The emission from HZ Herculis in the first three Balmer lines of hydrogen and in 4686-A line of He II was calculated as a function of the orbital phase for different values of various parameters of the system. The results support the picture in which the lines (including the emission lines, in contrast to what is usually assumed) come from the atmosphere of HZ Herculis, heated by the observed X-ray flux. A small amount of soft X-rays is needed to produce the emission lines. The observed soft flux, when corrected for interstellar absorption in the standard way, is too high to contribute to the heating of HZ Herculis. The sensitivity of the observed quantities to the assumed mass ratio in the system is studied.
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Mordehai Milgrom (1976) studied this question.
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