10/29/2008 - Giant Planet Formation

SETI Institute Colloquium Series Videos

SETI Institute Colloquium Series Videos에서 제공하는 콘텐츠입니다. 에피소드, 그래픽, 팟캐스트 설명을 포함한 모든 팟캐스트 콘텐츠는 SETI Institute Colloquium Series Videos 또는 해당 팟캐스트 플랫폼 파트너가 직접 업로드하고 제공합니다. 누군가가 귀하의 허락 없이 귀하의 저작물을 사용하고 있다고 생각되는 경우 여기에 설명된 절차를 따르실 수 있습니다 https://ko.player.fm/legal.

15y ago

QUICKTIME•에피소드 홈

저장한 시리즈 ("피드 비활성화" status)

When? This feed was archived on September 13, 2022 18:20 (1+ y ago). Last successful fetch was on June 10, 2022 09:10 (2y ago)

Why? 피드 비활성화 status. 잠시 서버에 문제가 발생해 팟캐스트를 불러오지 못합니다.

What now? You might be able to find a more up-to-date version using the search function. This series will no longer be checked for updates. If you believe this to be in error, please check if the publisher's feed link below is valid and contact support to request the feed be restored or if you have any other concerns about this.

Dr. Jack Lissauer, Space Sciences Division, NASA Ames Research Center
The observed properties of giant planets, models of their evolution, and observations of protoplanetary disks all provide constraints on the formation of gas giant planets. The four largest planets in our Solar System contain considerable quantities of hydrogen and helium, which could not have condensed into solid planetesimals within the protoplanetary disk. The preponderance of evidence supports the core nucleated gas accretion model of formation of the giant planets. According to this model, giant planets begin their growth by the accumulation of small solid bodies, as do terrestrial planets. However, unlike terrestrial planets, the growing giant planet cores become massive enough that they are able to accumulate substantial amounts of gas before the protoplanetary disk dissipates. During this talk, Dr. Lissauer will present the first models of giant planet formation that account for both the planet's internal energy budget and gas flows within the protoplanetary disk.

play video

17 에피소드