prominences and euv filaments (what we have learnt with sumer?)
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PROMINENCES AND EUV FILAMENTS (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. - PowerPoint PPT PresentationTRANSCRIPT
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
Prominence in multi-wavelength
Prominence H(Bialkov)SUMMER SLIT
(Ondrejov)
Prominence in hydrogen L-alpha
TRACE (NASA)
SUMER:L line spectra in Filament and Prominence
Central reversed profiles in filamentNo reversed profiles in prominence
Lyman lines
Scattered light of the chromosphere
with/without PCTR
PRD/CRD L-alpha profiles
(Gouttebroze, Vial, Heinzel 1987)
Isthermal and isobaric slab model
OSO8
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
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 ?
Lyman Series L4, L5,L6 , same behaviour
Models of prominences: importance of the PCTR
PCTR
(Heinzel, Schmieder, Vial, Kotrc A et A, 2001)
Case of a thick PCRT
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
Filament is visible in the centre of Lyman lines
3x 0.045 A, = 0.135 A
(Schmieder, Heinzel, Kucera, Vial 1998)
SUMER Spectra Lto Ly c
Lc
Reversed profiles
L L L L
The central intensity I0 = 0
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
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)
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)
Meudon spectroheliograph (H)
SoHO/EIT (He II)
Filament Ha and EUV (Filament Ha and EUV (> 912 A)> 912 A)
typical example : sept 14, 1999
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
EUV-filament
THEMIS – H-alpha
SOHO/CDS EUV rasters
(Heinzel, Schmieder, Tziotziou, 2001)
TRACE 195
TRACE 171A
SVST(Engvold)
CDS fov
(Schmieder, Yong Lin, Heinzel, Schwartz 2004)
Other example of a EUV filament located at high latitude
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
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?
Geometrical model
photosphere
coronaAbsorption mechanism andVolume blocking
(Heinzel, Anzer , Schmieder 2003)
Halpha Meudon
Ha VTT/MSDP
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
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)
Lyman lines in EUV filament
H fil: reversed Lyman line profile EUV fil: unreversed profiles WHY?
(Schwartz, Heinzel, Schmieder, Anzer 2005)
SUMER slit
(Schwartz, Heinzel, Anzer, Schmieder,
2004 , Saint Petersburg)
H/D
Model for EUV filament
Hydrogen ionisationdegree
T
Electron
density
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)
THEMIS MTR6302 A
B vect over Hmap
(Large angle with the vertical)
local vertical (Schmieder, Lopez 2004)
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)
(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
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