TY - JOUR
T1 - Disk Structure around the Class i Protostar L1489 IRS Revealed by ALMA
T2 - A Warped-disk System
AU - Sai, Jinshi
AU - Ohashi, Nagayoshi
AU - Saigo, Kazuya
AU - Matsumoto, Tomoaki
AU - Aso, Yusuke
AU - Takakuwa, Shigehisa
AU - Aikawa, Yuri
AU - Kurose, Ippei
AU - Yen, Hsi Wei
AU - Tomisaka, Kohji
AU - Tomida, Kengo
AU - MacHida, Masahiro N.
N1 - Funding Information:
We thank M. Yamaguchi for the fruitful discussion. J.S. was supported by the Subaru Telescope Internship Program and is supported by Academia Sinica Institute of Astronomy and Astrophysics. S.T. acknowledges a grant from JSPS KAKENHI grant No. JP18K03703 in support of this work. T.M. is supported by the JSPS KAKENHI grant Nos. JP18H05436, JP18H05437, JP17K05394, and JP17H02863. Y.A. is grateful for NAOJ ALMA scientific Research grant No. of 2019-13B. H.-W.Y. acknowledges support from MOST 108-2112-M-001-003-MY2. This work was supported by NAOJ ALMA Scientific Research grant No. 2017-04A.
Funding Information:
2020-04-01 2020-04-15 14:10:52 cgi/release: Article released bin/incoming: New from .zip JSPS KAKENHI JP18K03703 NAOJ ALMA scientific Research 2019-13B MOST 108-2112-M-001-003-MY2 JSPS KAKENHI JP18H05436 JSPS KAKENHI JP18H05437 JSPS KAKENHI JP17K05394 JSPS KAKENHI JP17H02863 yes
Publisher Copyright:
© 2020. The American Astronomical Society. All rights reserved.
PY - 2020/4/10
Y1 - 2020/4/10
N2 - We have observed the Class I protostar L1489 IRS with the Atacama Millimeter/submillimeter Array (ALMA) in Band 6. The C18O J = 2-1 line emission shows flattened and non-axisymmetric structures in the same direction as its velocity gradient due to rotation. We discovered that the C18O emission shows dips at a radius of ∼200-300 au while the 1.3 mm continuum emission extends smoothly up to r ∼ 400 au. At the radius of the C18O dips, the rotational axis of the outer portion appears to be tilted by ∼15° from that of the inner component. Both the inner and outer components with respect to the C18O dips exhibit the r -0.5 Keplerian rotation profiles until r ∼ 600 au. These results not only indicate that a Keplerian disk extends up to ∼600 au but also that the disk is warped. We constructed a three-dimensional warped-disk model rotating at the Keplerian velocity, and demonstrated that the warped-disk model reproduces main observed features in the velocity channel maps and the PV diagrams. Such a warped-disk system can form by mass accretion from a misaligned envelope. We also discuss a possible disk evolution scenario based on comparisons of disk radii and masses between Class I and Class II sources.
AB - We have observed the Class I protostar L1489 IRS with the Atacama Millimeter/submillimeter Array (ALMA) in Band 6. The C18O J = 2-1 line emission shows flattened and non-axisymmetric structures in the same direction as its velocity gradient due to rotation. We discovered that the C18O emission shows dips at a radius of ∼200-300 au while the 1.3 mm continuum emission extends smoothly up to r ∼ 400 au. At the radius of the C18O dips, the rotational axis of the outer portion appears to be tilted by ∼15° from that of the inner component. Both the inner and outer components with respect to the C18O dips exhibit the r -0.5 Keplerian rotation profiles until r ∼ 600 au. These results not only indicate that a Keplerian disk extends up to ∼600 au but also that the disk is warped. We constructed a three-dimensional warped-disk model rotating at the Keplerian velocity, and demonstrated that the warped-disk model reproduces main observed features in the velocity channel maps and the PV diagrams. Such a warped-disk system can form by mass accretion from a misaligned envelope. We also discuss a possible disk evolution scenario based on comparisons of disk radii and masses between Class I and Class II sources.
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U2 - 10.3847/1538-4357/ab8065
DO - 10.3847/1538-4357/ab8065
M3 - Article
AN - SCOPUS:85084751115
VL - 893
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1
M1 - 51
ER -