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75 results on '"Dullemond, Cornelis Petrus"'

3. Contents

Author

Beuther, Henrik, Klessen, Ralf S., Dullemond, Cornelis Petrus, and Henning, Thomas K.

Published
2014

5. Preface

Author

Beuther, Henrik, Klessen, Ralf S., Dullemond, Cornelis Petrus, and Henning, Thomas K.

Published
2014

12. Massive Star Formation

Author

Beuther, Henrik, Klessen, Ralf S., Dullemond, Cornelis Petrus, and Henning, Thomas K.

Published
2014

13. Ages of Young Stars

Author

Beuther, Henrik, Klessen, Ralf S., Dullemond, Cornelis Petrus, and Henning, Thomas K.

Published
2014

39. Exoplanetary Atmospheres

Author

Beuther, Henrik, Klessen, Ralf S., Dullemond, Cornelis Petrus, and Henning, Thomas K.

Published
2014

40. Planet Population Synthesis

Author

Beuther, Henrik, Klessen, Ralf S., Dullemond, Cornelis Petrus, and Henning, Thomas K.

Published
2014

44. Image Plates

Author

Beuther, Henrik, Klessen, Ralf S., Dullemond, Cornelis Petrus, and Henning, Thomas K.

Published
2014

48. Index

Author

Beuther, Henrik, Klessen, Ralf S., Dullemond, Cornelis Petrus, and Henning, Thomas K.

Published
2014

49. Cloudlet capture by Transitional Disk and FU Orionis stars

Author

Dullemond, Cornelis Petrus, Küffmeier, Michael, Goicovic, Felipe, Fukagawa, Misato, Oehl, Veronika, and Kramer, Manuel

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

After its formation, a young star spends some time traversing the molecular cloud complex in which it was born. It is therefore not unlikely that, well after the initial cloud collapse event which produced the star, it will encounter one or more low mass cloud fragments, which we call "cloudlets" to distinguish them from full-fledged molecular clouds. Some of this cloudlet material may accrete onto the star+disk system, while other material may fly by in a hyperbolic orbit. In contrast to the original cloud collapse event, this process will be a "cloudlet flyby" and/or "cloudlet capture" event: A Bondi-Hoyle-Lyttleton type accretion event, driven by the relative velocity between the star and the cloudlet. As we will show in this paper, if the cloudlet is small enough and has an impact parameter similar or less than $GM_{*}/v^2_\infty$ (with $v_\infty$ being the approach velocity), such a flyby and/or capture event would lead to arc-shaped or tail-shaped reflection nebulosity near the star. Those shapes of reflection nebulosity can be seen around several transitional disks and FU Orionis stars. Although the masses in the those arcs appears to be much less than the disk masses in these sources, we speculate that higher-mass cloudlet capture events may also happen occasionally. If so, they may lead to the tilting of the outer disk, because the newly infalling matter will have an angular momentum orientation entirely unrelated to that of the disk. This may be one possible explanation for the highly warped/tilted inner/outer disk geometries found in several transitional disks. We also speculate that such events, if massive enough, may lead to FU Orionis outbursts.

Published
2019
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50. Redistribution of CO at the Location of the CO Ice Line in evolving Gas and Dust Disks

Author

Stammler, Sebastian Markus, Birnstiel, Tilman, Panić, Olja, Dullemond, Cornelis Petrus, and Dominik, Carsten

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Ice lines are suggested to play a significant role in grain growth and planetesimal formation in protoplanetary disks. Evaporation fronts directly influence the gas and ice abundances of volatile species in the disk and therefore the coagulation physics and efficiency and the chemical composition of the resulting planetesimals. Aims. In this work we investigate the influence of the existence of the CO ice line on the particle growth and on the distribution of CO in the disk. Methods. We include the possibility of tracking the CO content and/or other volatiles in particles and in the gas in our existing dust coagulation and disk evolution model and developed a method for evaporation and condensation of CO using the Hertz-Knudsen equation. Our model does not include fragmentation, yet, which will be part of further investigations. Results. We find no enhanced grain growth just outside the ice line where the particle size is limited by radial drift. Instead we find a depletion of solid material inside the ice line which is solely due to evaporation of the CO. Such a depression inside the ice line may be observable and may help to quantify the processes described in this work. Furthermore, we find that the viscosity and diffusivity of the gas heavily influence the re-distribution of vaporized CO at the ice line and can lead to an increase in the CO abundance by up to a factors of a few in the region just inside the ice line. Depending on the strength of the gaseous transport mechanisms the position of the ice line in our model can change by up to 10 AU and consequently, the temperature at that location can range from 21 K to 23 K., Comment: Accepted to A&A. 16 pages, 11 figures

Published
2017
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