3D simulations of magnetospheric accretion in T Tauri stars: I. Disk truncation, stellar torques, and application to observations
Abstract
Young stars accrete material from their circumstellar disk through their magnetosphere and undergo contraction; these two processes impact their rotational evolution. We investigate stable and unstable accretion regimes (due to the interchange instability) and examine the associated stellar torques to assess the spin evolution of young stars. We performed 3D MHD simulations of disk accretion onto an inclined stellar dipole. We ran 21 simulations with varying stellar rotation rates, dipole field strengths and obliquities, and mass accretion rates. We find that stars with a ratio of truncation to corotation radius Rt/Rco ≳ 0.80−0.85 accrete via a stable regime, while accretion becomes unstable otherwise. In addition, our Rt/R∗ parametrization weakly depends on the mass accretion rate and the dipolar intensity, while strongly depending on the stellar rotation rate. We derive torque formulae for each flow component affecting the stellar rotation, i.e., accretion, magnetospheric ejections and stellar winds. Finally, we apply our results to a sample of young stars with measured magnetic fields, mass accretion rates, and rotational periods and find that most of them should currently accrete in an unstable regime and undergo spin-up torques. Our study confirms and expands upon previous results. Unstable accretion should lead to a net spin-up torque on the central star, while stable accretion can lead to stellar spin-down. When applying our truncation radius and torque prescriptions to observational data, we find that most young stars in our sample should be in a spin-up state. Thus, the angular momentum problem for young stars remains.
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BibTeX
@misc{pantolmos2026simulations,
title = {{3D simulations of magnetospheric accretion in T Tauri stars: I. Disk truncation, stellar torques, and application to observations}},
author = {George Pantolmos and Claudio Zanni and Jérôme Bouvier},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2608.17869},
eprint = {2608.17869},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2608.17869},
}
RIS
TY - UNPB
TI - 3D simulations of magnetospheric accretion in T Tauri stars: I. Disk truncation, stellar torques, and application to observations
AU - George Pantolmos
AU - Claudio Zanni
AU - Jérôme Bouvier
PY - 2026
DA - 2026/10/05
PB - arXiv
DO - 10.48550/arxiv.2608.17869
UR - https://arxiv.org/abs/2608.17869
AB - Young stars accrete material from their circumstellar disk through their magnetosphere and undergo contraction; these two processes impact their rotational evolution. We investigate stable and unstable accretion regimes (due to the interchange instability) and examine the associated stellar torques to assess the spin evolution of young stars. We performed 3D MHD simulations of disk accretion onto an inclined stellar dipole. We ran 21 simulations with varying stellar rotation rates, dipole field strengths and obliquities, and mass accretion rates. We find that stars with a ratio of truncation to corotation radius R_t/R_co ≳ 0.80−0.85 accrete via a stable regime, while accretion becomes unstable otherwise. In addition, our R_t/R_∗ parametrization weakly depends on the mass accretion rate and the dipolar intensity, while strongly depending on the stellar rotation rate. We derive torque formulae for each flow component affecting the stellar rotation, i.e., accretion, magnetospheric ejections and stellar winds. Finally, we apply our results to a sample of young stars with measured magnetic fields, mass accretion rates, and rotational periods and find that most of them should currently accrete in an unstable regime and undergo spin-up torques. Our study confirms and expands upon previous results. Unstable accretion should lead to a net spin-up torque on the central star, while stable accretion can lead to stellar spin-down. When applying our truncation radius and torque prescriptions to observational data, we find that most young stars in our sample should be in a spin-up state. Thus, the angular momentum problem for young stars remains.
ER -