Runaway stars as progenitors of supernovae and gamma-ray bursts

TL;DR

This study models the velocities and evolution of runaway stars and binaries resulting from supernovae, predicting their distances traveled and implications for supernovae, gamma-ray bursts, and compact object mergers.

Contribution

It provides comprehensive population synthesis predictions for runaway stars, their velocities, and their role as progenitors of various supernovae and gamma-ray bursts, including effects of asymmetric black hole kicks.

Findings

Predicted runaway OB star velocities broadly match observations.

Black holes likely receive asymmetric kicks to explain fastest WR runaways.

Type IIP supernova progenitors can travel up to 48 pc on average.

Abstract

When a core collapse supernova occurs in a binary system, the surviving star as well as the compact remnant emerging from the SN, may reach a substantial space velocity. With binary population synthesis modelling at solar and one fifth of solar metallicity, we predict the velocities of such runaway stars or binaries. We compile predictions for runaway OB stars, red supergiants and Wolf-Rayet stars. For those stars or binaries which undergo a second stellar explosion we compute their further evolution and the distance travelled until a Type II or Type Ibc SN or a long or short gamma-ray burst occurs. We find our predicted population of OB runaway stars broadly matches the observed population of stars but, to match the fastest observed WR runaway stars, we require that black holes receive an asymmetric kick upon formation. We find that at solar metallicity Type Ic SN progenitors travel shorter distances than the progenitors of other SN types because they are typically more massive and thus have shorter lifetimes. Those of Type IIP SN can fly farthest about 48 pc on average at solar metallicity. In considering the consequences of assuming that the progenitors of long GRBs are spun-up secondary stars that experience quasi-homogeneous evolution, we find that such evolution has a dramatic effect on the population of runaway WR stars and that some 30 per cent of GRBs could occur a hundred parsecs or more from their initial positions. We also consider mergers of double compact object binaries consisting of neutron stars and/or black holes. We find the most common type of visible mergers are neutron star--black hole mergers that are roughly ten times more common than neutron star--neutron star mergers. We also find that there may be a population of low-velocity neutron stars that are ejected from a binary rather than by their own natal kick.