On the Formation of Runaway Stars BN and x in the Orion Nebula Cluster

Abstract

We explore scenarios for the dynamical ejection of stars BN and x from source I in the Kleinmann-Low nebula of the Orion Nebula Cluster (ONC), which is important for being the closest region of massive star formation. This ejection would cause source I to become a close binary or a merger product of two stars. We thus consider binary-binary encounters as the mechanism to produce this event. By running a large suite of $N$-body simulations, we find that it is nearly impossible to match the observations when using the commonly adopted masses for the participants, especially a source I mass of $7{\mathrm{M}}_{\odot }$. The only way to recreate the event is if source I is more massive, i.e., $\sim 20{\mathrm{M}}_{\odot }$. However, even in this case, the likelihood of reproducing the observed system is low. We discuss the implications of these results for understanding this important star-forming region.

7 pages, 4 figures, 1 table. Accepted by A&A Letters

References in corpus (6)

• The distance to the Orion Nebula
• The Gould's Belt Distances Survey (GOBELINS) II. Distances and structure towards the Orion Molecular Clouds
• The ALMA View of the OMC1 Explosion in Orion
• ALMA Observations of Orion Source I at 350 and 660 GHz
• The Proper Motions of the Double Radio Source n in the Orion BN/KL Region
• New Evidence for the Dynamical Decay of a Multiple System in the Orion Kleinmann-Low Nebula

Cited by in corpus (12)

• A Keplerian disk around Orion Source I, a ~15 Msun YSO
• Runaway and walkaway stars from the ONC with Gaia DR2
• Evidence for feedback and stellar-dynamically regulated bursty star cluster formation: the case of the Orion Nebula Cluster
• Stellar Proper Motions in the Orion Nebula Cluster
• The Orion Protostellar Explosion and Runaway Stars Revisited: Stellar Masses, Disk Retention, and an Outflow from BN
• Hunting for Runaways from the Orion Nebula Cluster
• OMC-1 dust polarisation in ALMA Band 7: Diagnosing grain alignment mechanisms in the vicinity of Orion Source I
• A 10-$M_{\odot }$ YSO with a Keplerian disk and a nonthermal radio jet
• Structure of the Source I disk in Orion-KL
• High spectral resolution observations toward Orion BN at 6 $\mu$m: no evidence for hot water
• Double trouble: Gaia reveals (proto)-planetary systems that may experience more than one dense star-forming environment
• Formation of Orion Fingers