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Snapshot of a magnetohydrodynamic disk wind traced with water masers

Published online by Cambridge University Press:  07 February 2024

Luca Moscadelli Open the ORCID record for Luca Moscadelli [Opens in a new window] ,
Alberto Sanna Open the ORCID record for Alberto Sanna [Opens in a new window] ,
Henrik Beuther ,
André Oliva Open the ORCID record for André Oliva [Opens in a new window]  and
Rolf Kuiper Open the ORCID record for Rolf Kuiper [Opens in a new window]
Luca Moscadelli*
Affiliation:
INAF-Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, Firenze 50125, Italy.
Alberto Sanna
Affiliation:
INAF-Osservatorio Astronomico di Cagliari, Via della Scienza 5, Selargius (CA) 09047, Italy Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, Bonn 53121, Germany
Henrik Beuther
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, Heidelberg 69117, Germany
André Oliva
Affiliation:
Institut für Astronomie und Astrophysik, Auf der Morgenstelle 10, Tübingen 72076, Germany Space Research Center (CINESPA), Ciudad Universitaria Rodrigo Facio, San José 11501, Costa Rica
Rolf Kuiper
Affiliation:
Faculty of Physics, University of Duisburg-Essen, Lotharstraße 1, Duisburg 47057, Germany
*
email: luca.moscadelli@inaf.it
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Abstract

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Disk-jet systems are common in astrophysical sources of different nature, from black holes to gaseous giant planets. The disk drives the mass accretion onto a central compact object and the jet ejects material along the disk rotation axis. Magnetohydrodynamic disk winds can provide the link between mass accretion and ejection, which is essential to ensure that the excess angular momentum is removed and accretion can proceed. However, up to now, we have been lacking direct observational proof of disk winds. This work presents a direct view of the velocity field of a disk wind around a forming massive star. Achieving a very high spatial resolution of 0.05 au, our water maser observations trace the velocities of individual streamlines emerging from the disk orbiting the forming star. We find that, at low elevation above the disk midplane, the flow co-rotates with its launch point in the disk, in agreement with magneto-centrifugal acceleration. Beyond the co-rotation point, the flow rises spiraling around the disk rotation axis along a helical magnetic field. We have performed (resistive-radiative-gravito-) magnetohydrodynamic simulations of the formation of a massive star and record the development of a magneto-centrifugally launched jet presenting many properties in agreement with our observations.

Keywords

ISM: jets and outflowsISM: kinematics and dynamicsStars: formationMasers
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S380: Cosmic Masers: Proper Motion toward the Next-Generation Large Projects , December 2022 , pp. 167 - 171
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

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