The loss of large amplitude pulsations at the end of AGB evolution. (arXiv:1811.06906v1 [astro-ph.SR])

The loss of large amplitude pulsations at the end of AGB evolution. (arXiv:1811.06906v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Engels_D/0/1/0/all/0/1">Dieter Engels</a> (Hamburger Sternwarte, Hamburg, Germany), <a href="http://arxiv.org/find/astro-ph/1/au:+Etoka_S/0/1/0/all/0/1">Sandra Etoka</a> (Jodrell Bank Centre for Astrophysics, Manchester, UK), <a href="http://arxiv.org/find/astro-ph/1/au:+Gerard_E/0/1/0/all/0/1">Eric Gerard</a> (GEPI, Observatoire de Paris, Meudon, France)

Since 2013 we are performing with the Nancay Radio Telescope (NRT) a
monitoring program of >100 Galactic disk OH/IR stars, having bright 1612-MHz OH
maser emission. The variations of the maser emission are used to probe the
underlying stellar variability. We wish to understand how the large-amplitude
variations are lost during the AGB – post-AGB transition. The fading out of
pulsations with steadily declining amplitudes seems to be a viable process.

Since 2013 we are performing with the Nancay Radio Telescope (NRT) a
monitoring program of >100 Galactic disk OH/IR stars, having bright 1612-MHz OH
maser emission. The variations of the maser emission are used to probe the
underlying stellar variability. We wish to understand how the large-amplitude
variations are lost during the AGB – post-AGB transition. The fading out of
pulsations with steadily declining amplitudes seems to be a viable process.

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