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
No takes yet. Share an insight, caveat, or question.
Shapiro et al. (1976) studied this question.