Monte Carlo radiative transfer in protoplanetary disks

By C. Pinte, F. Ménard, G. Duchêne, P. Bastien. 2006

300 citations recorded by the source corpus.

Aims.We present a new continuum 3D radiative transfer code, MCFOST, based on a Monte-Carlo method. MCFOST can be used to calculate (i) monochromatic images in scattered light and/or thermal emission; (ii) polarisation maps; (iii) interferometric visibilities; (iv) spectral energy distributions; and (v) dust temperature distributions of protoplanetary disks. Methods: .Several improvements to the standard Monte Carlo method are implemented in MCFOST to increase efficiency and reduce convergence time, including wavelength distribution adjustments, mean intensity calculations, and an adaptive sampling of the radiation field. The reliability and efficiency of the code are tested against a previously-defined benchmark, using a 2D disk configuration. No significant difference (no more than 10% and usually much less) is found between the temperatures and SEDs calculated by MCFOST and by other codes included in the benchmark. Results: . A study of the lowest disk mass detectable by Spitzer, around young stars, is presented and the colours of "representative" parametric disks compared to recent IRAC and MIPS Spitzer colours of solar-like young stars located in nearby star-forming regions.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/4d2ed52af40cfb12252bf4426e17e12a9c940742

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In Astronomy and Astrophysics

1. Simon Bruderer
2. C. Dullemond
3. E. Dishoeck
4. G. Herczeg
5. L. Testi
6. Th. Henning
7. G. Blake
8. S. Doty

In Atmospheric Science

1. Simon Bruderer
2. C. Dullemond
3. C. Pinte
4. S. Doty
5. G. Herczeg
6. J. Fritz
7. D. Mentiplay
8. I. Gregorio-Monsalvo

Citations in the corpus

• Three-Dimensional Dust Radiative Transfer ∗ (2013, methodology): “In this hybrid method, the photon packages are followed through the domain using the instantaneous dust emission technique, but the final dust emission spectrum of the cells, used to create images and SEDs, is calculated based on the continuous absorption approach (Pinte et al. 2006).”
• Radiative transfer in very optically thick circumstellar disks (2009, methodology): “The required flexibility for radiative transfer can be obtained by using a Monte Carlo method (see e.g. Bjorkman & Wood 2001; Niccolini et al. 2003; Pinte et al. 2006).”
• Radiation thermo-chemical models of protoplanetary disks I. Hydrostatic disk structure and inner rim (2009, result): “The ProDiMo results are shown with blue diamonds in comparison to the MCFOST results (Pinte et al., 2006) with blacklines. all frequencies,Jsmall=10−30erg cm−2s−1Hz−1sr−1) is larger than some threshold (∼0.01), the source functions are re-calculated and the radiative transfer is solved again.”
• Direct mapping of the temperature and velocity gradients in discs Imaging the vertical CO snow line around IM Lupi (2017, methodology): “We use the Monte Carlo radiative transfer code MCFOST (Pinte et al. 2006, 2009) to build a simple model of the CO emission.”
• Kinematic Evidence for an Embedded Protoplanet in a Circumstellar Disk (2018, methodology): “Software: CASA(McMullinetal.2007),phantom(Price et al. 2017), splash (Price 2007), mcfost (Pinte et al. 2006, 2009).”
• Accretion disks in luminous young stellar objects (2015, methodology): “Popular RT codes publicly available and suitable for young star disk studies are RADMC (Dullemond, 2011), HoChunk (Whitney et al., 2013), MC3D (Wolf, 2003), MCFOST (Pinte et al., 2006).”
• Survival of molecular gas in cavities of transition disks - I. CO (2013, methodology): “The fraction of photon packages emitted by the protostar, the dust and the interstellar radiation field or cosmic microwave background is chosen according to their relative contribution to the luminosity at one wavelength (e.g. Pinte et al. 2006; Harries 2011).”
• Probing dust grain evolution in IM Lupi's circumstellar disc. Multi-wavelength observations and mo (2008, methodology): “Synthetic images and spectral energy distributions are computed using MCFOST, a 3D continuum radiative transfer code based on the Monte Carlo method (Pinte et al. 2006).”
• Unveiling the gas-and-dust disk structure in HD 163296 using ALMA observations (2013, methodology): “To extend beyond the simple power-law fitting, the threedimensional Monte Carlo radiative transfer code MCFOST was used to model the data presented in this work (see Pinte et al. 2006, 2009 for a more detailed description).”
• The warm gas atmosphere of the HD 100546 disk seen by Herschel - Evidence of a gas-rich, carbon-poor atmosphere? (2012, methodology): “We implement a method proposed by Pinte et al. (2006) and measure the ambient radiation field using the estimator given in Lucy (1999) during the propagation of the photons.”
• Protoplanetary disk lifetimes vs stellar mass and possible implications for giant planet populations (2015, methodology): “To test how much this dependence might affect our results, we computed a grid of radiative transfer models of circumstellar disks using the code MCFOST (Pinte et al. 2006).”
• DUST AND GAS IN THE DISK OF HL TAURI: SURFACE DENSITY, DUST SETTLING, AND DUST-TO-GAS RATIO (2015, methodology): “For each of these models, synthetic MCFOST images were calculated, visibilities computed using the CASA simulator and the total χ2 calculated.”
• EFFICIENT THREE-DIMENSIONAL NLTE DUST RADIATIVE TRANSFER WITH SKIRT (2011, background): “…the construction of 2D and 3D realistic radiative transfer models is now possible (e.g. Xilouris et al. 1999; Popescu et al. 2000; Gordon et al. 2001; Steinacker et al. 2003; Electronic address: maarten.baes@ugent.be Semionov & Vansevičius 2005; Pinte et al. 2006; Jonsson 2006; Bianchi 2008).”