Formation and evolution of protostellar accretion discs – II. From 3D simulation to a simple semi-analytic model of Class 0/I discs

@article{Xu2021FormationAE,
  title={Formation and evolution of protostellar accretion discs – II. From 3D simulation to a simple semi-analytic model of Class 0/I discs},
  author={Wenrui Xu and Matthew W. Kunz},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2021}
}
  • Wenrui Xu, M. Kunz
  • Published 15 September 2021
  • Physics
  • Monthly Notices of the Royal Astronomical Society
We use a 3D radiative non-ideal magnetohydrodynamic simulation to investigate the formation and evolution of a young protostellar disc from a magnetized pre-stellar core. The simulation covers the first ${\sim }10\, {\rm kyr}$ after protostar formation and shows a massive, weakly magnetized disc with radius that initially grows and then saturates at ${\sim }30\, {\rm au}$. The disc is gravitationally unstable with prominent large-amplitude spiral arms. We use our simulation results and a… Expand

References

SHOWING 1-10 OF 53 REFERENCES
Self‐regulated gravitational accretion in protostellar discs
We present a numerical model for the evolution of a protostellar disc that has formed self-consistently from the collapse of a molecular cloud core. The global evolution of the disc is followed forExpand
The role of disc self-gravity in the formation of protostars and protostellar discs
We use time-dependent, one-dimensional disc models to investigate the evolution of protostellar discs that form through the collapse of molecular cloud cores and in which the primary transportExpand
What determines the formation and characteristics of protoplanetary discs?
Planets form in protoplanetary discs. Their masses, distribution, and orbits sensitively depend on the structure of the protoplanetary discs. However, what sets the initial structure of the discs inExpand
The Mass Evolution of Protostellar Disks and Envelopes in the Perseus Molecular Cloud
In the standard picture for low-mass star formation, a dense molecular cloud undergoes gravitational collapse to form a protostellar system consisting of a new central star, a circumstellar disk, andExpand
Long-term evolution of protostellar and protoplanetary disks. I. Outbursts
As an initial investigation into the long-term evolution of protostellar disks, we explore the conditions required to explain the large outbursts of disk accretion seen in some young stellar objects.Expand
Decoupling of magnetic fields in collapsing protostellar envelopes and disc formation and fragmentation
Efficient magnetic braking is a formidable obstacle to the formation of rotationally supported disks (RSDs) around protostars in magnetized dense cores. We have previously shown, through 2DExpand
Gravitational Instabilities in Circumstellar Disks
[Abridged] Star and planet formation are the complex outcomes of gravitational collapse and angular momentum transport mediated by protostellar and protoplanetary disks. In this review we focus onExpand
The First Two Thousand Years of Star Formation
Starting from a prestellar core with a size of $1.2\times10^4$ AU, we calculate the evolution of a gravitationally collapsing core until $\sim2000$ yr after protostar formation using aExpand
Different modes of star formation – II. Gas accretion phase of initially subcritical star-forming clouds
The accretion phase of star formation is investigated in magnetically-dominated clouds that have an initial subcritical mass-to-flux ratio. We employ nonideal magnetohydrodynamic simulations thatExpand
Disc formation and fragmentation using radiative non-ideal magnetohydrodynamics
We investigate the formation and fragmentation of discs using a suite of three-dimensional smoothed particle radiative magnetohydrodynamics simulations. Our models are initialised as 1M$_\odot$Expand
...
1
2
3
4
5
...