'Missing link' black hole lurks in strange binary system with red giant star

A red glowing sphere next to a purple cloud of smoke with a pitch black center
An illustration of a red giant star orbited by a shadowy stellar mass black hole. (Image credit: Robert Lea (created with Canva))

For astronomers, finding a new black hole orbiting an aged red dwarf star is an exciting find in itself, but when that black hole seems to be a "missing link" stellar-mass black hole, you can crank the excitement up to 11! That is exactly what seems to be lurking in binary system G3425, estimated to be around 5,800 light-years away.

The visible component of G3425 is a red giant star, the kind of stellar body you get when a star exhausts its supply of hydrogen fuel and can no longer conduct nuclear fusion in its core. This causes its outer layers (where fusion continues) to "puff out" to as much as 100 times the star's original width. 

Our own star, the sun, is currently in its middle age. This means that in around 5 billion years, it will enter its red giant phase and swell up to around the orbit of Mars, swallowing the inner planets, including Earth. Even then, what the red giant sun almost certainly won't have is a stellar-mass black hole as a companion. The team's research is published in the journal Nature Astronomy

The red dwarf in this system has a mass of around 2.7 times the mass of our sun, but what is really interesting to scientists is the mass of its compact dark companion. This newfound black hole was weighed by a team led by Wang Song from the National Astronomical Observatories of the Chinese Academy of Sciences (NAOC). Its mass is between 3.1 and 4.4 times that of the sun, probably about 3.6 solar masses. 

"The black hole falls within the famous mass gap, making it one of the lightest black holes discovered so far," Song told Space.com. "This discovery not only confirms the existence of mass-gap black holes but also shows that binaries containing low-mass black holes can survive a supernova explosion."

Song and colleagues detected this stellar-mass black hole in data collected by the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) and from the Gaia space telescope, which precisely measures the positions of billions of stars in the Milky Way and beyond. 

This combination of data and techniques allowed the researchers to observe the black hole's gravitational "tug" on its companion red dwarf star, forcing it to reveal itself.

Related: Scientists waited ages to find a 'missing link' black hole — then stumbled upon 2

Mystery of the missing masses

Black holes have very few defining characteristics, a fact that physicist John Wheeler once described by saying, "Black holes have no hair." In addition to electric charge and angular momentum, one of the characteristics black holes do have that allows astronomers to set them apart is their mass.

The kings of mass are the supermassive black holes that lurk at the hearts of most, if not all, large galaxies, and have masses millions to billions of times that of the sun. More diminutive are elusive intermediate-mass black holes, which have masses between 100 and 100,000 solar masses. 

Both of these types of black holes are too massive to form when a star runs out of fuel for nuclear fusion and after repeated collapses and expansion episodes, resulting in a complete collapse under its own gravity. Thus, they grow by greedily feasting on matter around them or by merging with other black holes over and over again.

The smallest astrophysical black holes that we know of are so-called stellar mass black holes, which we find with masses up to 100 times that of the sun. These black holes are just the right size to be born when a star at least eight times as massive as the sun can no longer fuse heavier and heavier elements, and thus can't generate the energy to battle against the inward push of its own gravity.

An illustration showing the three types of astrophysical black holes, staring from the most massive on the left to the least massive on the right (Image credit: Robert Lea (created with Canva))

Over the past 60 years or so, astronomers have found dozens of stellar-mass black holes that fit within a distribution of 5 to 25 solar masses. So far, so good, but there is a problem.

Theories of black hole birth suggest that after a star has lost the majority of its mass via a tremendous supernova explosion that signals gravity's victory, those stars that hang on to just three times the mass of the sun should still be able to form a stellar-mass black hole. So, with that said, the question becomes: where are all the 3 to 5 solar mass black holes?

An illustration of the G3425 with a red dwarf star and a black hole. (Image credit: Wang Song)

One possibility is that there is some mechanism that comes into play during a supernova that prevents black holes with 3 to 5 solar masses from forming. 

Alternatively, lower-mass black holes may be more likely to get disrupted by "kicks" delivered to them during a supernova explosion and, therefore, less likely to linger in a binary with a visible companion that makes them easier to spot.

This arises from the fact that all black holes, no matter the mass, are bounded by a light-trapping surface called an event horizon that makes them effectively invisible. Black holes in a binary, like the one in G3425, can be inferred by the effect they have on their visible companion. Thus, an unaccompanied "supernova-kicked" black hole won't be visible by these effects because they have no companion to impact.

If that is the case, how did this black hole manage to survive that mechanism and/or resist the kick that should have sent it spiraling away from its companion?

Another puzzle surrounds this system. G3425 is a wide binary with an orbital period of approximately 880 Earth days. The orbit has zero "eccentricity," which means that it is a near-perfect circle. The team can't currently explain this through standard binary evolutionary processes. 

"The most surprising thing is the wide circular orbit of the binary," Song said. "The formation of such a binary, especially involving a low-mass black hole, presents a significant challenge to current theories of binary evolution and supernova explosion."

The formation of this red dwarf/black hole binary with a surprisingly wide circular orbit may challenge current binary evolution and supernova explosion theories, but it has delivered a few positives.

These findings prove that quiet and invisible objects in binaries can be detected via the effect they have on their companions and that uncovering lurking low-mass black holes can deliver insights into the evolution of binary systems.

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Robert Lea
Senior Writer

Robert Lea is a science journalist in the U.K. whose articles have been published in Physics World, New Scientist, Astronomy Magazine, All About Space, Newsweek and ZME Science. He also writes about science communication for Elsevier and the European Journal of Physics. Rob holds a bachelor of science degree in physics and astronomy from the U.K.’s Open University. Follow him on Twitter @sciencef1rst.

  • Unclear Engineer
    First, this article keeps switching between calling the visible star a "red giant" and a "red dwarf". It is a giant, not a dwarf. Somebody please fix that.

    On to the science: To try to explain how a black hole and a red giant might be in orbit around each other, it seems like first we need to describe the orbit properly. This article says that the mass of the visible star is 2.7 solar masses, while the mass of the black hole is 3.6 solar masses. It describes the orbit of the visible star as "nearly circular", but it is orbiting the center of mass of the pair, not the black hole.

    The article talks about black holes getting a "kick" in some direction due to some lack of exact symmetry in their collapse. But, that seems to be a random effect. So, unless there is some theory that shows a particular type of asymmetry always occurs during those supernova events, it seems reasonable that a few might not be unsymmetrical enough to produce much of a "kick".

    Or, how about a "capture" scenario for a black hole that was not near the other star when it became a black hole? Getting a nearly perfectly circular orbit with a capture would seem to require a lot of "drag" on the black hole as it and the red giant pass each other. Is the red giants expanded outer layer big enough to cause much drag on a passing black hole? Some stars have generated large and rather dense "shells" of ejected matter over their lifetimes, such as Wolf -Rayet types - maybe there are other types as well. And, the relative velocity between the two might not have been very much to begin with when they tried to "pass" on their original paths.
    Reply
  • Questioner
    Plunging in with my (latest) hypothesis that BHs are actually singularities due to contracted space of mass fields.

    A singularity cannot respond gravitationally.

    Other non-absolute zero, non-singularities can however respond gravitationally to a singularity's mass field. Making it one-sided gravity.

    The near circular orbit of the red giant fits that very neatly.

    The pair may have been spiraling towards one another prior to the supernova,
    & now with only one-sided gravity a stable orbiting is what remains.

    A singularity/BH post nova ends with whatever inertia it had at that time.

    Which means if a binary pair's orbit depended on mutual gravitational response one side or that orbit inward acceleration is gone when one of them becomes a BH.

    The one-sided gravity may be insufficient to sustain the pairing.

    That might likely have the luminal partner wandering off leaving the BH isolated and difficult to identify.

    So perhaps small BHs tend to be isolated and difficult to find rather than being actually smaller of population.
    Reply