1. Spectroscopy of solar prominences simultaneously from space and ground
Spectroscopy of solar prominences simultaneously from space and ground Stellmacher, G. et al. 2003, Sol. Phys. 217, 133.
S. Kamio
Solar Seminar

2. Prominence
Co-existing (unresolved) hot and cool plasma Higher charged ions (O IV, N V, S V, …) Neutral or singly charged ions (H I, He I, Ca II, …)
(i) Cold threads surrounded by hot transition layer
(ii) Isothermal threads of different temperatures

3. Instruments
VTT/Tenerife (Vacuum Tower Telescope) Filter image: Hβ4862Å, Ca II 8542Å
GCT/Tenerife (Gregory Coude Telescope) Spectrum: Ca II 8542Å, He I 10830Å
SUMER/SOHO Cool lines(N I, C I, Si I), Lyman lines, Hot lines(O IV, S V, N V, …)
TRACE Lyman α, 1600Å, and 171Å

4. Observation Prominences above the limb E/70N E/42N 1600Å 171Å Lymanα
SUMER slit is indicated
1600Å Å Lymanα

5. He I 10830Å triplet
Total optical thickness (τ0) can be derived from red/blue component ratio 1Å
blue red components
He I spectrum on the limb (by courtesy of I. Tohmura)

6. Excitation temperature
Tex was estimated from observed intensity andτ
Tex=3750K (mean) 4100K (peak for E/42N) 3850K (peak for E/70N)

7. Line width Estimated kinetic temperature and non-thermal broadening
Brighter prominence (E/42N) is cooler T
Vnth
T(K)
V(km/s)
E/70N
3-6
E/42N
<7

8. Lyman series Oscillator strength versus line width
τ>100 for prominence plasma (optically thick)
Lyman lines may be emitted from outer part of prominence
19  k  5

9. Spatial distribution Hot lines (2x105K) S V, O V, …
Cool lines (104K) Fe II, Si II, …
Difficult to determine prominence models

10. Temperature and width E/70N E/42N
Line width increases with formation temperature
Large non-thermal velocity of E/70N is due to low density and magnetic field?

11. Summary 2 prominences were observed in different temperature lines.
Optical thickness is derived from He I 10830Å red/blue ratio.
Lyman lines may be emitted from outer part of prominence.
Spatial distribution in hot and cool lines are different.
Line width increases with formation temperature

12. Template
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