2004/01/31 by Jonathan C. Tan · 12 citations
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/421721
published as Astrophys.J. 607 (2004) L47-L50 · 6 pages, accepted to ApJ Letters
arxiv created 2004/04/07 · openalex publication_date 2004/04/22 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/01
We attempt to explain the properties of the Becklin-Neugebauer (BN) object as a runaway B star, as originally proposed by Plambeck et al. This is one of the best-studied bright infrared sources, located in the Orion Nebula Cluster—an important testing ground for massive star formation theories. From radio observations of the BN object's proper motion, we trace its trajectory back to Trapezium star θ 1 Ori C, the most massive (45 M ☉ ) in the cluster and a relatively tight (17 AU) visual binary with a B star secondary. This origin would be the most recent known runaway B star ejection event, occurring only ~4000 years ago and providing a unique test of ejection models. Although highly obscured, we can constrain the BN object's mass (≃7 M ☉ ) from both its bolometric luminosity and the recoil of θ 1 Ori C. Interaction of a runaway B star with dense ambient gas should produce a compact wind bow shock. We suggest that X-ray emission from this shocked gas may have been seen by Chandra : the offset from the radio position is ≃300 AU in the direction of the BN object's motion. Given this model, we constrain the ambient density, wind mass-loss rate, and wind velocity. The BN object made its closest approach to the massive protostar, source "I," 500 years ago. This may have triggered enhanced accretion and thus outflow, consistent with previous interpretations of the outflow being a recent (~10 3 yr) "explosive" event.