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A High-mass, Young Star-forming Core Escaping from Its Parental Filament

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Title: A High-mass, Young Star-forming Core Escaping from Its Parental Filament
Authors: Zhiyuan Ren, Xi Chen, Tie Liu, Emma Mannfors, Leonardo Bronfman, Fengwei Xu, Siyi Feng, Hongli Liu, Fanyi Meng, Amelia M. Stutz, Shanghuo Li, Chang Won Lee, Ke Wang, Jianwen Zhou, Di Li, Chen Wang, Chakali Eswaraiah, Anandmayee Tej, Long-Fei Chen, Hui Shi
Source: The Astrophysical Journal, Vol 955, Iss 2, p 104 (2023)
Publisher Information: IOP Publishing, 2023.
Publication Year: 2023
Collection: LCC:Astrophysics
Subject Terms: Star formation, Young stellar objects, Dense interstellar clouds, Interstellar filaments, Gravitational collapse, Astrophysics, QB460-466
More Details: We studied the unique kinematic properties in massive filament G352.63-1.07 at 10 ^3 au spatial scale with the dense molecular tracers observed with the Atacama Large Millimeter/submillimeter Array. We find the central massive core M1 (12 M _⊙ ) being separated from the surrounding filament with a velocity difference of $v-{\overline{v}}_{\mathrm{sys}}=-2\,\mathrm{km}\,{{\rm{s}}}^{-1}$ and a transverse separation within 3″. Meanwhile, as shown in multiple dense-gas tracers, M1 has a spatial extension closely aligned with the main filament and is connected to the filament toward both its ends. M1 thus represents a very beginning state for a massive, young star-forming core escaping from the parental filament, within a timescale of ∼4000 yr. Based on its kinetic energy (3.5 × 10 ^44 erg), the core escape is unlikely solely due to the original filament motion or magnetic field but requires more energetic events such as a rapid intense anisotropic collapse. The released energy also seems to noticeably increase the environmental turbulence. This may help the filament to become stabilized again.
Document Type: article
File Description: electronic resource
Language: English
ISSN: 1538-4357
Relation: https://doaj.org/toc/1538-4357
DOI: 10.3847/1538-4357/aced54
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  Data: A High-mass, Young Star-forming Core Escaping from Its Parental Filament
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  Data: <searchLink fieldCode="AR" term="%22Zhiyuan+Ren%22">Zhiyuan Ren</searchLink><br /><searchLink fieldCode="AR" term="%22Xi+Chen%22">Xi Chen</searchLink><br /><searchLink fieldCode="AR" term="%22Tie+Liu%22">Tie Liu</searchLink><br /><searchLink fieldCode="AR" term="%22Emma+Mannfors%22">Emma Mannfors</searchLink><br /><searchLink fieldCode="AR" term="%22Leonardo+Bronfman%22">Leonardo Bronfman</searchLink><br /><searchLink fieldCode="AR" term="%22Fengwei+Xu%22">Fengwei Xu</searchLink><br /><searchLink fieldCode="AR" term="%22Siyi+Feng%22">Siyi Feng</searchLink><br /><searchLink fieldCode="AR" term="%22Hongli+Liu%22">Hongli Liu</searchLink><br /><searchLink fieldCode="AR" term="%22Fanyi+Meng%22">Fanyi Meng</searchLink><br /><searchLink fieldCode="AR" term="%22Amelia+M%2E+Stutz%22">Amelia M. Stutz</searchLink><br /><searchLink fieldCode="AR" term="%22Shanghuo+Li%22">Shanghuo Li</searchLink><br /><searchLink fieldCode="AR" term="%22Chang+Won+Lee%22">Chang Won Lee</searchLink><br /><searchLink fieldCode="AR" term="%22Ke+Wang%22">Ke Wang</searchLink><br /><searchLink fieldCode="AR" term="%22Jianwen+Zhou%22">Jianwen Zhou</searchLink><br /><searchLink fieldCode="AR" term="%22Di+Li%22">Di Li</searchLink><br /><searchLink fieldCode="AR" term="%22Chen+Wang%22">Chen Wang</searchLink><br /><searchLink fieldCode="AR" term="%22Chakali+Eswaraiah%22">Chakali Eswaraiah</searchLink><br /><searchLink fieldCode="AR" term="%22Anandmayee+Tej%22">Anandmayee Tej</searchLink><br /><searchLink fieldCode="AR" term="%22Long-Fei+Chen%22">Long-Fei Chen</searchLink><br /><searchLink fieldCode="AR" term="%22Hui+Shi%22">Hui Shi</searchLink>
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  Data: The Astrophysical Journal, Vol 955, Iss 2, p 104 (2023)
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  Data: IOP Publishing, 2023.
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  Data: <searchLink fieldCode="DE" term="%22Star+formation%22">Star formation</searchLink><br /><searchLink fieldCode="DE" term="%22Young+stellar+objects%22">Young stellar objects</searchLink><br /><searchLink fieldCode="DE" term="%22Dense+interstellar+clouds%22">Dense interstellar clouds</searchLink><br /><searchLink fieldCode="DE" term="%22Interstellar+filaments%22">Interstellar filaments</searchLink><br /><searchLink fieldCode="DE" term="%22Gravitational+collapse%22">Gravitational collapse</searchLink><br /><searchLink fieldCode="DE" term="%22Astrophysics%22">Astrophysics</searchLink><br /><searchLink fieldCode="DE" term="%22QB460-466%22">QB460-466</searchLink>
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  Label: Description
  Group: Ab
  Data: We studied the unique kinematic properties in massive filament G352.63-1.07 at 10 ^3 au spatial scale with the dense molecular tracers observed with the Atacama Large Millimeter/submillimeter Array. We find the central massive core M1 (12 M _⊙ ) being separated from the surrounding filament with a velocity difference of $v-{\overline{v}}_{\mathrm{sys}}=-2\,\mathrm{km}\,{{\rm{s}}}^{-1}$ and a transverse separation within 3″. Meanwhile, as shown in multiple dense-gas tracers, M1 has a spatial extension closely aligned with the main filament and is connected to the filament toward both its ends. M1 thus represents a very beginning state for a massive, young star-forming core escaping from the parental filament, within a timescale of ∼4000 yr. Based on its kinetic energy (3.5 × 10 ^44 erg), the core escape is unlikely solely due to the original filament motion or magnetic field but requires more energetic events such as a rapid intense anisotropic collapse. The released energy also seems to noticeably increase the environmental turbulence. This may help the filament to become stabilized again.
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      – SubjectFull: Star formation
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      – SubjectFull: Young stellar objects
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      – SubjectFull: Dense interstellar clouds
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      – SubjectFull: Interstellar filaments
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