M33 X-7 is a black hole binary system in the
Triangulum Galaxy. The system is made up of a
stellar-mass black hole and a companion star. The black hole in M33 X-7 has an estimated mass of 15.65 times that of the
Sun () (formerly the largest known stellar black hole, though this has now been superceeded amongst electromagnetically-observed black holes by an increased mass estimate for
Cygnus X-1, and also by many of the
LVK-detected binary black hole components). The total mass of the system is estimated to be around , which would make it the most massive black hole binary system. The black hole is consuming its partner, a 70 solar mass blue giant star.
Location
M33 X-7 lies within the
Triangulum Galaxy which is approximately 3 million
light-years (ly) distant from the
Milky Way in constellation Triangulum. This would make M33 X-7 one of the furthest confirmed stellar mass black holes known.
System
M33 X-7 orbits a companion star that eclipses the black hole every 3.45 days. The companion star also has an unusually large mass, . This makes it the most massive companion star in a binary system containing a black hole.
Observational data
The black hole was studied in combination by NASA's
Chandra X-ray Observatory and the
Gemini telescope on Mauna Kea, Hawaii.
The properties of the M33 X-7 binary system are difficult to explain using conventional models for the evolution of massive stars. The parent star for the black hole must have had a mass greater than the existing companion to have formed a black hole before the companion star. Such a massive star would have had a radius larger than the present separation between the stars, so the stars must have been brought closer while sharing a common outer atmosphere. This process typically results in a large amount of mass being lost from the system, so much that the parent star should not have been able to form a black hole.
File:M33 X-7 Composite.jpg, M33 X-7 composite
File:M33 X-7 Optical.jpg, M33 X-7 Optical
File:M33 X-7 X-ray.jpg, M33 X-7 X-ray
File:M33x7 xray bright.jpg, M33 X-7
In new models of the formation of the black hole, the star that will form the black hole is nearly 100 times the mass of the Sun, orbiting a second star with mass of about .
In such an orbit, the future black hole is able to start transferring mass while it is still fusing
hydrogen into
helium. As a result, it loses most of its hydrogen becoming a
Wolf–Rayet star and shedding the rest of the envelope in the form of stellar wind, exposing its core. Its companion grows more massive in the process, becoming more massive of the two stars.
Finally, the star collapses creating the black hole, and begins absorbing material from its companion, leading to X-ray emissions.
Future
Due to the mass, it is assumed that the companion will collapse into a black hole, creating a
binary black hole
A binary black hole (BBH) is a system consisting of two black holes in close orbit around each other. Like black holes themselves, binary black holes are often divided into stellar binary black holes, formed either as remnants of high-mass binary ...
system.
References
{{DEFAULTSORT:M33 X-7
Stars in the Triangulum Galaxy
Triangulum (constellation)
Triangulum Galaxy
Stellar black holes
Extragalactic stars
O-type bright giants