1. Ion dynamics and shock front nonstationarity in supercritical perpendicular shocks: impact of the pickup ions Zhongwei YANG 1 and Quanming LU 2 1 SOA Key Laboratory for Polar Science, Polar Research Institute of China, Shanghai, 200136, China. 2 CAS Key Laboratory of Basic Plasma Physics, University of Science and Technology of China, Hefei, 230026, China 2012 West Lake International Symposium on Plasma Simulation program, ZJU

2.  Introduction  Simulation model  Simulation results  Conclusions 04/2012 Contents

3. Upstream of the termination shock (quasi-perpendicular), ions primarily consist of ions of two distinct components: the solar wind ions (SWs) and the pickup ions (PUI or PIs). [ Vasyliunas and Siscoe, 1976; Fisk and Gloeckler, 2006; Wu et al., 2009,2010 ] 1. Introduction We thank NASA for this cartoon. 70-100AU Interstellar neutral gas Pickup ions Anomalous cosmic rays (ACRs) Solar wind protons ANOMALOUS COSMIC RAYS, Klecker, Mewaldt et al., SSRv, 1998

4. 1. Liewer et al. [1993] investigated the impact of PUI on the termination shock structure by using 1-D hybrid simulation. For quasi-perpendicular shocks with 0-20% PUI, they found the PUI lead to the formation of an extended foot (quasi-stationary). The amplitude of the extended foot increases with the PUI%. 1. Introduction

5. 2. Similar results (extended foot) are retrieved by PIC simulations [Lee et al. 2005, Chapman et al., 2005]. Moreover, they found that 10% PUI do not modify the dynamics of the reforming shock. Shock speed increases with PUI%. High-energy part of the downstream distribution of the solar wind ions decreases with the relative density of the pickup ions. 1. Introduction 10%PUI 0%PUI Distributions of the solar wind ions

6. 3. Zank et al. [2010] developed a model for the termination shock. They have two assumptions of downstream proton distributions. 1. Introduction Solar wind protons Transmitted solar wind protons Transmitted pickup ions High-energy tail: reflected and accelerated pickup ions k-distribution used in global MHD simulations (Heerikhuisen et al. 2008) Maxwellian distributions with the downstream density and temperature for reference

7. Main questions (present goal): 1.First, what’s the impact of pickup ions on the shock front structure? 2. Second, whether the reforming shock solutions found previously persist no matter how large the relative density of pickup protons is? 3.Third, to what extent are acceleration mechanisms of both solar wind protons and pickup protons in the resulting self- reforming, nonstationary shock profiles? 1. Introduction

8. 2. Simulation model We use a one-dimensional PIC code including pickup ions to simulate the supercritical perpendicular shock. The shock is produced by the Injection / reflection wall method as in previous works [e.g. Quest, 1985; Burgess et al., 1989; Nishimura et al., 2003; Chapman et al., 2005]. (1) Setups: --------------------------------------------------------------------------------------------------- θ Bn =90 o, Injection bulk velocity V in =3, B 0 =1 along y direction, m i /m e =100, ω pe /Ω ce =2, c=20 --------------------------------------------------------------------------------------------------- (2) Upstream plasma parameters: e - : Maxwellian distribution SWs: Maxwellian distribution PUI: Shell distribution [e.g. Kucharek and Scholer, 1995; Lee et al., 2005; Wu et al., 2009; Scholer et al., 2011]

9. PUI%=0 PUI%=25 3. Simulation results 3.1. Impact of the PIs% on the shock front reformation. RunPIs% 00 15 210 315 420 525 630 …… 1155 1260 PUI%=55 Upstream Downstream

10. 3. Simulation results 2. Pickup ions [By and Ex are also shown for reference]

11. 3. Simulation results 2. Pickup ions

12. 3. Simulation results 2. Pickup ions SDA ions SSA ions Core: DT ions

13. 4. conclusions 1. Shock front reformation can be persisted well at supercritical perpendicular shocks when PUI%<40. 2. Impact of the PUI% on the shock front micro-structure are as follows: 3. SDA is the most important acceleration mechanism. SSA also exists. Injection angle domains of SSA shifts due to the Pickup ion extended foot. Brief summary Low PUI%High PUI% extended foot (dominated by PUI & Lorentz term)stationary foot in solar wind ion gyro-scale (Lorentz and Hall term are competing with each other) nonstationary- ramp in electron inertial scale (dominated by SWs & Hall term) nonstationarystationary

14. Thank you!