2024 APS April Meeting
Wednesday–Saturday, April 3–6, 2024;
Sacramento & Virtual
Session E00: Poster Session I & Welcome Reception (5:30PM - 7:30PM PT)
5:30 PM,
Wednesday, April 3, 2024
SAFE Credit Union Convention Center
Room: Exhibit Hall A, Floor 1
Sponsoring
Unit:
APS
Abstract: E00.00029 : Universal scaling laws for SMBH-bulge and Super-Eddington evolution
Abstract
Presenter:
Zhijie Xu
(Pacific Northwest National Laboratory)
Author:
Zhijie Xu
(Pacific Northwest National Laboratory)
Most galaxies host a central supermassive black hole. SMBHs with a mass of 109 Msun are known to exist as early as z=7. It is not yet clear how they can become so massive in such a short time. The classical Eddington limit for black hole (BH) growth was derived based on the balance between the static weight of surrounding gases and BH radiation. However, gases are never static. The turbulent flow of surrounding gases involves an energy cascade and a "cascade" force (turbulent pressure gradient) that must be balanced by the BH radiation, which might lead to a super-Eddington growth in early stage of SMBH evolution. In this work, we propose a super-Eddington growth of SMBHs enabled by the energy cascade in turbulent flow of gases. We identify two types of energy cascade in bulge: i) a localized energy cascade from large to small scales where energy is eventually dissipated by gas cooling; and ii) a radial energy cascade (due to random motion in radial flow) from bulge scale rb down to the radiation scale rp, below which the cascaded potential energy can be dissipated by SMBHs. A time-dependent rate of the energy cascade εb≈ σb3/rb=10-4a-5/2m2/s3 was identified that connects the co-evolution of SMBH and host galaxy, where a is the scale factor and σb is bulge velocity dispersion. Scaling laws associated with the energy cascade, i.e. the bulge mass-size (Mb-rb) relation can be expressed as Mb ≈εb2/3rb5/3G-1. The SMBH accretion can be super-Eddington in early universe because of the much greater rate of the energy cascade εb. Models were compared against the BH accretion history from the quasar luminosity function, local galaxy and SMBH data, and high redshift quasars from SDSS DR7 and CFHQS surveys. More details can be found at 10.5281/zenodo.7490501.