Becklin–Neugebauer Object

BN moves towards the northwest with respect to other stars in the Kleinmann-Low nebula. A proper motion of between 21 and 27 km/s in the northwest region and a redshift of about 11 km/s with respect to the OMC1 was measured for this star. BN is therefore considered a runaway star.{{Cite journal |last1=Bally |first1=John |last2=Ginsburg |first2=Adam |last3=Arce |first3=Hector |last4=Eisner |first4=Josh |last5=Youngblood |first5=Allison |last6=Zapata |first6=Luis |last7=Zinnecker |first7=Hans |date=2017-03-01 |title=The ALMA View of the OMC1 Explosion in Orion |journal=The Astrophysical Journal |volume=837 |issue=1 |pages=60 |doi=10.3847/1538-4357/aa5c8b |arxiv=1701.01906 |bibcode=2017ApJ...837...60B |issn=0004-637X|hdl=10150/623202 |s2cid=119348763 |hdl-access=free |doi-access=free }}

It was proposed that Theta1Ori C ejected BN about 4000 years ago, but it is more likely that BN and two other runaway stars, called Source I (Src I) and Source n (Src n), were ejected from a position about 500 years ago. Source I and Source n both move in opposite directions, away from BN.

With more recent VLA proper motion measurements it was realised that at least six compact sources recede from a common point: BN, source I, Orion MR (formerly source n), X, IRc23 and Zapata 11. Almost all these sources were ejected about 500 years ago.{{Cite journal |last1=Rodríguez |first1=Luis F. |last2=Dzib |first2=Sergio A. |last3=Zapata |first3=Luis |last4=Lizano |first4=Susana |last5=Loinard |first5=Laurent |last6=Menten |first6=Karl M. |last7=Gómez |first7=Laura |date=2020-04-01 |title=Proper Motions of the Radio Source Orion MR, Formerly Known as Orion n, and New Sources with Large Proper Motions in Orion BN/KL |journal=The Astrophysical Journal |volume=892 |issue=2 |pages=82 |doi=10.3847/1538-4357/ab7816 |arxiv=2002.12513 |bibcode=2020ApJ...892...82R |issn=0004-637X|doi-access=free }} The ejection of BN and source I was proposed to have occurred in the year 1475±6 (about 550 years ago).{{Cite journal |last1=Rodríguez |first1=Luis F. |last2=Dzib |first2=Sergio A. |last3=Loinard |first3=Laurent |last4=Zapata |first4=Luis |last5=Gómez |first5=Laura |last6=Menten |first6=Karl M. |last7=Lizano |first7=Susana |date=2017-01-01 |title=The Proper Motions of the Double Radio Source n in the Orion BN/KL Region |journal=The Astrophysical Journal |volume=834 |issue=2 |pages=140 |doi=10.3847/1538-4357/834/2/140 |issn=0004-637X|arxiv=1612.00107 |bibcode=2017ApJ...834..140R |s2cid=119470863 |doi-access=free }} IRc23 was ejected only 300 years ago.

At the time of the ejection four or more protostars dynamically interacted with each other, leading to the ejection of the stars in different directions. In the classical three-body scenario, the dynamical interaction either formed a compact binary or the merger of two stars. The large number of ejected stars suggest a more complex interaction, such as the interaction of a tight binary with a compact star cluster.

This dynamical interaction released a large amount of energy, causing an infrared-only flare on the scale of a nova or supernova with an energy of about 10⁴⁸ erg.

Alternatively the explosion was not a multi-system interaction but a supernova.{{Cite journal |last1=Raga |first1=A. C. |last2=Rivera-Ortiz |first2=P. R. |last3=Cantó |first3=J. |last4=Rodríguez-González |first4=A. |last5=Castellanos-Ramírez |first5=A. |date=2021-11-01 |title=An orbital release model for the Orion BN/KL fingers |journal=Monthly Notices of the Royal Astronomical Society |volume=508 |issue=1 |pages=L74–L78 |doi=10.1093/mnrasl/slab072 |doi-access=free |issn=0035-8711|arxiv=2107.11189 |bibcode=2021MNRAS.508L..74R }}

{{Main articles|Kleinmann–Low Nebula}}

The remnant of the explosion is called Kleinmann-Low nebula.{{Cite web |title=APOD: March 2, 1999 - The Kleinmann Low Nebula |url=https://apod.nasa.gov/apod/ap990302.html |access-date=2022-09-26 |website=apod.nasa.gov}} Multi-wavelength observations and carbon monoxide (CO) observations with ALMA reveal the mostly spherical remnant of an explosion at the intersection point of the BN object and Source I. The ALMA observations revealed hundreds of CO streamers moving with up to 100 km/s. Some of these CO streamers nearly reach the shocked gas and dust observed in molecular hydrogen and iron [Fe II].

Becklin's star (IRC -10093) is located at 5h 35.3m / -5° 23', very near the Becklin-Neugebauer object.Sky Catalogue 2000.0, Volume 2: Double Stars, Variable Stars and Nonstellar Objects - Glossary of Selected Astronomical Names, page xlv

File:Becklin-Neugebauer object JHK.jpg|The BN object (bright star in the center) in near-infrared with ESO HAWKI.

File:ESO-M42-Phot-03a-01.jpg|Near-infrared view of the central region of the Orion Nebula. In the center is the Trapezium cluster and the red region above contains the BN object.

File:STScI-01EVVBQ8Q34VVZ562Q0MK3GE86.png|Hubble image showing the proper motion of source x away from the explosion center. The image also shows the BN object.

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{{Stars of Orion}}

{{DEFAULTSORT:Becklin-Neugebauer Object}}

Category:Orion (constellation)

Category:Orion molecular cloud complex

Category:Star formation

Category:Protostars

Orionis, V2254