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A study of the long-term behaviour patterns of the variation of the emission lines in the spectra of some Be type stars

Abstract

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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Top: Far-encounter picture (No. 73) of Mars, taken by the Mariner 7 spacecraft on 4 August 1969 from a distance of 471 750 km from the planet.Bottom: Near-encounter picture (No. 21) of Mars, taken by Mariner 6 on 30 July 1969 at the time of its closest approach to the surface of the planet. The size of the field is approximately 690×890 km on the Martian surface This photograph recorded more than 100 individual craters, the largest of which is about 260 km in diameter.

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Kitchin, C.R. A study of the long-term behaviour patterns of the variation of the emission lines in the spectra of some Be type stars. Astrophys Space Sci 8, 3–11 (1970). https://doi.org/10.1007/BF00651649

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Keywords

  • Emission Line
  • Behaviour Pattern
  • Line Intensity
  • Sunspot Cycle
  • Type Star