Star Cluster Formation in Orion A

Lim, Wanggi; Nakamura, Fumitaka; Wu, Benjamin; Bisbas, Thomas G.; Tan, Jonathan C.; Chambers, Edward; Bally, John; Kong, Shuo; McGehee, Peregrine; Lis, Dariusz C.; Ossenkopf-Okada, Volker; Sánchez-Monge, Álvaro

doi:10.48550/arxiv.2004.03668

Cited by 2 publications

(2 citation statements)

References 38 publications

(53 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Several recent papers have argued for a cloud-cloud collision scenario for the formation of the ONC (Fukui et al 2018;Lim et al 2020), NGC2023 (Yamada et al 2020), NGC2024 (Enokiya et al 2020), and NGC 2068/2071(Fujita et al 2020 in the Orion complex. The cloud-cloud collision argument is made based on the analysis of the radial velocity of the CO gas, in particular a jump in the velocities at particular star-formation rich regions, like the Head of the Orion A cloud.…”

Section: Implications For the Cloud-cloud Collision Scenario For The ...mentioning

confidence: 99%

3D dynamics of the Orion cloud complex -- Discovery of coherent radial gas motions at the 100-pc scale

Großschedl,

Alves,

Meingast

et al. 2020

Preprint

View full text Add to dashboard Cite

We present the first study of the 3D dynamics of the gas in the entire Southern Orion cloud complex. We used the YSO's proper motions from Gaia as a proxy for the gas proper motion, together with gas radial velocities from archival CO data, to compute the space motion of the different star-forming clouds in the complex, including sub-regions in Orion A, Orion B, and two outlying cometary clouds. From the analysis of the cloud's orbits in space and time we find that they were closest about 6 Myr ago and are moving radially away from roughly the same region in space. This coherent 100-pc scale radial motion supports a scenario where the entire complex is reacting to a major feedback event that we name the Orion−6 event. This event, that we tentatively associate with the recently discovered Orion X population, shaped the distribution and kinematics of the gas we observe today, although it is unlikely to have been the sole major feedback event in the region. We argue that the dynamics of most of the YSOs carry the memory of the feedback-driven star formation history in Orion and that the majority of the young stars in this complex are a product of large-scale triggering, that can raise the star formation rate by at least an order of magnitude, as in the case of the Orion A's Head (the Integral Shape Filament). Our results imply that at the genesis of the Orion Nebula Cluster (and NGC 2023/2024 in Orion B) lies a feedback/compression/triggering process.

show abstract

Section: Implications For the Cloud-cloud Collision Scenario For The ...mentioning

confidence: 99%

3D dynamics of the Orion cloud complex -- Discovery of coherent radial gas motions at the 100-pc scale

Großschedl,

Alves,

Meingast

et al. 2020

Preprint

View full text Add to dashboard Cite

show abstract

“…As a result, the cloud collision could have triggered MR and created a dense filamentary cloud, which is the Orion A we see today. Recently, Lim et al (2020) also suggested a cloud-cloud collision scenario for Orion A formation but based on the gas-star kinematics.…”

Section: Cmr In Orion Amentioning

confidence: 99%

The CARMA-NRO Orion Survey: Filament Formation via Collision-Induced Magnetic Reconnection -- The Stick in Orion A

Kong,

Ossenkopf-Okada,

Arce

et al. 2020

Preprint

Self Cite

View full text Add to dashboard Cite

A unique filament is identified in the Herschel maps of the Orion A giant molecular cloud. The filament, which, we name the Stick, is ruler-straight and at an early evolutionary stage. Transverse position-velocity diagrams show two velocity components closing in on the Stick. The filament shows consecutive rings/forks in C 18 O(1-0) channel maps, which is reminiscent of structures generated by magnetic reconnection. We propose that the Stick formed via collision-induced magnetic reconnection (CMR). We use the magnetohydrodynamics (MHD) code Athena++ to simulate the collision between two diffuse molecular clumps, each carrying an anti-parallel magnetic field. The clump collision produces a narrow, straight, dense filament with a factor of >200 increase in density. The production of the dense gas is seven times faster than free-fall collapse. The dense filament shows ring/fork-like structures in radiative transfer maps. Cores in the filament are confined by surface magnetic pressure. CMR can be an important dense-gas-producing mechanism in the Galaxy and beyond.

show abstract

Star Cluster Formation in Orion A

Cited by 2 publications

References 38 publications

3D dynamics of the Orion cloud complex -- Discovery of coherent radial gas motions at the 100-pc scale

3D dynamics of the Orion cloud complex -- Discovery of coherent radial gas motions at the 100-pc scale

The CARMA-NRO Orion Survey: Filament Formation via Collision-Induced Magnetic Reconnection -- The Stick in Orion A

Contact Info

Product

Resources

About