Accretion and the Evolution of T Tauri Disks

Hartmann, L.; Calvet, Nuria; Gullbring, E.; D’Alessio, Paola

doi:10.1086/305277

Cited by 1,473 publications

(1,875 citation statements)

References 58 publications

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“…Such evolution agrees with the numerical evolutionary models of Ruden & Lin (1986) or Ruden & Pollack (1991). It is also consistent with the decrease of the mass accretion rate with increasing age observed in T Tauri stars (Hartmann et al 1998). The model takes also into account that, under the action of turbulence, the nebula spreads out viscously with time.…”

Section: Solar Nebula Modelsupporting

confidence: 90%

Turbulent Radial Mixing in the Solar Nebula as the Source of Crystalline Silicates in Comets

Bockelée‐Morvan

Gautier

Hersant

et al. 2003

The Origin of Stars and Planets: The VLT View

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Abstract. There is much debate about the origin of crystalline silicates in comets. Silicates in the protosolar cloud were likely amorphous, however the temperature of the outer solar nebula was too cold to allow their formation in this region by thermal annealing or direct condensation. This paper investigates the formation of crystalline silicates in the inner hot regions of the solar nebula, and their diffusive transport out to the comet formation zone, using a turbulent evolutionary model of the solar nebula. The model uses time-dependent temperature and surface density profiles generated from the 2-D α-disk model of Hersant et al. (2001). It is shown that turbulent diffusion is an efficient process to carry crystalline silicates from inner to outer disk regions within timescales of a few 10 4 yr. The warmest solar nebula models which reproduce the D/H ratios measured in meteorites, comets, Uranus and Neptune (Hersant et al. 2001) provide a mass fraction of crystalline silicates in the Jupiter-Neptune region in agreement with that measured in comet Hale-Bopp.

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Section: Solar Nebula Modelsupporting

confidence: 90%

Turbulent Radial Mixing in the Solar Nebula as the Source of Crystalline Silicates in Comets

Bockelée‐Morvan

Gautier

Hersant

et al. 2003

The Origin of Stars and Planets: The VLT View

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“…The latter can provide a complementary estimate of disk (gas) mass assuming a typical accretion history for the disk (Hartmann et al 1998). Tables 1 and 2 tabulate the disk dust masses M dust calculated from submillimeter continuum fluxes (Appendix B).…”

Section: Disk Masses and Gravitational Instabilitymentioning

confidence: 99%

Spiral Arms in Disks: Planets or Gravitational Instability?

Dong

Najita

Brittain

2018

ApJ

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Spiral arm structures seen in scattered-light observations of protoplanetary disks can potentially serve as signposts of planetary companions. They can also lend unique insights into disk masses, which are critical in setting the mass budget for planet formation but are difficult to determine directly. A surprisingly high fraction of disks that have been well studied in scattered light have spiral arms of some kind (8/29), as do a high fraction (6/11) of wellstudied Herbig intermediate-mass stars (i.e., Herbig stars >1.5 M e ). Here we explore the origin of spiral arms in Herbig systems by studying their occurrence rates, disk properties, and stellar accretion rates. We find that two-arm spirals are more common in disks surrounding Herbig intermediate-mass stars than are directly imaged giant planet companions to mature A and B stars. If two-arm spirals are produced by such giant planets, this discrepancy suggests that giant planets are much fainter than predicted by hot-start models. In addition, the high stellar accretion rates of Herbig stars, if sustained over a reasonable fraction of their lifetimes, suggest that disk masses are much larger than inferred from their submillimeter continuum emission. As a result, gravitational instability is a possible explanation for multiarm spirals. Future observations can lend insights into the issues raised here.

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“…The analysis of the accretion properties of the stellar populations belonging to young clusters using highresolution (R ∼ 20 000) spectroscopy is a powerful tool to investigate these questions. σ Ori and λ Ori are two of the richest young clusters near the Sun in the age range (1−10 Myr) during which young stars lose their circumstellar disk and stop accreting material from it (Hartmann et al 1998;Haisch et al 2001;Sicilia-Aguilar et al 2005. The σ Ori cluster was discovered by the ROSAT satellite (Wolk 1996;Walter et al 1997) around the O9.5 V binary star σ Orionis AB (distance 352 +166 −85 pc, Perryman et al 1997).…”

Section: Introductionmentioning

confidence: 99%

FLAMES spectroscopy of low-mass stars in the young clusters σ Ori and λ Ori

Sacco

Franciosini²,

Randich

et al. 2008

A&A

181

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Aims. We performed a detailed membership selection and studied the accretion properties of low-mass stars in the two apparently very similar young (1-10 Myr) clusters σ Ori and λ Ori. Methods. We observed 98 and 49 low-mass (0.2-1.0 M ) stars in σ Ori and λ Ori respectively, using the multi-object optical spectrograph FLAMES at the VLT, with the high-resolution (R ∼ 17 000) HR15N grating (6470-6790 Å). We used radial velocities, Li and Hα to establish cluster membership and Hα and other optical emission lines to analyze the accretion properties of members. Results. We identified 65 and 45 members of the σ Ori and λ Ori clusters, respectively, and discovered 16 new candidate binary systems. We also measured rotational broadening for 20 stars and estimated the mass accretion rates in 25 stars of the σ Ori cluster, finding values between 10 −11 and 10 −7.7 M yr −1 and in 4 stars of the λ Ori cluster, finding values between 10 −11 and 10 −10.1 M yr −1 . Comparing our results with the infrared photometry obtained by the Spitzer satellite, we find that the fraction of stars with disks and the fraction of active disks is larger in the σ Ori cluster (52 ± 9% and 78 ± 16%) than in λ Ori (28 ± 8% and 40 ± 20%). Conclusions. The different disk and accretion properties of the two clusters could be due either to the effect of the high-mass stars and the supernova explosion in the λ Ori cluster or to different ages of the cluster populations. Further observations are required to draw a definitive conclusion.

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Accretion and the Evolution of T Tauri Disks

Cited by 1,473 publications

References 58 publications

Turbulent Radial Mixing in the Solar Nebula as the Source of Crystalline Silicates in Comets

Turbulent Radial Mixing in the Solar Nebula as the Source of Crystalline Silicates in Comets

Spiral Arms in Disks: Planets or Gravitational Instability?

FLAMES spectroscopy of low-mass stars in the young clusters σ Ori and λ Ori

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