Issue 
A&A
Volume 507, Number 2, November IV 2009



Page(s)  611  616  
Section  Astrophysical processes  
DOI  https://doi.org/10.1051/00046361/200912432  
Published online  15 September 2009 
A&A 507, 611616 (2009)
Characteristics of magnetised plasma flow around stationary and expanding magnetic clouds
G. Dalakishvili^{1}  S. Poedts^{1}  H. Fichtner^{2}  E. Romashets^{3}
1  Centre for Plasma Astrophysics, K.U.Leuven,
Celestijnenlaan 200B,
3001 Leuven, Belgium
2  Institut für Weltraum und Astrophysik, RuhrUniversität Bochum,
Universitätsstrasse 150, 44780 Bochum, Germany
3  Solar Observatory of Prairie View A & M University, Prairie View, TX 77446, USA
Received 6 May 2009 / Accepted 4 September 2009
Abstract
Aims. Studies of interplanetary magnetic clouds have shown
that the characteristics of the region ahead of these objects, which
are moving away from the Sun in the solar wind, play a role in
determining their geoefficiency, i.e. the kind and the degree of their
effects on the Earth environment. Therefore, our main goal is to model
and study the plasma parameters in the vicinity of interplanetary
magnetic clouds.
Methods. To this end we present a model in which the magnetic
clouds are immersed in a magnetised plasma flow with a homogeneous
magnetic field. We first calculate the resulting distortion of the
external magnetic field and then determine the plasma velocity by
employing the frozenin condition.
Results. Subsequently, the plasma density and pressure are expressed as functions of the magnetic field and the velocity field.
Conclusions. The plasma flow parameters are determined by
solving the timeindependent ideal MHD equations for both the
stationary regime and for the case of an expanding cylindrical magnetic
cloud, thus extending previous results that appeared in the literature.
Key words: magnetohydrodynamics (MHD)  magnetic fields  plasmas  Sun: solar wind
1 Introduction
A magnetic cloud (MC) is a specific type of interplanetary coronal mass ejection (see Burlaga 1995; WimmerSchweingruber et al. 2006; Démoulin et al. 2008) and can be considered as a magnetically isolated structure moving in the solar wind. There are various studies of MCs, particularly of their inner structure (e.g., Nakwacki et al. 2008), their interaction with the solar wind streams (e.g., Lepping et al. 2008), and their expansion (e.g., Démoulin et al. 2008, and further references therein). While in these investigations the authors mainly deal with the internal cloud dynamics, in the present paper we focus on how an expanding MC perturbs the physical parameters of its ambient environment. In order to enable an analytical description of the structure of both the MC and its immediate surroundings, it has been suggested that MCs are forcefree magnetic field configurations (Vandas et al. 2006; Lepping et al. 1990; Burlaga 1988,1991). Numerical studies (Manchester et al. 2004; Chane et al. 2006; De Sterck & Poedts 2000; De Sterck & Poedts 1999), exploring the character of magnetised plasma flows near MCs, in which these structures are considered as superconductors (De Sterck & Poedts 2000; De Sterck & Poedts 1999), as well as observational data analysis efforts (Owens et al. 2005), have revealed that the region in front of an interplanetary MC has a rather complicated magnetic structure and a complex plasma structure as well. In order to get more insight into the characteristics of this region and the physical phenomena within it, and in order to better understand the geoefficiency of MCs, an analytical treatment of the magnetised plasma flow in their vicinity is beneficial.
In mathematical models of forcefree magnetic flux ropes (Vandas et al. 2006; Lepping et al. 1990; Burlaga 1988), the radial component of the magnetic field is zero all throughout the MC including the boundary region. The boundary condition on the MC surface (equal normal components of the magnetic field on both sides) then naturally leads to the requirement that the ambient field must be tangential to the surface of a MC, i.e. the same requirement that is to be satisfied for a superconductor. Analytical expressions for the magnetic field satisfying such boundary conditions can be found by Vandas et al. (2003) and Romashets & Poedts (2007). In these papers, MCs are considered as superconductors placed in a given ambient magnetic field and the distortion of the external magnetic field has been calculated. First, by Vandas et al. (2003) both spherical and cylindrical shapes of MCs were considered and the existing quantitative models of magnetic field behaviour around MCs were summarised. Second, by Romashets & Poedts (2007) analytical expressions for the plasma velocity, pressure and density were derived.
In the present study, we consider a MC that is placed in a magnetised plasma flow with an initially homogeneous magnetic field. We assume that the normal component of the magnetic field vanishes at the boundary of the MC and that far from the MC the magnetic field approaches its undisturbed value. We thus generalise the solutions given by Romashets & Poedts (2007) for a cylindrical superconductor: both the cases B_{z}=0 and are considered (cylindrical coordinates are used). In addition, we present the solution for the magnetic field for the case of a spherical superconductor. We consider solutions for the distortion of the external magnetic field decreasing as r^{k} (where r is the distance from the axis/centre of the superconductor); where the case k=3 leads to the particular solution derived and discussed by Romashets & Poedts (2007). Finally, we also study the plasma flow parameters around a cylindrical MC that is radially expanding during its evolution in the ambient plasma flow.
The paper is organised as follows: in Sects. 2 and 3 we consider the characteristics of the stationary plasma flow in the case of cylindrical and spherical MCs, respectively. In Sect. 4, the case of an expanding cylindrical MC is investigated. In Sect. 5, we summarise and discuss our results.
2 Physical parameters of a magnetised plasma flow around a cylindrical superconductor
In this section, we define twodimensional distributions of the magnetic,
velocity, density and pressure fields in a plasma flow around a cylindrical
MC with radius r_{0}. Using cylindrical coordinates
,
we start
with constructing a magnetic field that is uniform far from the cylinder
(i.e. for
)
and tangential to the cylinder surface, i.e. B_{r}=0 at
r=r_{0}, and that has a vanishing zcomponent, i.e. B_{z}=0:
B_{r}  =  (2.1)  
=  (2.2)  
B_{z}  =  0.  (2.3) 
In order to determine the velocity of the steady state plasma flow around the cylindrical superconductor, the frozenin condition is used:
(2.4a) 
It is convenient to rewrite Eq. (2.4a) in the following way (see Romashets & Poedts 2007):
(2.4b) 
From Eq. (2.4b) it then follows that:
=  (2.5a)  
V_{z}B_{r}  =  (2.5b)  
=  (2.5c) 
Equation (2.4b) is solved using a variable separation ansatz, i.e:
(2.6) 
Upon substituting this ansatz in Eqs. (2.5a) and (2.5b) one obtains:
(2.7) 
Equation (2.7) leads to a set of ordinary differential equations (ODEs) for R and . The solutions of these ODEs are given by:
(2.8a) 
Where:
After this substitution we get:
and
(2.8b) 
Here, A_{r} and are constants. For Z(z) we use the same expression as in paper of Romashets & Poedts (2007), i.e. . With D, , and z_{0} constants. This choice satisfies Eqs. (2.5a)(2.5c).
Equations (2.5a)(2.5c) yield a relation between
F, the magnetic field and the velocity. Combining Eqs. (2.5c) with Eqs. (2.1), (2.2), (2.8a), and (2.8b) and
choosing C=1 (see Romashets & Poedts 2007) we obtain:
(2.9a) 
to ensure that V_{r} is finite everywhere, should be proportional to . For , the expression proposed by Romashets & Poedts (2007) could be used:
(2.9b) 
and Eq. (2.5b) gives:
(2.9c) 
In general, the magnetic field could be expressed as a linear combination of Eqs. (2.1)(2.3) i.e.:
B_{r}  =  (2.10a)  
=  (2.10b)  
B_{z}  =  0.  (2.10c) 
In the case when , it is possible to express the magnetic field as follows:
(2.11) 
(2.12) 
(2.13) 
The general form of the magnetic field reads:
(2.14) 
(2.15) 
(2.16) 
In analogy with the results obtained by Romashets & Poedts (2007), we can formulate a relationship between the components of the velocity, namely:
(2.17) 
In order to determine the plasma pressure P and the density of the plasma flow, in addition to Eqs. (2.1)(2.4) we should consider the equation of motion, the continuity equation, and the equation of state. These equation read, respectively:
(2.18) 
(2.19) 
and
(2.20) 
Here corresponds to the specific heat ratio. From the system of Eqs. (2.1)(2.4) and (2.18)(2.20), the expressions for the plasma density and pressure can be derived (see Romashets & Poedts 2007):
(2.21) 
and
P  =  
(2.22) 
Note, however, that the obtained mathematical solutions for the plasma pressure P and the plasma density , can become negative and thus loose their physical meaning. In order to obtain physically correct solutions for each value of k, proper values of the free parameters should be chosen. For the parameter value k=2, these plasma quantities become zero.
Figure 1: Distribution of the plasma velocity stream lines and magnetic field lines around cylindrical MC, in the plane z=0 and with B_{z}=0. The dashed lines correspond to streamlines and the solid lines represent magnetic field lines. Panel a) corresponds to the case when k=3; panel b) corresponds to the case k=5; panel c) shows the case k=7; and panel d) corresponds to k=20. 

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Figure 2: Contour plots of the magnitude of the magnetic field around cylindrical MC in the plane z=0 for nT, B_{z}=0. Panel a) corresponds to the case k=3; panel b) represents the case k=7; panel c) shows the case k=11 and panel d) corresponds to the case k=25. The magnetic field B is given in nT. 

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Figures 1 and 2 illustrate how the magnitude of the parameter kinfluences the character of the plasma flow and the magnetic field around the MC. In Fig. 1, in panels a) to d) the streamlines and the magnetic field lines are displayed for the different cases k=3, 5, 7, and 20, respectively. This figure illustrates that as the value of k is increased, the shape of both the streamlines and the magnetic field lines changes and both gradually evolve into straight lines, except of course in the immediate neighborhood of the MC where the flow and the magnetic field are both deflected around the MC (due to the imposed boundary conditions).
In Fig. 2 we plot the strength of magnitude of the magnetic field for nT and for the cases for k=3, 7, 11, and 25, in the panels a) to d), respectively. This figure clearly demonstrates that for increasing values of the model parameter k, the magnetic field becomes ever more uniform in the surroundings of the cylinder and its value increases in the immediate vicinity of the MC surface (in Fig. 2 one can see dark red region indicating a comparably strong magnetic field).
Figures 3 and 4 present contour plots of the plasma density and the plasma velocity V for k=1, km s^{1}, km s^{1}, z=0, z_{0}=r_{0}, and . One can see that the density decreases just in front and behind of the MC.
Figure 3: Contour plots of the magnitude of the plasma density around cylindrical MC in the plane z=0 for the parameter values km s^{1}, km s^{1}, z=0, z_{0}=r_{0}, and , k=1. Density is given in kg/m^{3}. 

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Figure 4: Contour plots of the magnitude of the plasma velocity around cylindrical MC in the plane z=0 for the parameter values km s^{1}, km s^{1}, z=0, z_{0}=r_{0}, and , k=1. Velocity is given in km s^{1}. 

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3 Magnetic field disturbance around a spherical magnetic cloud
In the present section, we define a three dimensional magnetic field
in a plasma flow around a spherical superconductor with radius
r_{0}. We consider a threedimensional magnetic field satisfying
the same boundary conditions as introduced in the previous section:
B_{r}  =  (3.1a)  
=  (3.1b)  
=  (3.1c) 
Note that we now used spherical coordinates denoted as usual by . In order to determine the steady state velocity field of the flow around the spherical superconductor, the frozenin condition is used again:
(3.2a) 
It is convenient to rewrite Eq. (3.2a) as follows (Romashets & Poedts 2007):
(3.2b) 
From Eq. (3.2a) it follows that
(3.2c) 
which shows that F is constant along the magnetic field lines.
Equation (3.2b) leads to a relation between F, the magnetic field and the velocity:
=  (3.3a)  
=  (3.3b)  
=  0.  (3.3c) 
After the definition of the magnetic field B and choosing a proper value for F, solving the system of Eqs. (3.3a)(3.3c) will give us an expression for the velocity field V.
In general, the magnetic field is a linear combination of Eqs. (3.1a)(3.1c):
B_{r}  =  (3.4a)  
=  (3.4b)  
=  (3.4c) 
4 Magnetic field and plasma velocity distribution around expanding cylindrical magnetic clouds
In this section, we define the magnetic field and the plasma flow velocity around an expanding MC. We consider a cylindrical MC with radius r_{0}. In previous studies, (Shimazu & Vandas 2002) and (Farrugia et al. 1995) considered the dynamics of the physical parameters inside the MC as a flux rope. In the present paper, on the contrary, we consider the perturbation of the plasma parameters outside the MC. It is assumed that the cylindrical MC expands radially, in a cylindrical symmetric manner i.e., r_{0}=r_{0}(t), where r_{0}(t) is a certain function of time.
Let us first determine the corresponding magnetic field. The
magnetic field should be tangential to the MC surface (i.e. B_{r}=0 at r_{0}) and uniform far from the cylinder, so for
). The components of the magnetic field that satisfies
these conditions can be expressed in the following way:
(4.1) 
(4.2) 
B_{z}=0.  (4.3) 
Here, we now have
r_{0}=r_{0}(t),  (4.4a) 
and
B_{0}=B_{0}(t).  (4.4b) 
From Faraday's law we obtain
(4.5) 
This then leads to the following equations:
(4.6) 
=  
(4.7) 
and
(4.8) 
For further considerations, it is convenient to introduce a new vector field :
(4.9) 
We assume symmetry along the cylindrical axis, this means:
(4.10) 
A combination of Eqs. (4.6)(4.10) then yields the related equations for the components of the vector potential :
(4.11) 
(4.12) 
and
(4.13) 
The component A_{z}, which satisfies Eqs. (4.11)(4.13), can be expressed as:
(4.14) 
From Eq. (4.9), the equations for the components of the velocity can then be determined:
(4.15) 
(4.16) 
and
(4.17) 
Equations (4.1)(4.3) and (4.17) then finally lead to an expression for the radial velocity component V_{r}:
V_{r}  =  
(4.18) 
From Eq. (4.18) we can see that at r=r_{0} the radial component of velocity . This simply means that, at the surface of the MC, the radial velocity is equal to the expansion velocity of the MC's surface. In other words, the external plasma flow velocity is tangential to the MC's surface. In order to provide finite values of V_{r} at , should be a function that is proportional to . For one can choose the same value as given in the paper Romashets & Poedts (2007). The simplest solution for A_{r} and , satisfying Eqs. (4.8), (4.9), and (4.13) is:
(4.19) 
Equations (4.15), (4.16), and (4.19) then yield that V_{z}=0. This solution could be generalised: any function will satisfy Eq. (5). The potential F could be the same function as the choice discussed by Romashets & Poedts (2007).
In order to ensure conservation of magnetic flux,
the following functions are chosen:
r_{0}(t)=(R_{0}(R_{0}+V_{E}(tt_{0})))^{1/2},  (4.20a) 
and
B_{0}(t)=R_{0}b_{0}/(R_{0}+V_{E}(tt_{0})).  (4.20b) 
Here R_{0} corresponds to the radius of the MC at time t=t_{0}, and b_{0} denotes the unperturbed magnetic field at the same moment in time. Note that V_{E} has the same order as the MC's expansion velocity and the values of this velocity are presented in Lepping et al. (2008).
5 Conclusions
In this paper, we first generalised the steady (timeindependent) solutions for the magnetic field and plasma flow velocity around a cylindrical MC as derived by Romashets & Poedts (2007) by considering more general distortions of the ambient magnetic field. While in the study by Romashets & Poedts (2007) the authors considered the case of a distortion of the ambient magnetic field decreasing with r^{3} from the MC axis, in the present paper we investigated a class of magnetic field distortions decreasing with r^{k}, where the parameter k determines the strength of the influence of the considered MC on the surrounding ambient magnetic field. We illustrated the distribution of the plasma density around the MC using the formulas given by Romashets & Poedts (2007). We remarked, however, that care has to be taken because not every set of free parameters leads to a physically consistent solution, and we found the right values for V_{0} and V_{1}^{0} in the case of k=1.The higher the value of k, the smaller or the less extensive the distortion around the MC. We calculated and illustrated how the value of k influences the configuration and magnitude of the magnetic field as well as the velocity field around a cylindrical MC treated as a superconductor (see Figs. 1, 2).
Note that different values of the model parameter k correspond to different current regimes. For example, when k=2 the plasma flow around a cylindrical superconductor with B_{z}=0 is current free. The same is true around a spherical superconductor, another extension of the previous analysis we studied as well. A third extension we considered involved a study of the character of the plasma flow parameters around a radially expanding cylindrical MC, instead of a steady flow around an MC with fixed radius.
These results can, on the one hand, be used as a starting point for an investigation of the interactions of interplanetary MCs with the ambient plasma flows and the characterisation of the forces acting on MCs or their surfaces. On the other hand, the new analytical expressions will serve as initial conditions for more involved numerical simulations, which will enable a study of the much more complicated dynamics of plasma flows around noncylindrical and/or nonspherical MCs. Such numerical simulations are expected to enable us to investigate the stability of the timeindependent solutions. Moreover, while we here presented solutions of the MHD equations for the region outside the MCs by prescribing general magnetic field configurations, the mentioned numerical studies will eventually allow us to construct selfconsistent solutions also for the region inside the MC.
AcknowledgementsThese results were obtained in the framework of the projects GOA/2009009 (K.U.Leuven), G.0304.07 (FWOVlaanderen) and C 90347 (ESA Prodex 9). Financial support by the European Commission through the SOLAIRE Network (MTRNCT2006035484) and by the Georgian National Science Foundation grant GNSF/ST06/4096 is gratefully acknowledged. The work also benefitted from the Forschergruppe 1048 (project FI 706/81) supported by the Deutsche Forschungsgemeinschaft (DFG).
References
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 Burlaga, L. F. 1991, Physics of the inner heliosphere 2, Particles, waves and turbulence, XI (Berlin Heidelber New York: SpringerVerlag), 352
 Burlaga, L. F. 1995, Interplanetary Magnetohydrodynamics (New York: Oxford University Press)
 Chane, E., Van der Holst, B., Jacobs, C., Poedts, S., & Kimpe, D. 2006, A&A, 447, 727 [EDP Sciences] [CrossRef] [NASA ADS]
 Démoulin, P., Nakwacki, M. S., Dasso, S., & Mandrini, S. H. 2008, Sol. Phys., 250, 347 [CrossRef] [NASA ADS]
 Farrugia, C. J., Osherovich, V. A., & Burlaga, L. F. 1995, Ann. Geophys., 13, 815 [CrossRef] [NASA ADS]
 Lepping, R. P., Burlaga, L. F., & Jones, J. A. 1990, J. Geophys. Res., 95, 11957 [CrossRef] [NASA ADS]
 Lepping, R. P., Wu, C. C., Berdichevsky, D. B., & Ferguson, T. 2008, Ann. Geophys., 26, 1919 [NASA ADS]
 Manchester, W. B., Gombosi, T. I., Roussev, I., et al. 2004, J. Geophys. Res., 109, A01102 [CrossRef]
 Nakwacki, M., Dasso, S., Mandrini, C., & Démoulin, P. 2008, J. Atmos. Sol. Terr. Phys., 70, 1318 [CrossRef]
 Owens, J. M., Cargill, P. J., Pagel, C., Siscoe, G. L., & Crooker, N. U. 2005, J. Geophys. Res., 110
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 De Sterck, H., & Poedts, S. 1999, A&A, 343, 641 [NASA ADS]
 De Sterck, H., & Poedts, S. 2000, Phys. Rev. Lett., 84, 5524 [CrossRef] [NASA ADS]
 Shimazu, H., & Vandas, M. 2002, EP&S, 54, 783 [NASA ADS]
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All Figures
Figure 1: Distribution of the plasma velocity stream lines and magnetic field lines around cylindrical MC, in the plane z=0 and with B_{z}=0. The dashed lines correspond to streamlines and the solid lines represent magnetic field lines. Panel a) corresponds to the case when k=3; panel b) corresponds to the case k=5; panel c) shows the case k=7; and panel d) corresponds to k=20. 

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In the text 
Figure 2: Contour plots of the magnitude of the magnetic field around cylindrical MC in the plane z=0 for nT, B_{z}=0. Panel a) corresponds to the case k=3; panel b) represents the case k=7; panel c) shows the case k=11 and panel d) corresponds to the case k=25. The magnetic field B is given in nT. 

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In the text 
Figure 3: Contour plots of the magnitude of the plasma density around cylindrical MC in the plane z=0 for the parameter values km s^{1}, km s^{1}, z=0, z_{0}=r_{0}, and , k=1. Density is given in kg/m^{3}. 

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In the text 
Figure 4: Contour plots of the magnitude of the plasma velocity around cylindrical MC in the plane z=0 for the parameter values km s^{1}, km s^{1}, z=0, z_{0}=r_{0}, and , k=1. Velocity is given in km s^{1}. 

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In the text 
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