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Binary and Multiple Star Systems
Schematic of a black
hole
accreting matter from a
blue supergiant star
Credit: CXC
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The fate of star B varies depending on the details of its orbit and the masses of
the two stars: (1) It could spiral into A to form a large black hole; (2) B could
explode as a supernova and disrupt the binary system; or (3) the supernova could
produce a neutron star or black hole, leading to (3a) binary neutron
stars—which have been observed—or (3b) a neutron star/black hole
binary—which may be observed with Chandra or some other sensitive X-ray
telescope, or (3c) binary black holes—which astronomers hope to observe
with one of the gravitational
wave detectors planned for the future.
If the masses of stars A and B are comparable to that of the Sun, the end
products are white dwarfs
instead of neutron stars and black holes. The dumping of matter from star A onto
star B can still result in a strong X-ray source and celestial fireworks, such as
a nova, or in rare cases when it transfers too much mass to
the white dwarf, a supernova.
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