1. PROMINENCES AND EUV FILAMENTS B.Schmieder
(What we have learnt with SUMER?)
B.Schmieder
New Advances in the field
New Observations SOHO/EIT/CDS/SUMER, TRACE with GBOs
New modelling: non LTE radiative transfer, MHD
SUMER spectrometer: Lemaire, Wilhelm, …..Poland
MEDOC; 7 campaigns!!!
Thesis : Labrosse, Cirigliano, Yong Lin
Work: Anzer, Aulanier, Delannée, Gouttebroze, Heinzel, Kucera,
Madjarska, Patsouros, Parenti, Schmieder, Schwartz, Vial, Wiik…..)
SUMER He I

2. Prominence in multi-wavelength
(Ondrejov)
SUMMER SLIT
Prominence Ha (Bialkov)

3. Prominence in hydrogen L-alpha
TRACE (NASA)

4. SUMER:Lb line spectra in Filament and Prominence
Central reversed profiles in filament
No reversed profiles in prominence

5. Lyman lines
Scattered light of
the chromosphere
with/without PCTR

6. PRD/CRD L-alpha profiles
Isthermal and isobaric slab model
OSO8
(Gouttebroze, Vial, Heinzel 1987)

7. GHV grid of NLTE models of solar prominences
La, Lb, Lg
Atom of Hydrogen
Lyman lines > 912 A
La, Lb, Lg
Balmer lines > 3646 A
Ha, Hb
Ha, Hb
Paschen linea
Ne, L cont, S(Ha)
(Gouttebroze, Heinzel, Vial1993)

8. Three prominences observed by SoHO/SUMER
Two types of profiles
of the Hydrogen Lyman
series: Why ?
La L b L g
May
unreversed
June
reversed
March
W ~1.5 A A A
(Heinzel, Schmieder,Vial, Kotrc, 2000)

9. Lyman Series L4, L5,L6 , same behaviour

10. Models of prominences: importance of the PCTR
Case of a thick PCRT
PCTR
(Heinzel, Schmieder, Vial, Kotrc A et A, 2001)

11. Non LTE modelling can reproduce unreversed profiles in prominence
Heinzel et al 2001 suggested that two types of PCTR can explain the profiles:
PCTR seen along the magnetic field lines (unreversed profiles)
PCTR seen across the field lines (reversed profiles)
New 2D model by Heinzel and Anzer (2002), application to SUMER in preparation

12. Filament is visible in the centre of Lyman lines
Dl = 3x A,
= A
(Schmieder, Heinzel, Kucera, Vial 1998)

13. SUMER Spectra Lb to Ly c Reversed profiles Ld Lb Lb Lb Lc
The central intensity I0 = 0

14. 1D-slab model of an filament
P=const
vt  5 km s-1
D=5000 km h Tc
The existence of a PCTR explains the behaviour of the Lyman profiles

15. Ha CME EIT 304 A SUMER can give the Velocity of the eruptive
prominence Ha
CME
(06:41 and 13:13 UT
MAY )
EIT 304 A
(Schmieder, Delannée, Deng, Vial, Majarska et al 2001)

16. SoHO/EIT et SUMER (Lyman L4) Velocity asymmetric profile = 100 km/s
MSDP + SUMER slit
(spectroscopic Diagnostic )
(Lyman L4)
Velocity asymmetric profile
= 100 km/s
EIT
SUMER
(Schmieder, Delannée, Deng, Vial, Madjarska )

17. Filament Ha and EUV (l > 912 A)
typical example : sept 14, 1999
SoHO/EIT (He II)
Meudon spectroheliograph (Ha)

18. Dark filament channels EIT, CDS, TRACE
Coronal lines
No void
But Volume blocking
I(fil)=Ibg+Ih+Ifg
Ih=0
Ifg
The dark channel is explained by cool plasma
if Ibf is relatively important
The dark channel due to missing plasma above (void ) or in the filament, for lines with small Ifg

19. EUV-filament THEMIS – H-alpha SOHO/CDS EUV rasters
(Heinzel, Schmieder, Tziotziou, 2001)

20. Other example of a EUV filament located at high latitude
TRACE 171A
SVST
(Engvold)
CDS fov
TRACE 195
(Schmieder, Yong Lin, Heinzel,
Schwartz 2004)

21. Absorption of coronal-line radiation by resonance hydrogen & helium continua in a cool prominence plasma
912 A
504 A
227 A HI
HeII
HeI
CDS lines
SUMER
CDS lines
EIT + TRACE
wavelength

22. Why the cool material is not visible in Ha?
t912 is
between 15 and 200 in the filament
between 0 and 15 in the EUV filament
this corresponds to
a t Ha lower than 0.1 and a too low contrast which does not allow to distinguish the filament from the chromosphere
Ha filament
EUV Filament
Lyman-continuum to H-alpha opacity ratios Heinzel et al., 2001, Tziotziou et al 2000

23. Geometrical model Absorption mechanism and Volume blocking corona
(Heinzel, Anzer , Schmieder 2003)
photosphere

24. Halpha Meudon
Ha VTT/MSDP

25. CDS –SUMER coalignment
SoHO/CDS
SoHO/SUMER, Ld raster
MgX Å
SoHO/CDS
The ratio of the intensities OV (CDS) and OVI (SUMER) permits to compute the optical thickness of EUV fil

26. 3D EUV filament Mass loading
The plasma density
r=1.4 mHnH ~1.4 mH n1 + ne
ne=C (n2) 1/2
nH depends on t 912 A
With non LTE transfer calculations of Lyman lines,
912 is computed .
EUV Filament mass of filament of Oct 15, 1999
(912) Mg
x 1014
x 1015
x 1015
With a spectroscopic model (Heinzel et al 2003, Schwartz et al. 2004)
Mass of EUV filament =Mass of Ha filament
(double the mass)

27. Lyman lines in EUV filament
SUMER slit
Ha fil: reversed Lyman line profile
EUV fil: unreversed profiles
WHY?
(Schwartz, Heinzel, Schmieder, Anzer 2005)

28. Model for EUV filament T Hydrogen ionisation degree r Electron density
H/D
(Schwartz, Heinzel, Anzer, Schmieder, 2004 , Saint Petersburg)

29. EUV filament model compared with Ha filament model
Using the non-LTE filament model (Heinzel, Schmieder and Vial,
1997), the observed Lyman profiles within the EUV-extensions can
be reproduced with:
EUV filament (Z=20000km)
Filament (Z=5000km)
temperature in the filament center
Tc≈2 ─ 3  104 K
Temperature
in the filament edge (PCTR) Ts=105 K
extensive PCTR
low gas pressure in 1D-slab
(p≈10-2 dyn cm-2)
Tc =8000 K
T = K
P= 0.08 dyn cm-2
This leads to (Schwartz, Heinzel, Schmieder, Anzer 2005)
of higher Lyman lines and the model
gives to(Ha)<<0.1 (not Ha filament)

30. THEMIS MTR 6302 A B vect over Ha map local vertical
(Schmieder, Lopez 2004)
B vect over Ha map
(Large angle with the vertical)

31. Simulation of the observations of cool plasma
Computations of the dips in each field line in the computation model box
(B . s) B > 0 h
altitude (z)
Bz = 0
Field line
dHa = Hg = 300 km
Dips filled by plasma
(Aulanier and Démoulin 1998)

32. 3D magneto-hydrostatic linear model with free parameters
(2) Extrapolation of B from SoHO/MDI
3D magneto-hydrostatic linear model with free parameters
constrained by the theory and the observations
Lignes de champ
filament
arcades coronales
Matière froide
z > 4 Mm
z < 4 Mm
CDS OV
08:12 UT
07:52 UT
Topology of B and distribution
of the cool matter
Aulanier G., Schmieder B., 2002, A&A, 386,

33. SUMER Lyman lines and non LTE Modelling
PCTR of the prominences : importance of orientation of the magnetic field lines versus the l.o.s
For Filament we need to have a PCTR to explain theLyman profiles with I0 different of 0.
EUV filament existence
What is the relationship between EUV filament and void?
Mass of prominences