Shell ejection phenomena in the hypergiant star P Cygni

Details Shell ejection phenomena in the hypergiant star P Cygni Shell ejection phenomena in the hypergiant star P Cygni

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984esasp.218..315l&link_type=abstract

In ESA Fourth European IUE Conf. p 315-317 (SEE N84-35135 24-88)

Physics

2

Cygnus Constellation, Giant Stars, Hot Stars, Radial Velocity, Stellar Mass Ejection, Line Spectra, Stellar Evolution, Stellar Winds

Scientific paper

The authors analyse the time evolution (1978 - 1983) of the shell lines in the hypergiant star P Cygni (B1Ia+). The wind of P Cygni is characterized by a stable shell formed at large distance from the star, only seen in low excitation lines (Fe II) at 206±1.5 km/s, and by a variable shell at lower velocities, seen also in Fe III in addition to Fe II. The variable shell is formed closer to the star and accelerates outwards as time increases. The analysis shows that a new variable shell is formed every 1 - 2 years, so indicating that the shell ejection in P Cygni is a recurrent phenomenon.

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