![]() This, together with the fact that the non-thermal energy needed to heat the corona must propagate through the chromosphere, explains why it is indeed a crucial interface region to solve many of the key problems in solar and stellar physics. Above the β = 1 surface, the magnetic field essentially dominates the structuring and dynamics of the plasma. As a result, the β = 1 corrugated surface, where the ratio of gas to magnetic pressure is unity, lies inside the chromosphere. Moreover, from the visible photospheric surface to the chromosphere-corona transition region (TR), the plasma density decreases exponentially by several orders of magnitude, more rapidly than the magnetic field strength. ![]() Although the temperature of the chromospheric plasma does not exceed 10 4 K, the fact that its density is much larger than that of the extended and rarified corona implies that much more mechanical energy is required to sustain the chromosphere than the million-degree corona. The chromosphere is a very important region of the solar atmosphere, with an extension of several thousand kilometers, located between the relatively cool surface layers of the photosphere and the overlying hot corona ( 1– 3). Vigil, Amy Winebarger, Ernest Alsina Ballester, Luca Belluzzi, Jiří Štěpán, Andrés Asensio Ramos, Mats Carlsson, and Jorrit Leenaarts Show Fewer Rachmeler, Ken Kobayashi, Hirohisa Hara, Masahito Kubo, Noriyuki Narukage, Taro Sakao, Toshifumi Shimizu, Yoshinori Suematsu, Christian Bethge, Bart De Pontieu, Alberto Sainz Dalda, Genevieve D. McKenzie, Frédéric Auchère, Ryouhei Kano, … Show All …, Donguk Song, Masaki Yoshida, Laurel A. Ryohko Ishikawa, Javier Trujillo Bueno, Tanausú del Pino Alemán, Takenori J.
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