Characterizing Magnetic Field Morphologies in Three Serpens Protostellar Cores with ALMA
Le Gouellec, Valentin J. M. (Université Paris-Saclay. Université Paris Diderot)
Hull, Charles L. H. (Joint ALMA Observatory)
Maury, Anaëlle J. (Université Paris-Saclay. Université Paris Diderot)
Girart, Josep Miquel (Institut de Ciències de l'Espai)
Tychoniec, Łukasz (Leiden University)
Kristensen, Lars E. (University of Copenhagen. Centre for Star and Planet Formation)
Li, Zhi Yun (Department of Astronomy. University of Virginia)
Louvet, Fabien (Universidad de Chile. Departamento de Astronomía)
Cortes, Paulo (National Radio Astronomy Observatory)
Rao, Ramprasad (Academia Sinica (Taiwan). Institute of Astronomy and Astrophysics)

Fecha:	2019
Resumen:	With the aim of characterizing the dynamical processes involved in the formation of young protostars, we present high-angular-resolution ALMA dust polarization observations of the Class 0 protostellar cores Serpens SMM1, Emb 8(N), and Emb 8. With spatial resolutions ranging from 150 to 40 au at 870 μm, we find unexpectedly high values of the polarization fraction along the outflow cavity walls in Serpens Emb 8(N). We use 3 mm and 1 mm molecular tracers to investigate outflow and dense-gas properties and their correlation with the polarization. These observations allow us to investigate the physical processes involved in the radiative alignment torques (RATs) acting on dust grains along the outflow cavity walls, which experience irradiation from accretion processes and outflow shocks. The inner core of SMM1-a presents a polarization pattern with a poloidal magnetic field at the bases of the two lobes of the bipolar outflow. To the south of SMM1-a we see two polarized filaments, one of which seems to trace the redshifted outflow cavity wall. The other may be an accretion streamer of material infalling onto the central protostar. We propose that the polarized emission we see at millimeter wavelengths along the irradiated cavity walls can be reconciled with the expectations of RAT theory if the aligned grains present at <500 au scales in Class 0 envelopes have grown larger than the 0. 1 μm size of dust grains in the interstellar medium. Our observations allow us to constrain the magnetic field morphologies of star-forming sources within the central cores, along the outflow cavity walls, and in possible accretion streamers.
Ayudas:	European Commission 679937 Ministerio de Economía y Competitividad AYA2017-84390-C2-R
Derechos:	Aquest document està subjecte a una llicència d'ús Creative Commons. Es permet la reproducció total o parcial, la distribució, la comunicació pública de l'obra i la creació d'obres derivades, fins i tot amb finalitats comercials, sempre i quan es reconegui l'autoria de l'obra original.
Lengua:	Anglès
Documento:	Article ; recerca ; Versió publicada
Materia:	ISM: jets and outflows ; ISM: magnetic fields ; Polarization ; Radiation mechanisms: thermal ; Stars:protostars
Publicado en:	The Astrophysical journal, Vol. 885, Núm. 2 (November 2019) , p. 106, ISSN 1538-4357

DOI: 10.3847/1538-4357/ab43c2

24 p, 8.8 MB

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