Observations of pores and surrounding regions with CO 4.66 micron lines by BBSO/CYRA
Observations of pores and surrounding regions with CO 4.66 micron lines by BBSO/CYRA
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通过 BBSO/CYRA 用 CO 4.66 微米线观察孔隙和周围区域
DOI：
10.1051/0004-6361/202244600
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发表时间：
2022-11
期刊：
影响因子：
--
通讯作者：
Mei Zhang
中科院分区：
文献类型：
--
作者：
Yongliang Song;Xianyong Bai;Xu Yang;Wenda Cao;Han Uitenbroek;Yuanyong Deng;Xin Li;Xiao Yang;Mei Zhang
太阳对一氧化碳（CO）的观测表明，在较低的太阳色球层中存在较低温度的气体。本文利用大熊太阳观测站的低温红外光谱仪（CYRA）用co4.66 {\mu}m谱线观测了孔隙区、静太阳区和网络磁场区。我们利用4.66 {\mu}m附近的强CO谱线，了解了不同太阳特征和不同磁场强度下太阳低层大气热结构的性质。观测还包括AIA 1700 {\AA}图像、HMI连续体图像和磁图。本文还首次利用Bifrost代码进行了三维辐射磁流体动力学（MHD）模拟，并与观测数据进行了比较。我们使用RH代码合成了网络区域的CO线轮廓。CO 3-2 R14线中心强度随磁场强度的增加而增强或减弱，这可能是由于不同尺寸磁通管的加热效果不同造成的。我们在CO 3-2 R14线中心强度图像中发现了几个“冷泡”，可分为两种类型。一种类型位于安静的太阳区域，没有磁场。另一种类型在过去很少被报道，它靠近或被磁场包围。值得注意的是，有些位于磁网的边缘。利用Bifrost和RH程序对两种冷泡进行了三维MHD模拟，再现了冷泡强度与网络磁场强度的关系。模拟还表明，在网络磁场附近存在一个冷等离子体斑点，导致了CO 3-2 R14线中心图像中观测到的冷气泡。我们的观察和模拟表明，磁场在一些CO冷泡的产生中起着至关重要的作用。
Solar observations of carbon monoxide (CO) indicate the existence of lower-temperature gas in the lower solar chromosphere. We present an observation of pores, and quiet-Sun, and network magnetic field regions with CO 4.66 {\mu}m lines by the Cryogenic Infrared Spectrograph (CYRA) at Big Bear Solar Observatory. We used the strong CO lines at around 4.66 {\mu}m to understand the properties of the thermal structures of lower solar atmosphere in different solar features with various magnetic field strengths. AIA 1700 {\AA} images, HMI continuum images and magnetograms are also included in the observation. The data from 3D radiation magnetohydrodynamic (MHD) simulation with the Bifrost code are also employed for the first time to be compared with the observation. We used the RH code to synthesize the CO line profiles in the network regions. The CO 3-2 R14 line center intensity changes to be either enhanced or diminished with increasing magnetic field strength, which should be caused by different heating effects in magnetic flux tubes with different sizes. We find several"cold bubbles"in the CO 3-2 R14 line center intensity images, which can be classified into two types. One type is located in the quiet-Sun regions without magnetic fields. The other type, which has rarely been reported in the past, is near or surrounded by magnetic fields. Notably, some are located at the edge of the magnetic network. The two kinds of cold bubbles and the relationship between cold bubble intensities and network magnetic field strength are both reproduced by the 3D MHD simulation with the Bifrost and RH codes. The simulation also shows that there is a cold plasma blob near the network magnetic fields, causing the observed cold bubbles seen in the CO 3-2 R14 line center image. Our observation and simulation illustrate that the magnetic field plays a vital role in the generation of some CO cold bubbles.
DOI：
10.1142/9789814533003
发表时间：
1995-08
期刊：
--
影响因子：
--
作者：
J. Kuhn;M. Penn
通讯作者：
J. Kuhn;M. Penn
DOI：
--
发表时间：
1992-08
期刊：
--
影响因子：
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作者：
M. Geller
通讯作者：
M. Geller