Glossary term: 흑체복사
Description: 흑체복사는 이상적인 물체(흑체)에서 나오는 전자기 복사입니다. 흑체는 자신에게 들어오는 모든 빛(복사)을 완전히 흡수하고, 열 평형 상태를 유지하면서 같은 양의 복사를 다시 내보내는 물체입니다. 흑체복사의 스펙트럼(파장에 따른 빛의 세기 분포)은 물체의 온도에 따라 정확하게 결정됩니다. 대부분의 별은 수천 켈빈(K)의 온도를 가지며, 이러한 온도에서 흑체와 비슷한 형태의 빛을 냅니다. 이는 싱크로트론복사나 다른 형태의 ‘비열적' 복사와 구별됩니다.
See this term in other languagesTerm 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: إشعاع الجسم الأسود
- 독일어: Schwarzkörperstrahlung
- 영어: Blackbody Radiation
- 프랑스어: Rayonnement du Corps noir
- 이탈리아어: Radiazione di corpo nero
- 일본어: 黒体放射 (external link)
- 마라티어: कृष्णिका प्रारण
- 브라질 포르투갈어: Radiação do corpo negro
- 중국어 간체: 黑体辐射
- 중국어 번체: 黑體輻射
Related Diagrams
Blackbody Radiation
Caption: The curves of emitted radiation from blackbodies of different temperatures. The x-axis shows wavelength and the y-axis shows the amount of energy emitted every second by a square meter of the surface of that blackbody at each wavelength.
The hotter the body, the shorter the wavelength and the bluer the light it emits its maximum amount of energy at. Despite the coolest body in this plot peaking in red light, the other hotter bodies all emit more red light than the coolest body.
Credit: IAU OAE/Niall Deacon
License: CC-BY-4.0 Creative Commons 저작자표시 4.0 국제 (CC BY 4.0) icons
Blackbody Radiation - UV Catastrophe
Caption: The curves of emitted radiation from blackbodies of different temperatures. The x-axis shows wavelength and the y-axis shows the amount of energy emitted every second by a square meter of the surface of that blackbody at each wavelength.
The hotter the body, the shorter the wavelength and the bluer the light it emits its maximum amount of energy at. Despite the coolest body in this plot peaking in red light, the other hotter bodies all emit more red light than the coolest body.
The dotted line shows the emitted radiation predicted by classical theory prior to modern quantum mechanics. This prediction tends to infinity at shorter wavelengths for any blackbody temperature above zero and was dubbed the ‘ultraviolet catastrophe’.
Credit: IAU OAE/Niall Deacon
License: CC-BY-4.0 Creative Commons 저작자표시 4.0 국제 (CC BY 4.0) icons
