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Recent high-resolution observations have shown stellar winds to harbourcomplexities which strongly deviate from spherical symmetry, generally assumedas standard wind model. One such morphology is the archimedean spiral,generally believed to be formed by binary interactions, which has been directlyobserved in multiple sources. We seek to investigate the manifestation in theobservables of spiral structures embedded in the spherical outflows of coolstars. We aim to provide an intuitive bedrock with which upcoming ALMA data canbe compared and interpreted. By means of an extended parameter study, we modelrotational CO emission from the stellar outflow of asymptotic giant branchstars. To this end, we develop a simplified analytical parametrised descriptionof a 3D spiral structure. This model is embedded into a spherical wind, and fedinto the 3D radiative transfer code LIME, which produces 3D intensity mapsthroughout velocity space. Subsequently, we investigate the spectral signatureof rotational transitions of CO of the models, as well as the spatial aspect ofthis emission by means of wide-slit PV diagrams. Additionally, the potentialfor misinterpretation of the 3D data in a 1D context is quantified. Finally, wesimulate ALMA observations to explore the impact of interefrometric noise andartifacts on the emission signatures. The spectral signatures of the COrotational transition v=0 J=3-2 are very efficient at concealing the dualnature of the outflow. Only a select few parameter combinations allow for thespectral lines to disclose the presence of the spiral structure. The inabilityto disentangle the spiral from the spherical signal can result in an incorrectinterpretation in a 1D context. Consequently, erroneous mass loss rates wouldbe calculated...

Simplified models of stellar wind anatomy for interpreting high-resolution data: Analytical approach to embedded spiral geometries