Tracing the large-scale magnetic field morphology in protoplanetary disks using molecular line polarization

(abridged) Magnetic fields are fundamental to the accretion dynamics of protoplanetary disks and they likely affect planet formation. Typical methods study magnetic field morphology observe polarization dust or spectral lines. However, it has recently become clear that dust-polarization in ALMA's regime does not always faithfully trace structure disks, which leaves line as a promising method for mapping morphologies such sources. We aim model emergent different molecular lines ALMA wavelength excited disks. explore variety disk models molecules identify those properties conducive emergence may therefore be viably used measurements PORTAL conjunction with LIME. Together, allowed us treat polarized radiative transfer complex three-dimensional physical structures. present simulations transitions regime. find thermalize at high densities, HCN, also most susceptible polarization. expected significantly while low CO, only outer regions. simulated maps range inclinations morphologies, we comment on observational feasibility linear observations