Glossary term: Granulación
Description: En las regiones exteriores del Sol, las corrientes de gas caliente ascienden, se expanden y se enfrían, para luego volver a descender. Este proceso de convección tiene lugar dentro de células individuales de unos 1500 kilómetros de diámetro cada una. El material caliente y recién ascendido en el centro de cada célula brilla más que los bordes más fríos y oscuros, donde el material vuelve a descender. Esto da lugar a un patrón de puntos brillantes con bordes oscuros conocidos como gránulos. Se trata de fenómenos temporales: cada gránulo dura solo unos minutos antes de que la masa en ebullición de corrientes convectivas del Sol lo desintegre.
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
- Árabe: حبيبات الشمس
- Alemán: Granulation
- Inglés: Granulation
- Francés: Granulation
- Italiano: Granulazione
- Japonés: 粒状斑 (external link)
- Nepalí: कणिकीकरण
- Portugués de Brasil: Granulação
- Chino simplificado: 米粒组织
- Chino tradicional: 米粒組織
Related Media
High-resolution image of the surface of the Sun
Caption: This high-resolution image of a small portion of the outermost visible "surface" of the Sun (the photosphere) covers an area 36,500 by 36,500 km. It was one of the first images taken by the Daniel K. Inouye Solar Telescope, as part of the telescope's Science Verification Phase. Each of the cells that are visible is about the size of the US state Texas, or of France, or of Afghanistan, or of Somalia. In the brighter centers of these cells, plasma from the underlying regions rises to the surface, cools off, and then sinks down again at the location of the darker lanes delineating the cells. In these dark lanes we can also see the tiny, bright markers of magnetic fields.
Credit: NSO/NSF/AURA
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License: CC-BY-4.0 Creative Commons Reconocimiento 4.0 Internacional (CC BY 4.0) icons
Close-up view of a sunspot
Caption: This image of a sunspot was taken by the Daniel K Inouye Solar Telescope (DKIST), operated by the U.S. National Science Foundation. It was taken only in light with a wavelength of 530 nanometers, within the greenish-yellow part of the visible spectrum.
The picture reveals the detail of the spot's structure and the Sun’s photosphere. The dark central region, known as the umbra, is surrounded by a lighter area called the penumbra with radially elongated features stretching towards the umbra. Note that the umbra and penumbra here are not the same as the umbra and penumbra that occur during an eclipse.
The sunspot measures approximately 5000 kilometres in diameter, roughly equivalent to the east-west span of China. While the umbra appears black, it is actually hot and bright. It only appears dark because it is a few thousand kelvin cooler than the surrounding solar photosphere. Surrounding the sunspot, granulation patterns of plasma are visible on the photospheric surface of the Sun.
Credit: NSO/NSF/AURA
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License: CC-BY-4.0 Creative Commons Reconocimiento 4.0 Internacional (CC BY 4.0) icons
