A. Dutrey, E. Chapillon, S. Guilloteau, Y. W. Tang, A. Boccaletti, L. Bouscasse, T. Collin-Dufresne, E. Di Folco, A. Fuente, V. Piétu, P. Rivière-Marichalar, D. Semenov
{"title":"原行星盘中作为冲击示踪剂的一氧化硫(SO):北极星AB的案例","authors":"A. Dutrey, E. Chapillon, S. Guilloteau, Y. W. Tang, A. Boccaletti, L. Bouscasse, T. Collin-Dufresne, E. Di Folco, A. Fuente, V. Piétu, P. Rivière-Marichalar, D. Semenov","doi":"10.1051/0004-6361/202451299","DOIUrl":null,"url":null,"abstract":"<i>Context.<i/> Sulfur monoxide (SO) is known to be a good shock tracer in molecular clouds and protostar environments, but its abundance is difficult to reproduce, even with state-of-the-art astrochemical models.<i>Aims.<i/> We investigate the properties of the observed SO emission in the protoplanetary disk of AB Auriga, a Herbig Ae star of 2.4 M<sub>⊙<sub/> in mass, located at 156 pc. The AB Aur system is unique because it exhibits a dust trap and at least one young putative planet orbiting at about 30 au from the central star.<i>Methods.<i/> We reduced ALMA archival data (projects 2019.1.00579.S, 2021.1.00690.S, and 2021.1.01216.S) and analyzed the three detected SO lines (SO 6<sub>5<sub/> − 5<sub>4<sub/>, 6<sub>7<sub/> − 5<sub>6<sub/> and 5<sub>6<sub/> − 4<sub>5<sub/>). We also used C<sup>17<sup/>O and C<sup>18<sup/>O 2–1 data to complement the interpretation of the SO data.<i>Results.<i/> For the three SO lines, the maximum SO emission in the ring is not located in the dust trap. Moreover, the inner radius of the SO ring is significantly larger than the CO emission inner radius, ∼160 au versus ∼90 au. The SO emission traces gas located in part beyond the dust ring. This emission likely originates from shocks at the interface of the outer spirals, observed in CO and scattered light emission, as well as those in the molecular and dust ring. Also, SO is detected within the cavity, at a radius of ∼20 − 30 au and with a rotation velocity compatible with the protoplanet P1. We speculate that this SO emission originates from accretion shocks onto the circumplanetary disk of the putative protoplanet P1.<i>Conclusions.<i/> These observations confirm that SO is a good tracer of shocks in protoplanetary disks and could serve as a powerful new tool for detecting embedded (proto)planets.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":null,"pages":null},"PeriodicalIF":5.4000,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"Sulfur monoxide (SO) as a shock tracer in protoplanetary disks: Case of AB Aurigae\",\"authors\":\"A. Dutrey, E. Chapillon, S. Guilloteau, Y. W. Tang, A. Boccaletti, L. Bouscasse, T. Collin-Dufresne, E. Di Folco, A. Fuente, V. Piétu, P. Rivière-Marichalar, D. Semenov\",\"doi\":\"10.1051/0004-6361/202451299\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"<i>Context.<i/> Sulfur monoxide (SO) is known to be a good shock tracer in molecular clouds and protostar environments, but its abundance is difficult to reproduce, even with state-of-the-art astrochemical models.<i>Aims.<i/> We investigate the properties of the observed SO emission in the protoplanetary disk of AB Auriga, a Herbig Ae star of 2.4 M<sub>⊙<sub/> in mass, located at 156 pc. The AB Aur system is unique because it exhibits a dust trap and at least one young putative planet orbiting at about 30 au from the central star.<i>Methods.<i/> We reduced ALMA archival data (projects 2019.1.00579.S, 2021.1.00690.S, and 2021.1.01216.S) and analyzed the three detected SO lines (SO 6<sub>5<sub/> − 5<sub>4<sub/>, 6<sub>7<sub/> − 5<sub>6<sub/> and 5<sub>6<sub/> − 4<sub>5<sub/>). We also used C<sup>17<sup/>O and C<sup>18<sup/>O 2–1 data to complement the interpretation of the SO data.<i>Results.<i/> For the three SO lines, the maximum SO emission in the ring is not located in the dust trap. Moreover, the inner radius of the SO ring is significantly larger than the CO emission inner radius, ∼160 au versus ∼90 au. The SO emission traces gas located in part beyond the dust ring. This emission likely originates from shocks at the interface of the outer spirals, observed in CO and scattered light emission, as well as those in the molecular and dust ring. Also, SO is detected within the cavity, at a radius of ∼20 − 30 au and with a rotation velocity compatible with the protoplanet P1. We speculate that this SO emission originates from accretion shocks onto the circumplanetary disk of the putative protoplanet P1.<i>Conclusions.<i/> These observations confirm that SO is a good tracer of shocks in protoplanetary disks and could serve as a powerful new tool for detecting embedded (proto)planets.\",\"PeriodicalId\":8571,\"journal\":{\"name\":\"Astronomy & Astrophysics\",\"volume\":null,\"pages\":null},\"PeriodicalIF\":5.4000,\"publicationDate\":\"2024-09-17\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Astronomy & Astrophysics\",\"FirstCategoryId\":\"101\",\"ListUrlMain\":\"https://doi.org/10.1051/0004-6361/202451299\",\"RegionNum\":2,\"RegionCategory\":\"物理与天体物理\",\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"Q1\",\"JCRName\":\"ASTRONOMY & ASTROPHYSICS\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Astronomy & Astrophysics","FirstCategoryId":"101","ListUrlMain":"https://doi.org/10.1051/0004-6361/202451299","RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q1","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}
引用次数: 0
摘要
背景。众所周知,一氧化硫(SO)是分子云和原初星环境中一种很好的冲击示踪剂,但即使使用最先进的天体化学模型也很难再现其丰度。我们研究了在 AB Auriga 星的原行星盘中观测到的 SO 发射的性质,AB Auriga 星是一颗质量为 2.4 M⊙的 Herbig Ae 星,位于 156 pc 处。AB Aur星系是一个独特的星系,因为它有一个尘埃陷阱,至少有一颗年轻的假定行星在距离中心恒星约30 au处运行。我们缩减了ALMA档案数据(项目:2019.1.00579.S、2021.1.00690.S和2021.1.01216.S),并分析了检测到的三条SO线(SO 65 - 54、67 - 56和56 - 45)。我们还使用了 C17O 和 C18O 2-1 数据来补充解释 SO 数据。对于三条 SO 线来说,环中的最大 SO 发射并不位于尘埃捕获器中。此外,SO环的内半径明显大于CO发射的内半径,分别为160au和90au。SO 辐射追踪的气体部分位于尘埃环之外。这种发射很可能来自外螺旋界面的冲击,在 CO 和散射光发射以及分子环和尘埃环中都能观测到。此外,我们还在空腔内检测到了 SO,其半径为 20 - 30 au,旋转速度与原行星 P1 相符。我们推测,这种 SO 发射源于对推定原行星 P1 的环行星盘的吸积冲击。这些观测结果证实,SO 是原行星盘中冲击的良好示踪剂,可以作为探测嵌入式(原)行星的强大新工具。
Sulfur monoxide (SO) as a shock tracer in protoplanetary disks: Case of AB Aurigae
Context. Sulfur monoxide (SO) is known to be a good shock tracer in molecular clouds and protostar environments, but its abundance is difficult to reproduce, even with state-of-the-art astrochemical models.Aims. We investigate the properties of the observed SO emission in the protoplanetary disk of AB Auriga, a Herbig Ae star of 2.4 M⊙ in mass, located at 156 pc. The AB Aur system is unique because it exhibits a dust trap and at least one young putative planet orbiting at about 30 au from the central star.Methods. We reduced ALMA archival data (projects 2019.1.00579.S, 2021.1.00690.S, and 2021.1.01216.S) and analyzed the three detected SO lines (SO 65 − 54, 67 − 56 and 56 − 45). We also used C17O and C18O 2–1 data to complement the interpretation of the SO data.Results. For the three SO lines, the maximum SO emission in the ring is not located in the dust trap. Moreover, the inner radius of the SO ring is significantly larger than the CO emission inner radius, ∼160 au versus ∼90 au. The SO emission traces gas located in part beyond the dust ring. This emission likely originates from shocks at the interface of the outer spirals, observed in CO and scattered light emission, as well as those in the molecular and dust ring. Also, SO is detected within the cavity, at a radius of ∼20 − 30 au and with a rotation velocity compatible with the protoplanet P1. We speculate that this SO emission originates from accretion shocks onto the circumplanetary disk of the putative protoplanet P1.Conclusions. These observations confirm that SO is a good tracer of shocks in protoplanetary disks and could serve as a powerful new tool for detecting embedded (proto)planets.
期刊介绍:
Astronomy & Astrophysics is an international Journal that publishes papers on all aspects of astronomy and astrophysics (theoretical, observational, and instrumental) independently of the techniques used to obtain the results.