Polytropic wind solutions via the Complex Plane Strategy

@article{Karageorgopoulos2021PolytropicWS,
  title={Polytropic wind solutions via the Complex Plane Strategy},
  author={Vasileios Karageorgopoulos and Konstantinos N. Gourgouliatos and Vassilis Geroyannis},
  journal={Astron. Comput.},
  year={2021},
  volume={36},
  pages={100491}
}

Figures from this paper

References

SHOWING 1-10 OF 50 REFERENCES
Numerical simulations of stellar winds: polytropic models
We discuss steady-state transonic outflows obtained by direct numerical solution of the hydrodynamic and magneto- hydrodynamic equations. We make use of the Versatile Advec- tion Code, a software
On the solution topologies of polytropic winds
We study steady polytropic wind flows by examining their solution topologies; effects included are departures from spherical symmetry and nonthermal momentum addition (such as by waves). The problem
Parker Winds Revisited: An Extension to Disk Winds
A simple 1D dynamical model of thermally driven disc winds is proposed, based on the results of recent, 2.5D axi-symmetric simulations. Our formulation of the disc wind problem is in the spirit of
Anisotropic winds from close-in extrasolar planets
We present two-dimensional hydrodynamic models of thermally driven winds from highly irradiated, close-in extrasolar planets. We adopt a very simple treatment of the radiative heating processes at
Multiple transonic solutions with a new class of shock transitions in steady isothermal solar and stellar winds
A new class of shock transitions are shown to arise in the transonic solutions of the steady isothermal solar wind equations when, for example, momentum deposition gives rise to multiple critical
Relativistic Parker winds with variable effective polytropic index
Spherically symmetric hydrodynamical outflows accelerated thermally in the vicinity of a compact object are studied by generalizing an equation of state with a variable effective polytropic index,
Dynamical properties of stellar coronas and stellar winds. i - integration of the momentum equation.
The hydrodynamic momentum and mass flow equations are integrated for a stellar corona with spherical symmetry about the center of the star. The coronal temperature is taken to be a known function
Numerical Treatment Of Hartle'S Perturbation Method For Differentially Rotating Neutron Stars Simulated By General-Relativistic Polytropic Models
We compute general-relativistic polytropic models of differentially rotating neutron stars. A brief description of our numerical treatment is given as follows. First, the relativistic
New predictions for radiation-driven, steady-state mass-loss and wind-momentum from hot, massive stars
Context. Radiation-driven mass loss plays a key role in the life cycles of massive stars. However, basic predictions of such mass loss still suffer from significant quantitative uncertainties. Aims.
Stellar wind regimes of close-in extrasolar planets
Close-in extrasolar planets of Sun-like stars are exposed to stellar wind conditions that differ considerably from those for planets in the solar system. Unfortunately, these stellar winds belong to
...
1
2
3
4
5
...