Spectral energy distributions of T Tauri stars - Disk flaring and limits on accretion

Kenyon, Scott J.; Hartmann, L.

doi:10.1086/165866

Cited by 638 publications

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“…in the limit h, R r. The term (d ln h/d ln r−1) is determined from the detailed vertical structure of the disk; its value is equal to 1/9 in the model by Kenyon & Hartmann (1987) or to 2/7 in the model by Chiang & Goldreich (1997). In our model (see BL99) at large radii the opening angle h/r does not depend on r and hence there is no flaring.…”

Section: Inclusion Of the Central Star And Of Disk Irradiationmentioning

confidence: 88%

“…(2)). If we try to follow the argument by Kenyon & Hartmann (1987), for the case of T Tauri stars, in order for the outer disk to produce the required infrared excess at wavelengths of the order of 25−100 µm, its temperature should be of the order of 100 K. Therefore, the required productṀM tot (r out ) can be estimated by fixing T s (r out ) = 100 K (with r out ≈ 20 AU; but note that a value of r out ≈ 10 AU would be more appropriate if we refer to the models described in Sect. 5 below).…”

Section: Simple Estimates Ofṁ and M Diskmentioning

confidence: 99%

“…The effect of irradiation is enhanced at large radii by the disk flaring, when the thickness of the disk increases rapidly with radius. Models of the vertical structure of these flared disks have been constructed (Kenyon & Hartmann 1987;Chiang & Goldreich 1997; but concerns about stability have been expressed by Dullemond 2000). On the other hand, in the case of flat spectrum sources and of most FU Orionis objects, flaring alone is ineffective and the far-infrared emission has been attributed to an infalling envelope of dust (Kenyon & Hartmann 1991;Calvet et al 1994).…”

Section: Introductionmentioning

confidence: 99%

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The spectral energy distribution of self-gravitating protostellar disks

Lodato

Bertin

2001

A&A

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Abstract. The long wavelength emission of protostellar objects is commonly attributed to a disk of gas and dust around the central protostar. In the first stages of disk accretion or in the case of high mass protostars, the disk mass is likely to be sufficiently large, so that the disk self-gravity may have an impact on the dynamics and the emission properties of the disk. In this paper we describe the spectral energy distribution (SED) produced by a simple, non-flaring, self-gravitating accretion disk model. Self-gravity is included in the calculation of the rotation curve of the disk and in the energy balance equation, as a term of effective heating related to Jeans instability. In order to quantify in detail the requirements on the mass of the disk and on the accretion rate posed on the models by realistic situations, we compare the SEDs produced by these models with the observed SEDs of a small sample of well-studied protostellar objects. We find that relatively modest disks -even lighter than the central star -can lead to an interesting fit to the infrared SED of the FU Orionis objects considered, while in the case of T Tauri stars the required parameters fall outside the range suggested as acceptable by the general theoretical and observational scenario. On the basis of the present results, we may conclude that the contribution of a selfgravitating disk is plausible in several cases (in particular, for FU Orionis objects) and that, in the standard irradiation, dominated disk scenario, it would help soften the requirements encountered by Keplerian accretion models.

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Section: Inclusion Of the Central Star And Of Disk Irradiationmentioning

confidence: 88%

Section: Simple Estimates Ofṁ and M Diskmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The spectral energy distribution of self-gravitating protostellar disks

Lodato

Bertin

2001

A&A

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“…Early in the lifetime of protostars disks are thought to be massive and turbulent, and accretion from the envelope onto these massive disks could cause gravitational instabilities that drive high accretion rates in young sources (e.g., Kenyon & Hartmann 1987). The disk mass also sets a limit on the amount of material available for forming planets and the ultimate outcomes of the planet formation process (e.g., Alibert et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

Sheehan

Eisner

2017

ApJ

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Class I protostars are thought to represent an early stage in the lifetime of protoplanetary disks, when they are still embedded in their natal envelope. Here we measure the disk masses of 10 Class I protostars in the Taurus Molecular Cloud to constrain the initial mass budget for forming planets in disks. We use radiative transfer modeling to produce synthetic protostar observations and fit the models to a multi-wavelength data set using a Markov Chain Monte Carlo fitting procedure. We fit these models simultaneously to our new Combined Array for Research in Millimeter-wave Astronomy 1.3 mm observations that are sensitive to the wide range of spatial scales that are expected from protostellar disks and envelopes so as to be able to distinguish each component, as well as broadband spectral energy distributions compiled from the literature. We find a median disk mass of  M 0.018 on average, more massive than the Taurus Class II disks, which have median disk mass of~ M 0.0025 . This decrease in disk mass can be explained if dust grains have grown by a factor of 75 in grain size, indicating that by the Class II stage, at a few Myr, a significant amount of dust grain processing has occurred. However, there is evidence that significant dust processing has occurred even during the Class I stage, so it is likely that the initial mass budget is higher than the value quoted here.

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“…This assumption is motivated by the relatively narrow ring (0.08 R⊙) found in the previous simulations. The vertical half thickness of the disc was varied between 1 m and approximately 10 7 m (0.015 R⊙, 0.13 R * ) with a step of (1, 2, 3, 4, ..., 9), (1, 2, ..., 9) ×10 1 , (1, 2, ..., 9) ×10 2 , ..., (1, 2, ..., 9, 10) ×10 6 m. The adopted minimum thickness corresponds to the smallest grossness of Saturn's rings (Reffet et al 2015), while the maximum explored height is parametrised from the expression given by Kenyon & Hartmann (1987):…”

Section: Effect Of Non-zero Inclinationmentioning

confidence: 99%

Spectral energy distribution simulations of a possible ring structure around the young, red brown dwarf G 196-3 B

Zakhozhay

Osorio

Béjar

et al. 2016

Mon. Not. R. Astron. Soc.

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The origin of the very red optical and infrared colours of intermediate-age (∼10-500 Myr) L-type dwarfs remains unknown. It has been suggested that low-gravity atmospheres containing large amounts of dust may account for the observed reddish nature. We explored an alternative scenario by simulating protoplanetary and debris discs around G 196-3 B, which is an L3 young brown dwarf with a mass of ∼ 15 M Jup and an age in the interval 20-300 Myr. The best-fit solution to G 196-3 B's photometric spectral energy distribution from optical wavelengths through 24 µm corresponds to the combination of an unreddened L3 atmosphere (T eff ≈ 1870 K) and a warm (≈ 1280 K), narrow (≈ 0.07-0.11 R ⊙ ) debris disc located at very close distances (≈ 0.12-0.20 R ⊙ ) from the central brown dwarf. This putative, optically thick, dusty belt, whose presence is compatible with the relatively young system age, would have a mass ≥ 7 × 10 −10 M ⊕ comprised of sub-micron/micron characteristic dusty particles with temperatures close to the sublimation threshold of silicates. Considering the derived global properties of the belt and the disc-to-brown dwarf mass ratio, the dusty ring around G 196-3 B may resemble the rings of Neptune and Jupiter, except for its high temperature and thick vertical height (≈ 6 × 10 3 km). Our inferred debris disc model is able to reproduce G 196-3 B's spectral energy distribution to a satisfactory level of achievement.

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Spectral energy distributions of T Tauri stars - Disk flaring and limits on accretion

Cited by 638 publications

References 0 publications

The spectral energy distribution of self-gravitating protostellar disks

The spectral energy distribution of self-gravitating protostellar disks

Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

Spectral energy distribution simulations of a possible ring structure around the young, red brown dwarf G 196-3 B

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