• Title, Summary, Keyword: stars: outflows

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MOLECULAR OUTFLOWS AND THE FORMATION PROCESS OF VERY LOW-MASS OBJECTS

  • PHAN-BAO, NGOC;DANG-DUC, CUONG;LEE, CHIN-FEI;HO, PAUL T.P.
    • Publications of The Korean Astronomical Society
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    • v.30 no.2
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    • pp.83-86
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    • 2015
  • We present observational results characterizing molecular outflows from very low-mass objects in ${\rho}$ Ophiuchi and Taurus. Our results provide us with important implications that clarify the formation process of very low-mass objects.

MOLECULAR OUTFLOWS FROM NEWLY FORMED MASSIVE STARS

  • KIM, KEE-TAE;KIM, WON-JU;KIM, CHANG-HEE
    • Journal of The Korean Astronomical Society
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    • v.48 no.6
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    • pp.365-380
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    • 2015
  • We map 6 massive young stellar objects (YSOs) in the CO J=2-1 line and survey 18 massive YSOs, including the six, in the HCO+ J=1−0, SiO J=2−1, H2O 616 − 523 maser, and CH3OH 70 − 61 A+ maser lines. We detect CO bipolar outflows in all the six mapped sources. Four of them are newly discovered (07299−1651, 21306+5540, 22308+5812, 23133+6050), while 05490+2658 is mapped in the CO J=2-1 line for the first time. The detected outflows are much more massive and energetic than outflows from low-mass YSOs with masses >20 M and momenta >300 M km s−1. They have mass outflow rates (3−6)×10−4 M yr−1, which are at least one order of magnitude greater than those observed in low-mass YSOs. We detect HCO+ and SiO line emission in 18 (100%) and 4 (22%) sources, respectively. The HCO+ spectra show high-velocity wings in 11 (61%) sources. We detect H2O maser emission in 13 (72%) sources and 44 GHz CH3OH maser emission in 8 (44%) sources. Of the detected sources, 5 H2O and 6 CH3OH maser sources are new discoveries. 20081+3122 shows high-velocity (>30 km s−1) H2O maser lines. We find good correlations of the bolometric luminosity of the central (proto)star with the mechanical force, mechanical luminosity, and mass outflow rate of molecular outflow in the bolometric luminosity range of 10−1−106 L, and identified 3 intermediate- or high-mass counterparts of Class O objects.

THE GALACTIC-SCALE MOLECULAR OUTFLOWS IN STARBURST GALAXIES NGC 2146 AND NGC 3628

  • TSAI, AN-LI;MATSUSHITA, SATOKI
    • Publications of The Korean Astronomical Society
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    • v.30 no.2
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    • pp.499-502
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    • 2015
  • Starburst galaxies have strong star formation activity and generate large scale outflows which eject a huge amount of gas mass. This process affects galaxy activity, and therefore, the detailed study of nearby starburst galaxies could provide valuable information for the study of distant ones. So far there have been only a few studies of galactic-scale molecular outflows due to the sensitivity limitation of telescopes. Our study provides two nearby examples, NGC 2146 and NGC 3628. We used Nobeyama Millimeter Array (NMA) CO(1-0) data, Chandra soft X-ray data, and NMA 3 mm data to study the kinematics of molecular outflows, their interaction with ionized outflows, and the star forming activity in the starburst region. We found that the gas ejected through molecular outflows is much more significant than that used to form stars.

SURVEY OF CARBON MONOXIDE OUTFLOWS ASSOCIATED WITH MOLECULAR HYDROGEN EMISSION FEATURES IN THE NORTHERN ORION A MOLECULAR CLOUD

  • Park Geum-Sook;Choi Min-Ho
    • Journal of The Korean Astronomical Society
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    • v.39 no.2
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    • pp.31-40
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    • 2006
  • Near-IR $H_2$ emission features in the northern region of the Orion A giant molecular cloud were observed in the $CO\;J\;=\;1\;{\rightarrow}\;0$ line in search of CO outflows. Out of the 30 sources surveyed, CO line wings were detected toward 28 positions, suggesting a strong correlation between $H_2$ jets and CO outflows. Blueshifted wings were detected toward 26 positions while redshifted wings were detected toward 15 positions, which suggests that there is a bias in the source selection. The bias is more severe in OMC 3 than in OMC 2. Since the protostars in OMC 3 are younger and more deeply embedded, the bias may be caused by the difference of extinction between blueshifted and redshifted outflows. Some physical parameters of the outflows were derived from the line profiles.

Interactions in Massive Colliding Wind Binaries

  • Corcoran, Michael F.
    • Journal of Astronomy and Space Sciences
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    • v.29 no.1
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    • pp.93-96
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    • 2012
  • There are observational difficulties determining dynamical masses of binary star components in the upper HR diagram both due to the scarcity of massive binary systems and spectral and photometric contamination produced by the strong wind outflows in these systems. We discuss how variable X-ray emission in these systems produced by wind-wind collisions in massive binaries can be used to constrain the system parameters, with application to two important massive binaries, Eta Carinae and WR 140.

UNVEILING COMPLEX OUTFLOW STRUCTURE OF UY Aur

  • PYO, TAE-SOO;HAYASHI, MASAHIKO;BECK, TRACY;DAVIS, CHRISTOPHER J.;TAKAMI, MICHIHIRO
    • Publications of The Korean Astronomical Society
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    • v.30 no.2
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    • pp.109-112
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    • 2015
  • We present [$Fe\;{\small{II}}$] ${\lambda}1.257{\mu}m$ spectra toward the interacting binary UY Aur with 0".14 angular resolution, obtained with the Near infrared Integral Field Spectrograph (NIFS) combined with the adaptive optics system Altair of the GEMINI observatory. In the [$Fe\;{\small{II}}$] emission, UY Aur A (primary) is brighter than UY Aur B (secondary). The blueshifted and redshifted emission between the primary and secondary show a complicated structure. The radial velocities of the [$Fe\;{\small{II}}$] emission features are similar for UY Aur A and B: ${\sim}-100km\;s^{-1}$ and ${\sim}+130km\;s^{-1}$ for the blueshifted and redshifted components, respectively. Considering the morphologies of the [$Fe\;{\small{II}}$] emissions and bipolar outflow context, we concluded that UY Aur A drives fast and widely opening outflows with an opening angle of ${\sim}90^{\circ}$ while UY Aur B has micro collimated jets.

Probing the Feedback Process in Local Type-2 AGNs with Integral-Field Spectroscopy

  • Luo, Rongxin;Woo, Jong-Hak;Shin, Jaejin;Kang, Daeun;Bae, Hyun-Jin;Karouzos, Marios
    • The Bulletin of The Korean Astronomical Society
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    • v.44 no.1
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    • pp.36.3-36.3
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    • 2019
  • Feedback process is one of the most important topics in the study of AGNs since it plays a key role in linking the SMBHs and their host galaxies. In order to further understand the co-evolution of SMBHs and their host galaxies, we probe the feedback process in local type-2 AGNs with a series of integral-field-spectroscopy observations. In the first part of my talk, I will introduce our GMOS observations of luminous type-2 AGNs at z < 0.1, which are selected using the integrated [O III] kinematics. Based on the dedicated emission-line diagnostics and kinematic studies, we identify the signatures of AGN-driven outflows and quantify the outflow size in the targets with extreme [O III] kinematics. For the targets without extreme [O III] kinematics, we find the presence of weak AGN-driven outflows, which are indicated by the significant differences between the kinematics of gas and stars. Then, I will present our recent study of 40 type-2 AGNs based on the SNIFS IFU. By comparing the radial profile of velocity dispersion of gas and stars, we measure the size of AGN-driven outflows in these targets and extend the outflow size-AGN luminosity relation in our previous GMOS studies. We also discuss the feedback effect of AGN-driven outflows by connecting the outflow velocity and host galaxy properties. These results highlight the importance of spatially-resolved observation in investigating gas kinematics and identifying the signatures of AGN-driven outflows.

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Gas and Stellar Kinematics of 9 Pseudo Bulge Galaxies

  • Jo, Kooksup;Woo, Jong-Hak
    • The Bulletin of The Korean Astronomical Society
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    • v.39 no.2
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    • pp.69.1-69.1
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    • 2014
  • We present the spatially resolved kinematics of ionized gas and stars along the major axis of 9 pseudo bulge galaxies. Using the high quality long-slit spectra obtained with the FOCAS at the Subaru telescope, we measured the flux, velocity, and velocity dispersion of the [OIII] and $H{\beta}$ lines to determine the size of the narrow-line region, rotation curve, and the radial profile of velocity dispersions. We compare ionized gas kinematics and stellar kinematics to investigate whether ionized gas shows any signs of outflows and whether stars and ionized gas show the same sigma-dip feature (i.e., decrease of velocity dispersion) at the very center.

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THE CONTRIBUTION OF STELLAR WINDS TO COSMIC RAY PRODUCTION

  • Seo, Jeongbhin;Kang, Hyesung;Ryu, Dongsu
    • Journal of The Korean Astronomical Society
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    • v.51 no.2
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    • pp.37-48
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    • 2018
  • Massive stars blow powerful stellar winds throughout their evolutionary stages from the main sequence to Wolf-Rayet phases. The amount of mechanical energy deposited in the interstellar medium by the wind from a massive star can be comparable to the explosion energy of a core-collapse supernova that detonates at the end of its life. In this study, we estimate the kinetic energy deposition by massive stars in our Galaxy by considering the integrated Galactic initial mass function and modeling the stellar wind luminosity. The mass loss rate and terminal velocity of stellar winds during the main sequence, red supergiant, and Wolf-Rayet stages are estimated by adopting theoretical calculations and observational data published in the literature. We find that the total stellar wind luminosity due to all massive stars in the Galaxy is about ${\mathcal{L}}_w{\approx}1.1{\times}10^{41}erg\;s^{-1}$, which is about 1/4 of the power of supernova explosions, ${\mathcal{L}}_{SN}{\approx}4.8{\times}10^{41}erg\;s^{-1}$. If we assume that ~ 1 - 10 % of the wind luminosity could be converted to Galactic cosmic rays (GCRs) through collisonless shocks such as termination shocks in stellar bubbles and superbubbles, colliding-wind shocks in binaries, and bow-shocks of massive runaway stars, stellar winds might be expected to make a significant contribution to GCR production, though lower than that of supernova remnants.