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Precessing Jet and Large Dust Grains in the V380 Ori NE Star-forming Region

Choi, Minho and Kang, Miju and Lee, Jeong-Eun and Tatematsu, Ken’ichi and Kang, Sung-Ju and Sayers, Jack and Evans, Neal J., II and Cho, Jungyeon and Kwon, Jungmi and Park, Geumsook and Ohashi, Satoshi and Yoo, Hyunju and Lee, Youngung (2017) Precessing Jet and Large Dust Grains in the V380 Ori NE Star-forming Region. Astrophysical Journal Supplement Series, 232 (2). Art. No. 24. ISSN 1538-4365.

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The V380 Ori NE bipolar outflow was imaged in the SiO and CO J = 1 → 0 lines, and dense cores in L1641 were observed in the 2.0–0.89 mm continuum. The highly collimated SiO jet shows point-symmetric oscillation patterns in both position and velocity, which suggests that the jet axis is precessing and the driving source may belong to a non-coplanar binary system. By considering the position and velocity variabilities together, accurate jet parameters were derived. The protostellar system is viewed nearly edge-on, and the jet has a flow speed of ~35 km s^(−1) and a precession period of ~1600 years. The CO outflow length gives a dynamical timescale of ~6300 years, and the protostar must be extremely young. The inferred binary separation of 6–70 au implies that this protobinary system may have been formed through the disk instability process. The continuum spectra of L1641 dense cores indicate that the emission comes from dust, and the fits with modified blackbody functions give emissivity power indices of β = 0.3–2.2. The emissivity index shows a positive correlation with the molecular line width, but no strong correlation with bolometric luminosity or temperature. V380 Ori NE has a particularly low value of β = 0.3, which tentatively suggests the presence of millimeter-sized dust grains. Because the dust growth takes millions of years, much longer than the protostellar age, this core may have produced large grains in the starless core stage. HH 34 MMS and HH 147 MMS also have low emissivity indices.

Item Type:Article
Related URLs:
URLURL TypeDescription
Kang, Miju0000-0002-5016-050X
Lee, Jeong-Eun0000-0003-3119-2087
Tatematsu, Ken’ichi0000-0002-8149-8546
Kang, Sung-Ju0000-0002-5004-7216
Sayers, Jack0000-0002-8213-3784
Evans, Neal J., II0000-0001-5175-1777
Cho, Jungyeon0000-0003-1725-4376
Kwon, Jungmi0000-0003-2815-7774
Park, Geumsook0000-0001-8467-3736
Additional Information:© 2017 The American Astronomical Society. Received 2017 May 25; revised 2017 September 7; accepted 2017 September 7; published 2017 October 9. We thank the TRAO and the CSO staffs for their support. NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. M. Kang was supported by Basic Science Research Program through the National Research Foundation of Korea funded by the Ministry of Science and ICT (grant No. NRF-2015R1C1A1A01052160). J.-E. Lee was supported by the Basic Science Research Program through the National Research Foundation of Korea (grant No. NRF-2015R1A2A2A01004769) and the Korea Astronomy and Space Science Institute under the R&D program (Project No. 2015-1-320-18) supervised by the Ministry of Science and ICT.
Funding AgencyGrant Number
National Research Foundation of KoreaNRF-2015R1C1A1A01052160
National Research Foundation of KoreaNRF-2015R1A2A2A01004769
Korea Astronomy and Space Science Institute (KASI)2015-1-320-18
Subject Keywords:dust, extinction – ISM: individual objects (V380 Ori NE) – ISM: jets and outflows – ISM: structure – stars: formation – stars: protostars
Issue or Number:2
Record Number:CaltechAUTHORS:20171009-151932855
Persistent URL:
Official Citation:Minho Choi et al 2017 ApJS 232 24
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:82233
Deposited By: Tony Diaz
Deposited On:09 Oct 2017 22:35
Last Modified:07 Nov 2019 00:11

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