Smoothed Particle Hydrodynamic Simulations of Galactic Gaseous Disk with Bar: Distribution and Kinematic Structure of Molecular Clouds toward the Galactic Center

1999 ◽  
Vol 513 (1) ◽  
pp. 242-251 ◽  
Author(s):  
C. W. Lee ◽  
H. M. Lee ◽  
H. B. Ann ◽  
K. H. Kwon
Keyword(s):  
Molecular Clouds ◽  
Galactic Center ◽  
Kinematic Structure ◽  
Hydrodynamic Simulations ◽  
Gaseous Disk ◽  
Smoothed Particle ◽  
Smoothed Particle Hydrodynamic

scholarly journals Forming misaligned stellar disks around a massive black hole: cloud infall in the Galactic center

2013 ◽  
Vol 9 (S303) ◽  
pp. 245-247
Author(s):  
William Lucas ◽  
Ian Bonnell ◽  
Melvyn Davies ◽  
Ken Rice
Keyword(s):  
Black Hole ◽  
Angular Momentum ◽  
Galactic Center ◽  
Massive Black Hole ◽  
Hydrodynamic Simulations ◽  
Large Spread ◽  
Smoothed Particle ◽  
The Creation ◽  
Sgr A ◽  
Smoothed Particle Hydrodynamic

AbstractThe innermost parsec around Sgr A* has been found to play host to two disks or streamers of O and W-R stars. They are misaligned by an angle approaching 90°. That the stars are approximately coeval indicates that they formed in the same event rather than independently. We have performed smoothed particle hydrodynamic simulations of the infall of a single prolate cloud towards a massive black hole. As the cloud is disrupted, the large spread in angular momentum can, if conditions allow, lead to the creation of misaligned gas disks. In turn, stars may form within those disks. We are now investigating the origins of these clouds in the Galactic center (GC) region.

scholarly journals The impact of episodic outflow feedback on stellar multiplicity and the star formation efficiency

2020 ◽  
Vol 500 (3) ◽  
pp. 3594-3612
Author(s):  
P F Rohde ◽  
S Walch ◽  
S D Clarke ◽  
D Seifried ◽  
A P Whitworth ◽  
...  
Keyword(s):  
Star Formation ◽  
Hydrodynamic Simulations ◽  
The Core ◽  
Subgrid Model ◽  
High Incidence ◽  
Smoothed Particle ◽  
The Mean ◽  
Smoothed Particle Hydrodynamic ◽  
Formation Efficiency ◽  
The Impact

ABSTRACT The accretion of material on to young protostars is accompanied by the launching of outflows. Observations show that accretion, and therefore also outflows, are episodic. However, the effects of episodic outflow feedback on the core scale are not well understood. We have performed 88 smoothed particle hydrodynamic simulations of turbulent dense $1 \, {{\mathrm{M}}}_{\odot }$ cores to study the influence of episodic outflow feedback on the stellar multiplicity and the star formation efficiency (SFE). Protostars are represented by sink particles, which use a subgrid model to capture stellar evolution, inner-disc evolution, episodic accretion, and the launching of outflows. By comparing simulations with and without episodic outflow feedback, we show that simulations with outflow feedback reproduce the binary statistics of young stellar populations, including the relative proportions of singles, binaries, triples, etc. and the high incidence of twin binaries with q ≥ 0.95; simulations without outflow feedback do not. Entrainment factors (the ratio between total outflowing mass and initially ejected mass) are typically ∼7 ± 2, but can be much higher if the total mass of stars formed in a core is low and/or outflow episodes are infrequent. By decreasing both the mean mass of the stars formed and the number of stars formed, outflow feedback reduces the SFE by about a factor of 2 (as compared with simulations that do not include outflow feedback).

scholarly journals 4.15. Dynamics of the Galactic center molecular clouds

1998 ◽  
Vol 184 ◽  
pp. 197-199
Author(s):  
C. W. Lee ◽  
H. M. Lee ◽  
H.B. Ann ◽  
K.H. Kwon
Keyword(s):  
Smoothed Particle Hydrodynamics ◽  
Molecular Clouds ◽  
Galactic Center ◽  
Combined Effects ◽  
Gravitational Perturbation ◽  
Particle Hydrodynamics ◽  
Smoothed Particle

We have performed Smoothed Particle Hydrodynamics (SPH) simulations in order to understand the dynamical structures of Galactic Center molecular clouds. In our study it was found that the structures of GC molecular clouds could be induced by the combined effects of a gravitational perturbation by rotating bar potential and the hydrodynamic collisions between the clouds.

Analysis of Contact Mechanics and Smoothed Particle Hydrodynamic Simulations of Viscoelastic Polymer Sine Waves

2015 ◽  
Author(s):  
Nick Cramer ◽  
Janet Chao ◽  
Travis Tollefson ◽  
M. Teodorescu
Keyword(s):  
United States ◽  
Head And Neck ◽  
Contact Mechanics ◽  
The United States ◽  
Head And Neck Cancers ◽  
Malignant Neoplasms ◽  
Invasive Procedures ◽  
Hydrodynamic Simulations ◽  
Smoothed Particle ◽  
Smoothed Particle Hydrodynamic

According the American Cancer Society’s data, in 2013, an estimated 53,640 people developed head and neck cancers [1], which accounts for about 3% to 5% of all cancers in the United States. Removing head and neck malignant neoplasms is one of the first stages towards patient recovery. However, these types of invasive procedures often lead to disfiguring scars and resections with functional and aesthetical drawbacks (see Figure 1).

scholarly journals Dynamically Driven Inflow onto the Galactic Center and its Effect upon Molecular Clouds

2021 ◽  
Vol 922 (1) ◽  
pp. 79
Author(s):  
H Perry Hatchfield ◽  
Mattia C. Sormani ◽  
Robin G. Tress ◽  
Cara Battersby ◽  
Rowan J. Smith ◽  
...  
Keyword(s):  
Molecular Clouds ◽  
Galactic Center ◽  
Critical Role ◽  
Average Density ◽  
Gas Flows ◽  
Hydrodynamic Simulations ◽  
Tracer Particles ◽  
Formation And Evolution ◽  
Self Gravity ◽  
Total Inflow

Abstract The Galactic bar plays a critical role in the evolution of the Milky Way’s Central Molecular Zone (CMZ), driving gas toward the Galactic Center via gas flows known as dust lanes. To explore the interaction between the CMZ and the dust lanes, we run hydrodynamic simulations in arepo, modeling the potential of the Milky Way’s bar in the absence of gas self-gravity and star formation physics, and we study the flows of mass using Monte Carlo tracer particles. We estimate the efficiency of the inflow via the dust lanes, finding that only about a third (30% ± 12%) of the dust lanes’ mass initially accretes onto the CMZ, while the rest overshoots and accretes later. Given observational estimates of the amount of gas within the Milky Way’s dust lanes, this suggests that the true total inflow rate onto the CMZ is 0.8 ± 0.6 M ⊙ yr−1. Clouds in this simulated CMZ have sudden peaks in their average density near the apocenter, where they undergo violent collisions with inflowing material. While these clouds tend to counter-rotate due to shear, co-rotating clouds occasionally occur due to the injection of momentum from collisions with inflowing material (∼52% are strongly counter-rotating, and ∼7% are strongly co-rotating of the 44 cloud sample). We investigate the formation and evolution of these clouds, finding that they are fed by many discrete inflow events, providing a consistent source of gas to CMZ clouds even as they collapse and form stars.

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