The Complete Evolution of a Neutron-star Binary through a Common Envelope Phase Using 1D Hydrodynamic Simulations

• Published in: Astrophysical journal. Letters 2019-10, Vol.883 (2), p.L45
• Main Authors: Fragos, Tassos, Andrews, Jeff J., Ramirez-Ruiz, Enrico, Meynet, Georges, Kalogera, Vicky, Taam, Ronald E., Zezas, Andreas
• Format: Article
• Language: English
• Subjects: Binary pulsars; Binary stars; Cataclysmic variables; Close binary stars; Coalescing; Compact binary stars; Compact objects; Companion stars; Computer simulation; Drag; Gravitational wave astronomy; Gravitational wave sources; Helium; High mass X-ray binary stars; Hydrogen; Interacting binary stars; Low-mass X-ray binary stars; Mass transfer; Massive stars; Neutron stars; Neutrons; Parameter estimation; Red giant stars; Separation; Spirals; Star formation; Stellar evolution; Stellar system evolution; Supergiant stars; X ray binaries; X ray sources; X ray stars; X-ray binary stars
• ISSN: 2041-8205; 2041-8213
• DOI: 10.3847/2041-8213/ab40d1

Over 40 years of research suggests that the common envelope phase, in which an evolved star engulfs its companion upon expansion, is the critical evolutionary stage forming short-period, compact-object binary systems, such as coalescing double compact objects, X-ray binaries, and cataclysmic variables. In this work, we adapt the one-dimensional hydrodynamic stellar evolution code, MESA, to model the inspiral of a 1.4 M neutron star (NS) inside the envelope of a 12 M red supergiant star. We self-consistently calculate the drag force experienced by the NS and the back-reaction onto the expanding envelope as the NS spirals in. Nearly all of the hydrogen envelope escapes, expanding to large radii (∼102 au) where it forms an optically thick envelope with temperatures low enough that dust formation occurs. We simulate the NS orbit until only 0.8 M of the hydrogen envelope remains around the giant star's core. Our results suggest that the inspiral will continue until another 0.3 M are removed, at which point the remaining envelope will retract. Upon separation, a phase of dynamically stable mass transfer onto the NS accretor is likely to ensue, which may be observable as an ultraluminous X-ray source. The resulting binary, comprised of a detached 2.6 M helium star and an NS with a separation of 3.3-5.7 R , is expected to evolve into a merging double neutron-star, analogous to those recently detected by LIGO/Virgo. For our chosen combination of binary parameters, our estimated final separation (including the phase of stable mass transfer) suggests a very high CE-equivalent efficiency of 5.