The spectral energy distribution of D-type symbiotic stars: the role of dust shells

TL;DR

This study models the spectral energy distribution of D-type symbiotic stars, revealing the presence of multiple dust shells, shock-related emissions, and the validation of the colliding wind scenario through multi-wavelength data analysis.

Contribution

It provides a comprehensive model of D-type symbiotic stars' spectral energy distribution, emphasizing the role of dust shells and shocks, and confirms the colliding wind model's applicability.

Findings

Presence of at least two dust shells at ~1000 K and ~400 K

Radio emission explained by thermal self-absorbed reverse shock

Predicted soft X-ray emission from bremsstrahlung downstream of shocks

Abstract

We have collected continuum data of a sample of D-type symbiotic stars. By modelling their spectral energy distribution in a colliding-wind theoretical scenario we have found the common characteristics to all the systems: 1) at least two dust shells are clearly present, one at \sim 1000 K and the other at \sim 400 K; they dominate the emission in the IR; 2) the radio data are explained by thermal self-absorbed emission from the reverse shock between the stars; while 3) the data in the long wavelength tail come from the expanding shock outwards the system; 4) in some symbiotic stars, the contribution from the WD in the UV is directly seen. Finally, 5) for some objects soft X-ray emitted by bremsstrahlung downstream of the reverse-shock between the stars are predicted. The results thus confirm the validity of the colliding wind model and the important role of the shocks. The comparison of the fluxes calculated at the nebula with those observed at Earth reveals the distribution throughout the system of the different components, in particular the nebulae and the dust shells. The correlation of shell radii with the orbital period shows that larger radii are found at larger periods. Moreover, the temperatures of the dust shells regarding the sample are found at 1000 K and <=400 K, while, in the case of late giants, they spread more uniformly throughout the same range.