1. Spectral Signature of Emergent Magnetic Flux D1 神尾 精 Solar Seminar 2003.05.19 Balasubramaniam,K.S., 2001, ApJ, 557, 366. Chae, J. et al., 2000, ApJ, 528, L119.

2. Overview Spectroheliogram in Ca II K line and vector magnetic field data are studied in detail. Ca II K spectral line anomalies are found at the location of small-scale magnetic flux emerging through the chromosphere. Balasubramaniam,K.S., 2001, ApJ, 557, 366.

3. Ca II Line Profile Typical line profile shows 5 reversals Enhanced K2 emission and red asymmetry in the impulsive phase of flares (Fang et al.1992) Observation in active regions suggest magnetic field influences the line profile (Martinez et al. 1990) K3K3 1Å K 2V K 2R K 1V K 1R λ

4. Transition Region Line Enhanced emission or broadening of UV lines are correlated with magnetic field (Dere et al. 1989) Broadening is caused by acceleration of plasma away from the heating site eg microflare (Linsky et al. 1995)

5. Observation 1995 Aug 5 AR 7896 near disk center Spectorgraph RBDST at Sacramento Peak/NSO 7.3Å band centered on Ca II K line Pixel size: 0”.258 x 0.018Å 23 min x 5 scans = 115 min Stokes Vector Polarimeter ASP at High Altitude Observatory/NSO Fe I 6301.5Å and 6302.5Å

6. Anomalous Profile 3 or 5 reversals Normal Others Anomalous Anomalous Separation of additional component from the line center is -16 ～ 50 km/s. Some profiles do not show recognizable K2 or K3 components.

7. Broadened Profile 3Å is much wider than the normal width of 1Å. Size of anomalous or broadened features are 1 ～ 2". 3Å3Å 1"

8. Distribution of Anomaly Anomalous profiles are found at the edge of strong magnetic field regions.

9. Temporal Variation Increase of magnetic flux indicates the emergent magnetic flux. Anomalous profiles are found in these regions 0+23+46+69 min

10. Spectral Images Anomalous profiles appear at the emergent flux regions. Duration of anomalous profile is longer than 2 scans or 46 min.

11. Discussion Anomalous profiles are caused by summation of several Doppler shifted profiles whose velocities range from -16 to 50 km/s. It suggests the existence of localized flow in the emergent flux. Enhanced emission of K line is most likely a response to heating.

12. Discussion (cont.) One possible explanation of heating is the shock caused by supersonic flow of plasma. Broadening of line profile can be interpreted as microturbulence due to magnetic reconnection, same as transition region explosive events. Dynamic model of multi component atmosphere is necessary to explain these line profiles.

13. UV/EUV Brightening Blinkers(γ) Profiles with enhanced wing, little broadening Explosive events(α) Broad spectral profiles indicate the presence of high velocity plasmas. Chae, J. et al., 2000, ApJ, 528, L119.

14. Observation 1997 Apr 26 16:00-20:30 UT SOHO/CDS obtained 3 scans of 244” x 240” area. He I, O V, and Mg IX SOHO/SUMER is fixed so that the slit scans the area of 120” x 43” by solar rotation. Si IV

15. Short-lived brightening Blinker consists of many small scale short lived berightening events. Duration and size of typical unit brightening events are 2-3 min and 3”-5”.

16. Discussion Explosive events Blinkers Explosive events and blinkers are caused by different magnetic reconnection geometries. Reconnection produces bidirectional flow, which appear as broadened profiles.