Bullet Shooting Cloud–Cloud Collision in MIR Bubble N65
We report that the formation of the twin-bubble system N65 and N65bis may be caused by the cloud–cloud collision (CCC) from the Bullet Nebula. The blueshifted ^13 CO gas component (N65a [47, 55] km s ^−1 ) is associated with the twin-bubble system, while the redshifted ^13 CO gas component (N65b [55...
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2025-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/adc9a3 |
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| author | En Chen Xi Chen Min Fang Xuepeng Chen Qianru He Tian Yang |
| author_facet | En Chen Xi Chen Min Fang Xuepeng Chen Qianru He Tian Yang |
| author_sort | En Chen |
| collection | DOAJ |
| description | We report that the formation of the twin-bubble system N65 and N65bis may be caused by the cloud–cloud collision (CCC) from the Bullet Nebula. The blueshifted ^13 CO gas component (N65a [47, 55] km s ^−1 ) is associated with the twin-bubble system, while the redshifted ^13 CO gas component (N65b [55, 62] km s ^−1 ) is linked to the Bullet Nebula. The distinct signatures of CCC, such as the bridge feature, the U-shaped cavity, and the complementary distribution with displacement, are found between N65a and N65b. The collision timescale is estimated to be 1.15–2.0 Myr, which is consistent with the dynamical ages of the two H ii regions in N65a (0.73 Myr for N65bis and 1.19 Myr for N65, respectively), indicating their CCC-related origin. A total of 354 young stellar objects (YSOs) are found, which are clustered into eight minimum spanning tree groups. The distribution of M1 (at the post-frontal edge) and M2, M3, M4 (at the pre-frontal edge) suggests that the CCC triggers star formation along the collision path of $b=0\mathop{.}\limits^{^\circ }35$ , with younger YSOs present at the pre-frontal edge. Therefore, the bipolar morphology of the twin-bubble system can be interpreted by the collision of N65a and N65b along $b=0\mathop{.}\limits^{^\circ }35$ about 2 Myr ago. |
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| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
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| spelling | doaj-art-b8a39cc0f5dc4c4f9eb8121d05f6ab8f2025-08-20T03:53:46ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01985112010.3847/1538-4357/adc9a3Bullet Shooting Cloud–Cloud Collision in MIR Bubble N65En Chen0https://orcid.org/0009-0002-8449-1734Xi Chen1https://orcid.org/0000-0002-5435-925XMin Fang2https://orcid.org/0000-0001-8060-1321Xuepeng Chen3https://orcid.org/0000-0003-3151-8964Qianru He4https://orcid.org/0000-0002-5077-9599Tian Yang5https://orcid.org/0000-0003-0559-5982Center for Astrophysics, Guangzhou University , Guangzhou 510006, People’s Republic of China ; chenxi@gzhu.edu.cnCenter for Astrophysics, Guangzhou University , Guangzhou 510006, People’s Republic of China ; chenxi@gzhu.edu.cnPurple Mountain Observatory & Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Nanjing 210034, People’s Republic of ChinaPurple Mountain Observatory & Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Nanjing 210034, People’s Republic of ChinaPurple Mountain Observatory & Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Nanjing 210034, People’s Republic of China; School of Astronomy and Space Science, University of Science and Technology of China , Hefei 230026, People’s Republic of ChinaCenter for Astrophysics, Guangzhou University , Guangzhou 510006, People’s Republic of China ; chenxi@gzhu.edu.cnWe report that the formation of the twin-bubble system N65 and N65bis may be caused by the cloud–cloud collision (CCC) from the Bullet Nebula. The blueshifted ^13 CO gas component (N65a [47, 55] km s ^−1 ) is associated with the twin-bubble system, while the redshifted ^13 CO gas component (N65b [55, 62] km s ^−1 ) is linked to the Bullet Nebula. The distinct signatures of CCC, such as the bridge feature, the U-shaped cavity, and the complementary distribution with displacement, are found between N65a and N65b. The collision timescale is estimated to be 1.15–2.0 Myr, which is consistent with the dynamical ages of the two H ii regions in N65a (0.73 Myr for N65bis and 1.19 Myr for N65, respectively), indicating their CCC-related origin. A total of 354 young stellar objects (YSOs) are found, which are clustered into eight minimum spanning tree groups. The distribution of M1 (at the post-frontal edge) and M2, M3, M4 (at the pre-frontal edge) suggests that the CCC triggers star formation along the collision path of $b=0\mathop{.}\limits^{^\circ }35$ , with younger YSOs present at the pre-frontal edge. Therefore, the bipolar morphology of the twin-bubble system can be interpreted by the collision of N65a and N65b along $b=0\mathop{.}\limits^{^\circ }35$ about 2 Myr ago.https://doi.org/10.3847/1538-4357/adc9a3Interstellar mediumMolecular cloudsStellar wind bubblesStar formationPre-main sequence |
| spellingShingle | En Chen Xi Chen Min Fang Xuepeng Chen Qianru He Tian Yang Bullet Shooting Cloud–Cloud Collision in MIR Bubble N65 The Astrophysical Journal Interstellar medium Molecular clouds Stellar wind bubbles Star formation Pre-main sequence |
| title | Bullet Shooting Cloud–Cloud Collision in MIR Bubble N65 |
| title_full | Bullet Shooting Cloud–Cloud Collision in MIR Bubble N65 |
| title_fullStr | Bullet Shooting Cloud–Cloud Collision in MIR Bubble N65 |
| title_full_unstemmed | Bullet Shooting Cloud–Cloud Collision in MIR Bubble N65 |
| title_short | Bullet Shooting Cloud–Cloud Collision in MIR Bubble N65 |
| title_sort | bullet shooting cloud cloud collision in mir bubble n65 |
| topic | Interstellar medium Molecular clouds Stellar wind bubbles Star formation Pre-main sequence |
| url | https://doi.org/10.3847/1538-4357/adc9a3 |
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