论文标题
关于内部heliosheath中0.11 keV至344 MeV离子光谱的属性，使用正规化的$κ$分布
On the properties of 0.11 keV to 344 MeV ion spectra in the inner heliosheath using regularized $κ$-distributions
论文作者
论文摘要
离子能光谱的形状在确定离子能量，加速度机制以及不同等离子体和外离子群的可能来源方面起着关键作用。确定总粒子光谱的确切形状，提供了解决内部螺旋壳（IHS）动力学的必要手段。除了各种建模工作之外，迄今为止尚未进行$ 0.11至344 MEV的扩展能源范围的直接拟合。 We use an extended set of combined 0.11-55 keV ENA measurements from the Interstellar Boundary Explorer (IBEX-Lo and IBEX-Hi) and Cassini/Ion and Neutral Camera (INCA), converted to protons, together with $\sim$28 keV to 344 MeV ion measurements from the Low Energy Charged Particle (LECP) and Cosmic Ray Subsystem (CRS) experiments on Voyager 2，在太阳能23（SC23）和上升期太阳能cylce 24（SC24）（2009-2016）的衰落阶段，以研究粒子能谱的特征。 我们将0.11 KEV拟合到344 MEV复合光谱，并具有一组正规的各向同性$κ$ - 分布功能（RKD），允许确定宏观物理特性。 我们证明，与SC23的下降阶段相对应的2009-2012频谱与三种不同的RKD相吻合，而与SC24上升相关的2013 - 2016年频谱只能与六个不同的RKD近似。 我们的结果通常与IHS内部发生额外加速的冲击加速颗粒一致。我们确定了低能传播颗粒的群体，超颗粒反射的种群以及由GCR调节的非常高的能量成分。 2013-2016时间段很可能与SC23和SC24的颗粒混合物有关，这反映了使用六个RDK。
The shape of the ion energy spectra plays a critical role toward determining the ion energetics, the acceleration mechanisms and the possible sources of different plasma and suprathermal ion populations. The determination of the exact shape of the total particle spectrum, provide the necessary means to address the inner heliosheath (IHS) dynamics. Apart from various modeling efforts, a direct fit to the measured ion spectra for an extended energy range of $\sim$0.11 to 344 MeV has not been performed to date. We use an extended set of combined 0.11-55 keV ENA measurements from the Interstellar Boundary Explorer (IBEX-Lo and IBEX-Hi) and Cassini/Ion and Neutral Camera (INCA), converted to protons, together with $\sim$28 keV to 344 MeV ion measurements from the Low Energy Charged Particle (LECP) and Cosmic Ray Subsystem (CRS) experiments on Voyager 2, over the declining phase of Solar Cyle 23 (SC23) and ascending phase Solar Cylce 24 (SC24) (2009-2016) to study the characteristics of the particle energy spectrum. We fit the 0.11 keV to 344 MeV composite spectra with a set of regularized isotropic $κ$-distribution functions (RKD) allowing the determination of the macroscopic physical properties. We demonstrate that the 2009-2012 spectrum that corresponds to the declining phase of SC23 is well fitted by three different RKDs, while the 2013-2016 spectrum, associated with the rise of SC24, can only be approximated with six different RKDs. Our results are generally consistent with shock accelerated particles that undergo additional acceleration inside the IHS. We identify a low energy transmitted population of particles, a suprathermal reflected population and a very high energy component that is modulated by GCRs. The 2013-2016 time period is most likely associated with a mixture of particles from SC23 and SC24, which is reflected by the need to employ six RDKs.
