Observation and modeling of proto-planetary disks
1 hour 4 mins 47 secs,
896.47 MB,
MPEG-4 Video
480x360,
25.0 fps,
44100 Hz,
1.84 Mbits/sec
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About this item
| Description: |
Dullemond, C (MPI for Astronomy)
Monday 28 September 2009, 11:30-12:30 |
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| Created: | 2009-10-09 11:16 | ||
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| Collection: | Dynamics of Discs and Planets | ||
| Publisher: | Isaac Newton Institute | ||
| Copyright: | Dullemond, C | ||
| Language: | eng (English) | ||
| Distribution: |
World
(downloadable)
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| Credits: |
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| Explicit content: | No | ||
| Aspect Ratio: | 4:3 | ||
| Screencast: | No | ||
| Bumper: | /sms-ingest/static/new-4x3-bumper.dv | ||
| Trailer: | /sms-ingest/static/new-4x3-trailer.dv | ||
| Abstract: | I will give an overview of what has been learned about the structure and evolution of protoplanetary disks since the first direct images of such disks were obtained by the HST in the mid nineties. This overview will cover both the various advances made in observations of these disks, as well as the theoretical modeling that was/is aimed to understand these observations. The ultimate aim of these studies is to get a better understanding of the environments in which planets form, and of what the solar nebula might have looked like 4.5 billion years ago. I will show that, while we have now a much better understanding of these issues than before the mid nineties, a great number of new fundamental questions have arisen that are still unsolved. I will end with some thoughts about which kind of observations and modeling need to be done in the next decade to finally be able to answer, at least partially, the question in which kind of environment planets are formed. |
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