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The dynamics of red supergiant winds
<span title="">2002</span>
<i title="Cambridge University Press (CUP)">
<a target="_blank" rel="noopener" href="https://fatcat.wiki/container/lxetaglz6zdw5doila4t3zfp6m" style="color: black;">Symposium - International astronomical union</a>
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During the red supergiant (RSG) stage of massive star evolution, emission from dust and molecules allows the copious stellar winds to be studied in great detail. This help us understand not only the evolutionary stages of the star (which are highly dependent on mass loss rates), but also the morphology of the eventual supernova remnant. Maser emission from OH and H2O has been mapped with milli-arcsec resolution (using MERLIN and the EVN/global VLBI) around RSG including VY CMa, S Per and VX
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... The H2O masers originate in clouds accelerating away from the star and OH mainlines masers interleave the outer parts of the H2O maser shell. Zeeman splitting of OH maser lines reveals the orientation and strength of stellar-centred magnetic fields.
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