HD 49798: Its History of Binary Interaction and Future Evolution

TL;DR

This study models the binary system HD 49798 to understand its past and future evolution, considering both white dwarf and neutron star companions, and discusses potential outcomes like pulsar formation.

Contribution

It provides detailed stellar evolution simulations of HD 49798 with both WD and NS companions, clarifying the system's possible evolutionary paths and final states.

Findings

A neutron star companion is more likely based on spin measurements.

Future evolution could lead to a binary pulsar or a solitary millisecond pulsar.

Mass transfer rates could resemble those in ultraluminous X-ray sources.

Abstract

The bright subdwarf-O star (sdO), HD 49798, is in a 1.55 day orbit with a compact companion that is spinning at 13.2 seconds. Using the measurements of the effective temperature ($T_{\rm eff}$), surface gravity ($\log g$), and surface abundances of the sdO, we construct models to study the evolution of this binary system using Modules for Experiments in Stellar Astrophysics ($\texttt{MESA}$). Previous studies of the compact companion have disagreed on whether it is a white dwarf (WD) or a neutron star (NS). From the published measurements of the companion's spin and spin-up rate, we agree with Mereghetti and collaborators that a NS companion is more likely. However, since there remains the possibility of a WD companion, we use our constructed $\texttt{MESA}$ models to run simulations with both WD and NS companions that help us constrain the past and future evolution of this system. If it presently contains a NS, the immediate mass transfer evolution upon Roche lobe (RL) filling will lead to mass transfer rates comparable to that implied in ultraluminous X-ray sources (ULXs). Depending on the rate of angular momentum extraction via a wind, the fate of this system is either a wide ($P_{\rm orb}{\approx} 3$ day) intermediate mass binary pulsar (IMPB) with a relatively rapidly spinning NS (${\approx} 0.3$ s) and a high mass WD (${\approx} 0.9 M_\odot$), or a solitary millisecond pulsar (MSP).