English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We use the POLARIS radiative transport code to generate predictions of thetwo main observables directly sensitive to the magnetic field morphology andstrength in filaments: dust polarization and gas Zeeman line splitting. Wesimulate generic gas filaments with power-law density profiles assuming twodensity-field strength dependencies, six different filament inclinations, andnine distinct magnetic field morphologies, including helical, toroidal, andwarped magnetic field geometries. We present idealized spatially resolved dustpolarization and Zeeman-derived field strengths and directions maps. Under theassumption that dust grains are aligned by radiative torques (RATs), dustpolarization traces the projected plane-of-the-sky magnetic field morphology.Zeeman line splitting delivers simultaneously the intensity-weightedline-of-sight field strength and direction. We show that linear dustpolarization alone is unable to uniquely constrain the 3D field morphology. Wedemonstrate that these ambiguities are ameliorated or resolved with theaddition of the Zeeman directional information. Thus, observations of both thedust polarization and Zeeman splitting together provide the most promisingmeans for obtaining constraints of the 3D magnetic field configuration. We findthat the Zeeman-derived field strengths are at least a factor of a few belowthe input field strengths due to line-of-sight averaging through the filamentdensity gradient. Future observations of both dust polarization and Zeemansplitting are essential for gaining insights into the role of magnetic fieldsin star and cluster forming filaments.

Magnetic fields in star forming systems (I): Idealized synthetic signatures of dust polarization and Zeeman splitting in filaments