Modelling and interpretation of SEDs

Woitke, P.

doi:10.1051/epjconf/201510200007

Cited by 14 publications

(10 citation statements)

References 32 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This is broadly the case independent of the choice of either grid fitting or MCMC fitting. But fits to SEDs alone are notoriously degenerate (Chiang et al 2001;Woitke 2015), and spatially resolved image data or interferometric visibilities are required in order to place robust constraints on many properties of interest. Only a handful of disk studies have successfully and rigorously fit models to heterogeneous observables, including SEDs and images or interferometric visibilities, but when this has been achieved it has often yielded particularly powerful constraints and detailed insights into disk structures (e.g., Pinte et al 2008; Duchêne et al 2010;Lebreton et al 2012;Carmona et al 2014;Milli et al 2015;Cleeves et al 2016).…”

Section: Radiative Transfer Modeling and Model Fitting Of Circumstellmentioning

confidence: 99%

Hubble Space Telescope Scattered-light Imaging and Modeling of the Edge-on Protoplanetary Disk ESO-Hα 569

Wolff

Perrin

Stapelfeldt

et al. 2017

ApJ

View full text Add to dashboard Cite

We present new Hubble Space Telescope (HST) Advanced Camera for Surveys observations and detailed models for a recently discovered edge-on protoplanetary disk around ESO-Hα569 (a low-mass T Tauri star in the Cha I star-forming region). Using radiative transfer models, we probe the distribution of the grains and overall shape of the disk (inclination, scale height, dust mass, flaring exponent, and surface/volume density exponent) by model fitting to multiwavelength (F606W and F814W) HST observations together with a literature-compiled spectral energy distribution. A new tool set was developed for finding optimal fits of MCFOST radiative transfer models using the MCMC code emcee to efficiently explore the high-dimensional parameter space. It is able to selfconsistently and simultaneously fit a wide variety of observables in order to place constraints on the physical properties of a given disk, while also rigorously assessing the uncertainties in those derived properties. We confirm that ESO-Hα569 is an optically thick nearly edge-on protoplanetary disk. The shape of the disk is well-described by a flared disk model with an exponentially tapered outer edge, consistent with models previously advocated on theoretical grounds and supported by millimeter interferometry. The scattered-light images and spectral energy distribution are best fit by an unusually high total disk mass (gas+dust assuming a ratio of 100:1) with a disk-tostar mass ratio of 0.16.

show abstract

Section: Radiative Transfer Modeling and Model Fitting Of Circumstellmentioning

confidence: 99%

Hubble Space Telescope Scattered-light Imaging and Modeling of the Edge-on Protoplanetary Disk ESO-Hα 569

Wolff

Perrin

Stapelfeldt

et al. 2017

ApJ

View full text Add to dashboard Cite

show abstract

“…For example, millimeter dust grains which emit at centimeter to submillimeter wavelengths can have emission that becomes optically thick, especially in the inner disk. In this case, the brightness temperature of the emission reveals the dust thermal temperature, which is equal to the gas temperature in the dense midplane where frequent collisions equilibrate these two components temperatures (e.g., Woitke 2015). A challenge of this method that has become apparent over recent years is that disks are much more structured than previously thought.…”

Section: Vertical Temperature Stratification and Constraints On Geome...mentioning

confidence: 99%

Setting the Stage for Planet Formation: Measurements and Implications of the Fundamental Disk Properties

Miotello¹,

Kamp²,

Birnstiel³

et al. 2022

Preprint

View full text Add to dashboard Cite

The field of planet formation is in an exciting era, where recent observations of disks around low-to intermediate-mass stars made with state of the art interferometers and high-contrast optical and IR facilities have revealed a diversity of substructures, some possibly planet-related. It is therefore important to understand the physical and chemical nature of the protoplanetary building blocks, as well as their spatial distribution, to better understand planet formation. Since PPVI, the field has seen tremendous improvements in observational capabilities, enabling both surveys of large samples of disks and high resolution imaging studies of a few bright disks. Improvements in data quality and sample size have, however, opened up many fundamental questions about properties such as the mass budget of disks, its spatial distribution, and its radial extent. Moreover, the vertical structure of disks has been studied in greater detail with spatially resolved observations, providing new insights on vertical layering and temperature stratification, yet also bringing rise to questions about other properties, such as material transport and viscosity. Each one of these properties -disk mass, surface density distribution, outer radius, vertical extent, temperature structure, and transport -is of fundamental interest as they collectively set the stage for disk evolution and corresponding planet formation theories. In this chapter, we will review our understanding of the fundamental properties of disks including the relevant observational techniques to probe their nature, modeling methods, and the respective caveats. Finally, we discuss the implications for theories of disk evolution and planet formation underlining what new questions have since arisen as our observational facilities have improved. Recent observational results, combined with advances in disk physical and chemical modelling, have resulted in a much more detailed and complex picture of the planet form-Protostars and Planets VII

show abstract

“…The model requires inputs for dust density and structure, dust opacity and a source. The dust density and structure are determined from our 𝑁-body outputs, and the source is a Sun-like blackbody emitter of 5800 K. The dust opacities are determined from the opacity tool developed to determine the DIANA standard opacities (Toon & Ackerman 1981;Woitke 2015;Min et al 2005;Dorschner et al 1995). The dust particles are dominated by silicates but with some carbonaceous material mixed in.…”

Section: Step 3: Synthetic Images (Radiative Transfer)mentioning

confidence: 99%

Planetary Embryo Collisions and the Wiggly Nature of Extreme Debris Disks

Watt,

Leinhardt,

2021

Preprint

View full text Add to dashboard Cite

In this paper, we present results from a multi-stage numerical campaign to begin to explain and determine why extreme debris disk detections are rare, what types of impacts will result in extreme debris disks and what we can learn about the parameters of the collision from the extreme debris disks. We begin by simulating many giant impacts using a smoothed particle hydrodynamical code with tabulated equations of state and track the escaping vapour from the collision. Using an 𝑁-body code, we simulate the spatial evolution of the vapour generated dust post-impact.We show that impacts release vapour anisotropically not isotropically as has been assumed previously and that the distribution of the resulting generated dust is dependent on the mass ratio and impact angle of the collision. In addition, we show that the anisotropic distribution of post-collision dust can cause the formation or lack of formation of the short-term variation in flux depending on the orientation of the collision with respect to the orbit around the central star. Finally, our results suggest that there is a narrow region of semi-major axis where a vapour generated disk would be observable for any significant amount of time implying that giant impacts where most of the escaping mass is in vapour would not be observed often but this does not mean that the collisions are not occurring.

show abstract

Modelling and interpretation of SEDs

Cited by 14 publications

References 32 publications

Hubble Space Telescope Scattered-light Imaging and Modeling of the Edge-on Protoplanetary Disk ESO-Hα 569

Hubble Space Telescope Scattered-light Imaging and Modeling of the Edge-on Protoplanetary Disk ESO-Hα 569

Setting the Stage for Planet Formation: Measurements and Implications of the Fundamental Disk Properties

Planetary Embryo Collisions and the Wiggly Nature of Extreme Debris Disks

Contact Info

Product

Resources

About