Presentation #206.04 in the session Galaxy Dynamics Posters.
Strong correlations exist between supermassive black holes (SMBHs) and their host galaxies. These correlations suggest a missing component in our current understanding: the role of energy cascade in SMBH-bulge coevolution. In this picture, energy is continuously cascaded from bulge scale rb down to the BH scale (Schwarzschild radius rs). Energy cascade has a scale-independent, but decreasing rate εb(t)~σb3/rb that regulates the coevolution, where σb is bulge velocity dispersion. The host galaxy mass-size relation follows a 5/3 law with Mb ~ εb2/3rb5/3G-1, or an equivalent density-size relation ρb~rb-4/3, with rate of cascade εb ~ a-5/2x10-4m2/s3, as confirmed by the galaxy survey. Here a is the scale factor and G is the gravitational constant. Since εb is much larger in the early universe, cascade theory predicts that BH accretion can be super-Eddington with luminosity LB exceeding the Eddington limit. In addition, the BH mass-velocity dispersion relation (MB ~σb5) is a natural result of the cascade theory. A three stage model is proposed for SMBH-host evolution involving co-evolution, transitional, and dormant stages, respectively. Models are finally compared against the BH accretion history from quasar luminosity function of 2dF Redshift Survey, local galaxy and SMBHs data, and high redshift quasars from SDSS DR7 and CFHQS surveys.