Lamers H.J.G.L.M., Najarro F., Kudritzki R.P., Morris P.W., Voors R.H.M., van Gent J.I., Waters L.B.F.M., de Graauw T., Beintema D., Valentijn E.A., Hillier D.J.
The free-free IR excess and the IR emission lines of H and He I of the Luminous Blue Variable P Cygni are observed with the ISO-SWS instrument. The observed profiles and the free-free emission are compared with predictions from a non-LTE model atmosphere with a stellar wind. The observations agree very well with a model that has the following properties: Teff=18100K, R*=76R
, He/H=0.30 by number, {dot}(M)=3.0x10-5M/yr and v{infinity}=185km/s.
We observed forbidden emission lines of [Fe II], [Fe III], [Ni II], [Ne II], [Ne III] and [Si II]. From the study of the [Ne II] and [Ne III] lines we find that the Ne abundance is about three times higher than normal. This may be due to clumping in the CS envelope at r=~103R*
Keywords:
stars: early-type - stars: mass-loss - stars: atmospheres - stars: supergiants - stars: individual: P Cygni (HD 193237)
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