An Indication for the Binarity of P Cygni from Its Seventeenth Century Eruption

TL;DR

The paper proposes that the 17th-century eruption of P Cygni was caused by mass transfer to a binary companion, suggesting all major LBV eruptions may involve binary interactions, with testable spectroscopic predictions.

Contribution

It introduces a binary interaction model for P Cygni's eruption, linking mass transfer to observed luminosity peaks and predicting a detectable orbital period.

Findings

Mass transfer of ~0.1 solar masses can explain the eruption energy.

Predicted orbital period of the companion is ~7 years.

Spectroscopic detection of Doppler shifts is possible.

Abstract

I show that the 17th century eruption of the massive luminous blue variable (LBV) star P Cygni can be explained by mass transfer to a B-type binary companion in an eccentric orbit, under the assumption that the luminosity peaks occurred close to periastron passages. The mass was accreted by the companion and liberated gravitational energy, part of which went to an increase in luminosity. I find that mass transfer of ~ 0.1 solar masses to a B-type binary companion of ~3-6 solar masses can account for the energy of the eruption, and for the decreasing time interval between the observed peaks in the visual light curve of the eruption. Such a companion is predicted to have an orbital period of ~7 years, and its Doppler shift should be possible to detect with high resolution spectroscopic observations. Explaining the eruption of P Cygni by mass transfer further supports the conjecture that all major LBV eruptions are triggered by interaction of an unstable LBV with a stellar companion.