Indication of the High Mass-Transfer Ratio in S-type Symbiotic Binaries

TL;DR

This paper models the neutral hydrogen column densities in specific symbiotic stars to derive wind velocity profiles and mass-loss rates, revealing enhanced wind activity at the orbital plane.

Contribution

It introduces a method to determine wind velocity profiles and mass-loss rates in S-type symbiotic binaries using H$^0$ column densities, highlighting wind enhancement at the orbital plane.

Findings

Strong wind enhancement at the orbital plane

Derived wind velocity profiles and mass-loss rates

Implications for mass transfer in symbiotic binaries

Abstract

By modelling H$^0$ column densities in eclipsing S-type symbiotic stars EG And and SY Mus, we derived the wind velocity profile and the corresponding mass-loss rate from their giants. Our analysis revealed a strong enhancement of the wind at the orbital plane.