Статья

A Sun-like star orbiting a black hole

Kareem El-BadryCenter for Astrophysics | Harvard & Smithsonian , 60 Garden Street, Cambridge, MA 02138, USAHans-Walter RixMax-Planck Institute for Astronomy , Königstuhl 17, D-69117 Heidelberg, GermanyEliot QuataertDepartment of Astrophysical Sciences, Princeton University , Princeton, NJ 08544, USAAndrew W. HowardDepartment of Astronomy, California Institute of Technology , Pasadena, CA 91125, USAHoward IsaacsonCentre for Astrophysics, University of Southern Queensland , Toowoomba, QLD 4350, AustraliaJim FullerDepartment of Astronomy, California Institute of Technology , Pasadena, CA 91125, USAKeith HawkinsDepartment of Astronomy, The University of Texas at Austin , 2515 Speedway Boulevard, Austin, TX 78712, USAKatelyn BreivikCenter for Computational Astrophysics, Flatiron Institute , 162 Fifth Ave, New York, NY, 10010, USAKaze W. K. WongCenter for Computational Astrophysics, Flatiron Institute , 162 Fifth Ave, New York, NY, 10010, USAAntonio C. RodriguezDepartment of Astronomy, California Institute of Technology , Pasadena, CA 91125, USACharlie ConroyCenter for Astrophysics | Harvard & Smithsonian , 60 Garden Street, Cambridge, MA 02138, USAS. ShahafDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science , Rehovot 7610001, IsraelT. MazehSchool of Physics and Astronomy, Tel Aviv University , Tel Aviv, 6997801, IsraelF. ArenouGEPI, Observatoire de Paris, Université PSL , CNRS, 5 Place Jules Janssen, F-92190 Meudon, FranceKevin B. BurdgeMIT-Kavli Institute for Astrophysics and Space Research 77 Massachusetts Ave. Cambridge , MA 02139, USADolev BashiSchool of Physics and Astronomy, Tel Aviv University , Tel Aviv, 6997801, IsraelS. FaiglerSchool of Physics and Astronomy, Tel Aviv University , Tel Aviv, 6997801, IsraelDaniel R. WeiszDepartment of Astronomy, University of California , Berkeley, 501 Campbell Hall #3411, Berkeley, CA 94720, USARhys SeeburgerMax-Planck Institute for Astronomy , Königstuhl 17, D-69117 Heidelberg, GermanySilvia Almada MonterMax-Planck Institute for Astronomy , Königstuhl 17, D-69117 Heidelberg, GermanyJennifer WojnoMax-Planck Institute for Astronomy , Königstuhl 17, D-69117 Heidelberg, Germany

2022en

ABI

Аннотация

ABSTRACT We report discovery of a bright, nearby ($G = 13.8;\, \, d = 480\, \rm pc$) Sun-like star orbiting a dark object. We identified the system as a black hole candidate via its astrometric orbital solution from the Gaia mission. Radial velocities validated and refined the Gaia solution, and spectroscopy ruled out significant light contributions from another star. Joint modelling of radial velocities and astrometry constrains the companion mass of $M_2 = 9.62\pm 0.18\, \mathrm{M}_{\odot }$. The spectroscopic orbit alone sets a minimum companion mass of $M_2\gt 5\, \mathrm{M}_{\odot }$; if the companion were a $5\, \mathrm{M}_{\odot }$ star, it would be 500 times more luminous than the entire system. These constraints are insensitive to the mass of the luminous star, which appears as a slowly rotating G dwarf ($T_{\rm eff}=5850\, \rm K$, log g = 4.5, $M=0.93\, \mathrm{M}_{\odot }$), with near-solar metallicity ($\rm [Fe/H] = -0.2$) and an unremarkable abundance pattern. We find no plausible astrophysical scenario that can explain the orbit and does not involve a black hole. The orbital period, Porb = 185.6 d, is longer than that of any known stellar-mass black hole binary. The system’s modest eccentricity (e = 0.45), high metallicity, and thin-disc Galactic orbit suggest that it was born in the Milky Way disc with at most a weak natal kick. How the system formed is uncertain. Common envelope evolution can only produce the system’s wide orbit under extreme and likely unphysical assumptions. Formation models involving triples or dynamical assembly in an open cluster may be more promising. This is the nearest known black hole by a factor of 3, and its discovery suggests the existence of a sizable population of dormant black holes in binaries. Future Gaia releases will likely facilitate the discovery of dozens more.

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Идентификаторы

DOI: 10.1093/mnras/stac3140

Цитирования и источники

Цитирований: 7Использованных источников: 0

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