标题： 从太阳色球到日冕的加热机制和射电响应 显示英文标题

标题： Heating Mechanisms and Radio Response from the Solar Chromosphere to Corona

摘要： 太阳大气（从色球层到日冕）的加热机制是现代天文学面临的最大挑战之一。 经典机制可分为两类：波加热（W）和磁重联加热（X）。 它们目前仍面临一些难以克服的问题。 最近，我们提出了一种新的机制，称为磁梯度泵浦加热（MGP，或P），它似乎克服了这些困难，但仍然缺乏足够的观测证据。 究竟哪一个真正解释了日冕高温的物理机制？ 如何利用观测来识别和验证加热机制？ 由于不同的加热机制会从不同加速过程产生非热粒子，并经历不同的传播过程，因此它们在宽带频谱射电观测中的响应也各不相同。 其中，W机制产生的非热电子与冲击波加速密切相关，其射电响应应为漂移率呈随机分布的一组尖峰爆发；X机制产生的非热电子由反向流动的重连电场加速，其射电响应应为III型电子对或尖峰对；P机制会产生高能粒子上行流，其射电响应应为具有适度负漂移率的单向纤维爆发。 因此，可以通过宽带动态频谱射电观测来识别和验证加热机制。 此外，利用高分辨率射电日面图和光谱成像观测，可以分别识别和验证不同区域的加热机制，从而揭示日冕高温的物理本质。 显示英文摘要

摘要： Heating mechanism in the solar atmosphere (from chromosphere to corona) is one of the top-challenges in modern astronomy. The classic mechanisms can be divided into two categories: wave heating (W) and magnetic reconnection heating (X). Both of them still face some problems currently difficult to overcome. Recently, we proposed a new mechanism, called magnetic-gradient pumping heating (MGP, or P) which seems to overcome those difficulties, but still lacks sufficient observational evidence. Which one really explained the physics of hot corona exactly? How can observations be used to identify and verify the heating mechanism? Since different heating mechanism will generate non-thermal particles from different accelerations and experience different propagations, they will have different response on the broadband spectral radio observations. Among them, the non-thermal electrons from W mechanisms are closely related to shock-wave acceleration, and their radio response should be group of spike bursts with random distribution of drifting rates; the non-thermal electrons from X mechanisms are accelerated by reconnecting electric field with bidirectional flow, and their radio response should be type III pairs or spike pairs; P mechanism will produce energetic particle upflows, and their radio response should be unidirectional fiber bursts with moderate negative drifting rates. Therefore, the heating mechanism can be identified and verified from the the broadband dynamic spectral radio observations. Additionally, using high-resolution radioheliographs and spectral-imaging observations, the heating mechanisms in different regions can be identified and verified separately, thereby demonstrating the physical essence of hot corona.