  I review here some of the open questions regarding the geometry and emission
mechanisms of galactic black hole candidates. For hard states, I concentrate on
the perspective of ``disk+Compton coronae'' models (for discussions of jet
models, see the papers by Sera Markoff). Specifically, I discuss the
implications from our 10 year long RXTE monitoring campaign of Cyg X-1. I then
present simultaneous RXTE/Chandra observations of the ``soft state'' black hole
candidate 4U 1957+11, and discuss to what extent it does or does not allow one
to test ``relativistic disk models''. The use of such models has been claimed
to measure black hole spin parameters. I then briefly present a particularly
freaky-weird observation of GX 339-4, where the source ``fell off'' the usual
radio/X-ray correlation in the low/hard state. Questions addressed by the above
observations include: are the Compton corona models unique fits to the data?
(No. Jets work equally well, and simple broken power laws work better still. We
argue that the latter models indicate multiple, broad-band continuum
components.) Is there good evidence for a receding disk as sources transit into
the hard state? (The jury is still out.) What does the relativistically
broadened Fe line tell us? (Sometimes the disk, even into quiescence, stays
very close to the central object, in contrast to expectations of ADAF models.)
How much better/more necessary are recently discussed relativistic disk models?
(I am very doubtful that such models will ever usefully measure black hole
spin.)
