Conditions for the formation of massive stars

Wolfire, M. G.; Cassinelli, J. P.

doi:10.1086/165503

Cited by 366 publications

(383 citation statements)

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“…Pressure on dust grains that absorb the radiation from the star or stars in an H ii region and the radiation from any shock at the base of an accretion flow where the flow decelerates can be competitive with the gravitational attraction of the stars (Mestel 1954;Larson & Starrfield 1971;Appenzeller & Tscharnuter 1974;Kahn 1974;Yorke & Krugel 1977;Wolfire & Cassinelli 1987) One can derive a limiting luminosity-to-mass ratio by balancing the outward force of the radiation against the inward force of gravity,…”

Section: Radiation Pressurementioning

confidence: 99%

“…Kahn (1974) and Wolfire & Casinelli (1986, 1987 have pointed out that the stellar radiation is absorbed in a thin boundary layer that is found at the point in the accretion flow where the gas temperature, which is increasing as the flow approaches the star, reaches the sublimation temperature of the dust. In front of this layer, the dust will be sublimated and therefore not available to absorb the stellar radiation.…”

Section: Radiation Pressurementioning

confidence: 99%

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The Formation of Massive Stars by Accretion through Trapped Hypercompact HiiRegions

Keto¹

2003

ApJ

197

189

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The formation of massive stars may take place at relatively low accretion rates over a long period of time if the accretion can continue past the onset of core hydrogen ignition. The accretion may continue despite the formation of an ionized H ii region around the star if the H ii region is small enough that the gravitational attraction of the star dominates the thermal pressure of the H ii region. The accretion may continue despite radiation pressure acting against dust grains in the molecular gas if the momentum of the accretion flow is sufficient to push the dust grains through a narrow zone of high dust opacity at the ionization boundary and into the H ii region where the dust is sublimated. This model of massive star formation by continuing accretion predicts a new class of gravitationally trapped, long-lived, hypercompact H ii regions. The observational characteristics of the trapped hypercompact H ii regions can be predicted for comparison with observations.

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Section: Radiation Pressurementioning

confidence: 99%

Section: Radiation Pressurementioning

confidence: 99%

The Formation of Massive Stars by Accretion through Trapped Hypercompact HiiRegions

Keto¹

2003

ApJ

197

189

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“…A particularly relevant set of papers by Wolfire & Cassinelli (1986, 1987 considered spherically infalling dust onto a massive protostar. Much of our argument parallels the calculation of these authors (especially at the high-mass limit), although the present application to T Tauri and Herbig Ae/Be stars span sufficiently different physical conditions to justify the specific calculation presented below.…”

Section: Effects Of Realistic Dust Propertiesmentioning

confidence: 99%

“…This effect will only occur for hot stars with significant UV luminosity and could qualitatively explain the trend toward undersized disks for the high-luminosity YSOs. Wolfire & Cassinelli (1986) considered a similar effect in calculating the equilibrium temperature structure around an accreting massive protostar. Indeed, Hartmann, Kenyon, & Calvet (1993) showed that the gaseous inner disk of a Herbig Ae/Be star can become optically thick for high accretion rates ( _ M Me10 À7 M ).…”

Section: Gas Absorption In the Inner Diskmentioning

confidence: 99%

On the Interferometric Sizes of Young Stellar Objects

Monnier

Millan-Gabet

2002

ApJ

228

240

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Long-baseline optical interferometers can now detect and resolve hot dust emission thought to arise at the inner edge of circumstellar disks around young stellar objects (YSOs). We argue that the near-infrared sizes being measured are closely related to the radius at which dust is sublimated by the stellar radiation field. We consider how realistic dust optical properties and gas opacity dramatically affect the predicted location of this dust destruction radius, an exercise routinely done in other contexts but so far neglected in the analysis of near-infrared sizes of YSOs. We also present the accumulated literature of near-infrared YSO sizes in the form of a size-luminosity diagram and compare with theoretical expectations. We find evidence that large (e1.0 lm) dust grains predominate in the inner disks of T Tauri and Herbig Ae/Be stars, under the assumption that the innermost gaseous disks are optically thin at visible wavelengths.

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“…This drawback is avoided by the so-called hybrid RT scheme, in which a frequency-dependent ray-tracing integral of the RT equation from the protostellar source is used to determine the intensity of the radiation field until it becomes optically thick, and the radiation field at this point is used as a boundary condition for the diffusion approximation in the rest of the computational domain. This method was first used in 1-D simulations of massive star formation by Wolfire & Cassinelli (1986, 1987 and was extended to higher dimensions by Kuiper et al (2010). Although more computationally expensive than FLD, the method has the advantage that it captures the physics of the first absorption of the protostellar radiation field by the dust, as well as any shadowing effects close to the source.…”

Section: Introductionmentioning

confidence: 99%

Radiation-hydrodynamical simulations of massive star formation using Monte Carlo radiative transfer – II. The formation of a 25 solar-mass star

Harries

Douglas

Ali

2017

Monthly Notices of the Royal Astronomical Society

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We present a numerical simulation of the formation of a massive star using MonteCarlo-based radiation hydrodynamics (RHD). The star forms via stochastic disc accretion and produces fast, radiation-driven bipolar cavities. We find that the evolution of the infall rate (considered to be the mass flux across a 1500 au spherical boundary), and the accretion rate onto the protostar, are broadly consistent with observational constraints. After 35 kyr the star has a mass of 25 M and is surrounded by a disc of mass 7 M and 1500 au radius, and we find that the velocity field of the disc is close to Keplerian. Once again these results are consistent with those from recent high-resolution studies of discs around forming massive stars. Synthetic imaging of the RHD model shows good agreement with observations in the near-and far-IR, but may be in conflict with observations that suggests that MYSOs are typically circularly symmetric on the sky at 24.5 µm. Molecular line simulations of a CH 3 CN transition compare well with observations in terms of surface brightness and line width, and indicate that it should be possible to reliably extract the protostellar mass from such observations.

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Conditions for the formation of massive stars

Cited by 366 publications

References 0 publications

The Formation of Massive Stars by Accretion through Trapped Hypercompact HiiRegions

The Formation of Massive Stars by Accretion through Trapped Hypercompact HiiRegions

On the Interferometric Sizes of Young Stellar Objects

Radiation-hydrodynamical simulations of massive star formation using Monte Carlo radiative transfer – II. The formation of a 25 solar-mass star

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