Series of core collapse numerical simulations (SOLANUM) I: Modelling the early and late infall in a sun-like protostar
Abstract
Magnetohydrodynamical simulations and interferometric observations toward young stellar objects reveal the accretion of gas that may alter the physical properties and chemical composition of protostellar disks. Our goal is to constrain the physical history and properties of late infalling gas, and assess its potential to change the physical and chemical properties of the disk. We carried out a core collapse simulation of 5 M⊙ of gas endowed with tracer and sink particles during ∼ 3.6× 105 yr. We analyzed the properties of the rotationally supported disk, and the origin and physical history of the gas from which it is initially formed. We also selected the tracer particles that describe the late infall to analyze their origin and physical history, and compare them to the information obtained from the disk. The final mass of the sink reaches 1.02 M⊙, while the mass of the disk stays fairly constant around 0.02 M⊙. Throughout its evolution, the disk radius increases up to ∼ 40 au and its density is reduced by a factor of ∼ 8. Filaments that channel gas from the envelope to the disk and sink appear as a result of the magnetic interchange instability. Tracer particles can identify late infalling gas, whose physical properties resemble that of observed streamers and are only accreted in the final snapshots of the simulation. The origin and physical history of the late infalling gas are different from those of the gas that initially forms the disk. Core collapse simulations predict the appearance of filaments that connect the envelope to the disk. The late accretion of gas through these channels has properties similar to those of streamers and brings gas to the disk with a different physical history that could translate into a different chemical composition.
Related
- Series of core collapse numerical simulations (SOLANUM)
- Gravitational waves from core collapse of rotating very-massive stars: 3D numerical relativity computation
- Charged-current neutrino opacity within the relativistic Hartree-Fock framework for astrophysical simulations of core-collapse supernovae and binary neutron star mergers
- Three-dimensional Core-Collapse Supernova Simulations: From shell burning to shock revival
- It Takes Two: nucleosynthesis in core-collapse supernova simulations of binary-star progenitors
BibTeX
@misc{navarroalmaida2026series,
title = {{Series of core collapse numerical simulations (SOLANUM) I: Modelling the early and late infall in a sun-like protostar}},
author = {D. Navarro-Almaida and B. Commerçon and U. Lebreuilly and P. Hennebelle and A. Ahmad and A. Fuente and P. Rivière-Marichalar and J. E. Pineda},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.08376},
eprint = {2609.08376},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.08376},
}
RIS
TY - UNPB
TI - Series of core collapse numerical simulations (SOLANUM) I: Modelling the early and late infall in a sun-like protostar
AU - D. Navarro-Almaida
AU - B. Commerçon
AU - U. Lebreuilly
AU - P. Hennebelle
AU - A. Ahmad
AU - A. Fuente
AU - P. Rivière-Marichalar
AU - J. E. Pineda
PY - 2026
DA - 2026/09/08
PB - arXiv
DO - 10.48550/arxiv.2609.08376
UR - https://arxiv.org/abs/2609.08376
AB - Magnetohydrodynamical simulations and interferometric observations toward young stellar objects reveal the accretion of gas that may alter the physical properties and chemical composition of protostellar disks. Our goal is to constrain the physical history and properties of late infalling gas, and assess its potential to change the physical and chemical properties of the disk. We carried out a core collapse simulation of 5 M_⊙ of gas endowed with tracer and sink particles during ∼ 3.6× 10^5 yr. We analyzed the properties of the rotationally supported disk, and the origin and physical history of the gas from which it is initially formed. We also selected the tracer particles that describe the late infall to analyze their origin and physical history, and compare them to the information obtained from the disk. The final mass of the sink reaches 1.02 M_⊙, while the mass of the disk stays fairly constant around 0.02 M_⊙. Throughout its evolution, the disk radius increases up to ∼ 40 au and its density is reduced by a factor of ∼ 8. Filaments that channel gas from the envelope to the disk and sink appear as a result of the magnetic interchange instability. Tracer particles can identify late infalling gas, whose physical properties resemble that of observed streamers and are only accreted in the final snapshots of the simulation. The origin and physical history of the late infalling gas are different from those of the gas that initially forms the disk. Core collapse simulations predict the appearance of filaments that connect the envelope to the disk. The late accretion of gas through these channels has properties similar to those of streamers and brings gas to the disk with a different physical history that could translate into a different chemical composition.
ER -