^that.
A 5 M
solar black hole smashing into the sun at pretty much any speed would destroy the solar system as we know it, though.
Depends on the disc. IIRC, some "interesting" ones have been observed with way more mass in them than they should have.
Remember, before fusion starts inside the protostar and blows the remaining gas away with solar wind and light pressures, there is a considerably greater amount of mass present than after the star ignites.
Two very massive objects will orbit each other around the system's barycenter. With a very small neutron star, and a massive protoplanetary disc, the mass difference between the two may be low enough for a stable barycentric orbit, but the gravitational effect of the neutron star companion would stretch the planetary gas disc, and make any bodies produced inside it have unusally eliptical orbits.
Even still, there might be stable configurations.
Oh, you're thinking of the cloud of gas before the star is actually formed? Sorry, I was always referring to the protoplanetary disk as the debris disk around a newly formed star. Maybe I should have not referred to it as a protostar, my fault on that one.
There are stable gas disks around binary stars, though, and they come in two types, p- and s-type. P-type disks are around both stars and s-type are around one of them with the companion star being off in the distance. Coincidentally, I just today was at my department's journal club where a guy talked about this in the form of
this paper. The paper is about a planet around a binary (p-type orbit) with an extremely circular orbit, and to answer the question of why it's so circular (it's strange since the binary stars would affect the orbit and make it eccentric by exerting a torque on the planet) they model a gas disk around the stars. The gas disk supposedly damps the effects of the binary on the planet.
Now, having two stars or one star and a neutron star would not make much of a difference if they had the same mass. So in theory you could just switch one of the stars for a NS and have the same orbital dynamics.