Issue 
A&A
Volume 531, July 2011



Article Number  A55  
Number of page(s)  8  
Section  Astrophysical processes  
DOI  https://doi.org/10.1051/00046361/201016135  
Published online  10 June 2011 
Electron acceleration in a wavy shock front
Astronomical Institute of the Academy of Sciences of the Czech Republic, 25165 Ondřejov, Czech Republic
email: vandas@ig.cas.cz
Received: 12 November 2010
Accepted: 22 April 2011
Context. It is known that electrons are accelerated at nearly perpendicular shocks by the drift mechanism. And it is also known that energy gain of electrons caused by this mechanism is not very high. Therefore it was suggested in the past that the energy gain might be increased if shocks had wavy fronts. For instance, there were attempts to explain coronal type II burst and their fine structure by electron acceleration in a wavy shock front.
Aims. We studied electron acceleration numerically at nearly perpendicular wavy shocks for coronal conditions and compared it with analytical results on electron acceleration at nearly perpendicular plane shocks.
Methods. An analytical model of a wavy shock front was used and trajectories of electrons in it and around it were calculated numerically in a guiding centre approximation.
Results. We found that energy gains of electrons at a wavy shock front and a corresponding smoothedintoplane shock on the average were comparable. That is why they do not depend significantly on the shock thickness, magnetic field profile inside the shock, and shock wavy form. They do depend on the angle between the smoothed shock front and ambient magnetic field.
Conclusions. On average, a wavy shock front does not significantly increase an acceleration efficiency. Energy gain remarkably exceeds an average level for some combinations of initial parameters. Distribution functions of accelerated electrons have a patchy structure, which is prone to inducing plasma instabilities that will generate plasma waves. This may have relevance to the problem of type II burst origin.
Key words: acceleration of particles / shock waves / magnetic fields / Sun: radio radiation
© ESO, 2011
1. Introduction
Holman & Pesses (1983) suggested that electrons were promptly accelerated by quasiperpendicular shocks in the solar corona. Theory of electron acceleration by nearly perpendicular plane shocks was formulated by Wu (1984) and Leroy & Mangeney (1984) and labelled as a fast Fermi process. Vandas (1989) and KraussVarban & Wu (1989) identified this process as a shock drift mechanism inside the shock layer. Energy gain of electrons during the process is not high, only several times the initial energy, therefore it was suggested that a wavy shock front could enable electrons to interact more times with the shock and so gain more energy (e.g., Zlobec et al. ). In this paper we examine this possibility quantitatively.
Influence of ripples in a shock wave front on particle acceleration has also been investigated by Decker (1990) and Gedalin (2001), but their studies are not directly applicable to our problem. The former studied a largescale rippling and proton acceleration, and the latter a small scale rippling and suprathermal proton and electron motion. Knocks et al. (2003) investigated the influence of rippling on interplanetary typeII burst generation by accelerated beams of electrons.
Vandas & Karlický (2000) investigated electron acceleration by a perpendicular wavy shock. This paper is hereafter referred to as Paper I. The perpendicular geometry treated in Paper I yielded that eventually all interacting electrons had been transmitted downstream. Here we treat cases with nearly perpendicular wavy shocks where some reflected electrons may escape upstream. And it is known that reflected electrons have on average a higher energy gain than do transmitted ones.
2. Model
A model of a wavy shock is shown in Fig. 1, and it is the same as in Paper I. The shock front is formed by a sinusoidal wave with the wavelength L and amplitude A (right part of the figure, plotted size of A is exaggerated). Upstream magnetic field lines were parallel to the Z axis (parallel to a smoothed shock front, a perpendicular shock) in Paper I. In the present analysis a small inclination of the field lines is allowed (a nearly perpendicular shock). Using a procedure described in Vandas (1995) and following Paper I, the wavy shock front is converted into a plane shock wave with the thickness d and B_{n} varying (left part of Fig. 1). B_{n} is the normal component of the upstream magnetic field with respect to the shock front, and its variation is specified later, in Eqs. (13) and (15). Electron motion in the guiding centre approximation inside and outside the shock layer is then calculated.
Fig. 1 Global view of the model wavy shock front on the right. Left part shows a wavy shock approximation of a magnified small piece of the wavy shock (see two dashed arrows) by a plane shock wave. X and Z scales are not the same, the X scale is zoomed in. 

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The shock front is defined by the equation (1)with (2)The orientations of the X and Z axes are shown in Fig. 1.
Electrons upstream and downstream are assumed to move in homogeneous fields, which is a simplification of a real situation. The upstream magnetic field in the XYZ system approximately is (3)where B_{1} = const. is the upstream magnetic field magnitude and θ_{B} = const. is the angle between the upstream magnetic field vector and a normal to the smoothed shock front. (This angle is usually denoted as θ_{Bn} for a plane shock wave, but θ_{Bn} varies for a curved shock wave.) Paper I treated the case with θ_{B} = 90°. Here, for a nearly perpendicular shock it is assumed that θ_{B} is close to 90°; therefore, we set sinθ_{B} ≈ 1. The downstream magnetic field is supposed to be (4)where ν is a shock magneticfield jump. The upstream plasma velocity is (5)and the electric field is assumed to be constant everywhere, (6) In the shock layer, electron motion is governed by equations in the guiding centre approximation (Vandas , Paper I) where m is the electron mass, e the elementary charge, μ the electron magnetic moment, E_{k} the electron kinetic energy, v_{ ∥ } the electron velocity along the magnetic field line, V_{1} and B_{1} (already introduced) are upstream plasma velocity and magnetic field, respectively. Dots denote time derivatives, and prime denotes derivatives by x. The equations are expressed in the system xyz of the transformed plane shock, which is different from the system XYZ (see Fig. 1). The system xyz is only used inside the model plane shock, and it holds x ∥ X, y ≡ Y, and z ≡ Z, while x = 0 and x = d describe the upstream and downstream edges of the shock layer, respectively.
The functions h and q define magnetic field inside the shock layer (0 ≤ x ≤ d), (12)so the function h(z) is related to the B_{n} component by (13)Because (14)where n pointing upstream is a unit vector to the shock surface (1), it follows from (13), (3), and (1) that (15)The function q(x) is related to a magnetic field profile in the shock layer and it holds q(0) = 1 and q(d) = ν. Paper I, in accordance with Vandas (1989), used the following expression for q, (16)It enabled them to solve the Eqs. (7) − (11) analytically. However, for a more complex h like (15), one can proceed analytically only half way. It has been shown by Vandas & Karlický (2005) (hereafter referred as Paper II), which contains preliminary results on electron acceleration by a nearly perpendicular wavy shock. Therefore a numerical treatment is necessary. It enabled abandoning the profile (16), which is somewhat artificial (Fig. 2), and unlike Paper II to use a more realistic profile (Vandas ) (17)with (18)The profile is shown in Fig. 2.
Fig. 2 Magnetic field profiles inside the model shock layer. The profile (17) used in calculations (solid line) is compared to the profile (16) drawn by the dotted line. The magnetic jump ν = 3 was used in the plot. 

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3. Results
The model shock parameters used in our numerical calculations were B_{1} = 0.5 mT (5 G), V_{1} = 1000 km s^{1}, ν = 1.6, and d = 50 m. The calculations showed that results were nearly the same for the same ratios A/L. Calculations are presented for the ratios of 0.1 and 0.2 with L = 1000 km. These parameters (corresponding to a coronal shock) were the same as used in Papers I and II, because it was our intention to have a direct comparison with their results. Calculations are presented for A / L = 0.1 if not said otherwise.
Fig. 3 Example of an electron trajectory around (right) and inside (left) the wavy shock. The electron is reflected (r) once and then transmitted (t) downstream. Relative vertical placement of r and ttrajectories is arbitrary (otherwise they would not fit both into the figure). A value of the angle θ_{B} is explicitly written. 

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3.1. Calculations of electron trajectories
For electron trajectory determination, the Eqs. (7) − (11) were solved numerically inside the shock layer and electron moved in homogeneous magnetic fields outside the layer. Figure 3 shows an example of an electron trajectory around and in the wavy shock with θ_{B} = 80°. The layout is similar to Fig. 1. The electron trajectory is drawn by the thick line. Horizontal (X and x) directions are zoomed in comparison with vertical (Z and z) directions, and the x direction is much more zoomed in than the X direction. The electron with initial energy E_{i} = 1 keV and pitch angle α_{i} = 105° is reflected once and then transmitted, and its final energy is E_{f} = 2.1 keV (“i” and “f” are used for initial and final values, respectively). For comparison, the same electron interacting with a corresponding smoothed shock wave (i.e., the wavy shock smoothed into a plane shock wave) with θ_{Bn} = 80° would be transmitted and its final energy would only be 1.1 keV. The pitch angle is the angle between the velocity and magnetic field vectors, and the pitch angle 0° has an upstream electron moving along the magnetic field towards the shock.
Fig. 4 Another example of an electron trajectory around (right) and inside (left) the wavy shock. Layout is similar to Fig. 3. The electron only changed its initial position and it is one time transmitted (t) downstream and one time transmitted (t) upstream. 

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If the initial position of the electron from Fig. 3 is shifted along Z by approximately L / 3, we get a trajectory shown in Fig. 4. The electron is transmitted downstream and then transmitted upstream, with a final energy of 1.7 keV. Overall, the electron can be regarded as reflected. Electron trajectory and its energy gain are quite sensitive to electron position with respect to a wavy shock front. For both cases the energy gain is higher than on the corresponding smoothed shock wave. However, this is not a rule.
Fig. 5 Example of an electron trajectory around (right) and inside (left) the wavy shock. Layout is similar to Fig. 3. The angle θ_{B} only changed. The electron is reflected (r_{1}, r_{2}) twice and then transmitted (t) downstream. 

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Figure 5 shows an electron trajectory of the same electron as in Fig. 3 but for a shock with θ_{B} = 85°. This electron interacting with a smoothed shock wave would be transmitted and its final energy be 1.9 keV. Even though the electron is reflected twice on the wavy shock front and then transmitted, its final energy is only 1.6 keV, i.e., lower. Electron acceleration is very sensitive to θ_{Bn}, so not only does number of interactions play a role, but also where on the wavy shock an electron interacts.
Calculations were made with the magnetic field profile (17). Similar calculations but with the magnetic field profile (16) were presented in Paper II. If we compare Fig. 3 here with Fig. 3 in Paper II or Fig. 5 here with Fig. 4 in Paper II, we see that trajectories are very similar and energy gains practically the same. This confirms conclusions by Vandas (1991, ) that energy gain does not significantly depend on a magnetic field profile in a curved shock (cf. for a plane shock wave, where the gain does not depend on it at all).
Fig. 6 Comparison of energy gain of electrons at the wavy shock with one at a smoothed shock. E_{f} and are final energies after interactions with the wavy shock and a smoothed shock, respectively, α_{i} is the initial pitch angle. The dashed line displays an average value. 

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Fig. 7 Comparison of energy gain of electrons at the wavy shock with one at a smoothed shock. E_{f} and are final energies after interactions with the wavy shock and a smoothed shock, respectively, Z_{i} is the initial position. The dashed line displays an average value. 

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Calculations show that electron trajectories and energy gains depend very much on θ_{B}, electron initial energy, pitch angle, and position. Sometimes electrons gain more energy than at a corresponding plane shock, sometimes less. To obtain a clearer picture, we calculated dependencies of energy gains on some initial parameters.
We started with the situation shown in Fig. 5. The shock had θ_{B} = 85°. The electron with initial energy E_{i} = 1 keV and pitch angle α_{i} = 105° was released from the place with X_{i} and Z_{i}. Its final energy was E_{f} = 1.6 keV. At a smoothed shock wave, its final energy would be = 1.9 keV. Now we change α_{i} (Fig. 6) or Z_{i} (Fig. 7) and compare energy gains on the wavy shock and a smoothed shock wave. The other parameters are kept constant. Figures 6 and 7 display this comparison, and arrows indicate the case from Fig. 5. We see frequent jumps up and down from 1, which reflects a sensitivity to initial parameters. In maxima the final energy for the wavy shock does not exceed three times the final energy at a corresponding smoothed shock. The average values are close to 1. It means that energy gains at a wavy shock and a smoothed shock are comparable on average. But for some “preferred” or “resonant” initial parameters, the energy gain at a wavy shock may be significantly larger.
Fig. 8 Examples of electron trajectories around the wavy shock. a) The electron is reflected (r) and then transmitted many times (t_{1}–t_{8}) upstream/downstream and vice versa. b) A similar trajectory but for a higher energy gain. The electron is reflected twice (r_{1} and r_{2}) and then transmitted many times (t_{1}, t_{2}, etc.). 

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The abovementioned sensitivity can be explained by complex interactions with the wavy shock. Figure 8 shows extreme examples, electrons, which are reflected and then transmitted downstream and upstream several times. They end upstream, so from a global point of view, they are regarded as reflected. Figure 8a plots a trajectory of an electron with the initial energy 1 keV and pitch angle 65°. The final energy was 2.3 keV. The same electron interacting with a smoothed shock wave would be transmitted and its final energy would be 1.3 keV. It is interesting to note that, despite this complex interaction, calculations with the different magnetic field profile (16) yield nearly the same trajectory and energy gain (cf. Fig. 5 in Paper II). Figure 8b displays the case of the first maximum in Fig. 7.
Sensitivity of the solution to initial parameters raises a question of computational accuracy. We examined this matter carefully. Paper I presents an analytical solution of electron trajectories for the shock magnetic field profile specified by (16) and θ_{B} = 90°. Comparison of this solution with numerical calculations used in the present paper yielded practically identical results. Numerical calculations of electron trajectories for cases where an analytical solution is absent (as in this paper) were checked through changes in integration time steps by several orders of magnitude, again with practically identical results.
3.2. Calculations with an electron distribution function
Using the above discussed trajectory calculations (but in backward direction with respect to time) and the Liouville theorem, a distribution function of accelerated electrons can be constructed from an initial distribution function. The same initial distribution function is used as in Papers I and II. It describes halo electrons (suprathermal tail) by a kappa function (19)where n_{H} is the halo density, v_{H} the characteristic halo electron velocity, (20)Γ is the gamma function, and κ determines the deviation of the halo distribution from a Maxwellian one. It is set = 0.6 keV and κ = 6 (as in Papers I and II, see discussion in Paper I), and value of n_{H} is not necessary for the present calculations.
Fig. 9 a) Angular distribution function of accelerated downstream electrons for a perpendicular wavy shock in an arbitrarily chosen downstream point (thin solid line). The direction of the magnetic field B_{2} is shown. The shock is located opposite to this direction. The distribution function is rotationally symmetric around B_{2}. It is a polar graph, where the polar angle corresponds to the pitch angle α and the radial distance (in a logarithmic scale) to a value of the distribution function f(v,α) of accelerated downstream electrons. The velocity v is constant here and its value corresponds to the energy of 3 keV. The dashed circle labelled 1 × represents the value of the initial distribution function f_{i}(v) from (19). For comparison, the thick solid line shows the angular distribution function of transmitted electrons through a perpendicular plane shock wave. b) The same as in a), but the thin solid line shows the angular distribution averaged along the shock front. 

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Fig. 10 a) Angular distribution function of accelerated downstream electrons with energy of 3 keV for a wavy shock with θ_{B} = 85° in an arbitrarily chosen downstream point (thin solid line). The layout is similar to Fig. 9. The thick line shows the distribution of transmitted electrons through a smoothed shock wave with θ_{Bn} = θ_{B}. b) The same as in a), but the thin solid line shows the angular distribution averaged along the shock front. 

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Fig. 11 a) Angular distribution function of accelerated upstream electrons with energy of 3 keV for a wavy shock with θ_{B} = 85° in an arbitrarily chosen upstream point (thin solid line). The figure complements the previous Fig. 10. The thick line shows the distribution of reflected electrons at a smoothed shock wave with θ_{Bn} = θ_{B}. The shock front is located in the direction of B_{1}. b) The same as in a), but the thin solid line shows the angular distribution averaged along the shock front. 

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The next figures display angular distribution functions of accelerated electrons with respect to the magnetic field direction. All angular distribution functions presented here are for A / L = 0.1. Papers I and II show some comparison with other A / L, but results are not very different. Figure 9a shows an angular distribution function of downstream electrons with the final energy of 3 keV at a wavy shock with θ_{B} = 90° (i.e., with θ_{B} treated in Paper I). In this geometry all electrons finally end downstream. The distribution is for an arbitrarily chosen place with X_{f} and Z_{f}. A spiky character reflects already discussed sensitivity to initial values. A different downstream place would yield a similar picture but with “spikes” at different α’s and with different sizes. It is obvious than in a real situation angular distributions will not be so spiky owing to diffusion processes (like pitch angle scattering) in the shock layer and around it, but it is not probable that they would be wiped out completely. Figure 9b shows the same distribution function as in Fig. 9a, but averaged over Z_{f} between 0 and L. We see that the averaged distribution function is similar to the distribution function at a corresponding plane shock.
Fig. 12 Differential density of accelerated upstream electrons for a wavy shock with θ_{B} = 88°. The dotted line shows seed population (initial distribution function (19)), the thick line is for a corresponding smoothed shock, the thin solid and dashed lines are for a wavy shock with A / L = 0.1 and 0.2, respectively. The differential density was averaged along the shock front. 

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Fig. 13 Differential density of accelerated downstream electrons for a wavy shock with θ_{B} = 88°. The layout is similar to Fig. 15. The differential density was averaged along the shock front. 

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Figures 10 and 11 display angular distributions for a nearly perpendicular wavy shock with θ_{B} = 85° in the downstream (globally transmitted) and upstream (globally reflected) regions, respectively. The situation is analogous to the perpendicular shock discussed above. Distribution functions of reflected and transmitted electrons are spiky, and the averaged angular distribution functions are similar to the distribution functions at a corresponding plane shock.
The final comparison between acceleration efficiency at a wavy shock and a corresponding smoothed shock wave is shown in Figs. 12 and 13, plotting differential density n_{d} of accelerated electrons calculated in the upstream and downstream regions, respectively. It was averaged along the shock front. The differential density is defined as (21)where μ = cosα and n is the density, (22)Looking at energetic tails, we see that accelerated electrons at the wavy shock have about one order of magnitude higher differential density than the seed population (initial distribution function), but this density is comparable to the one at a smoothed shock.
Fig. 14 a) Histogram showing a distribution of the number N_{i} of interactions of electrons with the shock. N is unitless and represents a fraction. More explanation is in the text. b) Relative energy gain of electrons at the wavy shock over one at a smoothed shock versus the number N_{i} of interactions. E_{f} and are final energies after interactions with the wavy shock and a smoothed shock, respectively. 

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Complex trajectories and many interactions of electrons with the shock (e.g., Fig. 8) lead to a question of a stochastic description of electron acceleration at a wavy shock and an application of a FokkerPlanck type equation to this process. We calculated trajectories of about 69 thousand electrons with initial energies 0.5 − 5 keV and evenly distributed pitch angles and positions along the shock, which had our nominal values with θ_{B} = 90°. Results are summarized in Fig. 14. Figure 14a shows a histogram of the number N_{i} of interactions of electrons with the shock, where N is the fraction from the total number ΣN_{i} of interactions. The distribution is rather flat with number of interactions in the tens. Figure 14b displays a scatter plot of the number N_{i} of interactions versus the total energy gain E_{f} relatively over the energy gain at a smoothed shock. For a stochastic process described by the FokkerPlanck equation, one would expect that energy gains are small for each interaction, and the electron energy increases with the number of interactions (because electrons gain energy at each interaction). But it is not the case, because Fig. 14b does not show such a dependence. In fact, a significant amount of energy electrons gain by one or a few interactions (reflections, cf. Fig. 8). Therefore the FokkerPlanck description is not applicable here.
4. Discussion and conclusions
Fig. 15 Contour plot of the normalized distribution function f(v,α) / f_{i}(v) of accelerated upstream electrons as a function of energy (in logarithmic scale) and pitch angle α for (left) a wavy shock with θ_{B} = 85° and (right) a smoothed shock wave with θ_{Bn} = θ_{B}. (Plots in Fig. 11a could be constructed from values of the horizontal cut at energy of 3 keV.) 

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We studied the interactions of electrons with a nearly perpendicular wavy shock front. The present analysis is a continuation of our previous Papers I and II. We found that energy gains of electrons did not depend significantly on the shock thickness, magnetic field profile inside the shock, and shock wavy form; on average, they mainly depended on the angle between the smoothed shock front and ambient magnetic field. It means that, on average, energy gains of electrons at a wavy shock front and a corresponding smoothed shock are comparable. However, we also found that energy gain significantly exceeds an average level for some combinations of initial parameters. One can speculate, that such a repetition of favourable initial conditions could cause a fine structure of type II burst (called herringbones), apparently created by repeated electron beams. Distribution functions of accelerated electrons have a patchy structure (Figs. 15, 16), which changes with position (and time if the wavy front is nonstationary). Such a structure is prone to induce plasma instabilities that will generate plasma waves. These waves may
Fig. 16 Contour plot of the normalized distribution function f(v,α) / f_{i}(v) of accelerated downstream electrons for a wavy perpendicular shock. (Plot in Fig. 9a could be constructed from values of the horizontal cut at energy of 3 keV.) 

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participate in further acceleration of a fraction of electrons and possibly help to form a herringbone structure.
Acknowledgments
This research was supported by grants 205/09/0170 and P209/10/1680 of the Grant Agency of the Czech Republic, by grant IAA300030701 of the Academy of Sciences of the Czech Republic, and by the MŠMT ČR project ME09009. The research leading to these results has also received funding from the European Commission’s Seventh Framework Programme (FP7/2007 − 2013) under the grant agreement SWIFF (project No. 263340, www.swiff.eu).
References
 Decker, R. B. 1990, J. Geophys. Res., 95, 11993 [NASA ADS] [CrossRef] [Google Scholar]
 Gedalin, M. 2001, J. Geophys. Res., 106, 21645 [NASA ADS] [CrossRef] [Google Scholar]
 Holman, G. D., & Pesses, M. E. 1983, ApJ, 267, 837 [NASA ADS] [CrossRef] [Google Scholar]
 Knock, S. A., Cairns, I. H., Robinson, P. A., & Kuncic, Z. 2003, J. Geophys. Res., 108, 1126 [NASA ADS] [CrossRef] [Google Scholar]
 KraussVarban, D., & Wu, C. S. 1989, J. Geophys. Res., 94, 15367 [NASA ADS] [CrossRef] [Google Scholar]
 Leroy, M., & Mangeney, A. 1984, Ann. Geophys., 2, 449 [NASA ADS] [Google Scholar]
 Vandas, M. 1989, Bull. Astron. Inst. Czech., 40, 189 [NASA ADS] [Google Scholar]
 Vandas, M. 1991, Bull. Astron. Inst. Czech., 42, 170 [NASA ADS] [Google Scholar]
 Vandas, M. 1995, J. Geophys. Res., 100, 23499 [NASA ADS] [CrossRef] [Google Scholar]
 Vandas, M., & Karlický, M. 2000, Sol. Phys., 197, 85 [NASA ADS] [CrossRef] [Google Scholar]
 Vandas, M., & Karlický, M. 2005, Proc. Solar Wind 11 – SOHO 16, Connecting Sun and Heliosphere, ESA SP592, 453 [Google Scholar]
 Wu, C. 1984, J. Geophys. Res., 89, 8857 [NASA ADS] [CrossRef] [Google Scholar]
 Zlobec, P., Messerotti, M., Karlický, M., & Urbarz H. 1993, Sol. Phys., 144, 373 [NASA ADS] [CrossRef] [Google Scholar]
All Figures
Fig. 1 Global view of the model wavy shock front on the right. Left part shows a wavy shock approximation of a magnified small piece of the wavy shock (see two dashed arrows) by a plane shock wave. X and Z scales are not the same, the X scale is zoomed in. 

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In the text 
Fig. 2 Magnetic field profiles inside the model shock layer. The profile (17) used in calculations (solid line) is compared to the profile (16) drawn by the dotted line. The magnetic jump ν = 3 was used in the plot. 

Open with DEXTER  
In the text 
Fig. 3 Example of an electron trajectory around (right) and inside (left) the wavy shock. The electron is reflected (r) once and then transmitted (t) downstream. Relative vertical placement of r and ttrajectories is arbitrary (otherwise they would not fit both into the figure). A value of the angle θ_{B} is explicitly written. 

Open with DEXTER  
In the text 
Fig. 4 Another example of an electron trajectory around (right) and inside (left) the wavy shock. Layout is similar to Fig. 3. The electron only changed its initial position and it is one time transmitted (t) downstream and one time transmitted (t) upstream. 

Open with DEXTER  
In the text 
Fig. 5 Example of an electron trajectory around (right) and inside (left) the wavy shock. Layout is similar to Fig. 3. The angle θ_{B} only changed. The electron is reflected (r_{1}, r_{2}) twice and then transmitted (t) downstream. 

Open with DEXTER  
In the text 
Fig. 6 Comparison of energy gain of electrons at the wavy shock with one at a smoothed shock. E_{f} and are final energies after interactions with the wavy shock and a smoothed shock, respectively, α_{i} is the initial pitch angle. The dashed line displays an average value. 

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In the text 
Fig. 7 Comparison of energy gain of electrons at the wavy shock with one at a smoothed shock. E_{f} and are final energies after interactions with the wavy shock and a smoothed shock, respectively, Z_{i} is the initial position. The dashed line displays an average value. 

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In the text 
Fig. 8 Examples of electron trajectories around the wavy shock. a) The electron is reflected (r) and then transmitted many times (t_{1}–t_{8}) upstream/downstream and vice versa. b) A similar trajectory but for a higher energy gain. The electron is reflected twice (r_{1} and r_{2}) and then transmitted many times (t_{1}, t_{2}, etc.). 

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In the text 
Fig. 9 a) Angular distribution function of accelerated downstream electrons for a perpendicular wavy shock in an arbitrarily chosen downstream point (thin solid line). The direction of the magnetic field B_{2} is shown. The shock is located opposite to this direction. The distribution function is rotationally symmetric around B_{2}. It is a polar graph, where the polar angle corresponds to the pitch angle α and the radial distance (in a logarithmic scale) to a value of the distribution function f(v,α) of accelerated downstream electrons. The velocity v is constant here and its value corresponds to the energy of 3 keV. The dashed circle labelled 1 × represents the value of the initial distribution function f_{i}(v) from (19). For comparison, the thick solid line shows the angular distribution function of transmitted electrons through a perpendicular plane shock wave. b) The same as in a), but the thin solid line shows the angular distribution averaged along the shock front. 

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In the text 
Fig. 10 a) Angular distribution function of accelerated downstream electrons with energy of 3 keV for a wavy shock with θ_{B} = 85° in an arbitrarily chosen downstream point (thin solid line). The layout is similar to Fig. 9. The thick line shows the distribution of transmitted electrons through a smoothed shock wave with θ_{Bn} = θ_{B}. b) The same as in a), but the thin solid line shows the angular distribution averaged along the shock front. 

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In the text 
Fig. 11 a) Angular distribution function of accelerated upstream electrons with energy of 3 keV for a wavy shock with θ_{B} = 85° in an arbitrarily chosen upstream point (thin solid line). The figure complements the previous Fig. 10. The thick line shows the distribution of reflected electrons at a smoothed shock wave with θ_{Bn} = θ_{B}. The shock front is located in the direction of B_{1}. b) The same as in a), but the thin solid line shows the angular distribution averaged along the shock front. 

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In the text 
Fig. 12 Differential density of accelerated upstream electrons for a wavy shock with θ_{B} = 88°. The dotted line shows seed population (initial distribution function (19)), the thick line is for a corresponding smoothed shock, the thin solid and dashed lines are for a wavy shock with A / L = 0.1 and 0.2, respectively. The differential density was averaged along the shock front. 

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In the text 
Fig. 13 Differential density of accelerated downstream electrons for a wavy shock with θ_{B} = 88°. The layout is similar to Fig. 15. The differential density was averaged along the shock front. 

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In the text 
Fig. 14 a) Histogram showing a distribution of the number N_{i} of interactions of electrons with the shock. N is unitless and represents a fraction. More explanation is in the text. b) Relative energy gain of electrons at the wavy shock over one at a smoothed shock versus the number N_{i} of interactions. E_{f} and are final energies after interactions with the wavy shock and a smoothed shock, respectively. 

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In the text 
Fig. 15 Contour plot of the normalized distribution function f(v,α) / f_{i}(v) of accelerated upstream electrons as a function of energy (in logarithmic scale) and pitch angle α for (left) a wavy shock with θ_{B} = 85° and (right) a smoothed shock wave with θ_{Bn} = θ_{B}. (Plots in Fig. 11a could be constructed from values of the horizontal cut at energy of 3 keV.) 

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In the text 
Fig. 16 Contour plot of the normalized distribution function f(v,α) / f_{i}(v) of accelerated downstream electrons for a wavy perpendicular shock. (Plot in Fig. 9a could be constructed from values of the horizontal cut at energy of 3 keV.) 

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In the text 
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