Current Investigation on Superbubble 30 Doradus C in the Large Magellanic Cloud

Subjects: Astronomy submitted time 2024-03-22 Cooperative journals: 《天文学进展》

CHEN Han-xiao CHI Yi-heng MENG Yi-fan CHEN Yang ZHOU Ping SUN Lei SUN Wei

Abstract： : Superbubbles are large shell-like interstellar medium structures formed by stel#2;lar winds from massive stars and supernovae. With obvious emission signatures in multiple wavelengths, superbubbles are important sites for studying the radiation mechanisms. 30 Doradus C (30 Dor C in short) is located southwest of 30 Dor in the Large Magellanic Cloud. Its location is basically consistent with OB association LH 90, suggesting that this super#2;bubble may have been created by it. Since 30 Dor C was detected in X-ray band by Einstein satellite in 1981, its X-ray emission has been observed and studied for many years. 30 Dor C is the only superbubble dominated by non-thermal emission in the Large Magellanic Cloud and it’s also the largest non-thermal X-ray emission source in the Local Group. The non#2;thermal emission covers the entire region of the superbubble and is most significant at the shell. Such bright non-thermal emission may due to particle acceleration in the superbubble, and to find out the evidence, the magnetic field conditions in the superbubble and radiation in other bands have also been studied. Compared to non-thermal emission, thermal emission in 30 Dor C is relatively faint. Most of the thermal emission is detected in the eastern region of 30 Dor C, and there are also a supernova remnant found outside the superbubble at the southeast of the shell. In recent years, with the advancement of radio observation, the s#2;tudy of molecular clouds of 30 Dor C has also increased. This paper reviews and summarizes the research of 30 Dor C up to now. The basic situation of thermal emission, non-thermal emission and other bands are discussed first. Meanwhile, a summary is provided on the point sources discovered inside the superbubble. The evidence of particle acceleration in#2;side 30 Dor C is discussed according to the radiation situation, as well as current particle acceleration models and the formation reasons of 30 Dor C.

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