The emission captured by these ALMA 338 GHz observations is generated by supersonic shocks excited by large convection cells abutting the stellar photosphere. The bright parts of each bubble correspond to hot gas rising through the stellar convective zone, moving towards us, and the darker regions between bubbles are due to sinking cool gas. According to mixing length theory (a method for parameterizing stellar convection), the bubbles’ sizes are related to fundamental stellar properties such as effective temperature and surface gravity. These observations enable testing of this theory, and agreement between observations and theory is generally found to be good. However, the comparison is not perfect, indicating that there is work to be done to improve understanding of stellar convection processes.

The movement of the observed surface ranges between –18 and +20 km s^–1 in velocity (with negative velocities indicating a radial motion inwards), which is low compared to the escape velocity of the star. Nevertheless, a small amount of material is able to escape the photosphere, and that material is then accelerated by radiation pressure on freshly condensed circumstellar dust grains and forms part of the stellar wind. Stellar winds from evolved stars are a crucial mechanism for distributing elements like carbon and nitrogen through the interstellar medium.

这些 ALMA 338 GHz 观测捕获的发射是由毗邻恒星光球层的大型对流单元激发的超音速激波产生的。每个气泡的明亮部分对应于通过恒星对流区上升并向我们移动的热气体，而气泡之间的较暗区域是由于下沉的冷气体造成的。根据混合长度理论（一种参数化恒星对流的方法），气泡的大小与恒星的基本特性有关，例如有效温度和表面重力。这些观察结果可以检验该理论，并且通常发现观察结果和理论之间的一致性是好的。然而，这种比较并不完美，这表明要提高对恒星对流过程的理解还有工作要做。

观察到的表面移动速度在 –18 到 +20 km s^–1 之间（负速度表示径向向内运动），与恒星的逃逸速度相比，这是较低的。尽管如此，少量物质能够逃离光球层，然后这些物质被新凝结的星际尘埃颗粒上的辐射压力加速，形成恒星风的一部分。来自演化恒星的恒星风是通过星际介质分配碳和氮等元素的重要机制。