prominences and euv filaments (what we have learnt with sumer?)

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