2.1. Single magnetized shock characterization

In our former experiments performed at JLF/Titan and LULI2000 (Yao et al. Reference Yao, Fazzini, Chen, Burdonov, Antici, Béard, Bolaños, Ciardi, Diab and Filippov2021, Reference Yao, Fazzini, Chen, Burdonov, Antici, Béard, Bolaños, Ciardi, Diab and Filippov2022; Fazzini et al. Reference Fazzini, Yao, Burdonov, Béard, Chen, Ciardi, d'Humières, Diab, Filippov and Kisyov2022), we investigated single shock formation, as well as shock–shock interactions, by having an expanding plasma drive a shock into an ambient gas in the presence of a strong (20 T) external magnetic field. Since the expanding plasma, the ambient gas and the magnetic field are all decoupled, we are able to vary the magnetic field independently of the expanding plasma and of the ambient gas, which allows us to investigate the essential role played by the magnetic field and to highlight the ion acceleration mechanism at play.

With the set-up shown in figure 1(a), we have been able to characterize the plasma density, temperature, as well as the electric field developed at the front of a single shock, and observe strong non-thermal accelerated ion populations linked with the ‘shock-surfing’ acceleration mechanism (Yao et al. Reference Yao, Fazzini, Chen, Burdonov, Antici, Béard, Bolaños, Ciardi, Diab and Filippov2021, Reference Yao, Fazzini, Chen, Burdonov, Antici, Béard, Bolaños, Ciardi, Diab and Filippov2022).

Figure 1.

(a) Set-up of the experiment to characterize a single magnetized shock (Yao et al. Reference Yao, Fazzini, Chen, Burdonov, Antici, Béard, Bolaños, Ciardi, Diab and Filippov2021, Reference Yao, Fazzini, Chen, Burdonov, Antici, Béard, Bolaños, Ciardi, Diab and Filippov2022). The whole scene is embedded in an H$_2$ gas of low density ($\sim 10^{18}$ cm$^{-3}$) emanating from a pulsed nozzle. Further, the whole assembly is embedded in a strong magnetic field (20 T). (b) Density measurement (integrated along the line of sight) 4 ns after the laser irradiation of the solid target. (c) Evolution of the shock front position along the $x$-axis and the corresponding velocity. (d) Evidence for the energization of protons picked up from the ambient medium. Proton energy spectra of both the experiment (red dots) and of three PIC simulations, the black solid line for the magnetized fast case with applied magnetic field along the z-direction, i.e., $B_z=20$ T and initial shock velocity $v=1500\,{\rm km}\,{\rm s}^{-1}$, the yellow dashed line for the unmagnetized fast one with $\boldsymbol{B}=0$ and $v=1500\,{\rm km}\,{\rm s}^{-1}$, and the purple dashed line for the magnetized slow one with $B_z=20$ T and $v=500\,{\rm km}\,{\rm s}^{-1}$, all measured at t = 2.6 ns in the simulations. The analytical thermal proton spectrum is shown with the red dash-dotted line (200 eV); and the experimental noise baseline is shown in cyan dotted line.

Specifically, the shock was generated by sending a plasma, generated from a high-power laser (1 ns duration, 70 J, $1.6\times 10^{13}$ W cm$^{-2}$) irradiating a solid target (Teflon, or CF$_2$), into a low-density gas (of density ${\sim }10^{18}$ cm$^{-3}$), and in the presence of a 20 T magnetic field that is homogeneous and steady state over the time scale of the experiment. This magnetic field is produced by our unique coil set-up (Albertazzi et al. Reference Albertazzi, Béard, Ciardi, Vinci, Albrecht, Billette, Burris-Mog, Chen, Da Silva and Dittrich2013; Higginson et al. Reference Higginson, Korneev, Ruyer, Riquier, Moreno, Béard, Chen, Grassi, Grech and Gremillet2019). A record of the plasma electron density, obtained by optical probing, is shown in figure 1(b). We can clearly observe the presence of an electron foot, likely reflected ahead of the shock by the moving shock front. To our knowledge, this is the first laboratory observation of such a structure, which was postulated (Dimmock et al. Reference Dimmock, Russell, Sagdeev, Krasnoselskikh, Walker, Carr, Dandouras, Escoubet, Ganushkina and Gedalin2019) and also verified to be present in magnetospheric shocks as recorded by satellite (Balogh & Treumann Reference Balogh and Treumann2013).

Figure 1(c) shows the evolution of the shock front position and the corresponding velocity deduced from it, which shows the very fast decrease in shock velocity over the first few nanoseconds. Before 2.6 ns, the shock front velocity is approximately ${v = 1500\,{\rm km}\,{\rm s}^{-1}}$, i.e. the shock is collisionless and super-critical with a mean free path larger than 10 mm and a magnetosonic Mach number larger than the critical value (see details in table 1), while after approximately 5 ns, it becomes sub-critical, with correspondingly lesser energization of the reflecting ions from the ambient (Yao et al. Reference Yao, Fazzini, Chen, Burdonov, Antici, Béard, Bolaños, Ciardi, Diab and Filippov2021, Reference Yao, Fazzini, Chen, Burdonov, Antici, Béard, Bolaños, Ciardi, Diab and Filippov2022). The ion spectrometer that was deployed in the experiment was set in the axis of the magnetic field, i.e. along the $z$-axis in figure 1(a), otherwise the ions energized out of the plasma could not be recorded, as they would be deflected away by the 20 T large-scale magnetic field.

Table 1.

Comparison between the parameters of the shocks we are able to produce with our platform, and the ones of the solar wind, as well as those from a non-relativistic SNR (see Yao et al. Reference Yao, Fazzini, Chen, Burdonov, Antici, Béard, Bolaños, Ciardi, Diab and Filippov2021, p. 10). The parameters used for the calculations are: $B = 20$ T, $T_e = 100$ eV, $n_e = 3\times 10^{18}$ cm$^{-3}$, $v_{{\rm shock}} = 1500\,{\rm km}\,{\rm s}^{-1}$ (see details in text). The plasma beta is defined as $\beta \equiv P_{{\rm therm}}/P_{{\rm mag}}$ i.e. the ratio of plasma pressure to magnetic field pressure. The magnetosonic Mach number $M_{{\rm ms}} = v_{s}/v_{{\rm ms}}$, is the ratio between the shock velocity and the magnetosonic velocity ($v_{{\rm ms}} \equiv \sqrt {v_A^2 + c_s^2}$) in the upstream medium, where $v_A$ is the Alfvén velocity and $c_s$ is the ion sound velocity. The fourth column allows one to evaluate that the shock is not affected by collisions. This requires that the ion–ion collision mean free path ($\lambda _{{\rm mfp}}$) be large compared with the shocked-ion gyroradius, $r_{L,i}$, which sets the scale of the shock transition.

The recorded proton spectrum is shown in figure 1(d) by red dots evidenced non-thermal proton energization. We have performed a series of particle-in-cell (PIC) simulations, using the code SMILEI (Derouillat et al. Reference Derouillat, Beck, Pérez, Vinci, Chiaramello, Grassi, Flé, Bouchard, Plotnikov and Aunai2018), with different magnetic fields and initial shock velocities. Those simulations help us identify the critical role played by the external magnetic field and fast shock velocity in the non-thermal proton energization, i.e. only in the case with both 20 T magnetic field and $1500\,{\rm km}\,{\rm s}^{-1}$ initial shock velocity can we well reproduce the experimental proton spectrum. Otherwise, the spectra will be lower than the noise baseline. Also note that there is no signal recorded above the noise baseline for cases with only the magnetic field or the ambient gas (i.e. when there will be no shock), indicating that the non-thermal particle populations are indeed coming from the shock.

The single shock front was also probed with protons in order to measure the electric field at that location (Yao et al. Reference Yao, Fazzini, Chen, Burdonov, Antici, Béard, Bolaños, Ciardi, Diab and Filippov2022). The probing protons accelerated by the Target Normal Sheath Acceleration (TNSA) (Mora Reference Mora2003) were sent parallel to the magnetic field, as can be seen in figure 1(a). As shown in figure 2(a), we could clearly observe the same structure as in figure 1(b), namely the front of the expanding plasma and a particular proton deflection structure at the shock front. From it, as shown in figure 2(b,c), we can infer that the electric field at the shock front had a double jump structure, with a field reversal. Detailed discussions can be found in Yao et al. (Reference Yao, Fazzini, Chen, Burdonov, Antici, Béard, Bolaños, Ciardi, Diab and Filippov2022).

Figure 2.

(a) Proton radiography (collected on a radiochromic film (RCF) and employing 19 MeV protons) of the same configuration as shown in figure 1(a), 5 ns after the laser pulse. (b) Hemispherical electric field $E_x$ in the $xz$-plane, with a radius of $R=5.1$ mm, estimated from (a). (c) Lineout of the proton dose modulation along the yellow line indicated in (a). The green full curve is the modulation from the experimental results, and the dashed blue curve is that from the ILZ simulation (Bolanos et al. Reference Bolanos, Smets, Chen, Grisolet, Filippov, Henares, Nastasa, Pikuz, Riquier and Safranova2022), which is obtained by imposing a bipolar electric field with hemispherical shape shown in (b). The red dash-dotted curve represents the lineout of the field $E_x$ in $z=0$ (Yao et al. Reference Yao, Fazzini, Chen, Burdonov, Antici, Béard, Bolaños, Ciardi, Diab and Filippov2022).

The main parameters of the shock that we can produce with our set-up are summarized in table 1, showing that they are collisionless and super-critical, and actually quite close to those of the solar wind. Yet, reaching higher velocity shocks, with applicability to supernova remnants (SNR), is not possible with presently accessible high-power lasers, but will be in the near future with e.g. Apollon (Burdonov et al. Reference Burdonov, Fazzini, Lelasseux, Albrecht, Antici, Ayoul, Beluze, Cavanna, Ceccotti and Chabanis2021).

2.2. Double magnetized shocks collision

Later, we investigated at LULI2000, the interpenetration of two sub-critical single shocks with a similar set-up, which is shown in figure 3(a). Since the distance between the two targets was large (i.e. 9 mm), due to constraints in the set-up, the shocks travel to the middle and collide after 11 ns, as can be seen in figure 3(c,d), thus having an average velocity lower than $500\,{\rm km}\,{\rm s}^{-1}$. This led us to be limited to exploring sub-critical shock encounters (Fazzini et al. Reference Fazzini, Yao, Burdonov, Béard, Chen, Ciardi, d'Humières, Diab, Filippov and Kisyov2022).

Figure 3.

(a) Set-up of the experiment with two high-power lasers ((1 ns, 100 J at 1 $\mathrm {\mu }$m wavelength, $1.6\times 10^{13}$ W cm$^{-2}$ intensity on target)) irradiate two solid targets (CF$_2$) embedded in ambient gas and strong $B$-field (20 T). (b–e) Temporal sequence of the density (along the $z$-axis) measurements showing the evolution of the collision of two magnetized shocks.

The measured ion spectrum is the same as shown in figure 1(d). Nevertheless, our PIC simulations have revealed an interesting particle dynamics at play during the sub-critical shock encounter, and which provides energy enhancement (see figure 4). By tracking a set of representative energetic protons, we have indeed been able to identify that this energy enhancement is a result of the ‘phase-locking effect’ between the transverse particle velocity ($V_y$) and the transverse $E$-field ($E_y$) after the collision, i.e. the work done by $E_y$ (i.e. $W_{Ey}$) is purely positive, which only exists in the shock colliding case and allows a further boost of the ion energy (Fazzini et al. Reference Fazzini, Yao, Burdonov, Béard, Chen, Ciardi, d'Humières, Diab, Filippov and Kisyov2022).

Figure 4.

The PIC simulation results demonstrating the enhanced particle acceleration in the sub-critical shock colliding case (b), compared with the single one (a). The final energy spectrum is in (c). See details of the three phases in Fazzini et al. (Reference Fazzini, Yao, Burdonov, Béard, Chen, Ciardi, d'Humières, Diab, Filippov and Kisyov2022).

Unfortunately, the phase-locking effect could not be observed at LULI2000 since the time-integrated spectrum of ions is produced by a combination of ions accelerated by the super-critical shock early in time and the collision of the slowed-downed subcritical shock that would produce the phase-locking acceleration. Since, the maximum energy produced by these sub-critical shocks is low, we are not able to separate the two sources in our past measurements. This is why we propose to move, using an improved set-up, to investigate the encounter to the moments where the shocks are still super-critical.