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Kinematics around t...
Kinematics around the B335 protostar down to au scales
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- Bjerkeli, Per, 1977 (author)
- Chalmers tekniska högskola,Chalmers University of Technology
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- Ramsey, Jon P (author)
- University of Virginia,Niels Bohr Institute
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- Harsono, Daniel (author)
- Universiteit Leiden (UL),Leiden University (UL)
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- Calcutt, Hannah, 1988 (author)
- Chalmers tekniska högskola,Chalmers University of Technology
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- Kristensen, L. E. (author)
- Niels Bohr Institute
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- van der Wiel, M. H. D. (author)
- Netherlands Institute for Radio Astronomy (ASTRON)
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- Jorgensen, Jes K. (author)
- Niels Bohr Institute
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- Muller, Sebastien, 1976 (author)
- Chalmers tekniska högskola,Chalmers University of Technology
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- Persson, Magnus V., 1983 (author)
- Chalmers tekniska högskola,Chalmers University of Technology
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(creator_code:org_t)
- 2019-10-22
- 2019
- English.
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In: Astronomy and Astrophysics. - : EDP Sciences. - 0004-6361 .- 1432-0746. ; 631
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Abstract
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- Context. The relationship between outflow launching and formation of accretion disks around young stellar objects is still not entirely understood, which is why spectrally and spatially resolved observations are needed. Recently, the Atacama Large Millimetre/sub-millimetre Array (ALMA) has carried out long-baseline observations towards a handful of sources, revealing connections between outflows and the inner regions of disks. Aims. Here we aim to determine the small-scale kinematic and morphological properties of the outflow from the isolated protostar B335 for which no Keplerian disk has, so far, been observed on scales down to 10 au. Methods. We use ALMA in its longest-baseline configuration to observe emission from CO isotopologs, SiO, SO$_2$ and CH$_3$OH. The proximity of B335 provides a resolution of ~3 au (0.03''). We also combine our long-baseline data with archival data to produce a high-fidelity image covering scales up to 700 au (7''). Results. $^{12}$CO has a X-shaped morphology with arms ~50 au in width that we associate with the walls of an outflow cavity, similar to what is observed on larger scales. Long-baseline continuum emission is confined to <7 au of the protostar, while short-baseline continuum emission follows the $^{12}$CO outflow and cavity walls. Methanol is detected within ~30 au of the protostar. SiO is also detected in the vicinity of the protostar, but extended along the outflow. Conclusions. The $^{12}$CO outflow shows no clear signs of rotation at distances $\gtrsim$30 au from the protostar. SiO traces the protostellar jet on small scales, but without obvious rotation. CH$_3$OH and SO$_2$ trace a region <16 au in diameter, centred on the continuum peak, which is clearly rotating. Using episodic, high-velocity, $^{12}$CO features, we estimate the launching radius of the outflow to be <0.1 au and dynamical timescales on the order of a few years.
Subject headings
- NATURVETENSKAP -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
- NATURAL SCIENCES -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)
Keyword
- jets and outflows
- formation
- ism
- accretion disks
- stars
- accretion
- protostars
Publication and Content Type
- art (subject category)
- ref (subject category)
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Bjerkeli, Per, 1 ...
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Ramsey, Jon P
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Harsono, Daniel
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Calcutt, Hannah, ...
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Kristensen, L. E ...
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van der Wiel, M. ...
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show more...
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Jorgensen, Jes K ...
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Muller, Sebastie ...
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Persson, Magnus ...
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- NATURAL SCIENCES
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NATURAL SCIENCES
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and Physical Science ...
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and Astronomy Astrop ...
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Chalmers University of Technology