1. Relationships between flares and CMEs FRIDAY 9:00 am – 12:00 pm SHINE 2009

2. Relationships between flares and CMEs This session solicits both observational and theoretical studies addressing the relationships between solar flares and CMEs. The questions include 1.Is there a causal relationship between flares and CMEs? 2.The energy partition among various aspects of the flare- CME system 3.The interpretation and connection between directly and indirectly observed flare and CME products and properties 4.Are there fundamental differences between the process producing flare-CME pairs and that producing flare-less CMEs?

3. STARTENDSESSION ACTIVITY 09:05 ---09:30 John Raymond The Energy Budget of Flare/CME Events 09:30 ---09:50 Discussion 09:50 ---10:15 Jiong Qiu + Jie Zhang Eruptive Flares and Fast CMEs Originating in Solar ARs + Statistical and Physical Relationships… 10:15 ---10:35 Discussion 10:35 ---10:45 Coffee break 10:45 ---11:00 James Chen Physical Connection btwn CME Accel. and Flare X-Ray Emission 11:00 ---12:00 Discussion Open Forum, General Contributions, Etc.

4. Session Abstracts (in order of submission) Robert T Duffin Type III-L Solar Radio Bursts and their Associations with Solar Energetic Proton Events Jie Zhang Statistical and Physical Relationships between Flares and Coronal Mass Ejections Robin C Colaninno Kinematics of CMEs Observed in SECCHI HI: Fast Solar Wind Acceleration of CMEs? Yan LiOrigins of Solar Minimum CMEs with ICMEs Hong XieFlux Rope CMEs Associated with Total and Partial Eruptive Prominences Jiong QiuEruptive Flares and Fast CMEs Originating in Solar Active Regions Oscar A Olmedo The Role of Overlying Magnetic Field and Poloidal Flux Injection in Modeling Coronal Mass Ejections Kathy K Reeves Current Sheet Energetics, Flare Emissions, and Energy Partition in a Simulated Solar Eruption James ChenPhysical Connection Between CME Acceleration and Flare X-Ray Emission John RaymondThe Energy Budgets of Flare/CME Events

5. Type III-L Solar Radio Bursts and their Associations with Solar Energetic Proton Events Robert T Duffin (George Mason Univ.), Stephen M. White (University of Maryland) Paul S. Ray (Naval Research Laboratory), Michael L. Kaiser (NASA/Goddard Space Flight Center) Type III-L bursts are a sub-class of type III solar radio bursts that tend to occur after the impulsive phase of flares; are longer in duration than individual type IIIs and tend to be low-frequency. There has been a proposal that type III-Ls are connected to solar energetic proton (SEP) events. Most work on this connection has started from samples of SEP events, but if type III-Ls are to be useful for prediction of SEP events, then we need to understand the properties of samples of type III-L bursts. This talk reports preliminary results from such a study. An operating definition based on previous work is used to identify type III-L events amongst M- and X-class flares from 2001; and then associations with other properties of these events are investigated, including association with SEP events. If there is an association with SEP events, one important factor that these bursts allow us to address is the question of whether acceleration takes place at an associated CME, or closer to the flare site well below the CME.

6. Robin Colaninno 1 and Angelos Vourlidas 2 Kinematics of CMEs observed in SECCHI HI: Fast solar wind interaction of CMEs? George Mason University, Fairfax, VA 22030, 2 Naval Research Laboratory, Washington, DC 20375 SHINE Meeting : August 2, 2009 Figure : a) and b) are longitudinal cuts at the longitude of the CME from the Croissant model. c) is a radial cut at the maximum height of the CME measured in HI1. d) is a latitudinal cut at the latitude of the CME from the Croissant model. 02-Jun- 2008 Point-n-click measurements of the CME, front, back and sides to determine the ratio of width and depth, Pancaking Factor and Rate. Fit geometric Croissant model to STEREO SECCHI- COR2 to determine the 3D position of the CME. Insert CME measures into the Predictive Science's solar wind velocity model using the position derived from the Croissant model.

7. Hong Xie 1,2, Holly Gilbert 2, Nat Gopalswamy 2, & Chris St Cyr 2 1 The Catholic University, and 2 Goddard Space Flight Center Flux Rope CMEs Associated with Total and Partial Eruptive Prominences Fig. 3 (a) and (b) A X-type magnetic structure (yellow arrow) and PEP associated with the 11-16-2007 CME in EUVI-A 171 and 304. (c) and (d) Superposition images of STEREO-A COR1 and EUVI 171 and 304. The mean speed of TEP-CMEs is greater than that of PEP-CMEs but smaller than that of flare-CMEs. The X_line-CMEs have similar mean speeds as PEP-CMEs.  Good anti- correlation between mass and speed among the 17 flux rope CMEs with correlation coefficient r = -0.63.  No such correlation exists among the 7 flare-CMEs.  In agreement with the conclusion that the mass of slow CMEs consist of material mainly from the streamer belt in the corona (Kramar et al., 2009) First direct observations of the X-line structures (a well-known location of current sheets and reconnections) in EUVI 171 images, with associated PEPs in 304 and flux rope CME in COR1. Fig. 4 Correlation between mass and speed of the 17 flux rope CMEs with V< 700 kms -1. Fig, 2. An example of the flux rope model fit for the 26 April 2008 CME. (left): (a), (b), (c), and (d) STEREO A and B COR1 and EUVI 304 composition images; (right) (b), (d), (f) and (h) STEREO A and B COR1 and COR2 images superposed with flux-rope model outline curves (yellow curves).