Glossarbegriffe: Planetenentstehung

Description: Wenn eine Gaswolke im Weltraum zu einem Stern kollabiert, wird der entstehende Stern von einer wirbelnden Scheibe aus Gas und Staub umgeben. Dies ist eine protoplanetare Scheibe, in der sich Planeten bilden: Eisbedeckte Staubteilchen haften aneinander und bilden etwas größere Klumpen, die weiter wachsen. Es gibt noch offene Fragen darüber, wie die nächsten Stadien ablaufen: Welche Rolle spielt zum Beispiel die turbulente Gasbewegung, die diese Klumpen näher zusammenbringt? Schließlich bilden sich sogenannte Planetesimale, die mehr als einen Kilometer groß sind. Einige dieser Planetesimale ziehen sich aufgrund der Schwerkraft gegenseitig an und bilden größere Planeten. Ein Teil der Planetesimale bleibt als Asteroiden übrig. Einige Protoplaneten können große Mengen an Gas ansammeln und werden zu Gasriesen. Einige andere Protoplaneten in kalten Regionen, die weit vom Zentralstern entfernt sind, akkretieren große Mengen an gefrorenem Material und Gas und werden zu Eisriesen. Andere, mit weniger Gas, werden zu Gesteinsplaneten.

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Term and definition status: The original definition of this term in English have been approved by a research astronomer and a teacher
The translation of this term and its definition is still awaiting approval

The OAE Multilingual Glossary is a project of the IAU Office of Astronomy for Education (OAE) in collaboration with the IAU Office of Astronomy Outreach (OAO). The terms and definitions were chosen, written and reviewed by a collective effort from the OAE, the OAE Centers and Nodes, the OAE National Astronomy Education Coordinators (NAECs) and other volunteers. You can find a full list of credits here. All glossary terms and their definitions are released under a Creative Commons CC BY-4.0 license and should be credited to "IAU OAE".

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The planet beta Pictoris b is a bright dot close to its parent star. Around this we see a warm disk edge-on

beta Pictoris b

Bildunterschriften: This composite of two images shows the planet beta Pictoris b and a disk of material both of which orbit the young star beta Pictoris. Both are taken in infrared light. The inner image was one of the first pictures taken of a planet around another star (an exoplanet). This image was made using a technique called adaptive optics which removes the blurring effect of the Earth's atmosphere that spreads out a star's light. The star's light is then concentrated tightly enough that it can be hidden behind a blocking circle (shown here in black) called a coronagraph. The ripples around this are artifacts of the imaging process. Beta Pictoris b, a gas giant planet about twelve times the mass of Jupiter, appears as a dot above and to the left of the black circle. The outer image shows the thermal emission from the warm disk of material surrounding the young star beta Pictoris. As we are viewing this disk edge-on it appears as a line. This disk of gas and dust provided the material to form beta Pictoris b.
Bildnachweis: ESO/A.-M. Lagrange et al. credit link

License: CC-BY-4.0 Creative Commons Namensnennung 4.0 International (CC BY 4.0) icons

A series of light and dark rings that resemble an archery target around the star TW Hydrae

Planet formation around the star TW Hydrae

Bildunterschriften: This image shows the disk around the young star TW Hydrae. This star is only about 10 million years old, young enough that planets are still forming in a disk of gas and dust around it. This image was created using an array of submillimetre telescopes, each of which looks like a satellite dish. The signals from these telescopes were combined by a central processing computer to make this image. The lighter and darker patches show areas of the disk where there is more or less dust respectively. The dark rings and bright rings are evidence that the dust in the disk has been shepherded into some orbits and away from others. This is likely because there is one or more planets that are still forming hidden in the disk. The whole image shows the disk around TW Hydrae out to a distance of about 70 astronomical units frm the central star. The two outer dark rings are separated from the central star by approximately the average distance between the Sun and Uranus and the average distance between the Sun and Pluto. The inner central hole appears to have been carved out by a planet orbiting TW Hydrae at a distance similar to the distance between the Earth and the Sun.
Bildnachweis: S. Andrews (Harvard-Smithsonian CfA); B. Saxton (NRAO/AUI/NSF); ALMA (ESO/NAOJ/NRAO) credit link

License: CC-BY-4.0 Creative Commons Namensnennung 4.0 International (CC BY 4.0) icons

Related Activities

Creating Asteroids

Creating Asteroids

astroEDU educational activity (links to astroEDU website)
Description: Have fun, building asteroids using clay!

License: CC-BY-4.0 Creative Commons Namensnennung 4.0 International (CC BY 4.0) icons

Tags: Hands-on , Model
Age Ranges: 4-6 , 6-8 , 8-10
Education Level: Pre-school , Primary
Areas of Learning: Modelling , Social Research
Costs: Medium Cost
Duration: 1 hour 30 mins
Group Size: Group
Skills: Communicating information , Developing and using models