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arXiv · 1610.04208

Disk formation in oblate B[e] stars

I. Araya·C. Arcos·M. Curé
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Abstract

We investigate the possible role of line-driven winds in the circumstellar envelope in B[e] stars, mainly the role of the $\Omega$-slow wind solution, which is characterized by a slower terminal velocity and higher mass-loss rate, in comparison with the standard (m-CAK) wind solution. In this work, we assume two scenarios: 1) a spherically symmetric star and 2) a scenario that considers the oblate shape, considering only the oblate correction factor. For certain values of the line force parameters (according to previous works), we obtain in both scenarios a density contrast $\gtrsim10^{2}$ between equatorial and polar densities, characterized for a fast polar wind and a slow and denser wind when the $\Omega$-slow wind solution is obtained. All this properties are enhanced when the oblate correction factor is included in our calculations.

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I. Araya, C. Arcos, M. Curé. 2016-10-13. Disk formation in oblate B[e] stars. https://arxiv.org/abs/1610.04208

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