![Page 1: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/1.jpg)
PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?) B.Schmieder
New Advances in the field1. New Observations SOHO/EIT/CDS/SUMER,
TRACE with GBOs2. New modelling: non LTE radiative transfer, MHD
SUMER spectrometer: Lemaire, Wilhelm, …..PolandMEDOC; 7 campaigns!!! Thesis : Labrosse, Cirigliano, Yong LinWork: Anzer, Aulanier, Delannée, Gouttebroze, Heinzel, Kucera, Madjarska, Patsouros, Parenti, Schmieder, Schwartz, Vial, Wiik…..)
SUMER He I
![Page 2: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/2.jpg)
Prominence in multi-wavelength
Prominence H(Bialkov)SUMMER SLIT
(Ondrejov)
![Page 3: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/3.jpg)
Prominence in hydrogen L-alpha
TRACE (NASA)
![Page 4: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/4.jpg)
SUMER:L line spectra in Filament and Prominence
Central reversed profiles in filamentNo reversed profiles in prominence
![Page 5: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/5.jpg)
Lyman lines
Scattered light of the chromosphere
with/without PCTR
![Page 6: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/6.jpg)
PRD/CRD L-alpha profiles
(Gouttebroze, Vial, Heinzel 1987)
Isthermal and isobaric slab model
OSO8
![Page 7: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/7.jpg)
GHV grid
of NLTE models of
solar prominences
Atom of Hydrogen
Lyman lines > 912 A L, L L
Balmer lines > 3646 AH, H
(Gouttebroze, Heinzel, Vial1993)
L, L L
H, H
Ne, L cont, S(H)
Paschen line
![Page 8: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/8.jpg)
LLL
Three prominences observed by SoHO/SUMER
May
June
March
unreversed
reversed
W
(Heinzel, Schmieder,Vial, Kotrc, 2000)
Two types of profilesof the Hydrogen Lyman
series: Why ?
![Page 9: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/9.jpg)
Lyman Series L4, L5,L6 , same behaviour
![Page 10: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/10.jpg)
Models of prominences: importance of the PCTR
PCTR
(Heinzel, Schmieder, Vial, Kotrc A et A, 2001)
Case of a thick PCRT
![Page 11: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/11.jpg)
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
![Page 12: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/12.jpg)
Filament is visible in the centre of Lyman lines
3x 0.045 A, = 0.135 A
(Schmieder, Heinzel, Kucera, Vial 1998)
![Page 13: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/13.jpg)
SUMER Spectra Lto Ly c
Lc
Reversed profiles
L L L L
The central intensity I0 = 0
![Page 14: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/14.jpg)
1D-slab model of an filament1D-slab model of an filament
Tc
h
P=constvt 5 km s-1
D=5000 km
The existence of a PCTR explains the behaviour of the Lyman profiles
![Page 15: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/15.jpg)
EIT 304 A
CME
(06:41 and 13:13 UT MAY 31 1997)
H
SUMER can give the Velocity of the eruptive prominence
(Schmieder, Delannée, Deng, Vial, Majarska et al 2001)
![Page 16: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/16.jpg)
SoHO/EIT et SUMER
(spectroscopic Diagnostic )
MSDP + SUMER slit
(Lyman L4)
Velocity asymmetric profile = 100 km/s
EIT SUMER
(Schmieder, Delannée, Deng, Vial, Madjarska 2000)
![Page 17: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/17.jpg)
Meudon spectroheliograph (H)
SoHO/EIT (He II)
Filament Ha and EUV (Filament Ha and EUV (> 912 A)> 912 A)
typical example : sept 14, 1999
![Page 18: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/18.jpg)
Dark filament channels EIT, CDS, TRACE
Coronal lines
No void But Volume blocking
Coronal lines
I(fil)=Ibg+Ih+Ifg
Ih=0
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
Ifg
![Page 19: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/19.jpg)
EUV-filament
THEMIS – H-alpha
SOHO/CDS EUV rasters
(Heinzel, Schmieder, Tziotziou, 2001)
![Page 20: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/20.jpg)
TRACE 195
TRACE 171A
SVST(Engvold)
CDS fov
(Schmieder, Yong Lin, Heinzel, Schwartz 2004)
Other example of a EUV filament located at high latitude
![Page 21: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/21.jpg)
Absorption of coronal-line radiation by resonance hydrogen
& helium continua in a cool prominence plasma
912 A
504 A
227 A
HIHeIHeII
CDS linesCDS linesEIT + TRACE
wavelength
SUMER
![Page 22: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/22.jpg)
EUV Filament
filament
Lyman-continuum to H-alpha opacity ratiosHeinzel et al., 2001, Tziotziou et al 2000
isbetween 15 and 200 in the filament between 0 and 15 in the EUV filament
this corresponds to a H lower than 0.1 and a too low contrast which does not allow to distinguish the filament from the chromosphere
Why the cool material is not visible in H?
![Page 23: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/23.jpg)
Geometrical model
photosphere
coronaAbsorption mechanism andVolume blocking
(Heinzel, Anzer , Schmieder 2003)
![Page 24: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/24.jpg)
Halpha Meudon
Ha VTT/MSDP
![Page 25: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/25.jpg)
CDS –SUMER coalignmentCDS –SUMER coalignment
MgX 624.94 Å
SoHO/CDS
SoHO/SUMER, L raster
SoHO/CDSThe ratio of the intensities OV (CDS) and OVI (SUMER) permits to compute the optical thickness of EUV fil
![Page 26: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/26.jpg)
Mass loading
The plasma density =1.4 mHnH ~1.4 mH n1 + ne
ne=C (n2) 1/2
nH depends on 912 A
With non LTE transfer calculations of Lyman lines,912 is computed .
EUV Filament mass of filament of Oct 15, 1999 (912) Mg1.0 8.6x 1014
5.0 2.2 x 1015
12 3.0 x 1015
D EUV filament
With a spectroscopic model (Heinzel et al 2003, Schwartz et al. 2004)
Mass of EUV filament =Mass of H filament (double the mass)
![Page 27: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/27.jpg)
Lyman lines in EUV filament
H fil: reversed Lyman line profile EUV fil: unreversed profiles WHY?
(Schwartz, Heinzel, Schmieder, Anzer 2005)
SUMER slit
![Page 28: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/28.jpg)
(Schwartz, Heinzel, Anzer, Schmieder,
2004 , Saint Petersburg)
H/D
Model for EUV filament
Hydrogen ionisationdegree
T
Electron
density
![Page 29: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/29.jpg)
EUV filament model compared with EUV filament model compared with HH filament model 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:
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)
This leads to (Schwartz, Heinzel, Schmieder, Anzer 2005)of higher Lyman lines and the modelgives o(H)<<0.1 (not H filament)
Tc =8000 K
T = 13 000 K
P= 0.08 dyn cm-2
EUV filament (Z=20000km)
Filament (Z=5000km)
![Page 30: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/30.jpg)
THEMIS MTR6302 A
B vect over Hmap
(Large angle with the vertical)
local vertical (Schmieder, Lopez 2004)
![Page 31: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/31.jpg)
Computations of the dips in each field line in the computation model box
Field line
dH = Hg = 300 km
altitude (z)(B . ) B > 0
Bz = 0
Simulation of the observations of cool plasma
Dips filled by plasma
(Aulanier and Démoulin 1998)
![Page 32: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/32.jpg)
(2) Extrapolation of B from SoHO/MDI
3D magneto-hydrostatic linear model with free parameters constrained by the theory and the observations
Aulanier G., Schmieder B., 2002, A&A, 386, 1106-1122
08:12 UT 07:52 UT
Lignes de champ
filament
arcades coronales
Matière froide
z > 4 Mm
z < 4 Mm
Topology of B and distribution of the cool matter
CDS OV
![Page 33: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/33.jpg)
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
![Page 34: PROMINENCES AND EUV FILAMENTS (What we have learnt with SUMER?)](https://reader035.vdocuments.site/reader035/viewer/2022062803/568146a4550346895db3c1c3/html5/thumbnails/34.jpg)