当前位置：
X-MOL 学术
›
Astron. Astrophys.
›
论文详情
Our official English website, www.x-mol.net, welcomes your feedback! (Note: you will need to create a separate account there.)
FAUST
Astronomy & Astrophysics ( IF 5.4 ) Pub Date : 2024-06-12 , DOI: 10.1051/0004-6361/202449949 M. De Simone , L. Podio , L. Chahine , C. Codella , C. J. Chandler , C. Ceccarelli , A. López-Sepulcre , L. Loinard , B. Svoboda , N. Sakai , D. Johnstone , F. Ménard , Y. Aikawa , M. Bouvier , G. Sabatini , A. Miotello , C. Vastel , N. Cuello , E. Bianchi , P. Caselli , E. Caux , T. Hanawa , E. Herbst , D. Segura-Cox , Z. Zhang , S. Yamamoto
Astronomy & Astrophysics ( IF 5.4 ) Pub Date : 2024-06-12 , DOI: 10.1051/0004-6361/202449949 M. De Simone , L. Podio , L. Chahine , C. Codella , C. J. Chandler , C. Ceccarelli , A. López-Sepulcre , L. Loinard , B. Svoboda , N. Sakai , D. Johnstone , F. Ménard , Y. Aikawa , M. Bouvier , G. Sabatini , A. Miotello , C. Vastel , N. Cuello , E. Bianchi , P. Caselli , E. Caux , T. Hanawa , E. Herbst , D. Segura-Cox , Z. Zhang , S. Yamamoto
Context. Understanding the connection between outflows, winds, accretion, and discs in the inner protostellar regions is crucial for comprehending star and planet formation processes.Aims. We aim to we explore the inner 300 au of the protostar IRAS 4A2 as part of the ALMA FAUST Large Program.Methods. We analysed the kinematical structures of SiO and CH3OH emission with 50 au resolution.Results. The emission arises from three zones: (i) a very compact and unresolved region (< 50 au) dominated by the ice sublimation zone, at ±1.5 km s−1 with respect to vsys, traced by methanol; (ii) an intermediate region (between 50 au and 150 au) traced by both SiO and CH3OH, between 2 and 6 km s−1 with respect to vsys, with an inverted velocity gradient (with respect to the large-scale emission), whose origin is not clear; (iii) an extended region (> 150 au) traced by SiO, above 7 km s−1 with respect to vsys, and dominated by the outflow. In the intermediate region, we estimated a CH3OH/SiO abundance ratio of about 120–400 and a SiO/H2 abundance of 10−8. We explored various possibilities to explain the origin of this region, such as, a rotating disc or inner envelope, a jet on the plane of the sky or precessing, and a wide-angle disc wind.Conclusions. We propose that CH3OH and SiO in the inner 100 au probe the base of a wide-angle disc wind. The material accelerated in the wind crosses the plane of the sky, giving rise to the observed inverted velocity gradient, and sputtering the grain mantles and cores releasing CH3OH and SiO. This is the first detection of a disc-wind candidate in SiO, and the second ever in CH3OH.
更新日期：2024-06-12
京公网安备 11010802027423号