A&A 486, 569-575 (2008)
P. D. Smith1 - J. I. Sakai2
1 - Institute for Materials Research, University of Salford, Greater Manchester, M5 4WT, UK
2 - Laboratory for Plasma Astrophysics, Faculty of Engineering, University of Toyama, 3190, Gofuku, Toyama, 930-8555, Japan
Received 20 February 2008 / Accepted 16 April 2008
Aims. We investigate magnetic reconnection rates during the coalescence of two current loops in the solar chromosphere, by altering the neutral-hydrogen to proton density ratio, ionisation/recombination coefficients, collision frequency, and relative helicity of the loops.
Methods. We used a newly developed two-fluid (ion-neutral) numerical code to perform 2.5D simulations of coalescing chromospheric current loops. Developed from the Artificial Wind scheme, the numerical code includes the effects of ion-neutral collisions, ionisation/recombination, thermal/resistive diffusivity, and collisional/resistive heating.
Results. It was found that the rates of magnetic reconnection strongly depend on the neutral-hydrogen to proton density ratio: increasing the density ratio a thousandfold decreased the rate of magnetic reconnection twentyfold. This result implies that magnetic reconnection proceeds significantly faster in the upper chromosphere, where the density of ions (protons) and neutral-hydrogen is comparable, than in the lower chromosphere, where the density of neutral-hydrogen is over a thousand times the ion density. This result also implies that jets associated with fast magnetic reconnection tends to occur in the upper chromosphere / lower corona. The inclusion of ionisation/recombination, an important physical effect in the chromosphere, increases the total reconnected magnetic flux, but does not alter the rate of magnetic reconnection. Reductions in the ion-neutral collision frequency result in small increases to the rates of magnetic reconnection. The relative helicity of the two current loops was not observed to have any significant effect on the rates of magnetic reconnection. Comparisons of two-fluid and MHD (Magnetohydrodynamic) simulations show significant differences in the measured rates of magnetic reconnection, particularly for the higher neutral density cases which represent the lower chromosphere. This demonstrates that MHD is not an appropriate model for simulating magnetic reconnection in the solar chromosphere.
Conclusions. The magnetic reconnection rates of coalescing current loops are strongly affected by the inclusion of neutral-hydrogen particles. It is therefore essential that ion-neutral collisions are included in future analytical/numerical models of chromospheric magnetic reconnection.
Key words: plasmas - methods: numerical - Sun: magnetic fields - Sun: chromosphere - Sun: photosphere
Magnetic reconnection is an important physical process in almost all cosmological and laboratory plasmas because it serves as a mechanism for converting stored magnetic field energy into heat and non-thermal plasma energy. Magnetic reconnection in fully ionised plasmas has been extensively investigated using the resistive-MHD (Biskamp 2005; Priest & Forbes 2000) and the Hall-MHD approximations, as well as in collisionless plasmas. The study of collisionless magnetic reconnection is summarised well by both the GEM (Birn et al. 2001) and Newton (Birn et al. 2005) reconnection challenges. In each challenge, a variety of different numerical codes were used to simulate the coalescence of magnetic islands (a Harris-type equilibrium).
Magnetic reconnection in weakly ionised plasmas is important in the solar photosphere/chromosphere (Bulanov & Sakai 1998; Furusawa & Sakai 2000; Litvinenko 1999; Sakai et al. 2006; Sakai 1996), as well as in the interstellar medium (Heitsch & Zweibel 2003; Dorman & Kulsrud 1995; Zweibel & Brandenburg 1997). Solar observations of spectroscopic line shifts and non-thermal broadening confirm that the photosphere, chromosphere, and lower corona of the Sun are all in a highly dynamical state. These indicate that mass supply and wave propagation are both important mechanisms for transferring energy from the photosphere/chromosphere to the corona and ultimately the solar wind. Studies conducted by SUMER (Solar Ultraviolet Measurements of Emitted Radiation: Wilhelm et al. 1995), part of the SOHO mission, clarified that observed explosive events are bi-directional jets generated by magnetic reconnection (Roussev & Galsgaard 2002; Innes & Tóth 1999; Innes et al. 1997). Observations have also shown evidence of magnetic reconnection in the chromosphere and photosphere (Bellot Rubio & Beck 2005; McIntosh 2007), where the neutral-hydrogen to proton density ratio changes from one to 104. Recent observations by Shibata et al. (2007) using the SOT (Solar Optical Telescope) instrument onboard the Hinode satellite show ubiquitous anemone jets in the chromospheres of active regions; this is strong indirect evidence for the existence of chromospheric magnetic reconnection.
Previously in an attempt to better understand the observed transient phenomena in the solar chromosphere, Sakai et al. (2006) developed a simulation code to describe the dynamics of two-fluid (ion-neutral) plasmas. The two fluids are coupled through proton/neutral-hydrogen collisions, as well as through ionisation/recombination. Sakai et al. (2006) were successfully able to simulate the coalescence of two counter-helical current loops (magnetic flux tubes) in the upper chromosphere. They found that the dynamics of two-fluid plasmas are quite different from those described by the single-fluid MHD approximation. During the simulated coalescence of the two current loops they also observed a number of dynamical effects, including proton heating, the formation of bi-directional proton jets and slow bi-directional plasma flows.
In this study we will attempt to extend the Sakai et al. (2006) investigation into the magnetic reconnection of coalescing current loops. To achieve this we have developed a new two-fluid numerical code, which we use to investigate how the magnetic reconnection rates of the coalescing current loops is altered by changing the: (a) neutral-hydrogen to proton density ratio; (b) ionisation/recombination coefficients; (c) ion-neutral collision frequency; and (d) relative helicities of the two current loops. The results will be applicable to both chromospheric and photospheric magnetic reconnection studies.
In Sect. 2 we present the two-fluid equations used to describe the dynamics of ion and neutral particles. In Sect. 3 we describe the numerical scheme used in our newly developed two-fluid code. In Sect. 4 we describe the simulation model and initial conditions used in this study. In Sect. 5 we present our simulation results, and finally in Sect. 6 we discuss the conclusions that can be drawn from this study.
In this section we present the basic equations used to describe two-fluid (ion-neutral) plasmas. In what follows the plasma density, pressure, velocity, and magnetic field are given respectively by ,
where the subscripts p and n refer to the ion (proton) and neutral fluids. We begin with the equations for the neutral fluid
We use a newly developed two-fluid numerical code to simulate the three-dimensional dynamics of the ion and neutral fluids present in the solar photosphere and chromosphere. In this numerical code, which we refer to as TwoYama, the fluids are coupled predominantly through ion-neutral collisions but also through ionisation/recombination effects. TwoYama was developed using the previously proposed Artificial Wind (AW) numerical scheme (Sokolov et al. 2002,1999), which was successfully used by Sakai et al. (2006) to simulate the magnetic reconnection of coalescing chromospheric current loops. The AW scheme is based on the fundamental physical invariance, Galilean (or more generally Lorentz), of the governing plasma equations. It works by choosing the frame of reference such that the flow under consideration is always supersonic, thus trivializing the upwinding process and enabling highly simplified forms of shock-capturing numerical schemes to be used. In practice this is achieved by adding an artificial velocity (hence Artificial Wind) to the flow under consideration. The result is a highly accurate shock-capturing numerical code that can simulate chromospheric problems substantially faster than other well known shock-capturing codes.
The TwoYama code was designed specifically to make use of MPI (Message Passing Interface) parallelisation so that large 3D simulations could be quickly simulated. The ionisation/recombination source terms seen in the previous section are solved using a time-splitting method at each half-time step, whilst the Joule heating, heat conduction, and magnetic diffusion terms are solved explicitly inside the AW scheme. To ensure unconditional stability of the stiff ion-neutral drag terms we use a time-implicit differencing method, adapted from Stone (1997) and Toth (1995) to include ionisation/recombination. The update of the ion/neutral momentum after each time-step, ,
is given by
In this study, we assume a plasma temperature of K and a plasma number density of m-3. Using these parameters, the background sound speed km s-1. For simplicity we choose a normalization time of s, such that the grid spacing km. Therefore the system resolution of Nx = Ny = 1024 corresponds to a system size of Mm. The initial background magnetic field, pressure, and density are given respectively by T, Pa, and kg m-3. Therefore, the corresponding background Alfvén and fast-magnetosonic speeds are respectively km s-1 and km s-1.
We simulate the 2.5D coalescence of two current loops in the upper chromosphere. The two current loops (i = 1, 2), each of radius
Mm, are located parallel to the z-axis and are each assumed to be initially in independent equilibrium states (
). The initial magnetic field components of each loop (see Fig. 1) are given by
The heat transfer constant, seen in the heat flux terms of Sect. 2, is held fixed in all simulations at kg m-1 s-1. The thermal conductivity coefficient can be obtained from the heat transfer constant using W m-1 K-1. The ion-neutral collision frequency is given by , where the collision cross-section, m2, and the ion thermal velocity, km s-1. Therefore Hz, giving a normalised ion-neutral collision coefficient , where . If we assume that radiative recombination is dominant, then using the formula by Kaplan & Pikelner (1970), m3 kg-1 s-1, gives a normalised recombination coefficient of . Initially we assume that recombination balances with ionisation, , and that .
Reconnection of magnetic fields occurs due to a non-zero magnetic diffusivity (or a finite conductivity). If we take the photospheric electron-hydrogen collision frequency as
-1010 Hz (Vranjes et al. 2008), then we can estimate the magnetic diffusivity due to collisions between electrons and hydrogen atoms as
To gauge the rate of magnetic reconnection during the coalescence of the two current loops we measure the total reconnected magnetic flux, ,
at the point
using the following expression
In this section we present the results of our numerical simulations. Unless stated, all of the results are given in normalised units according the normalization specified in Table 1.
Table 1: Normalization constants.
|Figure 1: The initial magnetic field: a contour plot of Bz overlayed by a vector (Bx-By) plot.|
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We begin with Fig. 1, where we show the initial magnetic field configuration for two co-helical current loops. The initial ion pressure in-balance between the two loops (Fig. 2) causes them to spontaneously collapse towards each other. During the initial coalescence phase, , strong inflows (Fig. 3) develop along the x-axis, with subsequent outflows along the y-axis. This inflow of plasma compresses oppositely directed magnetic field lines, seen in the central region of Fig. 4, to form a strong reverse current sheet (see Fig. 5) parallel to the y-axis. The current sheet is then dissipated by the plasma's finite conductivity, leading to reconnection of the (Bx-By) magnetic field lines. The significant heating (Joule and collisional) generated during the reconnection process is clearly visible in Fig. 6, where we see a 30% rise in ion temperature along the current sheet. Conversely, in Fig. 7 we see a 5-10% reduction in neutral temperature along the current sheet due to collisional cooling. This implies that 20-25% of the increase in ion temperature is due to Joule heating, while a further 5-10% increase is due to collisional heating with neutral particles. In Fig. 8 we see that during the initial coalescence phase, reconnection of magnetic fields lines reduces the magnetic energy, or magnetic pressure, relative to the ion thermal pressure. This is turn accelerates the ion and neutral fluids (due to ion-neutral collisions) into the central region. This effect is clearly seen in Fig. 8 by the rapid increase in ion and neutral kinetic energy. In the later coalescence stage, t>1000, collisional heating is seen to slowly convert the ion and neutral kinetic energy into internal (thermal) plasma energy. Figure 8 demonstrates that the main effect of the magnetic reconnection process is the conversion of magnetic energy into kinetic and thermal energy.
|Figure 2: Time development of the ion pressure for two co-helical current loops, where .|
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|Figure 3: Time development of the ion velocity (Vx-Vy) for two co-helical current loops, where .|
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|Figure 4: Time development of the magnetic field (Bx-By) for two co-helical current loops, where .|
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Firstly, we investigate how the rate of magnetic reconnection is altered by increasing the neutral-hydrogen to proton density ratio, . We present numerical results for the coalescence of two co-helical current loops using density ratios of . The normalised collision frequency is held fixed at , while ionisation and recombination effects are ignored ( ).
|Figure 5: Time development of the current density, Jz, for two co-helical current loops, where .|
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|Figure 6: Time development of the ion temperature for two co-helical current loops, where .|
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It is well known that the neutral-hydrogen to proton density ratio increases with depth in the chromosphere/photosphere. Changing this density ratio therefore effectively corresponds to a change in depth at which the simulated current loop coalescence and subsequent magnetic reconnection takes place. The density ratio is representative of the upper chromosphere, while is representative of the lower chromosphere. In Fig. 9 we use a normalised form of Eq. (19) to plot the total reconnected magnetic flux as a function of time for various neutral-hydrogen to proton density ratios. The slope of each line is a direct measure of the magnetic reconnection rate (as measured at ). From this figure it is immediately clear that increasing the neutral-hydrogen to proton density ratio strongly decreases the magnetic reconnection rate. Comparing the lines representing and , we see that a tenfold increase in density ratio reduces the magnetic reconnection rate by a factor of two. Whilst comparing the lines representing and , we see that a thousandfold increase in density ratio reduces the magnetic reconnection rate by a factor of twenty. The simulation results seen in Fig. 9 therefore suggest that, in the case of coalescing current loops, magnetic reconnection proceeds faster in the upper chromosphere than in the lower chromosphere.
|Figure 7: Time development of the neutral temperature for two co-helical current loops, where .|
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|Figure 8: Time development of plasma energy for two co-helical current loops ( ). Kinetic and magnetic energy plots: (solid) x-component, (dotted) y-component, and (dashed) z-component. Internal energy plot: (solid) ions and (dashed) neutral. Each energy component is normalised to the total plasma energy.|
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|Figure 9: Effect of neutral-hydrogen to proton density ratio on the reconnected magnetic flux for two co-helical current loops. (solid) , (dotted) , (dashed) , and (dot-dashed) .|
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Figure 9 shows a direct correlation between magnetic reconnection rate and density ratio; however, the correlation between the peak reconnected magnetic flux, , and the density ratio is less clear. The peak value for the lines and are approximately equivalent at , whereas the lines representing the higher density ratios of -1000 appear to indicate a reduction in the peak reconnected magnetic flux with increasing density ratio.
Finally, comparisons of magnetic and velocity vector plots for various density ratios, in addition to Fig. 9, appear to show that the density of neutral particles does not alter the fundamental dynamics of coalescence process itself, but simply the rate at which it occurs.
The recombination of protons and electrons to form neutral hydrogen is an important physical process occurring in the partially ionised upper chromosphere. We therefore investigate how the magnetic reconnection rate is altered by including the effects of ionisation and recombination. We show results for two co-helical current loops using a density ratio of . The normalised collision frequency is fixed at , while the normalised ionisation and recombination coefficients are set to , 0.15, 0.015, 0.0.
For clarity in Fig. 10 we do not show the two cases of , 1.5, since these gave visually indistinguishable results to the case. From the figure we see that the inclusion of ionisation/recombination effects has no effect on the rate of magnetic reconnection. We do however see an increase in the total reconnected magnetic flux by 5%. This phenomena was previously explained by Sakai (1996) as resulting from a decrease in ion pressure at the current sheet formed during the coalescence process (see Fig. 5). This decrease in ion pressure results from protons and electrons in the current sheet recombining to form neutral hydrogen. Since it is the magnetic field which drives the reconnection process, any reduction of the ion pressure, which alone balances the magnetic pressure, will result in enhanced magnetic reconnection.
|Figure 10: Effect of ionisation/recombination on the reconnected magnetic flux for two co-helical current loops ( ). (solid) , and (dotted) .|
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Next we investigate how the magnetic reconnection rate is altered by changing the ion-neutral collision frequency. We show simulation results for two co-helical current loops using normalised collision frequencies of , 3.0, 0.03, 0.0. The density ratio is fixed at , while ionisation and recombination effects are ignored ( ).
Firstly, in Fig. 11 we note that the lines representing and produce nearly identical results (only is visible). This is because both cases represent strongly coupled ion-neutral plasmas, where the ion-neutral collisions cause the ion and neutral particles to behave as a single heavy fluid with a combined ion-neutral density. Whereas for the case the ion and neutral particle dynamics are completely decoupled. The ions therefore move as a single light fluid (equivalent to a MHD simulation). The collapse and eventual coalescence of the two current loops is driven by a continuous reduction in magnetic pressure (due to magnetic reconnection) which is balanced only by the ion thermal pressure. The neutral particles by definition are not influenced by the magnetic field and therefore play no part in balancing the magnetic pressure. However, the effective inertia of the initially stationary fluids does depend on both the neutral-hydrogen to proton density ratio and the ion-neutral collision frequency. Given that the initial conditions for the ion particles and magnetic field are the same in each simulation, the initial acceleration of the fluids can only therefore depend on their effective inertia. In strongly coupled ion-neutral plasmas, where the effective inertia is relatively high, we would expect the coalescence and subsequent magnetic reconnection to proceed, at least initially, relatively slowly. Whereas in weakly coupled ion-neutral plasmas, where the effective inertia is relatively low, we would expect the reverse to be true. This appears to be confirmed by Fig. 11 where we see a slight increase in the rate of magnetic reconnection with decreasing ion-neutral collision frequency.
|Figure 11: Effect of ion-neutral collision frequency on the reconnected magnetic flux for two co-helical current loops ( ). (solid) , (dotted) , (dashed) , and (dot-dashed) (MHD).|
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In Fig. 11, the rate of magnetic reconnection for the MHD case ( ) does not differ significantly from the two-fluid cases ( ). We note however, that this is only true for the low neutral density case where . If we compare the MHD case of Fig. 11 to the case of Fig. 9, we see a twentyfold difference in the magnetic reconnection rates. The MHD approximation is therefore not an appropriate model to describe magnetic reconnection in the lower chromosphere or photosphere.
Finally in Fig. 11, we note that the peak reconnected magnetic flux appears to decrease with decreasing ion-neutral collision frequency. We speculate that the increased effective inertia of ion-neutral fluids may extend the time for loop coalescence, thus leading to an increased reconnected magnetic flux. This effect is of course balanced by the reduced initial acceleration, caused by increased neutral density, discussed above. The results of Fig. 9 would therefore suggest that neutral-hydrogen to proton density ratios of -10 would lead to optimum amounts of reconnected magnetic flux.
In this final subsection we investigate how the magnetic reconnection rate is altered by changing the relative helicities of the two current loops. We show simulation results for two counter-helical (opposite Bz) current loops, using density ratios of . The normalised collision frequency is held fixed at , while ionisation and recombination effects are ignored ( ).
|Figure 12: Effect of neutral-hydrogen to proton density ratio on the reconnected magnetic flux for two counter-helical current loops. (solid) , (dotted) , (dashed) , and (dot-dashed) .|
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In Fig. 12 we see that, as previously seen in the co-helical case, the rate of magnetic reconnection strongly depends on the density ratio. Comparisons of Fig. 12 to the co-helical case seen in Fig. 9, show only minor variations in the both the rates of magnetic reconnection and the total reconnected magnetic flux. We expect that this result holds true only for the 2.5D case studied here, since previous 3D studies have shown that the relative helicities of the loops does indeed affect the magnetic reconnection process. A subsequent 3D study will investigate the relative helicity further.
In this study we investigated the magnetic reconnection of two coalescing chromospheric current loops. We conducted 2.5D simulations of the coalescence using a newly developed two-fluid (ion-neutral) code, which includes the effects of ion-neutral collisions, ionisation/recombination, thermal/resistive diffusivity, and collisional/resistive heating.
In the results of the previous section we found that the fundamental physical dynamics of the coalescence process was not altered by changing: (a) the neutral-hydrogen to proton density ratio, (b) the ionisation/recombination coefficients, (c) the ion-neutral collision frequency, or (d) the relative helicities of the two loops. We did find however that the rate of magnetic reconnection was susceptible to each parameter to a varying degree:
The main result of this study shows that the rates of magnetic reconnection for coalescing current loops are strongly affected by the inclusion of ion-neutral collisions. We therefore conclude that it is essential that the effects of neutral particles are included in future analytical/numerical models of chromospheric magnetic reconnection.
This research was supported by the Japan Society for the Promotion of Science (JSPS).