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The suggestion that the observed 0.25 keV X-ray background and O VI sabsorption lines are produced by a new, hot (T∼106 K), diffuse component of the medium is examined in the context of both a steady-state and a time-dependent model. It is concluded that such a component can explain the two observations only if (1) the pressure of the cooler interstellar medium is 10 times higher than the previously estimated p/k∼2000 cm-3K; (2) a mechanism such as the proposed convective-radiative "galactic fountain" exists to cool the hot gas; and (3) another component is responsible for the presence of O VI at temperatures below 106 K. Subject headings: interstellar: matter - X-rays: general
Shapiro et al. (Sat,) studied this question.