7-14The defining observational characteristics of AM Her polars are their intense polarization. One specifies their magnetic fields from the measured polarizations. Here, the relationship between polarization and the properties of the magnetic field for time-dependent oscillating shocks is investigated. The properties of the polarization on time scales large compared to the oscillation period are discussed
Local time dependence of polarization of geomagnetic sudden commencements (SC\u27s) at geostationary...
Context. We investigate the linear polarization produced by interstellar dust aligned by the magneti...
Context. Massive star winds are complex radiation-hydrodynamic (sometimes magnetohydrodynamic) outfl...
Aims: This paper extends previous studies in modeling time varying linear polarization due to axisym...
Aims. This paper extends previous studies in modeling time varying linear polarization due to axisy...
Context. Strong, globally-organized magnetic fields are found for a small fraction of O, B, and A st...
[[sponsorship]]天文及天文物理研究所[[note]]已出版;[SCI];有審查制度;具代表性[[note]]http://gateway.isiknowledge.com/gateway...
Magnetic fields can be found at the surface of non-degenerate stars all over the HR diagram. Their n...
Everything started back in 1978, with the discovery by McLean & Coyne of hydrogen emission line...
Context. Efforts to compare polarization measurements with synthetic observations from magnetohydrod...
International audienceZeeman-Doppler imaging (ZDI) has successfully mapped the large-scale magnetic ...
Context.Clumping in the winds of massive stars may significantly reduce empirical mass-loss rates, a...
Massive star winds are complex radiation-hydrodynamic (sometimes magnetohydrodynamic) outflows that ...
Local time dependence of polarization of geomagnetic sudden commencements (SC\u27s) at geostationary...
Context. We investigate the linear polarization produced by interstellar dust aligned by the magneti...
Context. Massive star winds are complex radiation-hydrodynamic (sometimes magnetohydrodynamic) outfl...
Aims: This paper extends previous studies in modeling time varying linear polarization due to axisym...
Aims. This paper extends previous studies in modeling time varying linear polarization due to axisy...
Context. Strong, globally-organized magnetic fields are found for a small fraction of O, B, and A st...
[[sponsorship]]天文及天文物理研究所[[note]]已出版;[SCI];有審查制度;具代表性[[note]]http://gateway.isiknowledge.com/gateway...
Magnetic fields can be found at the surface of non-degenerate stars all over the HR diagram. Their n...
Everything started back in 1978, with the discovery by McLean & Coyne of hydrogen emission line...
Context. Efforts to compare polarization measurements with synthetic observations from magnetohydrod...
International audienceZeeman-Doppler imaging (ZDI) has successfully mapped the large-scale magnetic ...
Context.Clumping in the winds of massive stars may significantly reduce empirical mass-loss rates, a...
Massive star winds are complex radiation-hydrodynamic (sometimes magnetohydrodynamic) outflows that ...
Local time dependence of polarization of geomagnetic sudden commencements (SC\u27s) at geostationary...
Context. We investigate the linear polarization produced by interstellar dust aligned by the magneti...
Context. Massive star winds are complex radiation-hydrodynamic (sometimes magnetohydrodynamic) outfl...