# Damping of Linear Nonadiabatic MHD Waves in a Flowing Prominence Medium

Authors: Nagendra Kumar; Anil Kumar; Himanshu Sikka; Pradeep Kumar
Journal: Advances in Astronomy
 (2014)

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## Abstract

We study the effect of shear flow on the time damping of linear nonadiabatic magnetoacoustic waves in a solar prominence. We consider a homogeneous, isothermal, and unbounded medium permeated by a uniform magnetic field. The adiabaticity is removed by including the optically thin radiative losses, thermal conduction, and heating term in energy equation. We present a local theory of MHD waves to obtain a dispersion relation. The dispersion relation is solved numerically to study the time damping of these waves. It is found that flow influences the damping time and damping per period of both the slow and fast waves significantly. Damping time and damping per period of slow waves are very much higher than the damping time and damping per period of fast waves.


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## Body

## 1. Introduction

A large number of observations of oscillations in large scale magnetic structures such as prominence have been observed from space-borne and ground based instruments [1–5]. Small amplitude oscillations observed in quiescent solar prominence can be interpreted in terms of linear magnetohydyrodynamic waves. To study these small amplitude oscillations, one of the damping mechanism nonadiabaticities has been extensively studied because linear nonadiabatic magnetoacoustic waves have interesting physical effects such as time and spatial damping of the disturbances. Carbonell et al. [6] studied the time damping of linear nonadiabatic magnetohydrodynamic waves in an unbounded plasma with coronal properties and found that behavior of the damping changes significantly when going from very small to very large wavenumbers and becomes almost constant for very large wavenumbers. Spatial damping of linear nonadiabatic magnetoacoustic waves in prominence medium has been studied and it is found that the spatial damping is dominated by thermal conduction at shorter periods while the spatial damping is dominated by radiation at the periods greater than 1 s [7]. Soler et al. [8] showed that nonadiabatic effects are efficient damping mechanism for magnetoacoustic modes.Ground and space-borne satellites observations have confirmed that the solar and space plasmas are always dynamic showing flow [9–11]. Therefore, all the theoretical models should include the presence of flow. Nakariakov and Roberts [12] theoretically investigated the effect of steady mass flow in coronal and photospheric slabs. Carbonell et al. [13] discussed the combined effects of nonadiabatic mechanism and steady flow on the time damping of slow modes and found that flow does not modify the damping time but increases the period of slow mode dramatically for the flow velocities very close to nonadiabatic sound speed. In all previous studies, shear flow has not been taken into account. Therefore, in the present study, we investigate the local behavior of time damping of linear nonadiabtic magnetoacoustic waves in the presence of shear flow.


## 2. Basic Equations and Dispersion Relation

The equilibrium configuration considered in the present work is made of a homogeneous slab that is infinite in all directions. The magnetic field is uniform and is oriented along thez-direction. The background flow in z-direction is assumed to vary linearly in the x-direction as v
0
=
v
0
(
x
)
z
^
=
a
x
z
^, with a constant a [14]. This assumption of the linear profile for velocity shear is applicable for wide variety of astrophysical shear flows. Parallel thermal conduction to the magnetic field, heating, and radiative losses are considered as nonadiabatic effects. The gravitational effects have been neglected because wavelengths are assumed much smaller than gravitational scale height. The basic MHD equations describing the plasma motion are given by
(1)
D
ρ
D
t
+
ρ
∇
·
v
=
0
,
ρ
[
∂
∂
t
+
v
·
∇
]
v
+
∇
p
=
(
∇
×
B
)
×
B
4
π
,
∂
B
∂
t
=
∇
×
(
v
×
B
)
,
1
γ
-
1
∂
p
∂
t
-
γ
p
ρ
(
γ
-
1
)
∂
ρ
∂
t
+
ρ
L
(
ρ
,
T
)
-
∇
·
(
κ
·
∇
T
)
=
0
,
p
=
2
ρ
k
B
T
m
p
.
Here, ρ, p, T, v, andB denote the density, gas pressure, temperature, velocity, and magnetic field, respectively. The term ∇
·
(
κ
·
∇
T
) represents the thermal conduction. The symbol L is heat-loss function and is given by
(2)
L
(
ρ
,
T
)
=
χ
ρ
T
α
,
where χ and α are piecewise continuous functions depending on temperature [6].Considering small perturbations from the equilibrium, the field quantities can be written as(3)
B
=
B
0
+
B
1
(
r
,
t
)
,
v
=
v
0
(
x
)
+
v
1
(
r
,
t
)
,
p
=
p
0
+
p
1
(
r
,
t
)
,
ρ
=
ρ
0
+
ρ
1
(
r
,
t
)
,
T
=
T
0
+
T
1
(
r
,
t
)
,
where the subscripts “0” and “1” refer to equilibrium and perturbed quantities, respectively. Here, the equilibrium magnetic field B
0 is homogeneous and is taken along z-axis; that is, B
0
=
B
0
z
^. The assumption about a homogeneous magnetic field may be reasonable for the large regions of quite sun but does not imply appropriate results. However, the assumption of a homogeneous magnetic field provides us a relatively simple mathematical model to study MHD waves in solar prominence. Several authors [6, 15, 16] used homogeneous magnetic field to study MHD waves in different regions of solar atmosphere. In the future, we will consider inhomogeneous magnetic field to study such MHD waves in solar prominence model and the results will be reported elsewhere.We linearise the basic equations (1) to obtain
(4)
∂
ρ
1
∂
t
+
(
v
0
·
∇
)
ρ
1
+
ρ
0
(
∇
·
v
1
)
+
ρ
1
(
∇
·
v
0
)
=
0
,
ρ
0
∂
v
1
∂
t
+
ρ
0
v
0
∂
v
1
∂
z
+
ρ
0
v
x
∂
v
0
∂
x
=
-
∇
p
1
-
B
0
×
(
∇
×
B
1
)
4
π
,
∂
B
1
∂
t
=
∇
×
(
v
0
×
B
1
)
+
∇
×
(
v
1
×
B
0
)
,
∂
p
1
∂
t
-
c
s
2
∂
ρ
1
∂
t
+
(
γ
-
1
)
[
L
ρ
ρ
1
+
L
T
T
1
]
ρ
0
=
(
γ
-
1
)
(
B
0
·
∇
)
[
κ
∥
B
0
2
(
B
0
·
∇
)
T
1
]
,
p
1
p
0
=
ρ
1
ρ
0
+
T
1
T
0
,
where κ
∥
=
1
0
-
11
T
5
/
2
W
m
-
1
K
-
1 is thermal conduction parallel to magnetic field. If background flow is spatially inhomogeneous in the vertical direction, we can not apply Fourier transformation and a nonlocal approach would be more appropriate in this context. Though the local approximation has limited applicability, in the present study we are interested in investigating the behavior of nonadiabatic waves in the initial stage of the evolution of wave perturbations. Since local approximation is restricted to short wavelength fluctuations, (4) can be analyzed using Fourier transform over space and time for the study of local behavior of waves [17–20]. So we perform Fourier analysis in plane waves and assume that all perturbations are of the form e
i
(
k
.
r
-
ω
t
), where k
=
k
x
x
^
+
k
z
z
^ is the wavenumber and ω is the frequency. From linear equations (4), we obtain the following dispersion relation:
(5)
(
Ω
ω
(
Ω
+
i
v
0
′
)
-
k
2
v
A
2
ω
+
i
v
A
2
k
x
k
z
v
0
′
)
(
Ω
A
1
ω
+
k
z
2
ρ
0
A
2
)
+
k
x
2
Ω
2
ω
ρ
0
A
2
=
0
,
where
(6)
Ω
=
ω
-
k
z
v
0
,
A
1
=
(
k
T
c
s
-
i
ω
)
,
A
2
=
ρ
0
c
s
3
γ
(
k
ρ
-
k
T
)
+
i
ρ
0
ω
c
s
2
,
k
T
=
A
T
0
p
0
c
s
,
k
ρ
=
H
ρ
0
p
0
c
s
,
A
=
(
γ
-
1
)
κ
∥
k
x
2
+
(
γ
-
1
)
ρ
0
L
T
,
H
=
(
γ
-
1
)
(
L
+
ρ
0
L
ρ
)
,
L
ρ
=
(
∂
L
∂
ρ
)
T
,
L
T
=
(
∂
L
∂
T
)
ρ
.
Here, v
A is the Alfven velocity, c
s is the sound velocity, and v
0
′ is the derivative of v
0 with respect to x. If we simplify the dispersion relation (5), we can obtain a sixth order polynomial in ω due to flow. Since we are solving this dispersion relation numerically, there is no need to simplify it in ω.In the absence of flow, the dispersion relation (5) reduces to
(7)
ω
(
(
k
ρ
-
k
T
)
γ
ω
5
+
i
k
T
c
s
ω
4
-
k
2
(
c
s
2
+
v
a
2
)
ω
3
kkk
-
i
k
2
(
v
a
2
k
T
c
s
+
c
s
3
(
k
T
-
k
ρ
γ
)
)
ω
2
kkk
+
k
2
v
a
2
k
z
2
c
s
2
ω
-
i
k
2
v
a
2
k
z
2
c
s
3
(
k
ρ
-
k
T
)
γ
)
=
0
.
Equation (7) yields the following fifth order dispersion relation in ω:
(8)
ω
5
+
i
k
T
c
s
ω
4
-
k
2
(
c
s
2
+
v
a
2
)
ω
3
-
i
k
2
(
v
a
2
k
T
c
s
+
c
s
3
(
k
T
-
k
ρ
γ
)
)
ω
2
+
k
2
v
a
2
k
z
2
c
s
2
ω
-
i
k
2
v
a
2
k
z
2
c
s
3
(
k
ρ
-
k
T
)
γ
=
0
,
which is similar to that obtained by Carbonell et al. [6] and it has been discussed by them in detail. So we will here solve and discuss the dispersion relation (5) to study the damping time and damping per period of fast and slow waves.


## 3. Results and Discussion

We solve the dispersion relation (5) numerically taking density, temperature, and magnetic field for the prominence region [21] corresponding to quiescent prominence conditions of solar atmosphere. The values of equilibrium parameters for the above mentioned prominence region are taken as T
0
=
8000 K, ρ
0
=
5
×
1
0
-
11 kg m−3, B
0
=
5 G, α
=
7.4, and χ
=
1.76
×
1
0
-
13 (Hildner [21]). Here we consider the real wavenumber and find the complex solutions of the frequency as ω
r
+
i
ω
i. We obtain two pairs of roots representing the fast and slow modes whereas purely imaginary root corresponds to thermal mode. The roots thus obtained do not represent instability because of small values of flow. For each pair (
ω
1
,
ω
2
), ω
1
=
ω
r
-
i
ω
i and ω
2
=
-
ω
r
-
i
ω
i, ω
1 corresponds to the parallel wave propagating towards the positive z-direction, whereas ω
2 corresponds to antiparallel wave propagating towards negative z-direction. The damping time is τ
d
=
1
/
ω
i and damping per period is D
p
=
ω
i
/
ω
r. We plot Figures 1–6 to study the effect of flow on damping time and damping per period of these waves with wavenumber. Figure 1 shows the variation of damping time of fast wave with wavenumber whereas Figure 2 shows the variation of damping time of slow wave with wavenumber for different values of flow. Damping time of both slow and fast waves decreases with the increase in the value of flow. For smaller values of wavenumber k damping time is higher than the larger values of wavenumber and becomes constant after a certain value of wavenumber. Damping time of slow wave is very much higher than the fast wave corresponding to the same set of values of flow as considered in fast wave. In the absence of flow, Figure 3 has been drawn to see the variation of damping time for slow and fast wave by changing X- and Y-scales from linear to log according to N. Kumar and P. Kumar [22] and it is found that results shown in Figure 3 are in agreement with results shown in Figure 1(b) of [22].Figure 1
Damping timeτ
d of fast waves versus wavenumberk.Figure 2
Damping timeτ
d of slow waves versus wavenumberk.Figure 3
Damping timeτ
d versus wavenumberk.Figure 4
Damping per periodD
p of fast waves versus wavenumberk.Figure 5
Damping per periodD
p of slow waves versus wavenumberk.Figure 6
Damping per periodD
p versus wavenumberk.Figures4 and 5 are drawn for damping per period versus wavenumber for fast and slow waves for the same set of values of flow, respectively. Damping per period of slow waves is very much higher than the damping per period of fast waves corresponding to similar values of flow. The patterns of increasing damping per period are almost similar for both slow and fast waves. Damping per period for both waves has linear dependence on wavenumber except for smaller values of k in case of slow waves. Figure 6 drawn in log scale depicts that the pattern of variation of damping per period is similar to that shown in Figure 1(c) by N. Kumar and P. Kumar [22] in the absence of flow.


## 4. Conclusions

Quiescent solar prominences and filaments are those features in solar atmosphere which show material flows and oscillations. So, in this paper, we have analyzed the time damping of MHD waves in nonadiabatic solar prominence plasma taking into account the effects of thermal conduction and shear flow. The nonadiabaticity is modeled by a general heat-loss function of thermodynamic parameters of plasma. We have obtained the dispersion relation using local approximation and solved it numerically to see the variations of damping time and damping per period of slow and fast MHD waves with wavenumber for different values of flow parameter. It is found that damping time of slow and fast waves decreases with the increase in flow and damping time of the slow wave is very much higher than that of the fast wave. It is observed that damping per period also decreases with the increase in flow.



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*Source: 541376-2014-05-15.xml*