The black hole low-mass X-ray binary V404 Cygni is part of a wide triple

Kevin B. Burdge (), Kareem El-Badry, Erin Kara, Claude Canizares, Deepto Chakrabarty, Anna Frebel, Sarah C. Millholland, Saul Rappaport, Rob Simcoe and Andrew Vanderburg
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Kevin B. Burdge: Massachusetts Institute of Technology
Kareem El-Badry: California Institute of Technology
Erin Kara: Massachusetts Institute of Technology
Claude Canizares: Massachusetts Institute of Technology
Deepto Chakrabarty: Massachusetts Institute of Technology
Anna Frebel: Massachusetts Institute of Technology
Sarah C. Millholland: Massachusetts Institute of Technology
Saul Rappaport: Massachusetts Institute of Technology
Rob Simcoe: Massachusetts Institute of Technology
Andrew Vanderburg: Massachusetts Institute of Technology

Nature, 2024, vol. 635, issue 8038, 316-320

Abstract: Abstract Evidence suggests that, when compact objects such as black holes and neutron stars form, they may receive a ‘natal kick’, during which the stellar remnant gains momentum. Observational evidence for neutron star kicks is substantial1,2, yet is limited for black hole natal kicks, and some proposed black hole formation scenarios result in very small kicks3–5. Here we report that the canonical black hole low-mass X-ray binary (LMXB) V404 Cygni is part of a wide hierarchical triple with a tertiary companion at least 3,500 astronomical units (au) away from the inner binary. Given the orbital configuration, the black hole probably received a sub-5 km s−1 kick to have avoided unbinding the tertiary. This discovery lends support to the idea that at least some black holes form with nearly no natal kick. Furthermore, the tertiary in this system lends credence to evolutionary models of LMXBs involving a hierarchical triple structure6. Remarkably, the tertiary is evolved, indicating that the system formed 3–5 billion years ago and that the black hole has removed at least half a solar mass of matter from its evolved secondary companion. During the event in which the black hole formed, it is required that at least half of the mass of the black hole progenitor collapsed into the black hole; it may even have undergone a complete implosion, enabling the tertiary to remain loosely bound.

Date: 2024
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DOI: 10.1038/s41586-024-08120-6

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