We present three-dimensional simulations of a protoplanetary disk subject to the effect of a nearby ( 0.3 pc distant ) supernova , using a time-dependent flow from a one dimensional numerical model of the supernova remnant ( SNR ) , in addition to constant peak ram pressure simulations .
Simulations are performed for a variety of disk masses and inclination angles .
We find disk mass-loss rates that are typically 10 ^ { -7 } to 10 ^ { -6 } M _ { \sun } yr ^ { -1 } ( but peak near 10 ^ { -5 } M _ { \sun } yr ^ { -1 } during the ‘ ‘ instantaneous ’ ’ stripping phase ) and are sustained for around 200 yr .
Inclination angle has little effect on the mass loss unless the disk is close to edge-on .
Inclined disks also strip asymmetrically with the trailing edge ablating more easily .
Since the interaction lasts less than one outer rotation period , there is not enough time for the disk to restore its symmetry , leaving the disk asymmetrical after the flow has passed .
Of the low-mass disks considered , only the edge-on disk is able to survive interaction with the SNR ( with 50 % of its initial mass remaining ) .
At the end of the simulations , disks that survive contain fractional masses of SN material up to 5 \times 10 ^ { -6 } .
This is too low to explain the abundance of short-lived radionuclides in the early solar system , but a larger disk and the inclusion of radiative cooling might allow the disk to capture a higher fraction of SN material .