Issue 
A&A
Volume 563, March 2014



Article Number  A69  
Number of page(s)  17  
Section  Interstellar and circumstellar matter  
DOI  https://doi.org/10.1051/00046361/201321151  
Published online  14 March 2014 
Online material
Appendix A: Set of MHD equations
A general set of the Eulerian continuity, momentum, and energy equations is the following (see e.g. Boyd & Sanderson 2003): (A.1)

v_{j}= fluid velocity

ρ_{j}= fluid density

E_{j}= internal energy of fluid

P_{j}= pressure of fluid

Î= unit tensor

= viscosity/stress tensor

F= external force per unit mass and volume

Q= heat flow

= sources and sinks

A_{j}= ambipolar diffusion between ions and neutrals
where the index j ∈ { H,H^{+},He,He^{+},He^{+ +},i,n }. As discussed above for the index j of the ionized fluid, the density is the sum of all densities of ionized species, the total pressure P_{j} = ∑ kP_{k}, the total energy E_{j} = ∑ kE_{k}, with k ∈ {H^{+}, He^{+}, He^{+ +} }.
The force densities, stress tensor and the heat transport on the righthand side of Eq. (A.1) are usually neglected in modeling the largescale structure of the heliosphere, that is, . While external forces, such as solar gravitation, can be neglected, the stress tensor will play an important role in studying the details of the termination shock or heliopause structure, but to our knowledge this was not discussed so far. Especially the heat transport by electrons can be expected to be significant, because of the high thermal speed of these particles, and will be analyzed in future work. If the righthand side of Eq. (A.1) vanishes, the set of equations is called ideal MHD.
From Eq. (27) it is evident that the interstellar helium contributes about 40% to the total mass density, thus the total mass density ρ_{n} in the above neutral continuity equation is ρ_{n} = ρ_{H} + ρ_{He} ≈ 1.4ρ_{H}. This results in an increased ram pressure and momentum flow ρ_{n}v_{n}. Together with the total pressure P_{n} = P_{H} + P_{He} = κ(n_{H}T_{H} + n_{He}T_{He}) and the previously made assumption T_{H} = T_{He} and n_{He} = 0.1n_{H} yields P_{n} = 1.1P_{H}. These estimates show, that helium contributions are not negligible. A similar consideration holds for the governing equations of the charged particles.
If the helium inflow velocity differs in direction from that of hydrogen (Lallement et al. 2005), helium has to be treated as a separate fluid and an additional complete set of the Eulerequations must be solved. If one can assume that the flow velocities of the neutrals and charged fluids are the same for all neutral and ionized species, it is sufficient to solve the two governing equations and treat the other species as tracer particles to calculate their densities and thermal pressures.
Handling the neutrals with a kinetic set of equations (Izmodenov 2007; Heerikhuisen et al. 2008) requires a similar approach for the collision integrals (see Eqs. (39) and (40)) to obtain the balance terms for the (M)HD equations of charged particles, when including heavier ions.
Appendix B: “Collision” speeds
For the interaction of particles with different masses (nonresonant charge exchange processes), the approach by McNutt et al. (1998) can be applied. Nevertheless, the relative velocities for the momentum exchange differ from those for the energy exchange, in contrast to what was discussed in McNutt et al. (1998)
As described in Eqs. (57) to (60) in McNutt et al. (1998), the relative speeds for the crosssections for charge exchange differ for all three Euler equations, as well as the speeds needed for the charge exchange crosssection. The speeds are denoted as above , where j ∈ {c, m, e, P} for the continuity, momentum, and energy equations and j = P for the thermal pressure, respectively. The governing energy equation contains the ram pressure and the thermal pressure, which are both influenced. The balance equations only contain the thermal pressure, because changes in the ram pressure or bulk speed are calculated in the governing equations with the assumption that all species flow with the same speed. The indices i ∈ {cx, rel} are the speeds needed for the charge exchange crosssection and corresponding relative speeds. With the definitions from McNutt et al. (1998) we have to solve the following type of integrals: (B.1)The following recursion holds: (B.2)Thus we need only to know the four integrals (Gradstein & Ryshik 1981), Nr. 3.562.33562.6: These integrals need to be multiplied by the factors given in McNutt et al. (1998).
With these integrals it is easy to calculate the required speeds (for details see McNutt et al. 1998):
The approximations in Eqs. (B.3) to (B.8) fit nicely, except for small errors (see Fig. B.1). Note that the fit in Eq. (B.6) differs by a factor 0.5 from that of McNutt et al. (1998).
Fig. B.1
Relative errors of the fitted characteristic collision speeds, where are the approximations given in Eqs. (B.3)−(B.8). 

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With the help of the integrals it is easy to calculate the higherorder correction terms. However, this is not necessary for the p + H reaction, because the secondorder derivatives of the crosssections, as shown in Fig. B.1, are orders of magnitudes lower than the crosssection. Shown in Fig. B.2 are the functional dependencies given by Fite et al. (1962) and by Lindsay & Stebbings (2005), that is
(B.9)where v_{rel} is given in cm/s and the σ in cm^{2}.
With the help of the computer algebra system wxMaxima^{3} it is easy to calculate the second derivatives of these commonly used crosssections for the p + H reaction and the integrals for the secondorder terms of the Taylorexpansion for σ^{cx}. For the terms needed in the continuity equation, we have to compare with the secondorder terms , where we neglected common factors for simplicity. In our notation . With some algebra, we find that and thus finally (B.10)The function h(v) defined above is small for all v, so that we can assume that the higherorder terms in the Taylor expansion of σ^{cx} vanish. In Fig. B.2 the function is shown for the two crosssections.
Fig. B.2
Ratio h(v) (Eq. (B.10)) of the secondorder integrated Taylorexpansion to the zeroth order for the two Hp charge exchange crosssections discussed by Fite et al. (1962) and Lindsay & Stebbings (2005). The bump between the two downward spikes in the LindsayStebbings curve is negative, but to represent it in a logarithmic scale, its absolute value was taken. See text for restrictions of the fit functions. 

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It can be seen in Fig. B.2 that for the Fite et al. (1962) crosssection the secondorder terms are nearly a factor 10 lower than the zerothorder term for all speeds. For the Lindsay & Stebbings (2005) crosssections this holds only for speeds lower than 4 × 10^{7} cm/s = 400 km s^{1}. Around these speeds, that is, a commonly used solar wind speed, the secondorder corrections are on the same order than the zerothorder term.
Gains and losses from the original populations.
In the latter case, that is, if the higherorder terms cannot be neglected, in the analytic representation this will lead to clumsy formulas, which also need some computational time. Thus, it might be better to solve the collision integrals numerically.
Note, that for the hydrogenproton reactions the fit function discussed in Fite et al. (1962) has an upper boundary of 10 keV, which corresponds to a relative speed of ≈1400 km s^{1}. The range in which the data were fitted by Lindsay & Stebbings (2005) has an upper boundary of 300 keV, which corresponds to a speed lower than ≈7500 km s^{1}. The data presented in Fig. 2 were taken from the Redbooks^{4} and reach to 63 keV, corresponding to ≈3400 km s^{1}. Some of the helium reactions have their maximum crosssection at higher energies, as can be seen in Table C.1, and their upper limits in energy/amu are higher than shown in Fig. 2.
All the fits given for the data from the Redbooks or the Aladdin database are mainly based upon a fit with Chebyshev polynomials. These polynomial fits are only good in the range given by the corresponding upper and lower (energy) boundaries and cannot be extended beyond these. Because usually it cannot be guaranteed in a largescale model that the relative speeds are always in that range, a better fit function is needed, which can be extended beyond the boundaries, keeping in mind not to violate quantum mechanical requirements.
We here only discussed the simplest case, that is, the collision terms for the continuity equation. Of course this analysis must be performed not only for the remaining set of MHD equations, but has, especially, to be verified for all interactions.
Appendix C: Interaction terms
Gains from the new populations.
In the following we provide an overview of possible ionization reactions. In Table C.1, the first column gives the interaction term in the continuity equation, indicating the particle species: X^{n} with X∈ {H,He}, while n ∈ { 0,1,2 } gives the ionization state (usually the index 0 is omitted). Newly created ions are named as PUI_{Xn} and energetic atoms by ENA_{X}. The reaction rates have the indices {cx, ei, pi} for charge exchange, electron impact, and photoionization, respectively. The rates are also denoted by ν(i,j), where i describes different reactants, while j stands for different products of the same reaction i. The tuple (i,j) is given in the fourth column, where a minus sign stands for losses and a plus sign for gains. To derive the total gains and losses one has to sum over all { i,j }. In the fifth and sixth column the maximal crosssection and its corresponding relative speed is given, respectively. In the third column the first reactant is a particle from the solar wind, while the second reactant is from the interstellar medium. This distinction is necessary to ensure correct sorting.
Note that in the charge exchange rate ν^{cx} = ρ_{X}σ^{cx}v_{rel} the density of the first reactant is included and is indicated in the table by ν_{cx,X}.
Table C.1 contains the losses, Table C.2 the gains. In Table C.1 the approximate highest values for the crosssection are listed. They may vary by a factor of three and only indicate the correct order of magnitude. If a range is given for the corresponding relative velocity, the crosssection is a flat curve in that range.
All reactions that have a charged particle as the second reactant cannot flow in from the interstellar medium. Because the heliopause is a contact discontinuity that separates the solar wind and interstellar medium plasma, there is no flow of charged particles across the heliopause. Thus in Tables C.1 and C.2 the reactions labeled (3,1), (4,1), (5,1), (6,1), (8,1), (10,1), and (12,1) can be neglected.
The reactions labeled with an asterisk are sorted in pickup channels, even though they do not create new PUIs. For example, the reaction He^{++}+H→He^{+}+H^{+} produces a new pickup hydrogen, but the change from doubly to singly charged helium does not change its character, that is He^{+} has the same bulk speed as He^{2+}. Only the charge is changed, thus the new He^{+} does not
affect the dynamics (the H^{+} does). Nevertheless, these processes can have an effect on magnetic field turbulence (e.g. Shalchi et al. 2012). This aspect is interesting in the description of the diffusion tensor to model cosmic rays (Effenberger et al. 2012). The role of these types of processes for the turbulence will also be considered in future work.
From these tables the interaction terms for the governing equations can be determined. For the neutral equation it is just the sum of all interaction terms. More care must be taken for the ion governing equation, because the pickup terms can cancel some of the ion terms, for example, the reaction H^{+} + H → H + H^{+} looses an original fast solar wind proton, but gains a slow interstellar hydrogen atom, which does not change the total ion mass.
To describe the interaction terms for the momentum and energy equation, similar tables can now easily be constructed and the governing equations determined.
© ESO, 2014
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