Disentangling the radio emission of the supernova remnant W51C with MHD simulations----中国科学院紫金山天文台

Seminar Title	Disentangling the radio emission of the supernova remnant W51C with MHD simulations

Speaker:	Dr. ZHANG Mengfei

Affiliation:	(NAOC)

When	Wednesday afternoon, Apr. 11, 14:30 p.m.

Where:	Room 402, Astronomy Building
	Welcome to Attend

	( PMO Academic Committee & Academic Circulating committee)

Abstract: SNR W51C is taken as a one-edge SNR next to two HII regions, W51A and W51B. However, the MHD simulation shows there should be another new edge overlapping with W51A (See Fig. 1). W51A is so luminous that the new edge cannot be detected directly. In fact, many years ago, some researchers found there are non-thermal emission toward W51A which should not generate non-thermal as a HII region. This problem lasts for many years. This MHD simulation brings the first light of solving the problem. The further analysis for the polarization data of Effelsberg 100 m radio telescope in Germany shows obvious polarization emission toward W51A, which is impossible for an HII region. However, a SNR can generate both of non-thermal emission and polarization emission. This result proves the prediction of MHD simulation and solve the difficult problem.

Zhang, Mengfei is a PhD candidate from National Astronomical Observatories of China. His main interests concern how the supernova remnants (SNRs) evolve in various surrounding environments and how the SNRs influence the whole Galactic interstellar medium (ISM). The former involves the morphology evolution of SNRs, the dust formation and destruction, the interaction with the ISM and the origin of cosmic rays. The latter is focused on the large-scale influence, such as the origin of local bubble, the Galactic diffuse electrons and the Galactic magnetic field. Zhang tries to improve the MHD simulations by analyzing the observation data to get more accurate initial conditions which is essential for a great MHD simulation.