[session no.]1 V: C5: Coronal Seismology Introduction: 5 min Talks: Viggo Hansteen: lower atmosphere (10 min) Stuart Jefferies: chromospheric wave propagation (5 min) Robertus Erdelyi: challenges in theory (15 min) Len Culhane: theory/spectroscopy/wave detection (10 min) Jean-Francois Hochedez: wave detection (10 min) Discussion: 20 min Next step(s): 5 min

[session no.]2 II: Science questions and tasks Primary scientific questions: The variety of oscillation modes observed with SOHO/TRACE in the TR and corona have opened up the new field of coronal seismology. By studying the properties, excitation, propagation and decay of these oscillations/waves, we can reveal fundamental physical properties of the TR/corona that cannot be accessed as well or at all otherwise, such as magnetic field, density, temperature, viscosity, sub-resolution structuring,...

[session no.]3 II: Science questions and tasks SDO/AIA science tasks: Task 5A: Defining the characteristics of transverse, longitudinal and newly discovered waves: excitation, propagation, decay Task 5B: Defining the characteristics of global coronal waves: excitation, propagation, decay Task 5C: Probing large scale coronal magnetic structure and topology Task 5D: Probing the small scale plasma structure and microphysics

[session no.]4 IV: Science investigation Hurdles, bottlenecks, uncertainties: Analytic models need to be improved to include 3D effects Analytic models need to be augmented by detailed 2/3D MHD codes 3D MHD codes need to include photospheric convection, non-LTE chromospheric radiative losses and a realistic corona to study the coupling to lower atmosphere

[session no.]5 IV: Science investigation Hurdles, bottlenecks, uncertainties: Need automated detection software for longitudinal/transverse waves and their triggers Automated global wave detection needs to be improved How can multi-thermal AIA data be used to restrain electron densities (crucial for many types of coronal seismology)? How reliable are density measurements from Solar B EIS?

[session no.]6 IV: Science investigation Hurdles, bottlenecks, uncertainties: NLFFF codes need to be improved (faster, more accurate) and coupled to codes which determine the magnetic field topology. Boundary conditions for field extrapolations need to be improved. How do we incorporate chromospheric fields and loop morphology into extrapolation codes? How do we use the coronal field models to determine field topology and constrain loop lengths? Reliable loop tracing software needs to be developed. (Topic I)

[session no.]7 IV: Science investigation Hurdles, bottlenecks, uncertainties: How do we use STEREO to improve our understanding of loop geometries/lengths? Full disk, high cadence (30 s) H  images needed to study Moreton waves simultaneously with EIT/AIA waves, also for prominence/filament oscillations and propagation from lower atmosphere into corona.

[session no.]8 III: Science context Expected advances in prior to SDO: Automated recognition software to detect global, longitudinal and transverse waves,… Detection of previously undetected wave modes (Solar-B), e.g., torsional modes Propagation of waves from lower atmosphere into corona: Solar-B, MHD modeling Significant improvement in coronal field extrapolations (see topic I), highly useful for studies of wave propagation, independent field determination, loop lengths, etc… Incorporation of 3D effects, e.g., magnetic curvature, sub- resolution structuring in current models Improved understanding of the global coronal wave phenomenon Determination of observable parameters from theoretical models

[session no.]9 III: Science context Anticipated SDO contributions: AIA cadence extends parameter space to higher frequencies (4-10 x TRACE, up to 0.25 Hz) Improved detection rate of all wave types, including previously undiscovered wave modes, because of large FOV, multi-thermal coverage, better S/N More accurate coronal seismology through AIA multi- thermal coverage: better estimates of densities and loop lengths (through field extrapolation codes), probing of sub-resolution structuring

[session no.]10 III: Science context Anticipated SDO contributions: Better understanding of triggering, propagation and damping of transverse oscillations through combined SDO and Solar-B spectroscopic and vector magnetic data Improved knowledge of coronal field topology/structure through observations of global EIT/AIA waves and 3D modeling Better understanding of damping and propagation of longitudinal waves (e.g., phase mixing) through multi- wavelength AIA data, and of triggering and damping of longitudinal waves on high-temperature (>5 MK) loops through AIA and Solar-B/EIS data

[session no.]11 III: Science context Anticipated SDO contributions: Oscillations in prominences (He II 304 A) and coupling to coronal volume Look for Alfven waves by tracking transverse motions of features in photosphere

[session no.]12 V: Implementation: general What do we need to make progress on the science questions in general ? TR&T: Automated wave and loop detection TR&T: Augment analytic models by comparing with simplified 2/3D MHD test models TR&T: Bootstrap off topic I’s focus on field extrapolation/boundary loop recognition SR&T: 3D MHD codes need to include photospheric convection, non-LTE chromospheric radiative losses and a realistic corona to study the coupling to lower atmosphere

[session no.]13 V: Implementation: general What do we need to make progress on the science questions in general ? SR&T: Analytic models need to be expanded to include 3D effects, e.g., micro-structuring, curvature, … Working group/workshop on automated wave detection software? Working group/workshop on wave propagation through lower atmospheric boundary: 3D MHD codes Funding??? [observables, models, codes, resources, people …]: see working groups?

[session no.]14 VI: Implementation: AIA+HMI What do we need from and for SDO to make progress on our major science? Significant progress can be made with the standard AIA observing mode High frequency domains can be explored by high cadence observations for limited fields of view and duration in a few select, high S/N passbands: 0.25 Hz is OK, it would be interesting to push this as much as possible Observing programs/sequences will be optimized based on initial observations of, especially, triggers of wave phenomena Data products: database of “events” with sample movies, ideally, automated software, or less ideally, high school students; full disk, high cadence H-alpha movies, density measurements (EIS?), coronal field extrapolations

[session no.]15 VII: AIA (+HMI+EVE) data products [list data products; differentiate ‘critical’, ‘desirable’, ‘useful’] SDO data:  1600/1700 at 20 s data  Pipeline for detecting oscillatory power in data? Supporting data from other observatories:  XRT, EIS, FPP, ISOON (full disk, high res, high cadence H-alpha), radio-data?

[session no.]16 VIII: AIA (+HMI+EVE) data production Assessment of required resources/codes/etc: [pipeline software] automated detection of oscillations [analysis software/studies] wave analysis toolkit to ssw [supporting software/models] [computational requirements (run time estimates, system requirements, …)] [storage requirements: size, duration, …] [access: web, archive, logs, search methods, …]

[session no.]17 IX: Business plan: Resources [What data and codes must we have to make SDO a success (at pipeline, supporting, and research levels)? Who will provide the required codes?] …

[session no.]18 X: Business plan: Implementation [Define key milestones, test procedures, and target dates, …] … [Communication: define or list meetings, topical sessions, etc., where progress can be presented, discussed, evaluated, …] …is there a need for knowing all oscillatory data in TRACE/EIT?