1. A NEW TECHNIQUE FOR DERIVING PROMINENCE MASS FROM SOHO/EIT Fe XII (19
A NEW TECHNIQUE FOR DERIVING PROMINENCE MASS FROM SOHO/EIT Fe XII (19.5 NANOMETERS) ABSORPTION FEATURES Holly R. Gilbert, Thomas E. Holzer, and R. M. MacQueen The Astrophysical Journal, 618: , 2005 January
太陽雑誌会 殿岡

2. Introduction Deriving prominence mass from SOHO EIT 195 image.
CME – Quiescent prominence
“What role the prominence plays in mass ejection initiation and dynamics.” Determining total prominence mass may help develop our understanding of CME dynamics.
Previous study:
Kucera et al EUV data from the Coronal Diagnostic Spectrometer (CDS)
Golub et al EUV data from the Transition Region and Coronal Explorer (TRACE)

3. 2. Observations
EIT 195A image
Eruptive prominence of 1999 July 12 near the southeast limb at ~17:13 UT.
LASCO C2 and C3 image

4. 3.1 Determining Foreground Radiation and Prominence Absorption

5. 3.1 Determining Foreground Radiation and Prominence Absorption (2)

6. 3.1.1. Determining for Quiescent and Erupting Prominences
Spatial-interpolative approach.
Temporal-interpolative approach.

7. 3.2 Inferring Column Density and Mass

8. 4.1 Analysis Using the Spatioal-Interpolative Approach

9. 4.2 Analysis Using the Temporal-Interpolative Approach

10. 4.2 Analysis Using the Temporal-Interpolative Approach (2)
Estimating Beta β = 1.05 ±0.01
Estimating Gamma γ = 0.2
Mp = (6.0±2.5)×10^14g
2 methods are consistent.
Temporal- .. is better in uncertainty.

11. 4.3 CME Analysis
The average mass: (2.37±0.38)x10^14g -> 60% less

12. 4.3 CME Analysis The total CME mass: (1.75±0.12)x10^15g
The velocity of the loop structre : ~510km/s
The velocity of the prominence : ~299km/s

13. 5. Assumptions
In the presence of a filamentary prominence, coronal radiation from within the prominence region is negligible.
In the absence of the prominence, coronal radiation from the volume that would have been occupied by the prominence can be estimated from calculations based on a spherically symmetric corona.

14. 5. Assumptions (2)
The foreground radiation declines in the radial direction with a scale height comparable to that of the mean off-limb intensity in regions near the prominence.
The prominence abundances and ionization fractions of hydrogen and helium can be estimated from models of the mean chromosphere.

15. 5. Assumptions (3)
A single mean absorption cross section and a single mean particle mass can be applied to the entire prominence.
The prominence column density does not vary over the light /dark region.
The effects of scattered light are negligible.

16. 5. Assumptions (4)
Interpolation using observations outside the prominence provides a reasonable approximation of the intensity that would be observed in the absence of the prominence.
In the spatial-interpolative approach, the effective prominence area can be reasonably estimated from the shapes of observed intensity contours and from the inferred maximum extinction factor.

17. 5. Assumptions (5)
In the temporal-interpolative approach, the value of I0 can be represented as an average of the values measured before and after the prominence eruption
In the temporal-interpolative approach, the foreground radiation throughout the prominence region can be estimated from a number of point inferences of the foreground radiation.

18. 6. Discussion
Mass
Importance of Consideringg Foregground Radiation
Comparison of Prominence Absorption Models

19. 7. Conclusions

20. Appendix A1. EFFECT OF PROMINENCE FINE STRUCTURE ON RADIATION FROM THE PROMINENCE REGION

21. Appendix A2. EFFECTIVE PROMINENCE AREA IN THE DETERMINATION OF PROMINENCE MASS

22. Appendix A2. EFFECTIVE PROMINENCE AREA IN THE DETERMINATION OF PROMINENCE MASS (2)