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- W3010147415 abstract "Abstract In star-forming environments, shock-compressed magnetic fields occur in cloud-cloud collisions, in molecular clouds exposed to supernova remnants (SNRs), and in photo-dissociation regions (PDRs). Besides their dynamical role, they increase the cosmic ray flux above the Galactic average, and the trapped particles contribute to the heating of the shocked gas. The associated dust emission is polarized perpendicularly to the sky plane projection of the field, B sky . In edge-on viewed shock planes, highly ordered polarization patterns are expected. In search of such a signature, the dust emission from the Orion bar (a prototypical PDR) and from a molecular cloud/SNR interface (IC443-G) was studied with a λ870μm polarimeter at the APEX (Wiesemeyer etal 2014 and references therein). While our polarization map of OMC1 confirms the hourglass shape of B sky (e.g., Schleuning 1998, Houde etal 2004), a deep integration towards the Orion bar reveals an alignment of B sky with the shock forming in response to the wind and to the ionizing radiation from the Trapezium cluster (Fig. 1). This structure suggests a compressed magnetic field accelerating cosmic-ray particles, a scenario proposed by [Pellegrini et al. (2009)] to explain the high excitation temperature of rotationally warm H 2 and CO (Shaw et al. 2009, Peng et al. 2012, respectively)." @default.
- W3010147415 created "2020-03-13" @default.
- W3010147415 creator A5047502490 @default.
- W3010147415 date "2018-08-01" @default.
- W3010147415 modified "2023-09-24" @default.
- W3010147415 title "Signposts of shock-induced magnetic field compression in star-forming environments" @default.
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- W3010147415 doi "https://doi.org/10.1017/s174392131900365x" @default.
- W3010147415 hasPublicationYear "2018" @default.
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