“Atlas” of numerical solutions for star-disk magnetospheric interaction. (arXiv:1811.02808v1 [astro-ph.SR])

<a href="http://arxiv.org/find/astro-ph/1/au:+Cemeljic_M/0/1/0/all/0/1">Miljenko Čemeljić</a>

Aims: I report results in numerical simulations of star-disk magnetospheric

interaction. A thin accretion disk with corona above a rotating stellar surface

is simulated in a parameter study, to find trends in the angular momentum flux.

The results are presented in the case of Young Stellar Objects, but they can be

rescaled to other objects with similar geometry.

Methods: In the performed resistive and viscous magneto-hydrodynamic

simulations, a quasi-stationary state is reached in the cases with different

parameters. Angular momentum fluxes in the different components of the flow are

computed, to compare the results.

Results: Results in the simulations are presented with the matter density

distribution and magnetic field geometry displayed in an `Atlas’ of solutions.

The torque exerted on the star is computed, together with the angular momentum

flux loaded into outflow, in the cases when a conical outflow is formed. In the

studied part of the parameter space, I find trends in both components of the

flow.

Aims: I report results in numerical simulations of star-disk magnetospheric

interaction. A thin accretion disk with corona above a rotating stellar surface

is simulated in a parameter study, to find trends in the angular momentum flux.

The results are presented in the case of Young Stellar Objects, but they can be

rescaled to other objects with similar geometry.

Methods: In the performed resistive and viscous magneto-hydrodynamic

simulations, a quasi-stationary state is reached in the cases with different

parameters. Angular momentum fluxes in the different components of the flow are

computed, to compare the results.

Results: Results in the simulations are presented with the matter density

distribution and magnetic field geometry displayed in an `Atlas’ of solutions.

The torque exerted on the star is computed, together with the angular momentum

flux loaded into outflow, in the cases when a conical outflow is formed. In the

studied part of the parameter space, I find trends in both components of the

flow.

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