Ishikawa Ryohko, Bueno Javier Trujillo, Del Pino Alemán Tanausú, Okamoto Takenori J, McKenzie David E, Auchère Frédéric, Kano Ryouhei, Song Donguk, Yoshida Masaki, Rachmeler Laurel A, Kobayashi Ken, Hara Hirohisa, Kubo Masahito, Narukage Noriyuki, Sakao Taro, Shimizu Toshifumi, Suematsu Yoshinori, Bethge Christian, De Pontieu Bart, Dalda Alberto Sainz, Vigil Genevieve D, Winebarger Amy, Ballester Ernest Alsina, Belluzzi Luca, Štěpán Jiří, Ramos Andrés Asensio, Carlsson Mats, Leenaarts Jorrit
National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan.
Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain.
Sci Adv. 2021 Feb 19;7(8). doi: 10.1126/sciadv.abe8406. Print 2021 Feb.
Routine ultraviolet imaging of the Sun's upper atmosphere shows the spectacular manifestation of solar activity; yet, we remain blind to its main driver, the magnetic field. Here, we report unprecedented spectropolarimetric observations of an active region plage and its surrounding enhanced network, showing circular polarization in ultraviolet (Mg ii & and Mn i) and visible (Fe i) lines. We infer the longitudinal magnetic field from the photosphere to the very upper chromosphere. At the top of the plage chromosphere, the field strengths reach more than 300 G, strongly correlated with the Mg ii line core intensity and the electron pressure. This unique mapping shows how the magnetic field couples the different atmospheric layers and reveals the magnetic origin of the heating in the plage chromosphere.
对太阳高层大气进行的常规紫外成像展示了太阳活动的壮观表现；然而，我们对其主要驱动因素——磁场却仍然一无所知。在此，我们报告了对一个活动区谱斑及其周围增强网络进行的前所未有的偏振光谱观测，观测显示在紫外（Mg ii和Mn i）以及可见光（Fe i）谱线中存在圆偏振现象。我们推断了从光球层到色球层最上层的纵向磁场。在谱斑色球层顶部，磁场强度超过300高斯，与Mg ii谱线核心强度和电子压力密切相关。这一独特的测绘展示了磁场如何耦合不同的大气层，并揭示了谱斑色球层加热的磁起源。
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