Simulations of the Milky Way’s central molecular zone - II. Star formationCitation formats

  • External authors:
  • Mattia C Sormani
  • Robin G Tress
  • Simon C O Glover
  • Ralf S Klessen
  • Cara D Battersby
  • Paul C Clark
  • H Perry Hatchfield

Standard

Simulations of the Milky Way’s central molecular zone - II. Star formation. / Sormani, Mattia C; Tress, Robin G; Glover, Simon C O; Klessen, Ralf S; Battersby, Cara D; Clark, Paul C; Hatchfield, H Perry; Smith, Rowan J.

In: Monthly Notices of the Royal Astronomical Society, 09.07.2020.

Research output: Contribution to journalArticle

Harvard

Sormani, MC, Tress, RG, Glover, SCO, Klessen, RS, Battersby, CD, Clark, PC, Hatchfield, HP & Smith, RJ 2020, 'Simulations of the Milky Way’s central molecular zone - II. Star formation', Monthly Notices of the Royal Astronomical Society. https://doi.org/10.1093/mnras/staa1999

APA

Sormani, M. C., Tress, R. G., Glover, S. C. O., Klessen, R. S., Battersby, C. D., Clark, P. C., Hatchfield, H. P., & Smith, R. J. (2020). Simulations of the Milky Way’s central molecular zone - II. Star formation. Monthly Notices of the Royal Astronomical Society. https://doi.org/10.1093/mnras/staa1999

Vancouver

Sormani MC, Tress RG, Glover SCO, Klessen RS, Battersby CD, Clark PC et al. Simulations of the Milky Way’s central molecular zone - II. Star formation. Monthly Notices of the Royal Astronomical Society. 2020 Jul 9. https://doi.org/10.1093/mnras/staa1999

Author

Sormani, Mattia C ; Tress, Robin G ; Glover, Simon C O ; Klessen, Ralf S ; Battersby, Cara D ; Clark, Paul C ; Hatchfield, H Perry ; Smith, Rowan J. / Simulations of the Milky Way’s central molecular zone - II. Star formation. In: Monthly Notices of the Royal Astronomical Society. 2020.

Bibtex

@article{cd3f026e73614269a16e9ccebdec39dc,
title = "Simulations of the Milky Way{\textquoteright}s central molecular zone - II. Star formation",
abstract = "The Milky Way{\textquoteright}s central molecular zone (CMZ) has emerged in recent years as a unique laboratory for the study of star formation. Here we use the simulations presented in Tress et al. 2020 to investigate star formation in the CMZ. These simulations resolve the structure of the interstellar medium at sub-parsec resolution while also including the large-scale flow in which the CMZ is embedded. Our main findings are as follows. (1) While most of the star formation happens in the CMZ ring at R ≳ 100 pc, a significant amount also occurs closer to SgrA* at R ≲ 10 pc. (2) Most of the star formation in the CMZ happens downstream of the apocentres, consistent with the “pearls-on-a-string” scenario, and in contrast to the notion that an absolute evolutionary timeline of star formation is triggered by pericentre passage. (3) Within the timescale of our simulations (∼100 Myr), the depletion time of the CMZ is constant within a factor of ∼2. This suggests that variations in the star formation rate are primarily driven by variations in the mass of the CMZ, caused for example by AGN feedback or externally-induced changes in the bar-driven inflow rate, and not by variations in the depletion time. (4) We study the trajectories of newly born stars in our simulations. We find several examples that have age and 3D velocity compatible with those of the Arches and Quintuplet clusters. Our simulations suggest that these prominent clusters originated near the collision sites where the bar-driven inflow accretes onto the CMZ, at symmetrical locations with respect to the Galactic centre, and that they have already decoupled from the gas in which they were born.",
author = "Sormani, {Mattia C} and Tress, {Robin G} and Glover, {Simon C O} and Klessen, {Ralf S} and Battersby, {Cara D} and Clark, {Paul C} and Hatchfield, {H Perry} and Smith, {Rowan J}",
year = "2020",
month = jul
day = "9",
doi = "10.1093/mnras/staa1999",
language = "English",
journal = "Royal Astronomical Society. Monthly Notices",
issn = "1365-2966",
publisher = "Oxford University Press",

}

RIS

TY - JOUR

T1 - Simulations of the Milky Way’s central molecular zone - II. Star formation

AU - Sormani, Mattia C

AU - Tress, Robin G

AU - Glover, Simon C O

AU - Klessen, Ralf S

AU - Battersby, Cara D

AU - Clark, Paul C

AU - Hatchfield, H Perry

AU - Smith, Rowan J

PY - 2020/7/9

Y1 - 2020/7/9

N2 - The Milky Way’s central molecular zone (CMZ) has emerged in recent years as a unique laboratory for the study of star formation. Here we use the simulations presented in Tress et al. 2020 to investigate star formation in the CMZ. These simulations resolve the structure of the interstellar medium at sub-parsec resolution while also including the large-scale flow in which the CMZ is embedded. Our main findings are as follows. (1) While most of the star formation happens in the CMZ ring at R ≳ 100 pc, a significant amount also occurs closer to SgrA* at R ≲ 10 pc. (2) Most of the star formation in the CMZ happens downstream of the apocentres, consistent with the “pearls-on-a-string” scenario, and in contrast to the notion that an absolute evolutionary timeline of star formation is triggered by pericentre passage. (3) Within the timescale of our simulations (∼100 Myr), the depletion time of the CMZ is constant within a factor of ∼2. This suggests that variations in the star formation rate are primarily driven by variations in the mass of the CMZ, caused for example by AGN feedback or externally-induced changes in the bar-driven inflow rate, and not by variations in the depletion time. (4) We study the trajectories of newly born stars in our simulations. We find several examples that have age and 3D velocity compatible with those of the Arches and Quintuplet clusters. Our simulations suggest that these prominent clusters originated near the collision sites where the bar-driven inflow accretes onto the CMZ, at symmetrical locations with respect to the Galactic centre, and that they have already decoupled from the gas in which they were born.

AB - The Milky Way’s central molecular zone (CMZ) has emerged in recent years as a unique laboratory for the study of star formation. Here we use the simulations presented in Tress et al. 2020 to investigate star formation in the CMZ. These simulations resolve the structure of the interstellar medium at sub-parsec resolution while also including the large-scale flow in which the CMZ is embedded. Our main findings are as follows. (1) While most of the star formation happens in the CMZ ring at R ≳ 100 pc, a significant amount also occurs closer to SgrA* at R ≲ 10 pc. (2) Most of the star formation in the CMZ happens downstream of the apocentres, consistent with the “pearls-on-a-string” scenario, and in contrast to the notion that an absolute evolutionary timeline of star formation is triggered by pericentre passage. (3) Within the timescale of our simulations (∼100 Myr), the depletion time of the CMZ is constant within a factor of ∼2. This suggests that variations in the star formation rate are primarily driven by variations in the mass of the CMZ, caused for example by AGN feedback or externally-induced changes in the bar-driven inflow rate, and not by variations in the depletion time. (4) We study the trajectories of newly born stars in our simulations. We find several examples that have age and 3D velocity compatible with those of the Arches and Quintuplet clusters. Our simulations suggest that these prominent clusters originated near the collision sites where the bar-driven inflow accretes onto the CMZ, at symmetrical locations with respect to the Galactic centre, and that they have already decoupled from the gas in which they were born.

U2 - 10.1093/mnras/staa1999

DO - 10.1093/mnras/staa1999

M3 - Article

JO - Royal Astronomical Society. Monthly Notices

JF - Royal Astronomical Society. Monthly Notices

SN - 1365-2966

ER -