Periastron Passage Triggering of the 19th Century Eruptions of Eta Carinae

TL;DR

This paper models Eta Carinae's 19th-century eruptions as triggered by binary periastron passages, constraining system parameters and suggesting stellar companions often trigger luminous blue variable eruptions.

Contribution

It introduces a binary interaction model linking periastron passages to major stellar eruptions, with new constraints on the system's mass and evolutionary behavior.

Findings

Eruptions likely triggered by periastron passages.

Total binary mass constrained to over 250 solar masses.

Mass transfer explains eruption energy and light curve peaks.

Abstract

We reconstruct the evolution of Eta Carinae in the last two centuries, under the assumption that the two 19th century eruptions were triggered by periastron passages, and by that constrain the binary parameters. The beginning of the Lesser Eruption (LE) at the end of the 19th century occurred when the system was very close to periastron passage, suggesting that the secondary triggered the LE. We assume that the 1838-1858 Great Eruption (GE) was triggered by a periastron passage as well. We also assume that mass transferred from the primary to the secondary star accounts for the extra energy of the GE. With these assumptions we constrain the total mass of the binary system to be M=M_1+M_2>~250 solar masses. These higher than commonly used masses better match the observed luminosity with stellar evolutionary tracks. Including mass loss by the two stars and mass transfer from the primary to the secondary we obtain a good match of periastron passages to the two peaks in the light curve of the GE. Based on these finding and a similar behavior of P Cygni, we speculate that major LBV eruptions are triggered by stellar companions, and that in extreme cases a short duration event with a huge mass transfer rate can lead to a bright transient event on time scales of weeks to months (a ``supernova impostor'').