Glossary term: 에프형별
Description: 스펙트럼으로 구별한 분광형이 "F"인 별. 천문학자들은 스펙트럼에서 적당히 강한 이온화된 칼슘선, 여러 금속 원자의 선, 그리고 약한 수소 흡수선을 보고 F형 별임을 알 수 있습니다. F형 별의 표면 온도(유효 온도)는 약 6,000켈빈(K)에서 7,400K 사이입니다. 다른 별들과 비교했을 때, 성간 적색화(별빛이 먼지를 지나며 붉어지는 현상)나 대기적색화가 크게 영향을 주지 않는다면, 사람 눈에는 흰색이나 황백색으로 보입니다.대표적인 예로 북극성(Polaris)이 F형 별에 속합니다.
Related Terms:
See this term in other languages
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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In Other Languages
- 아랍어: النجم من النوع الطيفي "F"
- 독일어: F-Stern
- 영어: F-type Star
- 스페인어: Estrella de tipo F
- 프랑스어: Étoile de type F
- 이탈리아어: Stella di tipo F
- 일본어: F型星 (external link)
- 브라질 포르투갈어: Estrela tipo F
- 중국어 간체: F 型星
- 중국어 번체: F 型星
Related Diagrams
Spectrum of an F-type star
Caption: 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.
Credit: IAU OAE/SDSS/Niall Deacon
License: CC-BY-4.0 Creative Commons 저작자표시 4.0 국제 (CC BY 4.0) icons
