The Exotic Eclipsing Nucleus of the Ring Planetary Nebula SuWt2

TL;DR

This paper investigates the central binary of the planetary nebula SuWt2, revealing a triple system with two A-type stars in a short-lived evolutionary phase, and proposes a formation scenario involving common envelope evolution and potential supernova fate.

Contribution

It provides detailed characterization of the central binary, suggests a hierarchical triple origin, and links the system's evolution to planetary nebula formation and supernova potential.

Findings

The binary consists of two nearly identical A1 V stars with a 4.9-day period.

The system is approximately 520 million years old, with stars in the 'blue-hook' phase.

The system likely includes an unseen third body, possibly a white dwarf, indicating a hierarchical triple origin.

Abstract

SuWt2 is a planetary nebula (PN) consisting of a bright ionized thin ring seen nearly edge-on. It has a bright (V=12) central star, too cool to ionize the PN, which we discovered to be an eclipsing binary. A spectrum from IUE did not reveal a UV source. We present extensive ground-based photometry and spectroscopy of the central binary collected over the ensuing two decades, resulting in the determination that the orbital period of the eclipsing pair is 4.9 d, and consists of two nearly identical A1 V stars, each of mass ~2.7 M_sun. The physical parameters of the A stars, combined with evolutionary tracks, show that both are in the short-lived "blue-hook" evolutionary phase that occurs between the main sequence and the Hertzsprung gap, and that the age of the system is about 520 Myr. One puzzle is that the stars' rotational velocities are different from each other, and considerably slower than synchronous with the orbital period. It is possible that the center-of-mass velocity of the eclipsing pair is varying with time, suggesting that there is an unseen third orbiting body in the system. We propose a scenario in which the system began as a hierarchical triple, consisting of a ~2.9 M_sun star orbiting the close pair of A stars. Upon reaching the AGB stage, the primary engulfed the pair into a common envelope, leading to a rapid contraction of the orbit and catastrophic ejection of the envelope into the orbital plane. In this picture, the exposed core of the initial primary is now a white dwarf of ~0.7 M_sun, orbiting the eclipsing pair, which has already cooled below the detectability possible by IUE at our derived distance of 2.3 kpc and a reddening of E(B-V)=0.40. The SuWt2 system may be destined to perish as a Type Ia supernova. (Abridged)