, for example, to find out how the kinetic helicity of subsurface flows relates to the magnetic helicity of flux tubes. Helicity-loaded fields are very probably responsible for the most geoeffective solar phenomena such as coronal mass ejections and flares. Events in the solar atmosphere can, on the other hand, produce seismic responses such as sunquakes, acoustic events generated by flares. These sunquakes appear to be related to the acceleration and propagation of electrons and ions during the impulsive phase of solar flares. Inclined magnetic field lines can provide, quite literally, a link between interior and atmosphere acting as magnetoacoustic `portals' that allow waves, which are evanescent in a non-magnetic atmosphere, to propagate into the chromosphere. I will discuss some of the latest results and what SDO can do for understanding these links.

9:00 Energy Storage & Release in Solar Flares , Terry ForbesUNH

· Most present-day models of flares are based on the principle that the energy that drives them comes from the magnetic energy associated with stressed magnetic fields in the solar corona. A primary question regarding models of this type is the nature of the mechanism that triggers the energy release. One attractive possibility is that onset is triggered by a combination of ideal (e.g. loss of equilibrium) and non-ideal (e.g. magnetic reconnection) processes acting together. The first process can explain the rapid onset of the eruption, but the second is needed to explain the large scale of the energy release. Although quite a few models are currently being developed, many important questions about flares remain unanswered. For example, how are the currents in the corona created, and what form do they take in a three-dimensional configuration? Can models of the above type account for the acceleration of energetic protons and electrons? What kind of interaction occurs between the erupted field and the surrounding non-erupted field and can such interactions be detected?

9:30 Evolution, Dynamics and Heating of Coronal Magnetic Flux Ropes , Aad van BallegooijenSAO

· The coronal magnetic field is anchored in the photosphere and continually evolves in response to changes in the photospheric boundary conditions. At the photosphere the field is concentrated into discrete flux elements that exhibit various random and systematic motions, and these elements frequently split-up or merge with each other. New flux emerges in the form of twisted bipoles that reconnect with preexisting coronal fields, and magnetic flux may be removed from the corona by submerging below photosphere. All of these effects cause electric currents to be induced in the corona, producing a complex magnetic field that deviates significantly from a potential field. The strongest deviations occur near polarity inversion lines where highly sheared, weakly twisted magnetic fields can exist for long periods of time. These "coronal flux ropes" contain large amounts of magnetic free energy and helicity. Occasionally the flux ropes erupt, causing helicity to be ejected into the heliosphere.

· In this talk I describe various models for the structure, dynamics and heating of coronal flux ropes. Global models describe the evolution of the coronal field on time scales of many months, and are important for understanding how the helicity that emerges in active regions is spread over the quiet Sun. Local models describe how coronal flux ropes interact with the dynamic flux elements in the photosphere. I also discuss a new theory for plasma heating in coronal flux ropes. According to this theory, the energy dissipated in flux ropes has two distinct contributions: one from photospheric footpoint motions, and another from the magnetic free energy of the flux rope. It is assumed that flux ropes contain stochastic magnetic fields, and that small-scale reconnection occurs at many sites with the flux rope. The effect of such reconnection on the mean magnetic field is described in terms of hyperdiffusion, a type of magnetic diffusion in which the magnetic helicity of the mean field is conserved (Taylor relaxation). Initial results from modeling the hyperdiffusive heating of coronal flux ropes are presented.

Thursday @ 10:30 a.m.

Coronal Magnetic Field Tools and Models II: Nonlinear Force-Free Models

Leader: Marc DeRosa

In this session we will discuss non-linear force-free coronal magnetic field models. The candidate models will be discussed, along with the associated issues of how to perform the preprocessing and validation of these models. We would like to determine which model to run, and how often, taking into account the uncertainties in the resulting magnetic field models.

Schedule

· 10:30 Session intro (DeRosa)

· 10:40 NLFFF preprocessing/methods overview (Wiegelmann)

· 11:00 Loop tracing methods overview (Aschwanden)

· 11:15 Community discussion (DeRosa)

Possible topics for the discussion session:

1. Given the current state of NLFFF modeling and validation, which model results are useful to the science community? Should the results be available, warts and all?

2. How often should the NLFFF models be run? Given the currently budgeted computational resources, we will likely have to trade off between the methods and the regions of interest.

3. Do we need additional resources to develop better H-alpha data (for the preprocessing), better loop tracing algorithms (for automated validation)?

Thursday @ 10:30 a.m.

EVE and the Solar Spectral Irradiance

Leader: Harry Warren

This will be a discussion of the data products and modeling needed to derive the next generation of solar EUV and soft X-ray irradiance models. Here we will also consider the status of the EVE calibration algorithms and the cross calibration between EVE and AIA. The relationship between EVE and other long term data sets (e.g., TIMED/SEE) will also be discussed.

Brief Talks (40-50 minutes total)

· Status of EVE calibration and data processing algorithms (Frank Eparvier)

· If EVE started returning data today would we be able to produce calibrated data products?

· Cross Calibration of EVE and AIA (Harry Warren)

· This presentation will discuss several algorithms for cross calibrating the AIA imagers with the EVE spectral irradiance measurements.

· Overview Talk: Recent EUV and XUV Irradiance Measurements and Models (Phil Chamberlin)

· This talk will focus on the strengths and weaknesses of recent solar irradiance measurements and the irradiance variability models derived from them.

· Sources of EUV Irradiance Variability (Tom Woods)

· This talk will give a brief overview of some previous work on associating solar variability with the evolution of photospheric, chromospheric, and coronal features.

Discussion Topics (50-40 minutes total)

· Requirements for future model development

· How will we use SDO observations from EVE, AIA, and HMI to produce the next generation of solar irradiance models? What will the main approaches be? Pixel-by-pixel DEM? Proxies for solar activity? Decomposition of solar features? What SDO data products will we need and what development needs to be pursued to bring them together?

· Documenting Operational EUV Models (Kent Tobiska)

Thursday @ 10:30 a.m.

HS 4: SDO Helioseismology Pipeline & Data Products

Leaders: Rick Bogart & Sasha Kosovichev

Agenda (90 min)

· Data preparation: tracking, remapping, processing strategy,data for testing and validation (25 min)

· Status and plans: R. Bogart (10 min)

· Discussion (15 min)

· Data types:

· a) synoptic

· b) AR

· c) events (emerging flux, flares, CMEs, etc)

· d) validation

· e) intercomparison with MDI and GONG

· Ring-diagram pipeline: Status & Schedule (25 min)

· Organization and data products - R.Bogart (10 min)

· Techniques and discussion (15 min)

· Time-Distance Helioseismology (TDH) pipeline Status & Schedule (25 min)

· Organization and data products - A.Kosovichev (5 min)

· Techniques, performance and testing - J.Zhao (10 min)

· Discussion (10 min)

· Far-side Imaging pipeline Status & Schedule (5 min)

· Data products and implementation - P. Scherrer (5 min)

· General discussion (10 min)

Thursday @ 10:30 a.m.

Technical Session on Coronal Oscillations - I

Leader: Bart DePontieu

First of three technical discussion group focused on developing software that automatically finds locations of significant oscillatory power in the corona.

Introduction on issues facing automated software that searches for locations of significant oscillatory power (reliability, false positive, CPU load, distinguishing longitudinal/transverse/moss oscillations, etc...) [10 min, Bart De Pontieu]

Brief talks by Valery Nakariakov, Jack Ireland, Ineke De Moortel, Bart De Pontieu on results of their codes [15 min each]

Discussion of first results

Thursday @ 2:30 p.m.

Coronal Magnetic Field Tools and Models III: MHD Models

Leader: Bill Abbett

This session will focus on dynamic models. We will first describe several promising techniques that allow photospheric flows and electric fields to be determined from time-sequences of magnetograms. We will then discuss the utility and efficiency of these methods, how they are validated, and how they might be included as pipeline products. Next, we will focus on the available MHD models --- their capabilities and limitations, how they are validated, and how best to incorporate these models into the suite of user tools.

· 2:30 - Introduction, W. Abbett

· 2:35 - Determining Surface Flows & Electric Fields from Vector Magnetograms, G.H. Fisher

· 2:55 - Discussion & Planning, B.T. Welsch

· 3:05 - MHD Models

· 3:05 Deducing Active Region Fields and Plasma Properties Using 3D MHD Models with Measurements as Input, S.T. Wu

· 3:25 Global MHD Modeling in Support of SDO, J. Linker

· 3:45 - Discussion & Planning

Thursday @ 2:30 p.m.

Space Weather - Photons

Leader: Frank Eparvier

This session will focus on solar irradiance impacts on the geospace environment with the following guiding questions:

· What are the irradiance forecasting/nowcasting needs of operational community?

· What's missing that SDO can provide?

· What tools need to be developed for SDO data to be used for space weather?

Agenda (90 minutes)

· Introduction, Eparvier (5 min)

· Currently Planned EVE SWx Products, Eparvier (10 min)

· Special topic: EVE helping with the current NOAA XRS crisis, Eparvier/Viereck/Woods (10 min)

· AIA/HMI Potential Irradiance-Related SWx Products, HMI rep/AIA rep (10 min)

· The NOAA/SWPC Perspective, Viereck (10 min)

· An Operational Irradiance Modeler's Perspective, Tobiska (10 min)

· The GAIM Perspective, Tobiska/Viereck (10 min)

· Discussion (25 min)

Thursday @ 2:30 p.m.

Global Helioseismology 5: Harmonics & Peak Bagging

Leader: Jesper Schou

Spherical Harmonic Generation

· To what maximum degree, l, do we go?

· Time series length?

· Both V and I?

· Gapfilling?

Contributions welcome!

Peakbagging

· Which methods will run in the pipeline by launch (in addition to J. Schou's) ?

· What length time-series and degrees?

· What other options?

· What are the advantages of the alternate methods at various degrees.

Likely speakers: Rachel Howe, Tim Larson, Ed Rhodes, Sylvain Korzennik/Cristina Coares Additional contributions welcome!

Thursday @ 2:30 p.m.

Technical Session on Coronal Oscillations - II

Leader: Bart DePontieu

Continuation of small technical discussion group focused on developing software that automatically finds locations of significant oscillatory power in the corona.

This session focuses on discussion of the effects of rebinning (how much can we rebin before losing crucial information), derotating data, despiking data, time range, etc... on finding locations with significant oscillatory power with the various codes.

Thursday @ 4:15 p.m.

Coronal Magnetic Field Tools and Models IV: Topology

Leader: Y. Liu

This session will focus on determination of topology structure in solar active regions. Recent studies show that topology structure can effectively classify active regions and pinpoint locations where magnetic reconnection occurs that leads to occurrence of solar eruption. Many techniques have been reported to be able to determine topology using observational data, and some of them shows potential to be robust and automatic. In this session, we will first describe several promising techniques. We will then discuss the tools to effectively present the topology result in a way that people can easily understand. Next we will discuss any possibilities for putting this structure into the pipeline as a product. We will also discuss matrix for validation of the results. We end up with a discussion whether or not we need a working group on this topic, and what the plan will be if we want to have one.

Schedule:

· 4:15 Coronal Magnetic Topology: How to Characterize it --- and Why (D. Longcope)

· 4:45 Topological Evolution & Magnetic Reconnection (C. Parnell)

· 5:05 The structure of eruptive magnetic fields and its relation to observational features" (V.S. Titov, Z. Mikic, J.A. Linker, and R. Lionello)

· 5:25 Community discussion (Y. Liu)

Discussion topics:

1. Find the best way to present topology structure

2. Which algorithm potentially to be automated

3. Validation

4. Ready to be a pipeline product?

5. Need a working group?

6. Plan toward a pipeline module

Thursday @ 4:15 p.m.

Vintner's Ballroom

DEM - Differential Emission Measure - Part 1

Leaders: Mark Weber and Paul Boerner

This is the first of two sessions on using AIA data for thermal (especially DEM) analysis. In this session, we will discuss the techniques and challenges of constraining a DEM using AIA, including instrumental calibration; atomic and plasma physics; spectral codes; and inversion techniques.

Brief Talks

· Regina Soufli (~10 min + discussion): Calibration of the EUV bandpasses on AIA

· Vinay Kashyap (~20 min + discussion): Overview of atomic physics issues; statistical uncertainties in DEM inversion

· Additional brief talks on DEM inversion techniques/applications welcome

Discussion Topics

In addition to the discussion of the specific issue raised in the talks, we will attempt to cover some of the broader issues, such as:

· What is the best way to identify and track the uncertainties in DEMs obtained from AIA data?

· What can be done to reduce the uncertainties involved in the instrument calibration, abundances, line strengths, and other atomic/plasma physics issues that go into DEM analysis?

· What inversion techniques are likely to prove most appropriate for AIA?

Thursday @ 4:15 p.m.

Global Helioseismology 6: Inversions and the MDI->HMI Transition

Leader: Jesper Schou

Inversions

· Which code are we going to have running?

· How automated?

Likely speakers: Sarbani Basu/Charles Baldner Additional contributions welcome!

The MDI to HMI Transition

· What types of comparisons/validations do we do?

· Dopplergrams? Time-series? Power spectra? Mode parameters? Inversions?

Likely Speaker: Rachel Howe Additional contributions welcome!

Thursday @ 4:15 a.m.

NVB:Stag's Leap

Trying out the Heliophysics Knowledge Base

Leader: KB Team

Get some hands on experience with the Knowledge Base as it is currently implemented.

Friday @ 8:30 a.m.

Collaborative Science - SDO's contribution to the Great Observatory

Leader: Mark Cheung

This brief introduction to a discussion of Collaborative Science will include two 10-minute talks

· S. Gibson - Science Planning of Coordinated Observing Campaigns: Lessons for the SDO Era

· K. Reeves - Coordinating observations: Lessons Learned and Wish List

We will then break into three splinter sessions to discuss ways to organize collaborative science.

SDO will make a key contribution to coordinated solar/heliospheric observational campaigns. Although SDO will provide continuous full-disk coverage, there is still a critical role for the active participation of SDO science teams in the planning of coordinated science campaigns. The reason is simple: given the immense data volume expected from SDO, one must plan in advance the best way to extract data from the archive not already delivered by the standard data pipeline (e.g. disambiguated vector magnetograms at a very high cadence, DEM inversions at full AIA resolution for a subregion etc.). In short, one must plan to "observe the SDO data archive."

Friday @ 9:00 a.m.

Heliophysics Observatories Bulletin Board: Design and implementation

Leaders: Mark Cheung

The aim of setting up a Heliophysics Observatory Bulletin Board is to encourage coordinated Heliophysics observations even when no joint observing programs have been planned and agreed upon. The concept of the Bulletin Board is to allow observers using different instruments/observatories to post up-to-date information (e.g. field of view of telescope) about their most recent (e.g. last 24 hours), current and planned upcoming (e.g. next 24 hours) observations. The anticipation is that if everyone knows what everyone else is/was observing, there will be a better chance of matching up complementary data sets for collaborative science studies.

One possible design of the Bulletin Board may simply be a webpage with an SDO image of a solar disk, overlaid with bounding boxes indicating the fields of view of different observatories in the same time period. Latest events and features from the Heliophysics Knowledge Base may also be included to provide context.

Everyone is invited to participate in the discussion to help design this system.

Friday @ 9:00 a.m.

Campaign Coordination in the SDO Era

Leaders: Sarah Gibson & Kathy Reeves

SDO will routinely provide comprehensive synoptic support for observing campaigns, but also has specific contributions it can make to campaigns. These include helpful resources for the planning process (daily summary observations etc.) but also special methodologies for observing the SDO data archive in ways that may be different than routine data processing pipeline.

In this splinter session we will discuss the state of the art in terms of resources for planning and coordinating observing campaigns, and assess what works well (or doesn't work well) already. We will consider what resources are missing or should be developed in light of the unique demands of future observations (e.g. high volume, etc.).

Friday @ 9:00a.m.

Technical Session on Coronal Oscillations - III

Leader: Bart DePontieu

Conclusion of small technical discussion group focused on developing software that automatically finds locations of significant oscillatory power in the corona.

We wrap up with discussions of how to proceed with interfacing with the knowledgebase, how to distinguish longitudinal/transverse/moss oscillations in an automated fashion, how to analyze properties of oscillations/waves in an automated fashion, etc...

Friday @ 10:30 a.m.

Magnetic Connections to the Heliosphere

Leader: Kelly Korreck

Likely presenters: Barbara Thompson, Kelly Korreck

In order to utilize the SDO data to the fullest, the solar data must be linked through modeling and observation to the heliosphere. Several models already exist and are readily available at the CCMC. The goals of this session:

· To identify complementary data sets that can be used with SDO- EVE, AIA, and HMI data (for example, ACE SWICS data, Stereo or Ground based radio observations)

· Identify the science topics that can reap the most benefit from the collaboration

· Source Regions of the solar wind

· CME initiation, liftoff and propagation

· Composition and Temperature of unprocessed solar wind

· To identify the current and/or future models (MHD, energetic particle transport etc) that will aid in this comparison

· To determine ways in which the CCMC can become involved with the larger effort

Agenda

· 10:30-10:35 Introduction to Session (Korreck)

· 10:35-10:50 Links of SDO data products to Heliosphere (Thompson)

· 10:50-11:05 LWS Capabilities (Marc DeRosa)

· 11:05-11:20 CISM plans (TBC)

· 11:20-11:40 Identify the SDO/Heliospheric data links and responsible individuals for their creation

· 11:40-12:00 Identify the SDO/Heliospheric coding connections and the responsible individuals

The last two items will be open discussions to look specifically at the goals of this session and identify the next action steps.

Friday @ 10:30 a.m.

Vintner's Ballroom

DEM - Differential Emission Measure - Part 2

Leaders: Mark Weber and Paul Boerner

Thermal studies with AIA

This is the second of two sessions on using AIA data for thermal (especially DEM) analysis. In this session, we will focus on the application of DEMs or related thermal data products from AIA. In particular, we will focus on two questions:

· How can DEMs be used to gain a deeper understanding of the physics of the solar atmosphere? How do they interface with physical models of coronal structures?

· Should there be an "automated DEM data product" that continuously produces thermal maps or shorthand DEMs at some substantial fraction of the AIA cadence and resolution? If so, what should that automatic DEM data product look like? What would it be used for?

Brief Talks

· Markus Aschwanden (~10 minutes + discussion): forward-modeling of theoretical DEMs (based on hydrodynamic evolutions of heating and cooling processes) to observations

· Mark Weber/Paul Boerner (~20 minutes + discussion): the Automated DEM data product; responses to a survey of potential end-users, and presentation of a strawman data product concept

Discussion Topics

In addition to the discussion of the specific issues raised in the talk, we will cover the broader issues of how DEMs can be used to do science, and how DEM-related thermal data products can be used to enhance the value of the AIA data

Friday @ 10:30 a.m.

Grand Ballroom: Syrah & Merlot

Knowledge Base Tools INPUT: Helioseismic & Magnetic Events

Leader: S. Kosovichev

This session discusses events below the solar surface that will be identified and analyzed with helioseismic tools, and related to the surface events and features. What kinds of events should be identified? What tools exist or need to be developed to identify the events and quantify their properties? What parameters should be derived/measured? The outcome of the sessions should be a prioritized list of events that will be of most use for the community, plus plans on how to incorporate, find, and validate these.

· A.Kosovichev, Introduction (5 min)

· A. Pevtsov, Characterization of magnetic properties of active regions (10 min)

· M. Hagenaar, Identification of emerging and ephemeral active regions (10 min)

· D. Haber, Characterization of sub-surface flows of emerging and evolving active regions (10 min)

· R. Nightingale, Detection and characterization of rotating sunspots (10 min)

· H. Wang, Characterization of pre-flare magnetic structures and flows (10 min)

· I. Gonzalez Hernandez, Identification of far-side events (10 min)

· C. Lindsey, Detection of flare oscillations and white-light flares (10 min)

· General discussion (15 min)

Friday @ 1:30 p.m.

AIA Early Observing Modes

Leader: Alan Title

Discussion of early modes of observation with the AIA instrument

Friday @ 1:30 p.m.

Knowledge Base: Technical Session on Keywords, Metadata, and IDs

Leaders: Neal Hurlburt

· Reports from Weneday KB Sessions, Session 'secretaries'

· Task list

This session will collect the results from the earlier knowledgebase sessions, and translate the discussions into lists of event types, their attributes, and properties.

A task list will be compiled along with an implementation plan for the next 12 months.

Friday @ 3:30 p.m.

SDO Science Working Group

Leaders: Dean Pesnell

Publication of Instrument Papers and other SDO science team project and programmatic topics

Author: Markus J. Aschwanden

Institution: LMSAL

Email: aschwanden@lmsal.comPoster Title:

Coronal Loop Modeling with non-equilibrium hydrodynamic models

Abstract:

We approximate the hydrodynamic evolution of the heating and cooling phase of coronal loops with analytical models that reproduce the non-equilibrium states, which allows us to model data analysis of EUV data from SOHO, TRACE, STEREO, HINODE, and SDO/AIA. Using these models we retrieve information onthe non-equilibrium heating and cooling phases.

Author: Auchere, F., Soubrie, E., Bocchialini, K.

Institution: Institut d'Astrophysique Spatiale

Email: frederic.auchere@ias.u-psud.frPoster Title:

FESTIVAL: A Multiscale Vizualisation Tool for Solar Images

Abstract:

We present here FESTIVAL, a SSW package originally developed to be able to map the SECCHI data into dynamic composite images of the sky as seen by the STEREO and SOHO probes. The five SECCHI instruments image the solar corona and the heliosphere on a wide range of angular scales, which causes a data visualization challenge. Similarly, the very large format of AIA data will prevent them from being visualized at once on a computer display. With FESTIVAL, the user can quickly and easily (with the mouse) zoom in and out and pan through these composite images to explore all spatial scales from EUVI to HI2 while keeping the native resolution of the original data. A large variety of numerical filters can be applied, and context data (i.e. coordinate grids, stars catalogs, etc.) can be overlaid on the images.

Author: V. Barra, V. Delouille, J.-F. Hochedez, J.M. Krijger

Institution: SIDC, Royal Observatory of Belgium ; LIMOS, Université Blaise Pascal Clermont II

Email: krijger@sidc.bePoster Title:

SPoCA: A Spatial Possibilistic Clustering Algorithm for EUV images

Abstract:

The study of the variability of the solar corona and the monitoring of its traditional regions (Coronal Holes, Quiet Sun and Active Regions) are of great importance in astrophysics as well as in view of the Space Weather and Space Climate applications.

We propose 'SPoCA', a Spatial Possibilistic Clustering Algorithm that

automatically segments EUV solar images into Coronal Holes, Quiet Sun and Active Regions. The use of fuzzy logic allows to manage the imprecision in the definition of the above mentioned regions. The process is fast and automatic. Moreover, when combined with a movement estimation method it allows to track Active Regions and Coronal Holes. SPoCA is applied to SoHO-EIT images taken from January 1997 till May 2005, spanning thus almost a full solar cycle. Results in terms of areas and intensity estimations are consistent with previous knowledge. The method reveal the rotational and other mid-term periodicities in the extracted time series across solar cycle 23. Further, such an approach paves the way to bridging observations between spatially resolved data from imaging telescopes and time series from radiometers.

Author: J.G. Beck, J Zhao, T.L. Duvall, Jr

Institution: Stanford Solar Observatories Group

Email: Beck@Sun.Stanford.EDUPoster Title:

Time-Distance Errors Due to Data Gaps

Abstract:

Time-distance measurements have provided a wealth of information about the layers beneath the photosphere. Cubes of tracked data are analyzed to find cross-correlations in the wave signals at different spatial locations. These cross-correlations yield travel times for wave packets which can be interpreted as various properties of the plasma through which the wave propagate. Often there are images which are missing or of low quality which must affect the cross-correlations and travel-time measurement. We examined the errors in travel time (and dependent quantities) due to data gaps in the time-series and compare common gap-filling techniques.

Author: Kelly Beck

Institution: Haas Center for Public Service, Stanford University

Email: kbeck@stanford.eduPoster Title:

Science in Service: Developing Leadership in Science Outreach

Abstract:

As part of their SDO outreach efforts Phil Scherrer and the Stanford Solar Observatories Group partnered with Stanford University's Haas Center for Public Service to develop a k-12 outreach program that involved the University's undergraduate science students. This paper will describe the resulting program called Science in Service, through which Stanford students are trained in best practices for teaching science and in principles of effective public service. The students then mentor science to children in local after-school programs. Details of the program will be described.

Author: Kevin Belkacem, Reza Samadi, Marie-Jo Goupil

Institution: Observatoire de Paris - Meudon

Email: kevin.belkacem@obspm.frPoster Title:

On the Amplitude of High-Angular-Degree P Modes

Abstract:

We have recently generalized the formalism of stochastic excitation of radial p modes to non-radial ones, which enables us to estimate the energy supplied to high-angular degree acoustic modes. We present the theoretical results obtained for those modes and emphasize the necessity to obtain accurate enough observational data for both the height and line-width of modes so as to get physical constraints on the upper-most layers of the solar

convection zone.

Author: Elena E. Benevolenskaya

Institution: Stanford University

Email: elena@sun.stanford.eduPoster Title:

Relationship between EUV corona and phospheric magnetic activity.

Abstract:

Solar Dynamic Observatory is coming to provide us EUV coronal and vector magnetic field data. It helps more detaily understand a relationship of the coronal and photospheric activity in the new solar cycle 24. Because of, the solar corona in Extreme-Ultraviolet emissions is visible on the solar disk, it is a good opportunity to investigate the coronal and magnetic activity, simultaneously.

Now, the EUV data of Extreme Ultraviolet Telescope (EIT) on board SOHO are available since 1996 up to the present time. And, here, we have represented the EUV data from SOHO/EIT in four wavelengths (171A, 195A, 284A, and 304A) in the form of coronal synoptic maps for 1996-2006. Our results reveal that the evolution of the coronal structure is closely related to the changing of the topology the magnetic activity. EUV synoptic investigations also find a strong solar cycle dependence which is presented in high and mid latitude.

Author: T. E. Berger

Institution: Lockheed Martin Solar and Astrophysics Lab

Email: berger@lmsal.comPoster Title:

Hinode/SOT Observations of plume upflows, cascading downflows, and oscillations in quiescent solar prominences

Abstract:

The Solar Optical Telescope (SOT) instrument on the recently launched Hinode satellite has obtained new observations of solar prominences in both the Ca II 396.8 nm “H-line” and the H I 656.3 nm Balmer-alpha (Hα) spectral bandpasses. The SOT prominence observations are characterized by spatial resolutions from 170 to 220 km, temporal resolutions of 30 to 40 seconds, and unprecedented temporal stability : 5 hour duration, diffraction-limited, movies of prominences are regularly obtained by the SOT. Here we show preliminary analyses of the prominence dynamics observed by SOT. One of the most striking SOT discoveries to date is the observation of impulsive dark upflows frequently seen ascending with ~20 km/sec speeds in quiescent prominences. The upflows originate below the prominence, show turbulent flow structuring, and rise to heights of 10--20 Mm above the photosphere. The dynamics of the flows implies that they are buoyant thermal plumes generated by an episodic mechanism in the photosphere or lower chromosphere. The existence of the plumes has implications for the prominence and cavity mass balance.

Author: T. E. Berger, G. L. Slater, R. Shine, T. D. Tarbell, A. M. Title, B. Lites, J. Okamoto, Y. Katsukawa, K. Ichimoto, Y. Suematsu, T. Sekii, T. Shimizu, S. Tsuneta

Institution: LMSAL, NAOJ

Email: berger@lmsal.comPoster Title:

Hinode/SOT Observations of Plume Upflows, Cascading

Downflows, and Oscillations in Quiescent Solar Prominences

Abstract:

We present the latest findings on quiescent prominence structure and dynamics from the Hinode/SOT instrument. The data show that quiescent prominences appear in two broad classes: vertically and horizontally structured. The reason for the delineation in appearance is not clear but may be related to line-of-sight angle and/or magnetic field strengths. In vertically structured prominences SOT observations reveal constant downflow streams with speeds of ~10 km/sec, frequent vortex flows, large scale "body" oscillations with periods on the order of 10 minutes and propagation speeds of ~10 km/sec, and, most surprisingly, episodic dark turbulent plume upflows with speeds of ~20 km/sec. The dark plumes originate below the base of the prominence and propagate upward to typical heights of 10 Mm or more. The speed of the plumes is relatively constant, as expected for thermal plumes balanced by fluid dynamic drag. The plumes represent a new source of prominence mass and may play a significant role in maintaining prominence structure against gravitational draining in the downflows.

Author: D. Berghmans and the SWAP team

Institution: Royal Observatory of Belgium

Email: david@oma.bePoster Title:

SWAP, yet another EUV imager launched soon

Abstract:

SWAP is a small EUV imager onboard PROBA2, an ESA technology demonstration platform. SWAP will image the solar corona in 17.5nm on a 1024x1024 CMOS APS detector at a 1 min cadence. PROBA2 was originally planned for launch in 2005 and would have been a useful addition to EIT (but with higher time resolution) and EUVI (but Earthbound). However, due to several delays, PROBA2 will now be launched in mid 2009 and will thus fully overlap with the SDO/AIA lifetime. In this poster we will explore the potential of SWAP and its possible synergies with the AIA imagers.

Author: D. Berghmans, B. Nicula, C. Marque

Institution: Royal Observatory of Belgium

Email: david@oma.bePoster Title:

The Solar Weather Browser, Recent Progress and Usage for AIA

Abstract:

We present version 1.2 of the Solar Weather Browser (SWB). The main innovation is its capability to combine data and metadata from multiple sites. This is important in relation to data distributed over different servers at different sites, as in Virtual Observatory networks. For example, the SWB will be the reference visualization platform for SOTERIA, a network of solar ground-based observatories funded by the EU. In this poster we will address in particular, our plans for visualizing AIA data and combining with metadata extracted from feature recognition processing chain developed at ROB.

Author: Luca Bertello, Roger K. Ulrich, John E. Boyden, and L.Webster

Institution: University of California, Los Angeles

Email: bertello@ucla.eduPoster Title:

Calibration of the magnetic field Strength

Abstract:

Photospheric magnetic field maps are the primary drivers of coronal and heliospheric models, and their calibration will ultimately test the diagnostic capabilities of these models. The determination of the solar magnetic field strength is one of the most difficult tasks in the construction of these maps. It is however a critical step to proper model the heliosphere. The solar physics group at UCLA has dedicated an extensive effort to this task, in particular with the interpretation of MDI and MWO magnetic field strength observations.

In an effort to improve our knowledge for the calibration of the future magnetic observations made by the HMI instrument aboard SDO, we have carried out a new series of observations aimed at establishing a more complete understanding of the scale factors relating different observing methodologies for determining the photospheric field strength.

During the interval 18 April 2007 to 8 May 2007 a set of five special magnetograms were obtained using the 24-channel system at the 150-foot solar tower telescope on Mount Wilson. The special spectrograph configuration used for these observations allowed us to compute the magnetic field from five different spectral sampling pairs of FeI 5233, in addition to the standard sampling of FeI 5250 usedas a part of the Mount Wilson synoptic program of magnetic observations. The analysis of these measurements and the main results are described in this poster. In particular, we derived a new scale factor to obtain unsaturated estimates from FeI 5250 magnetic field measurements which would have been measured at FeI 5233.

Author: S. Buhr, M. McCaffrey, M. Murillo, F. Eparvier

Institution: CIRES, St. Vrain School District and MESA program, LASP

Email: mark.mccaffrey@colorado.eduPoster Title:

A Partnership Between English Language Learners and a Team of Rocket Scientists: EPO for the NASA SDO Extreme Ultraviolet Variability Experiment

Abstract:

Extreme-Ultraviolet Variability Experiment (EVE) project. The students were enrolled in a pilot course as part of the Math, Engineering and Science Achievement MESA) program. For many of the students, this was the only science option available to them due to language limitations. The English Language Learner (ELL) students doubled their achievement on a pre- and post-assessment on the content of the course. Students learned scientific content and vocabulary in English with support in Spanish, attended field trips, hosted scientist speakers, built and deployed space weather monitors as part of the Stanford SOLAR project, and gave final presentations in English, showcasing their new computer skills. Teachers who taught the students in other courses noted gains in the students' willingness to use English in class and noted gains in math skills. The MESA-EVE course won recognition as a Colorado MESA Program of Excellence and is being offered again in 2007-08. The course has been

Broken into modules for use in shorter after-school environments, or for use by EVE scientists who are outside of the Boulder area. Other EVE EPO includes professional development for teachers and content workshops for journalists.

Author: R Burston, L Gizon, Y Saidi

Institution: Max-Planck-Institut für Sonnensystemforschung

Email: burston@mps.mpg.dePoster Title:

German Data Center for the Solar Dynamics Observatory

Abstract:

The German Data Center (GDC) for the Solar Dynamics Observatory (SDO), hosted by the Max Planck Institute for Solar System Research, will provide SDO data access to the German solar physics community. The GDC-SDO will make available all the relevant HMI data for helioseismology and smaller selected AIA data sets. This project is funded by the German Aerospace Center (DLR) until 2012.

An important component of the GDC-SDO is the Data Record Management System (DRMS), developed and distributed by the Stanford/Lockheed Joint Science Operations Center (JSOC). The DRMS is currently fully operational at the GDC-SDO. Efforts are underway to design a GDC-SDO data processing pipeline. The GDC-SDO hardware will comprise 2x 16 CPU core machines to run the DRMS software and deliver rapid searches through a PostgreSQL database, a 16 CPU core machine for preprocessing the data, and 3x 48 TB hard disks for storage, which all communicates over a fast InfiniBand network. A 160 TB tape library/robot will provide near-line data storage. Additional information about the GDC-SDO can be found at http://www.mps.mpg.de/projects/seismo/GDC1/index.html.

Author: O. Burtseva and F. Hill

Institution: NSO/GONG, 950 N. Cherry Ave., Tucson, AZ 85719

Email: burtseva@noao.eduPoster Title:

Lifetimes of high-l solar p-modes: effect of surface activity

Abstract:

We study effect of surface activity on measurements of lifetimes of high-l solar p-modes with SOHO/MDI data using time-distance technique. Active regions were masked out and lifetimes with and without masking of active regions were compared. Obtained results will be discussed.

Author: B.W. Caplins (1), D.A.N. Mueller (1), J. Ireland (2), G.Dimitoglou (1), B. Fleck (1)

Institution: (1) European Space Agency at NASA GSFC, (2) ADNET Systems at NASA GSFC

Email: dmueller@esa.nascom.nasa.govPoster Title:

J HelioViewer - A JPEG 2000 Solar Image Browser

Abstract:

We present a prototype of a novel solar data browser geared towards SDO's AIA data. It is based on the JPEG 2000 compression standard for highly efficient browsing in time and space. Our approach is both flexible, scalable and platform-independent. The random code stream access of the JPEG 2000 interactive protocol minimizes data transfer and can encapsulate meta data as well as multiple spectral channels in one data stream. This approach is therefore perfectly suited for dealing with the large volume of AIA data.

We present progress made in developing the required technologies to enable the various interacting components of J HelioViewer. We discuss the synergy and eventual merging with the tile-based HelioViewer (see poster of J. Ireland et al.) and the feasibility of making the full SOHO and SDO science data catalogs intuitively browsable with this new tool.

Author: Phillip C. Chamberlin, Thomas N. Woods, Francis G. Eparvier

Institution: LASP/U. of Colorado

Email: phil.chamberlin@lasp.colorado.eduPoster Title:

SDO EVE Contributions and Improvements to the Flare Irradiance Spectral Model (FISM)

Abstract:

The Flare Irradiance Spectral Model (FISM) is a model of the solar spectral irradiance from 0.1-190 nm with a temporal resolution of 1-minute. FISM daily values are currently based on measurements from TIMED SEE, UARS SOLSTICE, and SORCE XPS. SDO EVE will provide daily measurements of the solar XUV and EUV (0.1-105 nm), as well as Lyman Alpha (121.6 nm), at a much higher accuracy and spectral resolution, especially below 27 nm, than these aforementioned measurements. EVE will allow FISM to make more accurate irradiance estimations, and will also allow FISM to improve its spectral resolution to 0.1nm. The FISM flare estimations are currently based only on 39 flares at various stages in the flare evolution from TIMED SEE and SORCE XPS. SDO EVE, with its ~100% duty cycle, will observe a large number of flares during solar cycle 24, and will observe the entire evolution of the flares concurrently at all wavelengths. Therefore, SDO EVE will also help lower the uncertainties of the FISM flare estimations. FISM will also be updated to use the SDO EVE space weather product as its proxies, which will also provide more representative, multiple wavelength flare proxies besides the GOES XRS and its derivative.

Author: Sebastien Couvidat

Institution: HEPL, Stanford University

Email: couvidat@stanford.eduPoster Title:

Thermal or Magnetic Origin of the Sound-Speed Perturbations Below Sunspots?

Abstract:

We apply the time-distance formalism on Doppler velocity data of 12 solar active regions observed by SOHO/MDI between 1997 and 2006.

Maps of the travel-time perturbations of acoustic waves are produced for 36 distances between source and receiver, and inverted for sound-speed perturbations below the solar surface down to 26.8 Mm.

The well-known two-region subsurface structure of a sunspot (a shallow region of decrease in sound-speed immediately below the surface followed by a region of increase in sound-speed deeper inside the Sun) is observed for every active region. We observe strong relations between surface line-of-sight magnetic flux, surface umbral temperature, and amplitudes of the sound-speed perturbation below the surface and transition depth between the two regions. These relations are used to comment on the hypotheses that the two-region structure is a thermal effect or a magnetic one.

Author: Ashley Crouch, Graham Barnes, KD Leka

Institution: NWRA/CoRA

Email: ash@cora.nwra.comPoster Title:

Ambiguity Resolution for the HMI Pipeline

Abstract:

We will give a status report on the tools that will be used to disambiguate the vector magnetogram data produced by the HMI pipeline. These are based on one of the best available methods for single height data and involve the global minimization of the "energy" over the field of view (here "energy" is a combination of the current and the divergence of the field). We test these methods on artificial data for active region patches and full-disk.

Author: J.L. Culhane, E.C. Auden, Y. P. Elsworth, A. Fludra, M. Thompson

Institution: Mullard Space Science Laboratory, University College London,

Email: jlc@mssl.ucl.ac.ukPoster Title:

eSDO: Algorithms, Visualization Movie Tool, and AstroGrid Data Integration

Abstract:

The UK-based SDO e-Science consortium has been funded by PPARC, now STFC, as a three year project to work with US SDO investigation teams to extract data products and enable data access by the UK Solar Physics community. Following a year of research into meeting the UK solar community’s needs through algorithms, data centre access and visualization tools, two years of eSDO development and implementation began in October, 2005. For more details, please visit http://www.mssl.ucl.ac.uk/twiki/bin/view/SDO.

The final project report and all code will be available from 1 October 2007 at http://www.mssl.ucl.ac.uk/twiki/bin/view/FinalDeliverables.

Author: I. De Moortel (1), S.J. Bradshaw (2)

Institution: (1) School of Mathematics and Statistics, University of St Andrews, UK; (2) Space and Atmospheric Physics Department, Imperial College London, UK

Email: ineke@mcs.st-and.ac.ukPoster Title:

Estimating Damping Rates of Intensity Oscillations Observed with AIA/SDO

Abstract:

Forward modelling is used to investigate the relation between given temperature and density perturbations and the resulting (synthesised) intensity perturbations. Complex and highly non-linear interactions between the components which make up the intensity (density, ionisation balance and emissivity) mean that it is non-trivial to reverse this process, i.e. obtain the density and temperature perturbations associated with observed intensity oscillations. In particular, it is found that the damping rate does not often 'survive' the forward modelling process, highlighting the need for a very careful interpretation of observed (intensity) damping rates. Although we use TRACE intensity oscillations as an example, the same effects are likely to be present in observations made by AIA/SDO.

Author: J. de Patoul, B. Nicula, J.M. Krijger, D. Bergmans, O. Podladchikova, S. Willems, B. Inhester, T. Wigelman, M. Kretzschmar

Institution: SIDC, Royal Observatory of Belgium ; Max Planck Institute for Solar System Research, Germany ; LPCE/CNRS Université d'Orleans, France

Email: krijger@sidc.bePoster Title:

SOFLEX, SOlar FLare EXtractor

Abstract:

The SOlar FLare EXtractor (SOFLEX) is built in order to study flare

events: to have a better understanding of the time profile of the event itself in different wavelengths and to have the full understanding of the behaviors of the flares through the solar cycle. In the first hand SOFLEX is a software package able to detect EUV flares in EUV data images, such as available from EIT and STEREO and soon SDO, with its principal characteristics. In the second hand, it allows of improving significantly our understanding of EUV flares phenomena with respect to better studied X-ray flaring processes.

Author: B. De Pontieu [1], S. McIntosh [2], V. Hansteen [3,1], M. Carlsson [3], T. Tarbell [1]

Institution: [1] LMSAL, [2] HAO, [3] University of Oslo

Email: bdp@lmsal.comPoster Title:

Hinode and the Corona's lower boundary: Spicules and Alfven Waves

Abstract:

Recently, observations with the Solar Optical Telescope (SOT) onboard

Hinode and ground-based telescopes combined with advanced numerical

simulations have provided us with unprecedented views and a better

understanding of the dynamics of the chromosphere and how the lower

boundary couples to the corona and solar wind.

We provide an overview of these results, with a focus on spicules and

Alfven waves and the implications for SDO observations. We show that

the dynamics of the magnetized chromosphere are dominated by at least

two different types of spicules -- dynamic jets of plasma that shoot

upward at velocities of order 20-150 km/s. We show that the first

type involves up- and downward motion that is driven by shock waves

that form when global oscillations and convective flows leak into the

chromosphere along magnetic field lines on on 3-7 minute

timescales. The second type of spicules is much more dynamic, forming

on timescales of 10s, and is most likely formed as a consequence of

magnetic reconnection, and may have a significant impact on the

coronal energy balance.

Our analysis of Hinode data also indicates that the chromosphere is

permeated by strong Alfven waves. Both types of spicules are observed

to carry these Alfven waves, which have significant amplitudes of

order 20 km/s, transverse displacements of order 500-1,000 km and

periods of 150-400 s. Estimates of the energy flux carried by these

Alfven waves and comparisons to advanced radiative MHD simulations

indicate that these waves most likely play a significant role in the

acceleration of the solar wind. We will discuss the implications of

these waves on the energy balance of the lower atmosphere.

Author: DeForest, C.E.

Institution: SwRI

Email: deforest@boulder.swri.eduPoster Title:

The Importance of Scattering and Deconvolution in EUV Observations

Abstract:

I have estimated the TRACE PSF scattering wings in the 171 A channel using the Venus occultation data. The results, and their effect on TRACE images, are surprising. I conclude that stray light analysis using the lunar limb or other external occulter will be important for correct interpretation of AIA images.

Author: Ed Deluca, R. Bruce Ward, and Mary Liscombe

Institution: Harvard-Smithsonian Center for Astrophysics and the Christa McAuliffe Challenger Learning Center (Framingham, MA)

Email: bward@cfa.harvard.eduPoster Title:

Integrating a Space-Weather Station into Challenger Learning Center Space Flight Simulations

Abstract:

The Harvard-Smithsonian Center for Astrophysics and the Christa McAuliffe Challenger Learning Center in Framingham, MA, have created discovery-based space-weather activities, both for use with student or general audiences, and particularly for those planning to take part in a mission simulation at a Challenger Learning Center (CLC). The simulation includes features related to effects the Sun could have on manned space missions. Currently both the CLC simulation scenarios for Return to the Moon and Voyage to Mars include a space-weather component.

Author: Leonid Didkovsky, Darrell Judge, and Seth Wieman

Institution: Space Sciences Center, University of Southern California, Los Angeles, USA

Email: leonid@usc.eduPoster Title:

Completely Restored Bastille Day Solar Flare EUV (26-34 nm) Profile from SOHO/CELIAS/SEM Measurements Using a New High Fidelity Restoration Algorithm

Abstract:

High-energy particles affect EUV measurements during strong solar flare events by significantly increasing the Particle Background Signal (PBS), and may exceed the measured EUV peak of the flare by more than an order of magnitude, and last tens of hours. SEM EUV measurements of the Bastille Day (BD) solar flare (July 14, 2000) in the first order channels (26 – 34 nm) were substantially contaminated by the PBS. A previous PBS restoration algorithm for the SEM first order channel data was based on using the GOES XL (0.1 – 0.8 nm) profile to approximate the post flare variability of the SEM EUV flux. That algorithm included some uncertainty due to different (and unknown) spectral variability in the EUV band-pass. Here we propose a new restoration algorithm for removing the PBS based on using the different particle response of the two SEM first order channels as an internal, accurate, particle reference signal, for the SEM data analysis. This new algorithm allows us to obtain a significantly improved, full restoration of the BD solar flare EUV (26 – 34 nm) profile, and will be used to remove the PBS from other strong solar flare event measurements.

Author: Emilie Drobnes

Institution: ADNET Systems, inc./NASA GSFC

Email: emilie.drobnes@nasa.govPoster Title:

Family Science Night: Changing Perceptions one Family at a Time

Abstract:

The NASA Goddard Space Flight Center Family Science Night program invites middle school students and their families to explore the importance of science and technology in our daily lives by providing a venue for families to comfortably engage in learning activities that change their perception and understanding of science - making it more practical and approachable for participants of all ages.

The Family Science Night program runs a monthly two-hour event throughout the academic year at the Goddard Visitor Center. Unlike most youth science programs, this is an event where the entire family must participate in all activities. Family Science Night strives to change the way that students and their families participate in science, within the program and beyond.

Author: Emilie Drobnes

Institution: ADNET Systems, inc./NASA GSFC

Email: emilie.drobnes@nasa.govPoster Title:

The Sunday Experiment

Abstract:

Science is part of our daily lives. Through hands-on science activities and one-on-one interaction with scientists, engineers and Education and Public Outreach professionals, we can change attitudes toward science as well as inform the general public about the great work that is being done at Goddard Space Flight Center. Community members generally do not realize the role science plays in our every day lives. They may think science is too complicated to understand, not realizing that science is everywhere and in everything we do. The Sunday Experiment aims to make science and engineering more approachable and fun so that visitors feel more comfortable being engaged ins science activities, ultimately improving their perception of science, technology, engineering and math.

Author: George H. Fisher, Brian T. Welsch, William P. Abbett, David J. Bercik

Institution: Space Sciences Lab, UC Berkeley

Email: fisher@ssl.berkeley.eduPoster Title:

A New Technique for Finding Electric Fields from Sequences of Vector Magnetograms

Abstract:

The advent of extensive ground-based and space-based vector magnetogram data will greatly improve our quantitative understanding of how magnetic fields evolve in the solar atmosphere. A problem of current interest is the derivation of electric fields or velocity fields from vector magnetogram data, as this is the crucial link between observation and future physics-based time-dependent models of the solar atmosphere.

Most previous techniques for deriving E or v have used only the normal component of the magnetic induction equation, as it is generally believed that depth derivatives contained in the magnetic induction equation cannot be derived from vector measurements taken within a single layer.

We will show that in fact, sufficient information exists within a sequence of vector magnetograms to determine a 3-dimensional electric field whose curl reproduces the observed changes in all 3 components of B. While this is certainly a major step forward, it is also true that the electric field E itself, as opposed to its curl, is under-constrained by the data. We will discuss how additional constraints may be used to uniquely determine all 3 components of the electric field.

Author: Manolis K. Georgoulis

Institution: JHU/APL

Email: manolis.georgoulis@jhuapl.eduPoster Title:

ARIA and NPFC: Automatic Active Region Identification and Azimuth Disambiguation Methods for the SDO/HMI Full-Disk Vector Magnetograms

Abstract:

The Non-Potential magnetic Field Calculation (NPFC) method is proposed for the automatic azimuth disambiguation of the vector magnetograms to be acquired by the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO). The NPFC method relies on firm physical grounds and has been tested extensively on data from various magnetographs. It was concluded that the NPFC method exhibits strong insensitivity to noise, accuracy, stability, and automatic functionality, all combined with remarkable computational speed. For the above, it is the method of choice for the disambiguation of the full-disk vector magnetograms acquired by the Vector Spectromagnetograph (VSM) of the NSO's SOLIS facility. While the NPFC method was originally conceived for azimuth disambiguation of active-region fields and is accompanied by an Active Region Identification Algorithm (ARIA) that allows to automatically pick up active regions from the solar disk, recent efforts suggest that it can be used just as effectively for full-disk disambiguation in SOLIS/VSM data, following a proper geometrical partitioning of the solar disk in individual tiles. Given the unprecedented ability of both SOLIS/VSM and SDO/HMI magnetograms to capture the magnetic field vector in the entire visible solar disk, we are confident that the ARIA/NPFC package will serve the best interests of SDO/HMI, as well, and will provide the user community with the state-of-the-art full- and partial-disk magnetic field solutions for further scientific applications. Author: Sarah Gibson

Institution: NCAR/HAO

Email: sgibson@ucar.eduPoster Title:

Space weather implications of partially-ejected flux ropes

Abstract:

The structure and evolution at the source of solar activity directly affects the nature of the space weather disturbance that reaches the Earth. We employ a three-dimensional numerical magnetohydrodynamic simulation of a coronal mass ejection (CME) to show how, in the course of its eruption, a coronal flux rope may writhe and reconnect both internally and with surrounding fields in a manner that alters its magnetic connectivity, helicity, orientation, and topology. Moreover, because the rope breaks in two during eruption, the surviving portion of the rope is a candidate for future eruptions. These changes would complicate how interplanetary CME (ICMEs) embedded in the solar wind relate to their solar source. In particular, the location and evolution of transient coronal holes, topology of magnetic clouds (``tethered spheromak''), and likelihood of interacting ICMEs would differ significantly from what would be predicted for a CME which did not undergo writhing and partial ejection during eruption.

Author: S. Gissot, J.-F. Hochedez, J.M.Krijger

Institution: SIDC, Royal Observatory of Belgium

Email: krijger@sidc.bePoster Title:

Velociraptor, a motion estimation algorithm analyzing the dynamics in

EUV movies of the solar atmosphere

Abstract:

Velociraptor is a multiscale motion estimation algorithm able to estimate simultaneously the apparent motion vector and the variation in brightness from two successive frames in a sequence of solar EUV images.

Here, we extend our motion analysis tool to the SDO multi-wavelength

capabilities. The objective is to monitor the multi-wavelength evolution of the solar atmospheric plasma, including e.g. oscillation analyses of the loop systems in active regions, or trackings of erupting filaments. Because of the rapid evolution of solar atmospheric features, as observed in the TRACE data, we propose to apply the Velociraptor processing algorithm on SDO high-cadence and multi-wavelength data. Using the brightness variation maps, it also permits the identification and the quantification of multi-wavelength intensity variations, and can be applied to precise flare detection and localization, as well as to dimming identification such as transient coronal holes.

Author: Mandy Hagenaar, Marc DeRosa, and Karel Schrijver

Institution: Lockheed Martin Solar and Astrophysics Laboratory

Email: hagenaar@lms