# Presentation: 498302

## SECCHI Overview

**R.A. Howard, J.D. Moses, A. Vourlidas, J. Newmark, J. Lemen, J.P Wuelser, J. Davila, W. Thompson, D.S. Socker, S. Plunkett, R. Harrison, C. Eyles, J.M Defise, J.P Halain, D. Wang, N. Rich, R. Baugh, D. McMullin, T. Carter, A. Hurley, S. Cooper and the rest of the SECCHI Team**
**STEREO-Solar B Science Planning Workshop**
**Turtle Bay, Hawaii**
**November 14-17, 2005**

## Outline

**SECCHI Science Overview**
**Specific Science Goals**
**Planned Data Sets**
**Analysis Tools**
**Observation Plans **

## SECCHI Primary Design Driver

**  **
** ****Observe CMEs from their launch at the Sun, track them through the corona and inner heliosphere and then their eventual impact at Earth with sufficient resolution and frequency to discern the physics of the launch, their propagation and their morphology.**

## SECCHI Science Overview

**SECCHI Science Overview**

- 021104-06SECCHI_CDR_Science.

## SECCHI InstrumentPerformance Requirements

## HI-1 FM-B Stray Light Image Equivalent Solar Brightness  (B/Bo)

**HI-1 FM-B Stray Light Image Equivalent Solar Brightness **** ****(B/Bo)**

**5x10****-14**** B/Bo**

**7x10****-13**** B/Bo**
**1x10****-13**** B/Bo**

**1.0x10****-13**** B/Bo**

**Stray Light Requirement Met**
** ****Performance Exceeds Requirement **

## HI-2 FM-B Stray Light Image Equivalent Solar Brightness  (B/Bo)

**HI-2 FM-B Stray Light Image ****Equivalent Solar Brightness **** ****(B/Bo)**

**5x10****-14**** B/Bo**

**5x10****-14**** B/Bo**

**Note that in the **
**HI 1&2 overlap**
**region, both **
**instruments observe**
**The same radiance.**
**Since HI 1&2 have **
**different diffraction **
**characteristics, the **
**observed levels **
**must that of the **
**be due to the **
**chamber, not the**
**Instrument.**

**End-to-end Stray Light Performance Requirement Met, **
** ****Measurement is Still Limited by Chamber Background**

## Overlap of Views From HI1 and CORs

**Overlap of Views From HI1 and CORs**

## “30 Day” Science Questions

**CME Morphology**
**What are the 3D pre-and post-CME configurations? **
**What is the 3D Structure of CMEs?**
**CME Initiation**
**How is the pre-CME energy partitioned and how does it repartition?**
**How does the pre-CME configuration evolve to initiate a CME?**
**What is the relative timing of the structures associated with the liftoff of CMEs?**
**What is the acceleration profile?  What are the forces involved?  **
**Can we rule out/confirm any mechanisms?**
**Propagation/Interaction with the Heliosphere**
**Where does the mass originate?**
**Where does the shock form? Type II? SEP?**
**What is the 3D nature of the shock?**
**How does the 3D nature of the CME evolve as it propagates?**
**What is the 3D acceleration/deceleration profile?**
**How does the CME interact with streamers in 3D?**

## SECCHI Data Sets

**Images **
**FITS Format**
**Level 0.5**
**Corrections That Do Not Involve Interpolations**
**Images Rotated to Put Ecliptic North at Image Top**
**Total Brightness and Percentage Polarization Images (QL)**
**IDL Routines to Convert the Level 0.5 Images to Level 1**
**Catalogues**
**Image Meta Data in an SQL Data Base**
**Lists of CME Events**
**Separate Lists for STEREO A/B and SOHO/LASCO**
**Automatically Generated with Automatic Measurements**
**Similar to LASCO CME Web Page**
**Movies and Synoptic Maps**
**All Data Will Be Available Via an IDL Query Tool, a Web-based Query Tool, As Well As Through Vxo Queries.**

## SECCHI Analysis Tools

**CME Measurements**
**Width, Location, Height Time positions**
**Acceleration/Deceleration**
**CME Mass, Center of Mass**
**3D Reconstruction**
**Tie Point Analysis**
**Loop Reconstruction**
**3D Inversion**
**Forward Modeling (White Light and UV)**
**Thomson Scattering Parametric Curves**
**Miscellaneous**
**Differential Emission Measure**
**Synoptic Maps**
**MHD Modeling**

## Modeling of LASCO CMEs as Fluxrope

## Radial Profiles of the CME Fronts

## Simulated CME from Sun to 1 AU (Ecliptic View)

**Ahead**

**Behind**

**HI-2**

**HI-2**

**HI-1**

**HI-1**

**COR**

**COR (Reversed)**

**Earth**

**Earth**

## Simulated CME from Sun to 15 R (Earth View)

## SECCHI Observation Plans

**The observations are intended to be synoptic in nature and go into a S/C buffer that has been set to not overwrite**
**But 20% of the telemetry has been allocated to special observations.  These observations go into another S/C buffer that has been set to recirculate, thus providing about 1-2 hours **
**To fill those special observations, we will have a series of planning meetings (web based) at quarterly, monthly and weekly intervals.  **
**Anyone may submit a request for special observations – a web page will explain the procedure, but it is based on the SOHO JOP.  **
**The synoptic observations will be carried out from both platforms, but the special observations may or may not.  **
**An example of such “special observations” might be a high cadence sequence trying to get higher cadence on the initial phases of the CME process.  The sequence might end by the on-board detection of a CME, which would freeze the circulating buffer.  The two spacecraft might not trigger on the detection of the CME at the same time, so those observations would be from one spacecraft alone.**

## Summary

**The unique and varying perspective observations from  STEREO, combined with the observations from Solar-B and other space- and ground- based assets and the well developed modeling provide an exciting opportunity for the community to address the specific STEREO mission objectives but also many others.**
**We welcome participation by anyone to use the SECCHI data in their analyses as well as to develop the special observing programs.**