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In this Letter, we provide constraints on the direction and magnitude of thepristine (i.e., unperturbed by the interaction with the Sun) local interstellarmagnetic field. The constraints are based on analysis of the interstellarmagnetic field components at the heliopause measured by magnetometerinstruments on board Voyager 1 and 2 spacecraft. The analysis was performedwith the help of our kinetic-magnetohydrodynamical (MHD) model of the globalheliosphere. The model shows that the solar-induced disturbances of theinterstellar magnetic field are extended relatively far from the Sun up to400-500 AU. The field is draped around the heliopause and compressed. Bycomparison of the model results with Voyager data we found that the modelprovides results comparable with the data for the interstellar magnetic fieldof  $B_{LISM}$ = 3.7-3.8 $\mu$G in magnitude and directed towards$\approx$125$^\circ$ in longitude, and $\approx$37$^\circ$ in latitude in theheliographic inertial (HGI) coordinate system.

Magnitude and direction of the local interstellar magnetic field inferred from Voyager 1 and 2 interstellar data and global heliospheric model