用RADYN模拟研究环形等离子体对纳耀斑加热的响应
Investigating the response of loop plasma to nanoflare heating using RADYN simulations
摘要：
我们提出的结果的一维流体动力学模拟的日冕循环受到纳米，造成的原位热加热，或非热电子（NTE）束。合成的强度和多普勒频移可以直接与IRIS和AIA观测到的日冕环过渡区（TR）的快速变化进行比较，与瞬态日冕加热有关。我们发现具有足够高的低能截止（E $_\textrm{C}$）的NTE在较低的TR和色球层中沉积能量，导致\emph{IRIS} \siiv ~线的蓝移（高达~ $\sim$ ~20 km/s），热传导不能再现。蓝移的E $_\textrm{C}$阈值取决于事件的总能量（对于10 $^{24}$尔格，$\approx$约为5 keV，对于10 $^{25}$尔格，最高可达15 keV）。所观察到的足点发射强度和流与模拟相结合，可以提供对加热事件的能量和E $_\textrm{C}$的约束。环等离子体对纳米火花的响应关键取决于电子密度：仅对于初始低密度环（$<$ ~10 $^{9}$ ~cm $^{-3}$）观察到显著的\siiv ~强度增强和流动。这提供了一个可能的解释的观测显着苔藓变异的相对稀缺。虽然可以清楚地观察到TR对单次加热事件的响应，但预测的单链日冕发射（AIA 94）低于当前的可检测性，并且只能在几条链在时间上紧密加热时观察到。最后，我们表明，IRIS \mgii ~色球线的分析可以帮助进一步限制的加热机制的属性。
英文摘要：
We present the results of 1D hydrodynamic simulations of coronal loops which are subject to nanoflares, caused by either in-situ thermal heating, or non-thermal electrons (NTE) beams. The synthesized intensity and Doppler shifts can be directly compared with IRIS and AIA observations of rapid variability in the transition region (TR) of coronal loops, associated with transient coronal heating. We find that NTE with high enough low-energy cutoff (E$_\textrm{C}$) deposit energy in the lower TR and chromosphere causing blueshifts (up to~$\sim$~20 km/s) in the \emph{IRIS} \siiv~lines, which thermal conduction cannot reproduce. The E$_\textrm{C}$ threshold value for the blueshifts depends on the total energy of the events ($\approx$~5 keV for 10$^{24}$ ergs, up to 15 keV for 10$^{25}$ ergs). The observed footpoint emission intensity and flows, combined with the simulations, can provide constraints on both the energy of the heating event and E$_\textrm{C}$. The response of the loop plasma to nanoflares depends crucially on the electron density: significant \siiv~intensity enhancements and flows are observed only for initially low-density loops ($<$~10$^{9}$~cm$^{-3}$). This provides a possible explanation of the relative scarcity of observations of significant moss variability. While the TR response to single heating episodes can be clearly observed, the predicted coronal emission (AIA 94Å) for single strands is below current detectability, and can only be observed when several strands are heated closely in time. Finally, we show that the analysis of the IRIS \mgii~chromospheric lines can help further constrain the properties of the heating mechanisms.
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