Transverse oscillations and an energy source in a strongly magnetized sunspot

Yuan, Ding; Fu, Libo; Cao, Wenda; Kuźma, BłaŻej; Geeraerts, Michaël; Trelles Arjona, Juan C.; Murawski, Kris; Van Doorsselaere, Tom; Srivastava, Abhishek K.; Miao, Yuhu; Feng, Song; Feng, Xueshang; Quintero Noda, Carlos; Ruiz Cobo, Basilio; Su, Jiangtao
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Nature Astronomy

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The solar corona is two to three orders of magnitude hotter than the underlying photosphere, and the energy loss of coronal plasma is extremely strong, requiring a heating flux of over 1,000 W m−2 to maintain its high temperature. Using the 1.6 m Goode Solar Telescope, we report a detection of ubiquitous and persistent transverse waves in umbral fibrils in the chromosphere of a strongly magnetized sunspot. The energy flux carried by these waves was estimated to be 7.52 × 106 W m−2, three to four orders of magnitude stronger than the energy loss rate of plasma in active regions. Two-fluid magnetohydrodynamic simulations reproduced the high-resolution observations and showed that these waves dissipate significant energy, which is vital for coronal heating. Such transverse oscillations and the associated strong energy flux may exist in a variety of magnetized regions on the Sun, and could be the observational target of next-generation solar telescopes.
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Solar and Stellar Magnetism
Magnetic fields are at the base of star formation and stellar structure and evolution. When stars are born, magnetic fields brake the rotation during the collapse of the mollecular cloud. In the end of the life of a star, magnetic fields can play a key role in the form of the strong winds that lead to the last stages of stellar evolution. During
Felipe García