A Study of the Long-Term Behaviour Patterns of the Variation of the Emission Lines in the Spectra of some Be Type Stars

Details A Study of the Long-Term Behaviour Patterns of the Variation of the Emission Lines in the Spectra of some Be Type Stars A Study of the Long-Term Behaviour Patterns of the Variation of the Emission Lines in the Spectra of some Be Type Stars

Jul 1970

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1970ap%26ss...8....3k&link_type=abstract

Astrophysics and Space Science, Volume 8, Issue 1, pp.3-11

Astronomy and Astrophysics

Astrophysics

8

Scientific paper

The ratio of the line intensity to that of the nearby continuum for an emission line, has been derived from objective prism spectra taken, at the Norman Lockyer Observatory, over the period, 1914 to 1959, for six stars (γ Cassiopeia, ϕ and ψ Persei, HD 20336, 25 Orionis, β Piscium). This has been combined with information already in the literature, to study the long-period behaviour of the stars. Long-term variations have been looked for, and it is found that, with the exception of one of the stars which is a spectroscopic binary, the variations tend to occur in outbursts which may last for 10 to 20 years, and which may show signs of semi-regular periodicities during the outburst. It is suggested, that while no stable long-term periodicities have been found, the outbursts may recur after long intervals, and that this possibility is demonstrated by one of these stars (γ Cassiopeia). It is also suggested that the semi-regular variations that occur during some of the outbursts may be ralated to an intrinsic cycle connected with the surface of the star, and possibly akin to the solar sunspot cycle.

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