Glossarbegriffe: F-Stern

Also known as Stern der Spektralklasse F oder Stern des Spektraltyps F

Description: Ein F-Stern gehört der Spektralklasse "F" an. Astronomen erkennen F-Sterne an ihren mäßig stark ionisierten Kalziumlinien und einigen anderen atomaren Metalllinien sowie an den schwachen Wasserstoff-Absorptionslinien in ihren Spektren. Sie haben typische (effektive) Temperaturen zwischen 6000 Kelvin (K) und 7400 K. Im Vergleich zu anderen Sternen erscheinen sie dem menschlichen Auge weiß oder gelblich-weiß, es sei denn, die interstellare oder atmosphärische Extinktion spielt eine Rolle. Ein Beispiel für einen F-Stern ist der Polarstern (Polaris) im Sternbild Kleiner Bär.

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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".

Related Diagrams

A relatively smooth line peaking about 430 nm then declining at longer wavelengths with a few fairly broad dips.

Spectrum of an F-type star

Bildunterschriften: The spectrum of the F-type star 2MASS J22243289+4937443. The colour of the line between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively. The black lines show spectral absorption lines caused by atoms and ions of different elements in the star’s atmosphere. These atoms and ions absorb at specific wavelengths, causing sharp, dark lines in the spectra. How strong these lines are depends on the temperature of the star’s atmosphere. Two stars made from the same mix of elements could have spectra with vastly different sets of lines in their spectra if they have different temperatures in their atmospheres. The lines from hydrogen atoms that are strongest in A-type stars are still relatively strong in F-type stars but lines from metals, particularly ionised calcium begin to become strong at this spectral type.
Bildnachweis: IAU OAE/SDSS/Niall Deacon

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