Chasing discs around O-type (proto)stars
Chasing discs around O-type (proto)stars
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围绕 O 型（原）恒星追逐圆盘
DOI：
--
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发表时间：
2018
影响因子：
6.5
通讯作者：
H. Zinnecker
中科院分区：
文献类型：
--
作者：
L. Maud;R. Cesaroni;M. Kumar;F. V. D. Tak;V. Allen;M. Hoare;P. Klaassen;D. Harsono;M. Hogerheijde;'A. S'anchez;P. Schilke;A. Ahmadi;M. Beltr'an;H. Beuther;T. Csengeri;S. Etoka;G. Fuller;R. Galv'an;C. Goddi;T. Henning;K. Johnston;R. Kuiper;S. Lumsden;L. Moscadelli;J. Mottram;T. Peters;V. Rivilla;L. Testi;S. Vig;W. D. Wit;H. Zinnecker
我们提供了高角分辨率（~0.2″）连续体和分子发射线，这是阿塔卡马大型毫米波/亚毫米波阵列（ALMA）在波段6（220−230 GHz）观测到的G17.64+0.16，这是寻找（原）o -恒星周围的星周盘运动的一部分。在~400 au的分辨率下，主连续体核心基本上是无法解析的，并且与其他强而致密的发射峰隔离开来。我们使用主ALMA阵列和阿塔卡马紧凑阵列（ACA）探测到SiO（5-4）发射，该发射在垂直于13 CO（2−1）线中看到的大规模流出方向上被边际分解和拉长。形态学上，SiO表现为圆盘状结构。通过参数化模型，我们证明了SiO的位置-速度分布与质量在10到30 M⊙之间的天体周围的圆盘的开普勒旋转是一致的，只有在另一个结构也有径向膨胀的情况下。径向运动分量可以解释为来自圆盘表面的圆盘风。中心恒星质量在20到30 M⊙之间的模型与恒星亮度（1 × 105 L⊙）最一致，表明是一颗o型恒星。H30α毫米复合线（231.9 GHz）也被检测到，但空间上无法确定，表明与尘埃连续体核心共空间有一个非常致密、热、电离的区域。H30α发射的宽线宽（全宽-半宽= 81.9 km s−1）不受压力增宽的支配，而是与下面的体运动相一致。这些速度与冲击将硅从尘埃颗粒释放到气相所需的速度相匹配。CH3 CN和CH3 OH的热发射也显示出两个弧形的羽流，这些羽流从圆盘平面向外弯曲。它们与OH脉泽发射的巧合表明，它们可以追踪由G17.64驱动的广角风的内部工作表面，该风在被重定向到大规模流出方向之前影响了弥漫性残余出生云。考虑到所有的观测结果，我们认为G17.64与一个处于原恒星组装最后阶段的o型年轻恒星物体一致，驱动着风，但尚未发展成致密的H II区域。G17.64中圆盘的存在和检测可能与它的孤立性和可能更进化的性质有关，这些特征可能是类似来源中圆盘的基础。
We present high angular resolution (~0.2″) continuum and molecular emission line Atacama Large Millimeter/sub-millimeter Array (ALMA) observations of G17.64+0.16 in Band 6 (220−230 GHz) taken as part of a campaign in search of circumstellar discs around (proto)-O-stars. At a resolution of ~400 au the main continuum core is essentially unresolved and isolated from other strong and compact emission peaks. We detect SiO (5–4) emission that is marginally resolved and elongated in a direction perpendicular to the large-scale outflow seen in the 13 CO (2−1) line using the main ALMA array in conjunction with the Atacama Compact Array (ACA). Morphologically, the SiO appearsto represent a disc-like structure. Using parametric models we show that the position-velocity profile of the SiO is consistent with the Keplerian rotation of a disc around an object between 10 and 30 M⊙ in mass, only if there is also radial expansion from a separate structure. The radial motion component can be interpreted as a disc wind from the disc surface. Models with a central stellar object mass between 20 and 30 M⊙ are the most consistent with the stellar luminosity (1 × 105 L⊙) and indicative of an O-type star. The H30α millimetre recombination line (231.9 GHz) is also detected, but spatially unresolved, and is indicative of a very compact, hot, ionised region co-spatial with the dust continuum core. The broad line-width of the H30α emission (full-width-half-maximum = 81.9 km s−1) is not dominated by pressure-broadening but is consistent with underlying bulk motions. These velocities match those required for shocks to release silicon from dust grains into the gas phase. CH3 CN and CH3 OH thermal emission also shows two arc shaped plumes that curve away from the disc plane. Their coincidence with OH maser emission suggests that they could trace the inner working surfaces of a wide-angle wind driven by G17.64 which impacts the diffuse remnant natal cloud before being redirected into the large-scale outflow direction. Accounting for all observables, we suggest that G17.64 is consistent with a O-type young stellar object in the final stages of protostellar assembly, driving a wind, but that has not yet developed into a compact H II region. The existance and detection of the disc in G17.64 is likely related to its isolated and possibly more evolved nature, traits which may underpin discs in similar sources.
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影响因子：
4.8
作者：
L. Maud;T. Moore;S. Lumsden;J. Mottram;J. Urquhart;M. Hoare
通讯作者：
L. Maud;T. Moore;S. Lumsden;J. Mottram;J. Urquhart;M. Hoare
寻找射向大质量年轻恒星的电离喷流
影响因子：
4.8
作者：
Purser S
通讯作者：
Purser S
影响因子：
6.5
作者：
M. Beltr'an;R. Cesaroni;V. Rivilla;'A. S'anchez-Monge;L. Moscadelli;A. Ahmadi;V. Allen;H. Beuther;S. Etoka;D. Galli;R. Galv'an-Madrid;C. Goddi;K. Johnston;A. Kolligan;R. Kuiper;M. Kumar;L. Maud;J. Mottram;T. Peters;P. Schilke;L. Testi;F. V. D. Tak;C. F. I. A. D. Arcetri;I. Institut;U. Koln;M. F. Astronomy;Heidelberg;K. Institute;U. Groningen;S. I. F. S. Research-S.-I.-F.-S.-Research-152214217;Groningen;J. B. C. F. Astrophysics;Manchester;Instituto de Radioastronom'ia y Astrof'isica Morelia-Instituto-de-Radioastronom'ia-y-Astrof'isica-2230372164;Department of AstrophysicsIMAPP;R. University;A. Observatory;Leiden University;S. O. Physics;Astronomy;Leeds;UK Astronomy Technology Centre;Royal Observatory of Edinburgh;I. O. Astronomy;Astrophysics;U. Tubingen;I. D. A. E. C. D. Espacco-I.-D.-A.-E.-C.-D.-Espacco-88742463;U. Porto;Centre for Gravitational Astrophysics;U. Hertfordshire;L. Observatory;M. F. Astrophysik;Garching;Eső
通讯作者：
M. Beltr'an;R. Cesaroni;V. Rivilla;'A. S'anchez-Monge;L. Moscadelli;A. Ahmadi;V. Allen;H. Beuther;S. Etoka;D. Galli;R. Galv'an-Madrid;C. Goddi;K. Johnston;A. Kolligan;R. Kuiper;M. Kumar;L. Maud;J. Mottram;T. Peters;P. Schilke;L. Testi;F. V. D. Tak;C. F. I. A. D. Arcetri;I. Institut;U. Koln;M. F. Astronomy;Heidelberg;K. Institute;U. Groningen;S. I. F. S. Research-S.-I.-F.-S.-Research-152214217;Groningen;J. B. C. F. Astrophysics;Manchester;Instituto de Radioastronom'ia y Astrof'isica Morelia-Instituto-de-Radioastronom'ia-y-Astrof'isica-2230372164;Department of AstrophysicsIMAPP;R. University;A. Observatory;Leiden University;S. O. Physics;Astronomy;Leeds;UK Astronomy Technology Centre;Royal Observatory of Edinburgh;I. O. Astronomy;Astrophysics;U. Tubingen;I. D. A. E. C. D. Espacco-I.-D.-A.-E.-C.-D.-Espacco-88742463;U. Porto;Centre for Gravitational Astrophysics;U. Hertfordshire;L. Observatory;M. F. Astrophysik;Garching;Eső
DOI：
10.1088/0067-0049/208/1/11
发表时间：
2013-08
期刊：
The Astrophysical Journal Supplement Series
影响因子：
--
作者：
S. Lumsden;M. Hoare;J. Urquhart;R. Oudmaijer;B. Davies;J. Mottram;H. Cooper;T. U. O. Leeds;Leeds;Uk;Max Planck Institut fur Radioastronomie;Bonn;Germany;A. R. Institute;Liverpool John Moores University;Liverpool;L. Observatory;Leiden University;Leiden;The Netherlands
通讯作者：
S. Lumsden;M. Hoare;J. Urquhart;R. Oudmaijer;B. Davies;J. Mottram;H. Cooper;T. U. O. Leeds;Leeds;Uk;Max Planck Institut fur Radioastronomie;Bonn;Germany;A. R. Institute;Liverpool John Moores University;Liverpool;L. Observatory;Leiden University;Leiden;The Netherlands
DOI：
10.3847/1538-4357/aaa24b
发表时间：
2018-01
期刊：
The Astrophysical Journal
影响因子：
--
作者：
A. Baez--Rubio-A.-Baez--Rubio-1388382687;I. Jiménez-Serra;Jesús Martín-Pintado;Qizhou Zhang;S. Curiel
通讯作者：
A. Baez--Rubio-A.-Baez--Rubio-1388382687;I. Jiménez-Serra;Jesús Martín-Pintado;Qizhou Zhang;S. Curiel