标题： 等离子体$β$在宁静太阳区域：多仪器视图 显示英文标题

标题： The Plasma $β$ in quiet Sun Regions: Multi-Instrument View

摘要： 一次由多个空间和地面观测站联合开展的活动，例如GREGOR太阳望远镜、极端紫外成像光谱仪（EIS）以及界面区域成像光谱仪（Hinode 观测计划381，2019年10月11日至22日），旨在研究宁静太阳区域中的等离子体$\beta$。 在本工作中，我们重点关注2019年10月13日、17日和19日，通过多高度观测数据获得不同高度处的等离子体$\beta$。 我们从GREGOR高分辨率快速成像仪（HiFI）、红外光谱仪（GRIS）、IRIS、EIS以及来自SDO/AIA的补充数据中获得了温度、密度和磁场估计值。 利用观测数据和模型（例如FALC和PFSS），我们确定了光球层、色球层、过渡区和日冕中的等离子体$\beta$。 获得的等离子体$\beta$值在太阳大气中的预期范围内。 然而，在EIS和AIA的日冕高度（从$1.03\ R_{\odot}$到$1.20\ R_{\odot}$）等离子体$\beta$值处于Gary（2001）定义的极限内；这种行为之前由Rodríguez Gómez等人（2019）报告过。 此外，我们从太阳光球层的不同光学深度从$\log\ \tau=-1.0$到$\log\ \tau=-2.0$获得了等离子体$\beta$。 这些值随着光学深度的增加而减少。 这项工作通过太阳大气揭示了宁静太阳区域等离子体$\beta$的完整图景，这是更好地理解太阳日冕底部等离子体动力学的前提条件。 显示英文摘要

摘要： A joint campaign of several space-borne and ground-based observatories, such as the GREGOR solar telescope, the Extreme-ultraviolet Imaging Spectrometer (EIS), and the Interface Region Imaging Spectrograph (Hinode Observing Plan 381, 11-22 October 2019) was conducted to investigate the plasma $\beta$ in quiet sun regions. In this work, we focus on October 13, 17, and 19, 2019, to obtain the plasma $\beta$ at different heights through the solar atmosphere based on multi-height observational data. We obtained temperature, density and magnetic field estimates from the GREGOR High-resolution Fast Imager (HiFI), and Infrared Spectrograph (GRIS), IRIS, EIS and complementary data from SDO/AIA. Using observational data and models (e.g., FALC and PFSS), we determined the plasma $\beta$ in the photosphere, chromosphere, transition region and corona. The obtained plasma $\beta$ values lie inside the expected ranges through the solar atmosphere. However, at EIS and AIA coronal heights (from $1.03\ R_{\odot}$ to $1.20\ R_{\odot}$) plasma $\beta$ values appear in the limit defined by Gary (2001); such behavior was previously reported by Rodr\'iguez G\'omez et al. (2019). Additionally, we obtained the plasma $\beta$ in the solar photosphere at different optical depths from $\log\ \tau=-1.0$ to $\log\ \tau=-2.0$. These values decrease with optical depth. This work provides a complete picture of plasma $\beta$ in quiet sun regions through the solar atmosphere, which is a pre-requisite of a better understanding of the plasma dynamics at the base of the solar corona.