TIPSY: Trajectory of Infalling Particles in Streamers around Young stars
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Context. Elongated trails of infalling gas, often referred to as "streamers"have recently been observed around young stellar objects (YSOs) at different evolutionary stages. This asymmetric infall of material can significantly alter star and planet formation processes, especially in the more evolved YSOs. Aims. In order to ascertain the infalling nature of observed streamer-like structures and then systematically characterize their dynamics, we developed the code TIPSY (Trajectory of Infalling Particles in Streamers around Young stars). Methods. Using TIPSY, the streamer molecular line emission is first isolated from the disk emission. Then the streamer emission, which is effectively a point cloud in three-dimensional (3D) position- position- velocity space, is simplified to a curve-like representation. The observed streamer curve is then compared to the theoretical trajectories of infalling material. The best-fit trajectories are used to constrain streamer features, such as the specific energy, the specific angular momenta, the infall timescale, and the 3D morphology. Results. We used TIPSY to fit molecular-line ALMA observations of streamers around a Class II binary system, S CrA, and a Class I/II protostar, HL Tau. Our results indicate that both of the streamers are consistent with infalling motion. For the S CrA streamer, we could constrain the dynamical parameters well and find it to be on a bound elliptical trajectory. On the other hand, the fitting uncertainties are substantially higher for the HL Tau streamer, likely due to the smaller spatial scales of the observations. TIPSY results and mass estimates suggest that S CrA and HL Tau are accreting material at a rate of ≳27 Mjupiter Myr- 1 and ≳5 Mjupiter Myr- 1, respectively, which can significantly increase the mass budget available to form planets. Conclusions. TIPSY can be used to assess whether the morphology and kinematics of observed streamers are consistent with infalling motion and to characterize their dynamics, which is crucial for quantifying their impact on the protostellar systems.
| Bidragets oversatte titel | Dynamical analysis of the streamers around S CrA and HL Tau |
|---|---|
| Originalsprog | Engelsk |
| Artikelnummer | A133 |
| Tidsskrift | Astronomy and Astrophysics |
| Vol/bind | 683 |
| ISSN | 0004-6361 |
| DOI | |
| Status | Udgivet - 2024 |
Bibliografisk note
Funding Information:
This work was partly funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) - 325594231. H.-W.Y. acknowledges support from National Science and Technology Council (NSTC) in Taiwan through grant NSTC 110-2628-M-001-003-MY3 and from the Academia Sinica Career Development Award (AS-CDA-111-M03). M.K. is supported by a global postdoctoral fellowship of the H2020 Marie Sklodowska-Curie Actions (897524) and a Carlsberg Reintegration Fellowship (CF22-1014). T.B. acknowledges funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme under grant agreement no. 714769 and funding by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under grants 361140270, 325594231, and Germany's Excellence Strategy - EXC-2094 - 390783311. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2019.1.01792.S and ADS/JAO.ALMA#2016.1.00366.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. We thank Carlo Manara, Jaime Pineda, Maria Teresa Valdivia-Mena, Amelia Bayo, Lukasz Tychoniec, Karina Mauco Coronado, and Claudia Toci for helpful insights and discussion. This work made use of Astropy (https://www.astropy.org): a community-developed core Python package and an ecosystem of tools and resources for astronomy (Astropy Collaboration 2013, 2018, 2022). The three-dimensional plots were made using TRIVIA (https://github.com/jaehanbae/trivia) and Plotly (https://plotly.com/python).
Funding Information:
This work was partly funded by the Deutsche Forschungs-gemeinschaft (DFG, German Research Foundation) – 325594231. H.-W.Y. acknowledges support from National Science and Technology Council (NSTC) in Taiwan through grant NSTC 110-2628-M-001-003-MY3 and from the Academia Sinica Career Development Award (AS-CDA-111-M03). M.K. is supported by a global postdoctoral fellowship of the H2020 Marie Sklodowska-Curie Actions (897524) and a Carlsberg Reintegration Fellowship (CF22-1014). T.B. acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme under grant agreement no. 714769 and funding by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under grants 361140270, 325594231, and Germany’s Excellence Strategy – EXC-2094 – 390783311. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2019.1.01792.S and ADS/JAO.ALMA#2016.1.00366.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. We thank Carlo Manara, Jaime Pineda, Maria Teresa Valdivia-Mena, Amelia Bayo, Lukasz Tychoniec, Karina Mauco Coronado, and Claudia Toci for helpful insights and discussion. This work made use of Astropy ( https://www.astropy.org ): a community-developed core Python package and an ecosystem of tools and resources for astronomy (Astropy Collaboration 2013, 2018, 2022). The three-dimensional plots were made using TRIVIA ( https://github.com/jaehanbae/trivia ) and Plotly ( https://plotly.com/python ).
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