FRB 180916B的RM也变化剧烈

FRB 180916B的RM也变化剧烈

arXiv:2205.09221 [pdf]

A Large Scale Magneto-ionic Fluctuation in the Local Environment of Periodic Fast Radio Burst Source, FRB 20180916B

R. Mckinven, B.M. Gaensler, D. Michilli, K. Masui, V.M. Kaspi, M. Bhardwaj, T. Cassanelli, P. Chawla, F. (Adam) Dong, E. Fonseca, C. Leung, D.Z. Li, C. Ng, C. Patel, E. Petroff, A.B. Pearlman, M. Rafiei-Ravandi, M. Rahman, K.R. Sand, K. Shin, P. Scholz, I.H. Stairs, K. Smith, J. Su, S. Tendulkar

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

Fast radio burst (FRB) source 20180916B exhibits a 16.33-day periodicity in its burst activity. It is as of yet unclear what proposed mechanism produces the activity, but polarization information is a key diagnostic. Here, we report on the polarization properties of 44 bursts from FRB 20180916B detected between 2018 December and 2021 December by CHIME/FRB, the FRB project on the Canadian Hydrogen Intensity Mapping Experiment the Canadian Hydrogen Intensity Mapping Experiment. In contrast to previous observations, we find significant variations in the Faraday rotation measure (RM) of FRB 20180916B. Over the nine month period 2021 April−2021 December we observe an apparent secular increase in RM of ∼50radm−2 (a fractional change of over 40%) that is accompanied by a possible drift of the emitting band to lower frequencies. This interval displays very little variation in the dispersion measure (ΔDM≲0.8pccm−3) which indicates that the observed RM evolution is likely produced from coherent changes in the Faraday-active medium's magnetic field. Burst-to-burst RM variations appear unrelated to the activity cycle phase. The degree of linear polarization of our burst sample (≳80%) is consistent with the negligible depolarization expected for this source in the 400-800 MHz bandpass of CHIME. FRB 20180916B joins other repeating FRBs in displaying substantial RM variations between bursts. This is consistent with the notion that repeater progenitors may be associated with young stellar populations by their preferential occupation of dynamic magnetized environments commonly found in supernova remnants, pulsar wind nebulae or near high mass stellar companions.

来源： https://arxiv.org/list/astro-ph/new

和别的重复暴一样， RM变化剧烈， DM没怎么变。

右上角有个看起来很明显的RM的演化。

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