Hydrodynamic ablation of protoplanetary discs via supernovae

Abstract

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 yr −1 (but peak near 10 −5 M 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 × 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.

The consequences of a nearby supernova on the early solar system

“…For this latter supernova, the disk mass can be enriched with > ∼ 10 −6 up to a distance of ∼ 0.2 pc, whereas for SN10a this amount is only achieved at a Article number, page 17 of 26 distance of < ∼ 0.12 pc. These results are consistent with earlier calculations of disk enrichment by a nearby supernova Ouellette et al (2007); Close & Pittard (2017).…”

The viscous evolution of circumstellar discs in young star clusters

“…Wijnen et al (2016Wijnen et al ( , 2017 demonstrated that face-on accretion of ambient gas in embedded star-forming regions can cause circumstellar disks to contract, while the ram pressure exerted by the interstellar medium strips the outer parts of the disks. Nearby supernovae could also have imporant repercussions on the morphology and mass of circumstellar disks (Close & Pittard 2017;Portegies Zwart et al 2018), but since our clusters are very young we ingore this effect. Encounters between stars with disks could result in the exchange of disk-material from one to the other and affect the shape and mass of both disks (Jílková et al 2016).…”

External photoevaporation of circumstellar discs constrains the time-scale for planet formation

“…Another process that can have important consequences in the evolution of circumstellar disks are supernovae explosions. Close & Pittard (2017) showed that nearby (0.3 pc) supernova explosions can cause mass loss rates of up to 1 × 10 −5 M yr −1 which can be sustained for about 200 yr. Only disks that are faced with the flow face-on manage to survive, but still lose 50% of their mass in the process. Portegies show that a supernova explosion at a distance between 0.15 and 0.4 pc could create a misalignment of ∼ 5 • .6 between the star and its disk, which is consistent with the inclination of the plane of the Solar System.…”

“…Since a non negligible fraction of stars are not born in isolation (Bressert et al 2010;King et al 2012), and gas left over from the star formation process can linger for a few Myr (Portegies Zwart et al 2010), during their first stages of evolution the disks remain embedded in an environment that is dense in gas and neighbouring stars. These conditions can be hostile for the disks in a myriad of ways: they can be subject to dynamical truncations (Vincke et al 2015;Vincke & Pfalzner 2016) or be affected by processes related to stellar evolution, such as stellar winds (Pelupessy & Portegies Zwart 2012), supernovae explosions (Close & Pittard 2017;, and photoevaporation due to bright OB stars in the vicinity (e.g. Guarcello et al 2016;Haworth et al 2017).…”