Vortical Amplification of the Magnetic Field at an Inward Shock of Supernova Remnant Cassiopeia A
AffiliationUniv Arizona, Dept Planetary Sci
Univ Arizona, Dept Astron
MetadataShow full item record
PublisherAMER PHYSICAL SOC
CitationFraschetti, F., Katsuda, S., Sato, T., Jokipii, J. R., & Giacalone, J. (2018). Vortical Amplification of the Magnetic Field at an Inward Shock of Supernova Remnant Cassiopeia A. Physical Review Letters, 120(25), 251101. https://doi.org/10.1103/PhysRevLett.120.251101
JournalPHYSICAL REVIEW LETTERS
Rights© 2018 American Physical Society.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at firstname.lastname@example.org.
AbstractWe present an interpretation of the time variability of the x-ray flux recently reported from a multiepoch campaign of 15 years of observations of the supernova remnant Cassiopeia A by Chandra. We show for the first time quantitatively that the [4.2-6] keV nonthermal flux increase up to 50% traces the growth of the magnetic field due to a vortical amplification mechanism at a reflection inward shock colliding with inner overdensities. The fast synchrotron cooling as compared with shock-acceleration time scale qualitatively supports the flux decrease.
VersionFinal published version
SponsorsNASA [NNX15AJ71G]; Smithsonian Institution Scholarly Studies [40488100HH00181]; Japan Society for the Promotion of Science KAKENHI [16K17673, 17H02864]; Leading Initiative for Excellent Young Researchers, MEXT, Japan; Special Postdoctoral Researchers Program in RIKEN