TY  - JOUR
AU  - Cappelluti, Nico
AU  - Pacucci, Fabio
AU  - Hasinger, Günther Gustav
TI  - Constraining Wind-driven Accretion onto Gaia BH3 with Chandra
JO  - The astrophysical journal / Part 1
VL  - 973
IS  - 2
SN  - 0004-637X
CY  - London
PB  - Institute of Physics Publ.
M1  - PUBDB-2024-07605
M1  - arXiv:2406.07602
SP  - 75
PY  - 2024
N1  - Accepted for publication in The Astrophysical Journal. 10 pages, 4 figures
AB  - Gaia BH3 is the most massive known stellar-origin black hole in the Milky Way, with a mass M<sub>•</sub> ≈ 33 M<sub>⊙</sub>. Detected from Gaia’s astrometry, this black hole is in the mass range of those observed via gravitational waves, whose nature is still highly debated. Hosted in a binary system with a companion giant star that is too far away for Roche-lobe mass transfer, this black hole could nonetheless accrete at low levels due to wind-driven mass loss from its companion star, thus accreting in advection-dominated accretion flow, or ADAF, mode. Using stellar wind models, we constrain its Eddington ratio in the range 10<sup>−9</sup> < f<sub>Edd</sub> < 10<sup>−7</sup>, corresponding to radiative efficiencies 5 × 10<sup>−5</sup> < ϵ < 10<sup>−3</sup>, compatible with radiatively inefficient accretion modes. Chandra ACIS-S observed this object and obtained the most sensitive upper bound of its [2–10] keV flux: F<sub>X</sub> < 3.25 × 10<sup>−15</sup> erg s<sup>−1</sup> cm<sup>−2</sup> at 90
LB  - PUB:(DE-HGF)16
UR  - <Go to ISI:>//WOS:001317245800001
DO  - DOI:10.3847/1538-4357/ad6f96
UR  - https://bib-pubdb1.desy.de/record/619400
ER  -