The building blocks of planets within the ‘terrestrial’ region of protoplanetary disks

@article{Boekel2004TheBB,
  title={The building blocks of planets within the ‘terrestrial’ region of protoplanetary disks},
  author={Roy van Boekel and Michiel Min and Ch. Leinert and L. B. F. M. Waters and Andrea Richichi and Olivier Chesneau and Carsten Dominik and Walter Joseph Jaffe and A. Dutrey and Uwe Graser and Th. Henning and Jeroen de Jong and Rainer K{\"o}hler and Alex de Koter and Bruno Lopez and Fabien Malbet and S'ebastien Morel and Francesco Paresce and Guy Perrin and Thomas Preibisch and Frank Przygodda and Markus Sch{\"o}ller and Markus Wittkowski},
  journal={Nature},
  year={2004},
  volume={432},
  pages={479-482}
}
Our Solar System was formed from a cloud of gas and dust. Most of the dust mass is contained in amorphous silicates, yet crystalline silicates are abundant throughout the Solar System, reflecting the thermal and chemical alteration of solids during planet formation. (Even primitive bodies such as comets contain crystalline silicates.) Little is known about the evolution of the dust that forms Earth-like planets. Here we report spatially resolved detections and compositional analyses of these… 
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285 Citations
Highly Influential Citations
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285 Citations

ON THE EVOLUTION OF DUST MINERALOGY, FROM PROTOPLANETARY DISKS TO PLANETARY SYSTEMS

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The chemistry of planet-forming regions is not interstellar.

It is argued that inner disk chemistry is, as expected, fundamentally different from prestellar chemistry, and the clearest discriminant may be the concentration of CO2, which is extremely low in disks, but one of the most abundant constituents of dense clouds and protostellar envelopes.

Dust in protoplanetary disks: observations

Solid particles, usually referred to as dust, are a crucial component of interstellar matter and of planet forming disks surrounding young stars. Despite the relatively small mass fraction of ≈1% (in…

Crystalline Silicates and Dust Processing in the Protoplanetary Disks of the Taurus Young Cluster

We characterize the crystalline-silicate content and spatial distribution of small dust grains in a large sample of protoplanetary disks in the Taurus-Auriga young cluster, using the Spitzer Space…

PROBING DYNAMICAL PROCESSES IN THE PLANET-FORMING REGION WITH DUST MINERALOGY

We present Herschel Space Observatory PACS spectra of GQ Lup, a protoplanetary disk in the Lupus star-forming region. Through spectral energy distribution fitting from 0.3 μm to 1.3 mm, we construct…

Episodic formation of cometary material in the outburst of a young Sun-like star

Mid-infrared features in the outburst spectrum of the young Sun-like star EX Lupi that were not present in quiescence are reported and it is concluded that the crystals were produced through thermal annealing in the surface layer of the inner disk by heat from the outburst, a process that has hitherto not been considered.

Reflected light from sand grains in the terrestrial zone of a protoplanetary disk

Observations of a 3-Myr-old star show that grains have grown to about millimetre size or larger in the terrestrial zone of this star, which complements the study of terrestrial zones of younger disks that have been recently resolved by interferometry.

The Formation and Evolution of Planetary Systems: Grain Growth and Chemical Processing of Dust in T Tauri Systems

This paper is one in a series presenting results obtained within the Formation and Evolution of Planetary Systems (FEPS) Legacy Science Program on the Spitzer Space Telescope. Here we present a study…

Extreme collisions between planetesimals as the origin of warm dust around a Sun-like star

An exceptionally large amount of warm, small, silicate dust particles around the solar-type star BD+20 307 (HIP 8920, SAO 75016) are reported, which could be explained by recent frequent or huge collisions between asteroids or other ‘planetesimals’ whose orbits are being perturbed by a nearby planet.

Flows of gas through a protoplanetary gap

Observations of diffuse CO gas inside the gap, with denser HCO+ gas along gap-crossing filaments are reported, which is sufficient to maintain accretion onto the star at the present rate.
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