Evolution of massive stellar triples and implications for compact object binary formation

ABSTRACT Most back hole and neutron star progenitors are found in triples or higher multiplicity systems. Here, we present a new triple stellar evolution code, ${\tt TSE}$, which simultaneously takes into account the physics of stars their gravitational interaction. TSE}$ is used to simulate massive galactic field from zero-age main sequence until they form compact objects. To this end, implement initial conditions that incorporate observed high correlation between orbital parameters early-type stars. We show interaction with tertiary companion can significantly impact inner binary. High eccentricities be induced by third-body dynamical effects, leading Roche lobe overflow even merger binary separations 103–$10^5\, \rm R_\odot$. In $\sim 5\, {{\ per\ cent}}$ systems, itself fills its lobe, while 10\, all systems become dynamically unstable. find $0.3{{\ $5{{\ stable an object binary, where exact fraction depends on metallicity natal kick prescription. these black holes companions. no any surviving triple, unless zero kicks assumed. About half binaries formed our models triples, majority, perturb long-term evolution. Our results interactions key full understanding formation.