1. 2005 May 22FASR Science Sims Meeting 1 / 13 FASR Science Simulations AGU/SPD Splinter Meeting 22 May 2005

2. 2005 May 22FASR Science Sims Meeting 2 / 13 Science Goals Table

3. 2005 May 22FASR Science Sims Meeting 3 / 13 Role of Simulations Two types of simulations Array Configuration Simulations –determine “best” configuration to meet imaging goals –quantify trade-offs in site selection, antenna constraints Science Simulations –determine FASR performance for certain science goals –determine observing strategies –determine calibration strategies –develop image processing algorithms –develop data analysis algorithms –guide to data visualization

4. 2005 May 22FASR Science Sims Meeting 4 / 13 Simulation Levels—Level 0 Images with complex structure, but no attempt at physics input or correct spatial scales. No frequency dependence. Examples are the FASR logo and TRACE partial frame images done by T. Bastian. These are of limited usefulness.

5. 2005 May 22FASR Science Sims Meeting 5 / 13 Level 0 Example, Bastian TRACE Loops

6. 2005 May 22FASR Science Sims Meeting 6 / 13 Level 1 2D Full-Sun models based on T, EM maps from TRACE/EIT or other input. Frequency dependence of brightness, scattering size, and shape may be included. Example is S. White’s SPIE paper, with set of radio images at several frequencies. Magnetic field component may be added based on MDI longitudinal magnetogram, and T, EM is limited to TRACE/EIT diagnostic range. These are useful for assessing performance of different configurations and different image reconstruction algorithms. Frequency dependence is for frequency-dependent spatial scales only, and not for spectral diagnostics.

7. 2005 May 22FASR Science Sims Meeting 7 / 13 Level 1 Example, Stephen White’s Full Disk Sims

8. 2005 May 22FASR Science Sims Meeting 8 / 13 Level 2 a Targeted physics-based 3D model with some limitation, such as limited spatial extent, or limited frequency range, but based on T, EM or n e, vector B with correct radiative transfer. Examples include D. Gary’s magnetic field model (based on Mok active region model), S. Tun’s coronal cavity model (based on Low analytical model), M. Aschwanden’s hot loop model, and Z. Liu’s type III model. These are useful for exploring physical diagnostics, but may be misleading due to lack of correct spatial scales, omission of confusing sources, or limited applicable frequency range. These are NOT useful for assessing performance of configurations, but may be useful for studying algorithms and are certainly good for PR.

9. 2005 May 22FASR Science Sims Meeting 9 / 13 Level 2 a Examples Aschwanden Loops, Gary AR Model

10. 2005 May 22FASR Science Sims Meeting 10 / 13 Level 2 b Same as level 2 a, but with dynamics added. These may be useful for assessing FASR time resolution for electron time of flight (ms timescale), or CME difference imaging (minutes timescale), type II, III, and U bursts, sunspot oscillations, filament eruptions, etc. We have no examples of this type yet. These have major implications for PR, however, and are needed for Level 4, below.

11. 2005 May 22FASR Science Sims Meeting 11 / 13 Level 3 Full-Sun 3D models with embedded 3D physics-based models from level 2. What is envisioned here is the placement of isolated AR, hot loop, flaring loop, filament, CME, and other models into a full-disk model (with chromospheric network?) Requires the ability to vary the geometry (placement) of the isolated models so that the effect of viewing angles can be studied. Such physics-based full-Sun models are essential for development of the algorithms and data- handling software, and to understand the limitations of the configuration and sensitivity on extraction of diagnostic information. For seamless insertion of embedded models, a geometrical framework is needed, including non-uniform gridding.

12. 2005 May 22FASR Science Sims Meeting 12 / 13 Level 4 To assess the interplay between time resolution and sensitivity limitations, we need to add dynamics to any or all of the embedded models. This includes flaring loop dynamics, particle transport and loss mechanisms, expanding CME geometry, filament eruptions, sunspot fluctuations/oscillations, network microflares, and so on. This level is also required for exercising of data- handling and real-time algorithms.

13. 2005 May 22FASR Science Sims Meeting 13 / 13 What is Needed for DDP? Configuration studies will require Level 1 models. Stephen will address this. Additional target-physics Level 2 models, especially with time dependence (Level 2 b ), but with allowance for transition to Levels 3 and 4 (i.e. think about what is needed for embedding into full Sun geometry). At least one Level 3 (full Sun) model is needed, with software for embedding.