Constraining Stellar Winds of Young Sun-like Stars

@article{Johnstone2013ConstrainingSW,
  title={Constraining Stellar Winds of Young Sun-like Stars},
  author={Colin P. Johnstone and Theresa L{\"u}ftinger and Manuel G{\"u}del and Bibiana Fichtinger},
  journal={Proceedings of the International Astronomical Union},
  year={2013},
  volume={9},
  pages={243 - 244}
}
Abstract As part of the project Pathways to Habitability (http://path.univie.ac.at/), we study the properties of the stellar winds of low-mass and Sun-like stars, and their influences on the atmospheres of potentially habitable planets. For this purpose, we combine mapping of stellar magnetic fields with magnetohydrodynamic wind models. 

References

SHOWING 1-6 OF 6 REFERENCES
Accretion-powered Stellar Winds. II. Numerical Solutions for Stellar Wind Torques
In order to explain the slow rotation observed in a large fraction of accreting pre-main-sequence stars (CTTSs), we explore the role of stellar winds in torquing down the stars. For this mechanism to
THREE-DIMENSIONAL NUMERICAL SIMULATIONS OF MAGNETIZED WINDS OF SOLAR-LIKE STARS
By means of self-consistent three-dimensional magnetohydrodynamics (MHD) numerical simulations, we analyze magnetized solar-like stellar winds and their dependence on the plasma-{beta} parameter (the
An empirical determination of the polytropic index for the free‐streaming solar wind using Helios 1 data
Observations of solar wind proton temperatures indicate that the solar wind is heated as it moves outward toward the orbit of Earth. This heating, which may be the result of electron heat conduction
Doppler Imaging of stellar magnetic fields. I. Techniques
We present an investigation of the magnetic field geometries and inhomogeneous distribution of chemical elements in the atmospheres of peculiar A and B stars. Our study combines high-quality
Self-gravitational adaptive mesh magnetohydrodynamics with the NIRVANA code
TLDR
An overview of the basic numerical ideas standing behind NIRVANA is given and the code is applied to the problem of protostellar core collaps and fragmentation.
Dynamics of the Interplanetary Gas and Magnetic Fields