TY - JOUR
T1 - Boundary layers of accretion discs
T2 - Discovery of vortex-driven modes and other waves
AU - Coleman, Matthew S.B.
AU - Rafikov, Roman R.
AU - Philippov, Alexander A.
N1 - Publisher Copyright:
© 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
PY - 2022/1/1
Y1 - 2022/1/1
N2 - Disc accretion on to weakly magnetized objects possessing a material surface st proceed via the so-called boundary layer (BL) - a region at the inner edge of the disc, in which the velocity of accreting material abruptly decreases from its Keplerian value. Supersonic shear arising in the BL is known to be conducive to excitation of acoustic waves that propagate into both the accretor and the disc, enabling angular momentum and mass transport across the BL. We carry out a numerical exploration of different wave modes that operate near the BL, focusing on their morphological characteristics in the inneost parts of accretion disc. Using a large suite of silations covering a broad range of Mach numbers (of the supersonic shear flow in the BL), we provide accurate characterization of the different types of modes, verifying their properties against analytical results, when available. We discover new types of modes, in particular, global spiral density waves launched by vortices foing in the disc near the BL as a result of the Rossby wave instability; this instability is triggered by the vortensity production in that region caused by the non-linear damping of acoustic waves. Azithal wavenumbers of the dominant modes that we observe appear to increase monotonically with the Mach number of the runs, but a particular mix of modes found in a silation is mildly stochastic. Our results provide a basis for better understanding of the angular momentum and mass transport across the BL as well as the emission variability in accreting objects.
AB - Disc accretion on to weakly magnetized objects possessing a material surface st proceed via the so-called boundary layer (BL) - a region at the inner edge of the disc, in which the velocity of accreting material abruptly decreases from its Keplerian value. Supersonic shear arising in the BL is known to be conducive to excitation of acoustic waves that propagate into both the accretor and the disc, enabling angular momentum and mass transport across the BL. We carry out a numerical exploration of different wave modes that operate near the BL, focusing on their morphological characteristics in the inneost parts of accretion disc. Using a large suite of silations covering a broad range of Mach numbers (of the supersonic shear flow in the BL), we provide accurate characterization of the different types of modes, verifying their properties against analytical results, when available. We discover new types of modes, in particular, global spiral density waves launched by vortices foing in the disc near the BL as a result of the Rossby wave instability; this instability is triggered by the vortensity production in that region caused by the non-linear damping of acoustic waves. Azithal wavenumbers of the dominant modes that we observe appear to increase monotonically with the Mach number of the runs, but a particular mix of modes found in a silation is mildly stochastic. Our results provide a basis for better understanding of the angular momentum and mass transport across the BL as well as the emission variability in accreting objects.
KW - accretion
KW - accretion discs
KW - hydrodynamics
KW - instabilities
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U2 - 10.1093/mnras/stab2962
DO - 10.1093/mnras/stab2962
M3 - Article
AN - SCOPUS:85121215161
SN - 0035-8711
VL - 509
SP - 440
EP - 462
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 1
ER -