A common origin for the circumnuclear disc and the nearby molecular clouds in the Galactic Centre

Ballone, Alessandro; Mapelli, Michela; Trani, Alessandro A.

doi:10.1093/mnras/stz2147

Cited by 5 publications

(5 citation statements)

References 88 publications

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“…They concluded that supernova feedback associated with the intense star formation activity in the CMZ can generate an inflow rate of ∼ 0.03 M yr −1 (< 5% of the inflow rate from large-scales; §4.1.1), by stochastically launching parcels of gas towards the centre and/or by randomly changing their angular momentum. At this rate the CND would only take ∼ 3 Myr to build up, consistent with the view inferred from observations that the CND is a transient structure on this timescale (Requena-Torres et al 2012;Mapelli and Trani 2016;Ballone et al 2019;Dinh et al 2021, §2.1.4).…”

Section: From the Cmz To The Nucleussupporting

confidence: 85%

“…The exact mechanism by which gas is transported from the CMZ to the inner 10-20 parsecs is an open question ( §4.1). However, there is some evidence that the CND is built up from the tidal disruption of molecular clouds located within the inner ∼ 10-20 pc (Ho et al 1991;Coil and Ho 2000;McGary et al 2001;Martín et al 2012;Mapelli and Trani 2016;Hsieh et al 2017Hsieh et al , 2019Tsuboi et al 2018;Ballone et al 2019). Several filamentary molecular gas structures, or "streamers", have been detected surrounding the CND.…”

Section: The Circumnuclear Discmentioning

confidence: 99%

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Star Formation in the Central Molecular Zone of the Milky Way

Henshaw¹,

Barnes²,

Battersby³

et al. 2022

Preprint

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The Central Molecular Zone (CMZ) is a ring-like accumulation of molecular gas in the innermost few hundred parsecs of the Milky Way, generated by the inward transport of matter driven by the Galactic bar. The CMZ is the most extreme star-forming environment in the Galaxy. The unique combination of large-scale dynamics and extreme interstellar medium conditions, characterised by high densities, temperatures, pressures, turbulent motions, and strong magnetic fields, make the CMZ an ideal region for testing current star and planet formation theories. We review the recent observational and theoretical advances in the field, and combine these to draw a comprehensive, multi-scale and multi-physics picture of the cycle of matter and energy in the context of star formation in the closest galactic nucleus.

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Section: From the Cmz To The Nucleussupporting

confidence: 85%

Section: The Circumnuclear Discmentioning

confidence: 99%

Star Formation in the Central Molecular Zone of the Milky Way

Henshaw¹,

Barnes²,

Battersby³

et al. 2022

Preprint

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“…(ii) They appear to be morphologically and kinematically connected to gaseous structures in the immediate vicinity SgrA * , such as the CND (Okumura et al 1991;Coil & Ho 2000;Liu et al 2012;Hsieh et al 2017;Takekawa, Oka & Tanaka 2017;Tsuboi et al 2018;Ballone, Mapelli & Trani 2019).…”

Section: The 20 and 50 Km S −1 Cloudsmentioning

confidence: 99%

Simulations of the Milky Way’s central molecular zone – I. Gas dynamics

Treß

Sormani

Glover

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We use hydrodynamical simulations to study the Milky Way’s central molecular zone (CMZ). The simulations include a non-equilibrium chemical network, the gas self-gravity, star formation and supernova feedback. We resolve the structure of the interstellar medium at sub-parsec resolution while also capturing the interaction between the CMZ and the bar-driven large-scale flow out to R ∼ 5 kpc. Our main findings are as follows: (1) The distinction between inner (R ≲ 120 pc) and outer (120 ≲ R ≲ 450 pc) CMZ that is sometimes proposed in the literature is unnecessary. Instead, the CMZ is best described as single structure, namely a star-forming ring with outer radius R ≃ 200 pc which includes the 1.3○ complex and which is directly interacting with the dust lanes that mediate the bar-driven inflow. (2) This accretion can induce a significant tilt of the CMZ out of the plane. A tilted CMZ might provide an alternative explanation to the ∞-shaped structure identified in Herschel data by Molinari et al. 2011. (3) The bar in our simulation efficiently drives an inflow from the Galactic disc (R ≃ 3 kpc) down to the CMZ (R ≃ 200 pc) of the order of $1\rm \, M_\odot \, yr^{-1}$, consistent with observational determinations. (4) Supernova feedback can drive an inflow from the CMZ inwards towards the circumnuclear disc of the order of $\sim 0.03\, \rm M_\odot \, yr^{-1}$. (5) We give a new interpretation for the 3D placement of the 20 and 50 km s−1 clouds, according to which they are close (R ≲ 30 pc) to the Galactic centre, but are also connected to the larger-scale streams at R ≳ 100 pc.

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“…Based on the observation that the CND appears to be disequilibrated because of the presence of internal transient structures, many publications model the formation of the CND as a recent event that resulted from the infall of a dense cloud toward the central black hole (Sanders 1998;Bradford et al 2005;Bonnell & Rice 2008;Wardle & Yusef-Zadeh 2008;Hobbs & Nayakshin 2009;Alig et al 2011;Oka et al 2011;Mapelli et al 2012;Mapelli & Trani 2016;Trani et al 2018;Goicoechea et al 2018;Ballone et al 2019). The idea rests on the assumption that a relatively massive cloud with a very small total angular momentum can somehow be produced near the black hole, or can be produced further away, but be unimpeded in its accelerating trajectory toward the black hole.…”

Section: Origin and Longevity Of The Cndmentioning

confidence: 99%

“…A popular model to account for the transient structures within the CND is that a passing cloud was gravitationally captured by the black hole. This "infalling cloud" was then tidally disrupted into what is now the CND (Sanders 1998;Bradford et al 2005;Bonnell & Rice 2008;Wardle & Yusef-Zadeh 2008;Hobbs & Nayakshin 2009;Alig et al 2011;Oka et al 2011;Mapelli et al 2012;Mapelli & Trani 2016;Trani et al 2018;Goicoechea et al 2018;Ballone et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Effects of turbulence in the Circumnuclear Disk

Dinh,

Salas,

Morris

et al. 2021

Preprint

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A Circumnuclear Disk (CND) of molecular gas occupies the central few parsecs of the Galactic Center. It is likely subject to turbulent disruptions from violent events in its surrounding environment, but the effect of such perturbations has not yet been investigated in detail. Here we perform 3D, Nbody/smoothed particle hydrodynamic (SPH) simulations with an adapted general turbulence driving method to investigate the CND's structural evolution, in particular its reaction to varied scales of injected turbulence. We find that, because of shear flow in the disk, transient arcs of gas (streams) naturally arise when turbulence is driven on large scales (up to ∼ 4 pc), as might occur when a supernova blast wave encounters the CND. Because energetic events arise naturally and often in the central parsecs of our Galaxy, this result suggests that the transient structures that characterize the CND do not imply that the CND itself is a transient structure. We also note that features similar to the density concentrations, or "clumps", detailed in literature emerge when we account for the observed orientation of the disk and for the spatial resolution of observations. As such, clumps could be an artifact of observational limitations.

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A common origin for the circumnuclear disc and the nearby molecular clouds in the Galactic Centre

Cited by 5 publications

References 88 publications

Star Formation in the Central Molecular Zone of the Milky Way

Star Formation in the Central Molecular Zone of the Milky Way

Simulations of the Milky Way’s central molecular zone – I. Gas dynamics

Effects of turbulence in the Circumnuclear Disk

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