Accretion disks in luminous young stellar objects
MT Beltrán, WJ de Wit - The Astronomy and Astrophysics Review, 2016 - Springer
An observational review is provided of the properties of accretion disks around young stars.
It concerns the primordial disks of intermediate-and high-mass young stellar objects in …
It concerns the primordial disks of intermediate-and high-mass young stellar objects in …
The role of magnetic fields in protostellar outflows and star formation
RE Pudritz, TP Ray - Frontiers in Astronomy and Space Sciences, 2019 - frontiersin.org
The role of outflows in the formation of stars and the protostellar disks that generate them is
a central question in astrophysics. Outflows are associated with star formation across the …
a central question in astrophysics. Outflows are associated with star formation across the …
A rotating protostellar jet launched from the innermost disk of HH 212
CF Lee, PTP Ho, ZY Li, N Hirano, Q Zhang… - Nature Astronomy, 2017 - nature.com
The central problem in forming a star is the angular momentum in the circumstellar disk,
which prevents material from falling into the central stellar core. An attractive solution to the …
which prevents material from falling into the central stellar core. An attractive solution to the …
Collapse of turbulent massive cores with ambipolar diffusion and hybrid radiative transfer-I. Accretion and multiplicity
R Mignon-Risse, M González, B Commerçon… - Astronomy & …, 2021 - aanda.org
Context. Massive stars form in magnetized and turbulent environments and are often located
in stellar clusters. The accretion and outflows mechanisms associated with forming massive …
in stellar clusters. The accretion and outflows mechanisms associated with forming massive …
ALMA discovery of a rotating SO/SO2 flow in HH212-A possible MHD disk wind?
B Tabone, S Cabrit, E Bianchi, J Ferreira… - Astronomy & …, 2017 - aanda.org
We wish to constrain the possible contribution of a magnetohydrodynamic disk wind (DW) to
the HH212 molecular jet. We mapped the flow base with ALMA Cycle 4 at 0. ̋13~ 60 au …
the HH212 molecular jet. We mapped the flow base with ALMA Cycle 4 at 0. ̋13~ 60 au …
Snapshot of a magnetohydrodynamic disk wind traced by water maser observations
L Moscadelli, A Sanna, H Beuther, A Oliva… - Nature Astronomy, 2022 - nature.com
The formation of astrophysical objects of different nature, from black holes to gaseous giant
planets, involves a disk–jet system, where the disk drives the mass accretion onto a central …
planets, involves a disk–jet system, where the disk drives the mass accretion onto a central …
Formation and evolution of disks around young stellar objects
Recent observations have suggested that circumstellar disks may commonly form around
young stellar objects. Although the formation of circumstellar disks can be a natural result of …
young stellar objects. Although the formation of circumstellar disks can be a natural result of …
The ALMA view of the OMC1 explosion in orion
J Bally, A Ginsburg, H Arce, J Eisner… - The Astrophysical …, 2017 - iopscience.iop.org
Most massive stars form in dense clusters where gravitational interactions with other stars
may be common. The two nearest forming massive stars, the BN object and Source I …
may be common. The two nearest forming massive stars, the BN object and Source I …
Disk-driven rotating bipolar outflow in Orion Source I
T Hirota, MN Machida, Y Matsushita, K Motogi… - Nature …, 2017 - nature.com
One of the outstanding problems in star formation theory concerns the transfer of angular
momentum so that mass can accrete onto a newly born young stellar object (YSO). From a …
momentum so that mass can accrete onto a newly born young stellar object (YSO). From a …
A Keplerian disk around Orion SrCI, a∼ 15 M⊙ YSO
A Ginsburg, J Bally, C Goddi, R Plambeck… - The Astrophysical …, 2018 - iopscience.iop.org
We report ALMA long-baseline observations of Orion Source I (SrcI), with a resolution 0 farcs
03–0 farcs 06 (12–24 au) at 1.3 and 3.2 mm. We detect both continuum and spectral line …
03–0 farcs 06 (12–24 au) at 1.3 and 3.2 mm. We detect both continuum and spectral line …