Multi-messenger emission of Accretion Induce Collapse of White Dwarfs

In his pivotal work, Chandrasekhar was able to show that an isolated White Dwarf (WD), in order to be stable, should have no more than ~1.4 solar masses, which is now known as the Chandrasekhar mass limit. As stars often occur in binary systems, it is common to find stars accreting mass from their companion. In this scenario, it should not come as a surprise if a WD is found to (temporarily) surpass the aforementioned limit. In this talk, I will discuss how this unstable WD will behave once the gravitational collapse is triggered. In particular, we will be interested in the case where the collapse is driven by an electron capture process, leading to an explosion, in an event named Accretion Induce Collapse. We will discuss the morphology of the multi-messenger signals of these sources with a larger focus on gravitational wave emission.