Abstract
The first helium star was discovered by Popper in 1942. It is the B3 star HD 124448. Since then the number of helium stars and hydrogen-deficient stars has increased to 40 stars. A major contribution comes from the spectral survey of the southern sky by MacConnell, Frye, and Bidelman (1970 and 1972). Furthermore, a number of quantitative spectral analyses as well as theoretical results on the interior structure and evolution have become available, calling for a review of the problem of helium stars, the central question being how these stars became helium stars and in which direction they evolve. It must be stated in the beginning that a definite answer cannot be given as yet, but that several aspects can be clarified. The reader is referred to previous reviews (Hill, 1964, 1965; Underhill, 1966; Jaschek and Jaschek, 1971; Scholz, 1972; Hack, 1967; Dinger, 1969) for assessment of the rapid progress in the field. A major part of the literature is found in the last two references.
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Hunger, K. (1975). Properties and Problems of Helium Stars. In: Baschek, B., Kegel, W.H., Traving, G. (eds) Problems in Stellar Atmospheres and Envelopes. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-80919-4_3
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