Abstract. Microquasars are black-hole binaries with jets. Nowadays, they are studied mostly in X- and gamma-rays where the inner accretion disk emits most of its energy. I will present new theoretical results from the model of Grenoble. In particular, I will show how this new model produce 3 disk solutions among which a very hot optically thin geometrically thick inner disk. This solution can be used to model the hard branch of the hysteresis diagram. I will show that the theoretical hard branch limits and its tilt represent new and strong(er) constraints on the behavior and caracteristics of microquasars accretion disk. I will finish by trying to replace microquasar's observations on a more global context. I will then present some speculative ideas about their potential as best targets for what is now called quantum astronomy, opened up 50 years ago by the intensity interferometry.

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