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Hydrostatic model ling of active region EUV and X-ray emis sion. J. Dudík 1 , E . Dzif čáková 1,2 , A. Kulinov á 1,2 , M. Karlický 2 1 – Dept. of Astronomy, Physics of the Earth and Meteorology, FM Ph I , Comenius University , Bratislava - PowerPoint PPT Presentation
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HydrostaticHydrostatic model modelling ling of active region of active region EUV EUV andand X-rayX-ray
emisemissionsion
J. Dudík J. Dudík 11, E, E.. Dzif Dzifčáková čáková 1,21,2, , A. KulinovA. Kulinová á 1,21,2, M. Karlický , M. Karlický 22
11 – – Dept. of Astronomy, Physics of the Earth and Dept. of Astronomy, Physics of the Earth and Meteorology,Meteorology, FM FMPhPhII, Comenius University, Comenius University, Bratislava, Bratislava
22 – Astronomic – Astronomical Institute of the Academy of Sciencees al Institute of the Academy of Sciencees of the Czech Republic, of the Czech Republic, Ondřejov Ondřejov
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I. Solar corona and coronal loops – an obligate introductionTemperature and density structure of solar coronaCoronal loops and the geometrical structure of magnetic field
II. Coronal heatingEmpirical factsModels: nanoeruptions & braiding
III. Scaling laws – simple, analytical, static modelEnergy equilibrium in static caseDerivation: homogeneous vs. inhomogeneous heating
IV. Model description and preliminary results
Solar corona Highest, extended “layer” of solar atmosphere
Highly structured: – in visible light: coronal streamers (mostly open, static? structures)– in EUV and X-ray: coronal loops, coronal holes, bright points, flares (open and closed structures, sometimes highly dynamical)
I.
Solar corona Solar corona consists of hot and tenuous plasma (Edlén, 1943):
Tcor 106 – 107 K ne,cor 1015 – 1016 m–3
high ionisation degree, plasma and field “frozen-in” optically thin (collisional excitation / spontaneous emission)
Corona and magnetic field Momentum equation dominated by the Lorentz force
force-free approximation:
Geometry given by the magnetic field
Anisotropy – multitemperature corona
(e.g. thermal conduction differs greatly along and across the field)
( , ) ( , ) ( , )B r t r t B r t
171 (1 MK)195 (1.5 MK)284 (2 MK)
Coronal heatingII. Solar corona is ~ 50 times hotter than chromosphere, and more than
order of magnitude more tenuous Without energy source the corona would be in energy equilibrium, with
low, chromospheric-like temperature decreasing outwards Turning off the heating would result in radiation cooling (in EUV
and X – ray spectral domains) of the solar corona during ~ 101 hours
An energy source (at least one) must exist – coronal heating problem
(chromospheric heating problem, solar wind „heating“ problem)
3 3 3 134 104(3 ) 5.10
3 3cor e pM R R n m R M
Coronal heating An estimate of the supplied energy can be obtained if we take into
account that heating must compensate at least for the radiative losses:
The coronal heating mechanism must meet following criteria:
– energy buildup in lower layers of the atmosphere
– energy transport across the chromosphere and
– energy dissipation in corona
Clear relationship exists between X–ray emission and photospheric magnetic flux systems
(Fisher et al., 1998; Benevolenskaya et al., 2002)
35 2 5 3
5 3 7 2 2 4
10 10 .
2
. 10 . .2,5.10 2,5.10 . 4.10
H rad e
pH
H H H
E E n W m
F E W m m W m L
Braiding & nanoeruptions Close et al. (2003): most of the photospheric magnetic flux “closes”
before reaching coronal heights Photospheric fluxtube footpoints are subject to random motions due
to convection (granullation) Fluxtubes braid along one another due to the random motions
(Parker, 1972). The angles between the fluxtube and the photosphere change over time
If the angle reaches critical limit, local reconnection sets in, relasing the stored magnetic energy and simplifying the local field geometry
Estimate of the released energy (Parker, 1988): 1017 W, which is nine orders of magnitude less than the energy released in largest flares
– 10–9 : nanoeruptions Sturrock & Uchida (1981) + Rosner, Tucker, Vaiana (1978): heating
parametrisation for heating due to braiding & nanoeruptions:
12 / 70H B L
Static energy equilibrium
In following, we shall assume static energy equilibrium.
In this case the losses due to radiation Erad and thermal conduction
must be compensated by energy source H:
. 0.rad condH E F
In solar corona the thermal conduction across the magnetic field is negligible. The thermal conduction tensor then has non-zero components only in the direction along the field and can be approximated as
where 0 9,2.10–11 W.m–1.K–7/2 is the Spitzer thermal conduction coefficient. This approximation allows us to solve the energy equilibrium equation in 1D Assumption: the coronal loop has constant cross section
.condF T
5/ 2 0 00 ,T B B
III.
Radiative loss function
Corona is optically thin environment, collisional excitation is compensated by spontaneous emission
Total radiative losses Erad depend on square of electron density and through the statistical equilibrium equation also on temperature. They can be approximated :
Erad = ne2Q(T) = ne
2T 10–32 ne2 T–1/2,
where the last expression holds in the temperature range of ~ 106 – 107.5 K.
Radiative loss function Q(T): RTV analytical approximation(Rosner, Tucker, Vaiana, 1978) Q(T) 10–32 T–1/2
(Priest, 1982: Solar MHD)
Heating function Not known. We parametrize it by the power-law function containing three
parameters:
where CH, ,= const. – free parameters
B0 – field strenght at loop footpoint,
L – loop half-lenght,sH – heating scale lenght
Bref = 10–2 T, Lref = 108 m – scaling constants
sH can be determined from the decrease of the field with height:
does not depend on
0
0 ,H H
s srefs s
Href
LBH H e C e
B L
( 1)( ) HH
ss
Scaling laws The solution of the energy equilibrium equation can be expressed in the
form of scaling laws, 1D analytical relations between loop half-length L, heating H, loop apex temperature T1 and base pressure p0 = p(s0) at the loop footpoint s0:
Rosner, Tucker & Vaiana (1978) – pionieer model, p = const, H(s) = const.
Serio et al. (1981) – inhomogeneous heating , hydrostatic decrease of gas pressure, no changes in gravitational acceleration :
Aschwanden & Schrijver (2002): linear terms added, constants as functions
1/31
7 / 6 5/ 6
1400( )
98000
T pL
H p L
/0 Hs sH H e
20.04
1/31 0
0.57 / 6 5/ 6
0
1400( )
98000
H p
H p
L L
s s
L L
s s
T p L e
H p L e
Scaling laws – derivation Generalized derivation containing radiative loss function Q(T) = T Assumptions: – p = qnekBT ; q = 23/12 H:He = 10:1, total ionisation
– Fcond (s=s0) 0 & Fcond (s=L) = 0 & Fcond (s s0,L) 0– symmetrical loop
Derivation:
0
1
2 /2/5/ 2 20
02 2
2 /2 2/5/ 2 1/ 2 5/ 20
02 2
2 /2/1/ 2 5/ 20
02 2
.
2
0
p
H
p
H
p
H
cond rad
s ss s
B
s ss s
B
T s ss s
BT
F E H
p ed dTT T H e
ds ds q k
p ed dT dTT T H T e
ds ds dsq k
p eT H T e dT
q k
0
0
0 0
/2 3/ 2 3/ 2/7 / 2 7 / 20 0 1
0 0 12 2
220
0 1 0 12 2
20
3/ 2 7
7 , 3 / 2
3 2
p
H
p H
L s sL s s
B
L s L ss s
B
p e T TH T T e
q k
pH T e e T T
q k
Scaling laws – derivation
We now write the integral as a function of the upper boundary T:
1
0 0
2 /2 2/5 1/ 2 5/ 20
02 2
( ) ( )332 25 7 / 2 7 / 20 22
0 112 2
2
4 4
7(3 2 )
p
H
p p
T s ss s
BT
L s L s
s s
B
p edTT T H T e dT
ds q k
pdTT T T e H T T e
ds q k
0
0 0
0
( )2 25 3/ 2 3/ 2 2 7 / 2 3/ 20
1 1 12 2
( ) ( )
3 3( )1/ 2 27 2 2 22042 2
1 1 1
4
(3 2 )
221
2 3
p
p p
p
L s
s
B
L s L s
s s
L s
s
B
pdTT e T T P T T T
ds q k
P e e
pdT T T TT e P
ds T T Tq k
0
0
1
1/ 2
2
( )1/ 2121
0 01 2 2
2 2
2 31 (1 )
7 2 30, 0, 2 0; 1
4 2
p
L s
s
BT
T
H p
x dxT p L s e
q kx P x P
P s s
Scaling laws – derivation
I(P)
1
0
7 2 3( , ) ; 0, 0, 2 0
4 21 (1 )
x dxI P
x P x P
Scaling laws Result:
0 0
0 00
( ) ( )2 22/ 74/ 7 7 74/ 7 2/ 7
1 0 0
4 2 11 24 82 2 8 472 77 70 00
2 22 1 (2 ) (2 )1 (2 )7 77
4( , )
7
3 2 4( , ) .
7 7
.
H H
p pH
L s L s
s s
B
L s L sL ss ss
T I P H L s e e
q kp I P H L s
e e e
Temperature and pressure Temperature – function of the position s
– analytical approximation (Aschwanden & Schrijver, 2002):
11
11
( )( )
10
( )( ) 50
1 100 0 0
0.3 ( ) 1
10.3 ( ) 1 1 log
2
b Ta T
H
b Ta T
H H
L L sT s T
s L s
s sL L s L L sT s T
s L s s L s L s
0 0
( ) 00 1
1 0
0
( ) ( ) ; ( )
( ) ( ) 1 1
p p
s s h h
s hp p
Bp e
H
L sp s p e p h e s h
h h
hqk hh T h
m g R R
pressure dependency – hydrostatic equilibrium:
confused by previous authors!
Scaling laws – Serio et al. (1981)
Apex temperature T1 and base pressure tlak v ukotvení p0 as functions of L
= 10–32, = –1/2, CH = 5.10–5 J.m–3.s–1, = 1,
B0 = 100, resp. 1000 G
= 0 = 1 = 2
RTV approximation to Q(T)
Motivation
Motivation: To study the dependency of coronal EUV and X-ray emission on heating function
Task: „Assemble“ a model of EUV and X-ray coronal emission of an active region in regular gridusing: magnetic field model (extrapolation)
radiative loss funcitonscaling lawspower-law heating function localised at loop footpoints
Results: (In)dependency of the heating scale length on the fieldEmission distributionConstrains to heating function
IV.
Loop geometry: L and H
For a given grid point, we trace the field line passing through it and obtain the L and B0 distributions
The heating scale lenght sH can be determined from the fall-off of the magnetic field induction with height
These values are then supplied into the scaling laws as the independent variables. We can in this way obtain the temperature and density distribution only from the knowledge of the photospheric longitudinal field!
Informations about the magnetic field can be obtained by extrapolating the photospheric longitudinal magnetogram using force-free approximation ( = const.):
using the method developed by Alissandrakis (1981)
B B
Filter response to emissivity Using the CHIANTI atomic database we compute the synthetic spectra (in a
given wavelenght range) for an entire range of temperature and density values. The spectra contain emission lines and continuum.
The synthetic spectra are then multiplied with the filter response functions and integrated. In this way we obtain the filter response to emissivity, which is a function of T a ne.
Scheme
Linear force-free
extrapolation
longitudinal magnetogram
Determine sH
Scaling lawsT1 p iterations
T1 and p0
Field line tracing L a B0
Synthetic emisison
T and ne
Filter response to emissivity
Comparison with observations,
Constrains on H
AR 10963 – field and sH
( 1)( ) HH
ss
AR 10963 – EIT observations
EIT 17,1 nm, linear scale EIT 19,5 nm, linear scale
AR 10963 – model & observationsEIT 171 EIT 195 EIT 284
model 171 model 195 model 284
Filter ratios --> temperature
195/171, observations195/171, model
= 10–32, = –1/2, CH = 5.105 J.m–3.s–1, = 1, = 2 = 1 = 0
Thank youThank youfor your attentionfor your attention