1. CME – Flare Relationship A survey combining STEREO and RHESSI observations S. Berkebile-Stoiser B. Bein A.Veronig M. Temmer

2. Aims Study on a statistical basis:  dynamics of CMEs (full acceleration profile)  relation to the energy release in the associated flare (high energy particles )  relation of the CME source region to the associated flares‘ energy release (location, size, magnetic field topology)

3. Data CME Data:  STEREO : - EUVI: 171 Å, 195 Å (cadence ≤ 2.5 min) - Cor 1, Cor 2 WL coronagraphs (cadence: ~2.5 min – 15 min ) → FoV: 1 – 15 R Θ  Flare Data: - RHESSI: flare X-ray emission > 3 keV (cadence: ~4s) - GOES: 0.5 – 8 Å

4. Data Products  Time distance curve of the CME leading edge → velocity/acceleration profile  Peak velocity, peak acceleration  Duration of impulsive acceleration phase  Height of initiation, peak and end of acceleration Goal: determine the kinematics of at least 50 CMEs Flares: comparison with RHESSI light curves, peak spectra

5. Event Selection 200720082009 (Jan - May) Class 1 and 2 CMEs (+ RHESSI flare) 211 (35) 152 (13)104 (5) Class 3 CMEs (+ RHESSI flare)44 (20)41 (11)14 (3) CMEs + GOES flare1671 → GOES class: ~80% A and B, ~17% C, ~3% M flares Qualitative classification of Cor 1 CMEs:

6. CME March 25, 2008 Automatic detection of the CME leading edge:  normalization, unsharp masking (EUVI), NRGF filter  Determination of CME front in difference images: - Iteratively searching for contours at increasing `intensity levels‘ -> distance of pixels from sun center - Stop when mean distance of the pixels on 2 level contours are similar movie 12-25 keV 25-50 keV a ≈ 410 m s -2

7. Problems: - association of flares and CMEs often ambigous - correct identification of LE in first Cor 1 image - numerical derivative method - …