Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 443, Issue 1, Pages 547-558Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stu1082
Keywords
instabilities; MHD; relativistic processes; shock waves; pulsars: general; pulsars: individual: Crab; ISM: supernova remnants
Categories
Funding
- STFC [ST/I001816/1]
- NASA [NNX13AC59G]
- FWO-Vlaanderen [G.0238.12]
- EC [263340]
- Belgian Space Science Policy Office [IAP P7/08 CHARM]
- NASA [476395, NNX13AC59G] Funding Source: Federal RePORTER
- Science and Technology Facilities Council [ST/I001816/1, ST/K000853/1] Funding Source: researchfish
- STFC [ST/K000853/1, ST/I001816/1] Funding Source: UKRI
Ask authors/readers for more resources
In this paper, we discuss the development of Rayleigh-Taylor (RT) filaments in axisymmetric simulations of pulsar wind nebulae (PWN). High-resolution adaptive mesh refinement magnetohydrodynamic simulations are used to resolve the non-linear evolution of the instability. The typical separation of filaments is mediated by the turbulent flow in the nebula and hierarchical growth of the filaments. The strong magnetic dissipation and field randomization found in recent global three-dimensional simulations of PWN suggest that magnetic tension is not strong enough to suppress the growth of RT filaments, in agreement with the observations of prominent filaments in the Crab nebula. The long-term axisymmetric results presented here confirm this finding.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available