Add to ORKGThe theoretical power spectrum of solar velocity field and flux variation is obtained with amplitudes of the unstable convective eigenmodes determined by linearly superposing these modes to yield the model convective flux profile. The numerical results are compared with the observed spectrum of solar convection and the technique is applied to other stars
. The convection in stellar atmospheres cause spectral lines to be more or less blue-shifted. The di...
International audienceWe discuss how the possibility to measure mode excitation rates through means ...
Hydrodynamical, 3D simulations of the outer layers of the Sun and α Cen A are used to obtain constra...
In spite of many attempts to solve the problem of convection in stellar atmospheres our present know...
[[abstract]]The properties of convective motions on the sun are studied using Kitt Peak Doppler imag...
A model for stellar convection zones based on linear convective modes using a nonlocal mixing length...
Understanding and characterization of solar convection is a key problem of heliophysics and astrophy...
The theoretical power spectrum of velocity fields, calculated at the solar photosphere using the sup...
grantor: University of TorontoIn this thesis, a new technique for studying convection is d...
[[abstract]]The properties of convective motion on the sun for the scales smaller than supergranules...
Excitation of solar-like oscillations is attributed to turbulent convection and takes place at the u...
Abstract. Spectra of the cellular photospheric flows are determined from observations acquired by th...
Abstract. Spectra of the cellular photospheric flows are determined from observations acquired by th...
We review the properties of solar convection that are directly observable at the solar surface, and ...
We review the properties of solar convection that are directly observable at the solar surface, and ...
. The convection in stellar atmospheres cause spectral lines to be more or less blue-shifted. The di...
International audienceWe discuss how the possibility to measure mode excitation rates through means ...
Hydrodynamical, 3D simulations of the outer layers of the Sun and α Cen A are used to obtain constra...
In spite of many attempts to solve the problem of convection in stellar atmospheres our present know...
[[abstract]]The properties of convective motions on the sun are studied using Kitt Peak Doppler imag...
A model for stellar convection zones based on linear convective modes using a nonlocal mixing length...
Understanding and characterization of solar convection is a key problem of heliophysics and astrophy...
The theoretical power spectrum of velocity fields, calculated at the solar photosphere using the sup...
grantor: University of TorontoIn this thesis, a new technique for studying convection is d...
[[abstract]]The properties of convective motion on the sun for the scales smaller than supergranules...
Excitation of solar-like oscillations is attributed to turbulent convection and takes place at the u...
Abstract. Spectra of the cellular photospheric flows are determined from observations acquired by th...
Abstract. Spectra of the cellular photospheric flows are determined from observations acquired by th...
We review the properties of solar convection that are directly observable at the solar surface, and ...
We review the properties of solar convection that are directly observable at the solar surface, and ...
. The convection in stellar atmospheres cause spectral lines to be more or less blue-shifted. The di...
International audienceWe discuss how the possibility to measure mode excitation rates through means ...
Hydrodynamical, 3D simulations of the outer layers of the Sun and α Cen A are used to obtain constra...