Effects of convection on pressure wave excitation in common envelopes

TY - JOUR

T1 - Effects of convection on pressure wave excitation in common envelopes

AU - Soker, Noam

PY - 1993/11/1

Y1 - 1993/11/1

N2 - We study the effect of the convective viscosity on p-waves propagating outward in star envelope. The main interest here is in p-waves which are excited by a low-mass secondary orbiting well inside the extended primary's envelope. These waves may influence the geometry of the mass loss from the envelope. We assume that the turbulent viscosity results from convective cells, with characteristic turnover time shorter by a factor of ∼2π than the oscillation period. We further assume a fully developed turbulence, and use the Kolmogoroff spectrum to describe the convective eddies. We find that the damping of outward-propagating p-waves in AGB stars' envelopes caused by convective viscosity is small. The inclusion of convective viscosity, therefore, does not alter the conclusions of the adiabatic calculation. The main result of the adiabatic calculation (presented in a previous paper) is that brown dwarfs, and possible Jupiter-like secondaries, can influence the mass loss geometry from AGB stars through p-waves excitation.

AB - We study the effect of the convective viscosity on p-waves propagating outward in star envelope. The main interest here is in p-waves which are excited by a low-mass secondary orbiting well inside the extended primary's envelope. These waves may influence the geometry of the mass loss from the envelope. We assume that the turbulent viscosity results from convective cells, with characteristic turnover time shorter by a factor of ∼2π than the oscillation period. We further assume a fully developed turbulence, and use the Kolmogoroff spectrum to describe the convective eddies. We find that the damping of outward-propagating p-waves in AGB stars' envelopes caused by convective viscosity is small. The inclusion of convective viscosity, therefore, does not alter the conclusions of the adiabatic calculation. The main result of the adiabatic calculation (presented in a previous paper) is that brown dwarfs, and possible Jupiter-like secondaries, can influence the mass loss geometry from AGB stars through p-waves excitation.

KW - Convection

KW - Planetary systems

KW - Stars: AGB and post-AGB

KW - Stars: mass loss

KW - Stars: oscillations

UR - http://www.scopus.com/inward/record.url?scp=12044252451&partnerID=8YFLogxK

U2 - 10.1086/173317

DO - 10.1086/173317

M3 - 文章

AN - SCOPUS:12044252451

VL - 417

SP - 347

EP - 350

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1

ER -