A MULTI-EPOCH STUDY OF THE RADIO CONTINUUM EMISSION OF ORION SOURCE. I. CONSTRAINTS ON THE DISK EVOLUTION OF A MASSIVE YSO AND THE DYNAMICAL HISTORY OF ORION BN/KL

We present new λ7 mm continuum observations of Orion BN/KL with the Very Large Array. We resolve the emission from the young stellar objects radio Source I and BN at several epochs. Radio Source I is highly elongated northwest-southeast, and remarkably stable in flux density, position angle, and ove...

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Bibliographic Details
Main Authors: Goddi, C. (Author), Humphreys, E. M. L. (Author), Greenhill, Lincoln J. (Author), Chandler, C. J. (Author), Matthews, Lynn D. (Contributor)
Other Authors: Haystack Observatory (Contributor)
Format: Article
Language:English
Published: Institute of Physics/American Astronomical Society, 2015-02-27T16:35:19Z.
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Online Access:Get fulltext
LEADER 02878 am a22002293u 4500
001 95732
042 |a dc 
100 1 0 |a Goddi, C.  |e author 
100 1 0 |a Haystack Observatory  |e contributor 
100 1 0 |a Matthews, Lynn D.  |e contributor 
700 1 0 |a Humphreys, E. M. L.  |e author 
700 1 0 |a Greenhill, Lincoln J.  |e author 
700 1 0 |a Chandler, C. J.  |e author 
700 1 0 |a Matthews, Lynn D.  |e author 
245 0 0 |a A MULTI-EPOCH STUDY OF THE RADIO CONTINUUM EMISSION OF ORION SOURCE. I. CONSTRAINTS ON THE DISK EVOLUTION OF A MASSIVE YSO AND THE DYNAMICAL HISTORY OF ORION BN/KL 
260 |b Institute of Physics/American Astronomical Society,   |c 2015-02-27T16:35:19Z. 
856 |z Get fulltext  |u http://hdl.handle.net/1721.1/95732 
520 |a We present new λ7 mm continuum observations of Orion BN/KL with the Very Large Array. We resolve the emission from the young stellar objects radio Source I and BN at several epochs. Radio Source I is highly elongated northwest-southeast, and remarkably stable in flux density, position angle, and overall morphology over nearly a decade. This favors the extended emission component arising from an ionized edge-on disk rather than an outwardly propagating jet. We have measured the proper motions of Source I and BN for the first time at 43 GHz. We confirm that both sources are moving at high speed (12 and 26 km s-1, respectively) approximately in opposite directions, as previously inferred from measurements at lower frequencies. We discuss dynamical scenarios that can explain the large motions of both BN and Source I and the presence of disks around both. Our new measurements support the hypothesis that a close (~50 AU) dynamical interaction occurred around 500 years ago between Source I and BN as proposed by Gomez et al. From the dynamics of encounter, we argue that Source I today is likely to be a binary with a total mass on the order of 20 M ☉ and that it probably existed as a softer binary before the close encounter. This enables preservation of the original accretion disk, though truncated to its present radius of ~50 AU. N-body numerical simulations show that the dynamical interaction between a binary of 20 M ☉ total mass (Source I) and a single star of 10 M ☉ mass (BN) may lead to the ejection of both and binary hardening. The gravitational energy released in the process would be large enough to power the wide-angle, high-velocity flow traced by H2 and CO emission in the BN/KL nebula. Assuming that the proposed dynamical history is correct, the smaller mass for Source I recently estimated from SiO maser dynamics (gsim7 M ☉) by Matthews et al., suggests that non-gravitational forces (e.g., magnetic) must play an important role in the circumstellar gas dynamics. 
520 |a National Science Foundation (U.S.) (NSF AST 0507478) 
546 |a en_US 
655 7 |a Article 
773 |t Astrophysical Journal