Stellar collision may explain why Orion Nebula's planet-forming disks appear younger than its stars

Stellar collision may explain why Orion Nebula's planet-forming disks appear younger than its stars Lisa Lock Scientific Editor Robert Egan Senior Editor The Orion Nebula is a large star-forming region visible to the naked eye. Some of the young stars in the nebula are surrounded by disks of gas and dust in which planets form. Radiation from the massive central star, 1 Ori C1 (Theta-1 Orionis C1), gradually strips material from these disks, giving them shapes that resemble tadpoles. The disks are losing mass so rapidly that, given the age of the stars (around 1 million years), they should have disappeared long ago. The large gas shell surrounding the central star poses another puzzle. The star sets the surrounding gas in motion, causing the shell to expand at around 13 kilometers per second (8 miles per second). Extrapolating backward from this speed suggests that the shell formed only a few hundred thousand years ago. The stars are therefore much older than both the gas shell and the dust disks (the "tadpoles") appear to be. This is the age paradox of the Orion Nebula. A simulated stellar collision Leiden astronomer Maite Wilhelm and her colleagues propose a new scenario that could explain both puzzles. They suggest that 1 Ori C1, which has a mass around 33.5 times that of the sun, formed when a binary star system merged. A binary system consists of two stars that orbit a common center of mass under the influence of their mutual gravity. The researchers suspect that a third star disrupted the system, knocking one of the stars out of its stable orbit and eventually causing the two stars to collide. If the two stars did merge a few hundred thousand years ago, the resulting star's luminosity (the amount of light it emits) must have increased sharply from that point onward. The researchers used computer simulations to investigate whether this scenario could explain the observations. The study is published in the journal Astronomy & Astrophysics. Simulations support the scenario The simulations showed that the scenario is plausible. Before the collision, the two stars emitted much less radiation, allowing the surrounding dust disks to survive for most of their lifetime. Only after the merger did the star's radiation increase sharply, triggering the rapid evaporation of the disks. The rapid expansion of the gas shell, however, requires an additional explanation. The merger alone is estimated to provide 30 times more driving force, whereas a factor of 100 is needed to explain the observed expansion. The researchers suspect that cool gas from the evaporating dust disks also plays a role. As this gas mixes with the hot gas inside the expanding bubble, it could provide the additional driving force needed. The proposed scenario could also account for two other unusual features of 1 Ori C1: its observed tilted magnetic field and a slight excess of nitrogen in the star. More stellar collisions in our cosmic neighborhood than previously thought Co-author Simon Portegies Zwart is enthusiastic about the findings. "This is the first time we have witnessed the consequences of a major stellar collision in our own cosmic neighborhood. It also shows that stellar collisions may be much more common than we previously thought, and that they can have far-reaching consequences." Wilhelm adds, "Our idea shows that subtle effects in triple-star systems can have a major impact on the environments in which stars form, and potentially even on planets that are still taking shape." Publication details M. J. C. Wilhelm et al., A triple-induced merger in θ1 solves the proplyd lifetime problem and the curiously young shell of M42, Astronomy & Astrophysics (2026). DOI: 10.1051/0004-6361/202662018 Journal information: Astronomy & Astrophysics Provided by Leiden University