Gravitational Slingshot of Young Massive Stars in Orion

Chatterjee, Sourav; Tan, Jonathan C.

doi:10.1088/0004-637x/754/2/152

Cited by 36 publications

(50 citation statements)

References 46 publications

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“…Tan (2004) argued that BN was ejected from the Trapezium roughly 4000 years ago as a result of an interaction with θ 1 Ori C, a compact binary with a total mass of 45 M . Chatterjee & Tan (2012) show that the observed orbital parameters of θ 1 C closely match the values required to eject BN, and argue that the likelihood that θ 1 C has these properties purely by chance is ∼ 10 −5 . Surprisingly, however, proper motion measurements indicate that SrcI is moving to the SE at 11.5±2.1 km s −1 (Goddi et al 2011), almost directly away from BN.…”

Section: Rethinking the Paradigmmentioning

confidence: 56%

ALMA OBSERVATIONS OF ORION SOURCE I AT 350 AND 660 GHz

Plambeck¹,

Wright

2016

ApJ

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Orion Source I ("SrcI") is the protostar at the center of the Kleinmann-Low Nebula. ALMA observations of SrcI with 0.2 angular resolution were made at 350 and 660 GHz to search for the H26α and H21α hydrogen recombination lines and to measure the continuum flux densities. The recombination lines were not detected, ruling out the possibility that SrcI is a hypercompact HII region. The deconvolved size of the continuum source is approximately 0. 23 × 0. 07 (∼ 100 × 30 AU); it is interpreted as a disk viewed almost edge-on. Optically thick thermal emission from ∼500 K dust is the most plausible source of the continuum, even at frequencies as low as 43 GHz; the disk mass is most likely in the range 0.02-0.2 M . A rich spectrum of molecular lines is detected, mostly from sulfur-and silicon-rich molecules like SO, SO 2 , and SiS, but also including vibrationally excited CO and several unidentified transitions. Lines with upper energy levels E U > 500 K appear in emission and are symmetric about the source's LSR velocity of 5 km s −1 , while lines with E U < 500 K appear as blueshifted absorption features against the continuum, indicating that they originate in outflowing gas. The emission lines exhibit a velocity gradient along the major axis of the disk that is consistent with rotation around a 5-7 M central object. The relatively low mass of SrcI and the existence of a 100 AU disk around it are difficult to reconcile with the model in which SrcI and the nearby Becklin-Neugebauer Object were ejected from a multiple system 500 years ago.

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Section: Rethinking the Paradigmmentioning

confidence: 56%

ALMA OBSERVATIONS OF ORION SOURCE I AT 350 AND 660 GHz

Plambeck¹,

Wright

2016

ApJ

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“…BN, thought to be an 8 to 15 M e star (Scoville et al 1983;Tan 2004;Goddi et al 2011b;Chatterjee & Tan 2012), is moving toward the northwest with respect to other stars in the Nebula. The proper motion has been measured to be 21.3 km s −1 toward PA=331° (Gómez et al 2008), 26.4 km s −1 toward PA=341° (Goddi et al 2011b), and 26.6 km s −1 toward PA=323° (Dzib et al 2016).…”

Section: Ejection Of Runaway Stars: Bn Source I and Source Nmentioning

confidence: 99%

“…The mass of the fastest ejected star, BN, has been estimated to be between 12 and 15M e  (Scoville et al 1983) or 8 to 10 M e  (Tan 2004;Chatterjee & Tan 2012). Assuming that Source I has an oppositely directed momentum, it must have a mass of 16-25 M e  (Goddi et al 2011b).…”

Section: The Masses Of the Omc1 Runaway Starsmentioning

confidence: 99%

The ALMA View of the OMC1 Explosion in Orion

Bally¹,

Ginsburg²,

Arce

et al. 2017

ApJ

105

157

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Most massive stars form in dense clusters where gravitational interactions with otherstars may be common. The two nearest forming massive stars, the BN object and Source I, located behind the Orion Nebula, were ejected with velocities of ∼29 and ∼13 km s −1 about 500 years ago by such interactions. This event generated an explosion in the gas. New ALMA observations show in unprecedented detail, a roughly spherically symmetric distribution of over a hundred 12 CO J=2−1 streamers with velocities extending from V LSR =−150 to +145 km s −1 . The streamer radial velocities increase (or decrease) linearly with projected distance from the explosion center, forming a "Hubble Flow" confined to within 50″ of the explosion center. They point toward the high proper-motion, shockexcited H 2 and [Fe II] "fingertips" and lower-velocity CO in the H 2 wakes comprising Orionʼs "fingers." In some directions, the H 2 "fingers" extend more than a factor of two farther from the ejection center than the CO streamers. Such deviations from spherical symmetry may be caused by ejecta running into dense gas or the dynamics of the N-body interaction that ejected the stars and produced the explosion. This ∼10 48 erg event may have been powered by the release of gravitational potential energy associated with the formation of a compact binary or a protostellar merger. Orion may be the prototype for a new class of stellar explosiozn responsible for luminous infrared transients in nearby galaxies.

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“…Because its proper motion is pointed away from the Trapezium stars, it has been proposed that BN was ejected 4000 years ago from a multiple system containing the most massive member of the Trapezium, θ 1 Ori C (Plambeck et al 1995;Tan 2004), which also helps explain some of the properties of that system (Chatterjee & Tan 2012). The proper motion of BN indicates that it may have passed near radio source I (Garay et al 1987;Churchwell et al 1987) in the KL Nebula ∼500 years ago.…”

Section: Introductionmentioning

confidence: 99%

New Evidence for the Dynamical Decay of a Multiple System in the Orion Kleinmann–Low Nebula*

Luhman

Robberto

Tan

et al. 2017

ApJL

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We have measured astrometry for members of the Orion Nebula Cluster with images obtained in 2015 with the Wide Field Camera 3 on board the Hubble Space Telescope. By comparing those data to previous measurements with NICMOS on Hubble in 1998, we have discovered that a star in the Kleinmann-Low Nebula, source x from Lonsdale et al. (1982), is moving with an unusually high proper motion of 29 mas yr −1 , which corresponds to 55 km s −1 at the distance of Orion. Previous radio observations have found that three other stars in the Kleinmann-Low Nebula (BN and sources I and n) have high proper motions (5-14 mas yr −1 ) and were near a single location ∼540 years ago, and thus may have been members of a multiple system that dynamically decayed. The proper motion of source x is consistent with ejection from that same location 540 years ago, which provides strong evidence that the dynamical decay did occur and that the runaway star BN originated in the Kleinmann-Low Nebula rather than the nearby Trapezium cluster. However, our constraint on the motion of source n is significantly smaller than the most recent radio measurement, which indicates that it did not participate in the event that ejected the other three stars.

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Gravitational Slingshot of Young Massive Stars in Orion

Cited by 36 publications

References 46 publications

ALMA OBSERVATIONS OF ORION SOURCE I AT 350 AND 660 GHz

ALMA OBSERVATIONS OF ORION SOURCE I AT 350 AND 660 GHz

The ALMA View of the OMC1 Explosion in Orion

New Evidence for the Dynamical Decay of a Multiple System in the Orion Kleinmann–Low Nebula*

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