磁制动吸积流MAD是近些年通过数值模拟发现的吸积模式，为拥有最大（饱和）磁场强度的热吸积流模型。该理论模型能够提供最强的喷流功率，已经在一些活动星系核中得到观测支持，有重要的应用前景。该理论模型仍处在早期发展阶段，主要局限在喷流性质的比较判断上。由于缺乏其辐射过程的计算，限制了它的应用。辐射将是区分天体处于MAD还是标准热吸积流SANE的重要手段，将为MAD的确立提供独立的验证。在本项目中，我们将借鉴现有数值模拟结果，给出磁制动吸积流MAD的动力学结构，并有望在国际上首次深入研究MAD的辐射特征，包括多波段连续谱，射电及X射线波段的偏振，MAD的辐射效率、临界光度等。我们将研究磁制动吸积流MAD跟目前的主流热吸积流模型（标准热吸积流SANE）在辐射上的区别，为区分这两种模型提供理论基础。进一步地，我们将理论与观测结合，研究银河系中心以及黑洞X射线双星爆发阶段是否会进入疯狂吸积状态。

Magnetically arrested disk (MAD) is a novel accretion mode discovered recently from numerical simulations, which has strongest possible magnetic fields. With observational support from certain types of active galactic nuclei, this model has a promising future. MAD is currently in its infant phase, and because of the lack of its spectral properties, the application of MAD is now limited to the comparision of jet properties between observation and theory. In this project, we will simplify the numerical simulation results and create an easier description of the dynamical structure of MAD, and then we focus on its radiative properties. We will investigate the continuum, the polarision (in radio and X-rays), the radiative efficiency and maximal luminosity of this model. We further compare the emission of MAD to that of the widely-recognized theoretical model (SANE accretion model), to probe their differences. We eventually apply our understanding to Sgr A* and black hole X-ray binaries, to check if they can possibly enter the MAD regime.