Investigating Shock Acceleration Physics in SN1006

SN1006 is a supernova remanent with X-ray and TeV emission concentrated into regions axisymmetric to the large-scale ambient magnetic field and roughly perpendicular to a large-scale density gradient roughly perpendicular. It is ideal for studying the differences between quasi-parallel and quasi-perpendicular shocks. We endeavor to characterize the spectra and morphology of SN1006 through variations in CR efficiency and magnetic field amplification. We investigate the shock acceleration physics of SN1006 with the aim of establishing the dependence of efficient CR acceleration on shock obliquity. We divide SN1006 into four quadrants, each with its own unique spectral signature, and model the shock dynamics separately. We estimate the non-thermal particle acceleration using a semi-analytic kinetic model of non-linear diffusive shock acceleration that accounts for the motion of magnetic fluctuations and amplification. We construct multi-wavelength spatially resolved spectra and radial profiles for each quadrant and compare with observations. We found that quasi-parallel shocks have efficient CR acceleration (about 20% efficiency), confirming the relationship between CR production and shock obliquity.