05.24.23

The Daniel K. Inouye Solar Telescope on Maui, Hawaii, is the largest and most powerful solar telescope on the planet, and the recent images it captured surely live up to those superlatives. The National Science Foundation released a set of eight new pictures last week, showing our sun in “unprecedented detail.” 

The shots provide a close-up look at the fiery solar surface, from massive sunspots and boiling plasma to the more quiet regions. In a press release, the foundation said they “will help solar scientists better understand the sun’s magnetic field and drivers behind solar storms.”

Astronomers also emphasized the Inouye telescope’s importance to gaining a better understanding of solar storms and weather back in January 2020, when its very first images were released. 

“On Earth, we can predict if it is going to rain pretty much anywhere in the world very accurately, and space weather just isn’t there yet,” Matt Mountain, president of the Association of Universities for Research in Astronomy, which manages the Inouye Solar Telescope, said in a statement at the time. “Our predictions lag behind terrestrial weather by 50 years, if not more. What we need is to grasp the underlying physics behind space weather, and this starts at the sun, which is what the Inouye Solar Telescope will study over the next decades.”

Three years later, the solar telescope is well on its way to achieving its mission, and this is just the beginning: The eight new images “make up a small fraction of the data obtained from the first cycle” of the telescope’s current operations phase. 

“As the Inouye Solar Telescope continues to explore the sun, we expect more new and exciting results from the scientific community — including spectacular views of our solar system’s most influential celestial body,” the recent press release reads. 

Scroll through the stunning pictures below and read their descriptions, courtesy of the National Science Foundation.

The lower atmosphere (chromosphere) of the Sun exists above the Sun’s surface (photosphere). In this image, dark, fine threads (fibrils) are visible in the chromosphere emanating from sources in the photosphere – notably, the dark pores/umbral fragments and their fine structure. A pore is a concentration of magnetic field where conditions are not met to form a penumbra. Pores are essentially sunspots that have not had or will never have a penumbra. Penumbra: The brighter, surrounding region of a sunspot’s umbra characterized by bright filamentary structures.
The lower atmosphere (chromosphere) of the Sun exists above the Sun’s surface (photosphere). In this image, dark, fine threads (fibrils) are visible in the chromosphere emanating from sources in the photosphere – notably, the dark pores/umbral fragments and their fine structure. A pore is a concentration of magnetic field where conditions are not met to form a penumbra. Pores are essentially sunspots that have not had or will never have a penumbra. Penumbra: The brighter, surrounding region of a sunspot’s umbra characterized by bright filamentary structures.
In this image, the fibrillar nature of the solar atmosphere is exemplified. Dark, fine threads (fibrils) are ubiquitous in the chromosphere. The outline of bright structures are signature of the presence of magnetic fields in the photosphere below. This image was captured by the Inouye Solar Telescope during a coordinated observation campaign with NASA’s Parker Solar Probe and ESA’s Solar Orbiter.
In this image, the fibrillar nature of the solar atmosphere is exemplified. Dark, fine threads (fibrils) are ubiquitous in the chromosphere. The outline of bright structures are signature of the presence of magnetic fields in the photosphere below. This image was captured by the Inouye Solar Telescope during a coordinated observation campaign with NASA’s Parker Solar Probe and ESA’s Solar Orbiter.
In this image, the fine-structure of the quiet Sun is observed at its surface or photosphere. Heating plasma rises in the bright, convective “bubbles” (granules) then cools and falls into the dark, intergranular lanes. Within these intergranular lanes, bright structures are observed, indicating the manifestations or signatures of magnetic field. The Inouye Solar Telescope helps to detect these “small” magnetic elements in great detail.
In this image, the fine-structure of the quiet Sun is observed at its surface or photosphere. Heating plasma rises in the bright, convective “bubbles” (granules) then cools and falls into the dark, intergranular lanes. Within these intergranular lanes, bright structures are observed, indicating the manifestations or signatures of magnetic field. The Inouye Solar Telescope helps to detect these “small” magnetic elements in great detail.
This image reveals the fine structures of a sunspot in the photosphere. Within the dark, central area of the sunspot’s umbra, small-scale bright dots, known as umbral dots, are seen. The elongated structures surrounding the umbra are visible as bright-headed strands known as penumbral filaments. Umbra: Dark, central region of a sunspot where the magnetic field is strongest. Penumbra: The brighter, surrounding region of a sunspot’s umbra characterized by bright filamentary structures.
This image reveals the fine structures of a sunspot in the photosphere. Within the dark, central area of the sunspot’s umbra, small-scale bright dots, known as umbral dots, are seen. The elongated structures surrounding the umbra are visible as bright-headed strands known as penumbral filaments. Umbra: Dark, central region of a sunspot where the magnetic field is strongest. Penumbra: The brighter, surrounding region of a sunspot’s umbra characterized by bright filamentary structures.
This image, taken by Inouye Solar Telescope in coordination with the ESA’s Solar Orbiter, reveals the fibrillar nature of the solar atmosphere. In the atmosphere, or chromosphere, fine, dark threads of plasma (fibril) are visible emanating from the magnetic network below. The outline of bright structures are signature of the presence of magnetic fields.
This image, taken by Inouye Solar Telescope in coordination with the ESA’s Solar Orbiter, reveals the fibrillar nature of the solar atmosphere. In the atmosphere, or chromosphere, fine, dark threads of plasma (fibril) are visible emanating from the magnetic network below. The outline of bright structures are signature of the presence of magnetic fields.
A light bridge is seen crossing a sunspot’s umbra from one end of the penumbra to the other. Light bridges are believed to be the signature of the start of a decaying sunspot, which will eventually break apart. Light bridges are very complex, taking different forms and phases. It is unknown how deep these structures form. This image shows one example of a light bridge in remarkable detail. Umbra: Dark, central region of a sunspot where the magnetic field is strongest. Penumbra: The brighter, surrounding region of a sunspot’s umbra characterized by bright filamentary structures.
A light bridge is seen crossing a sunspot’s umbra from one end of the penumbra to the other. Light bridges are believed to be the signature of the start of a decaying sunspot, which will eventually break apart. Light bridges are very complex, taking different forms and phases. It is unknown how deep these structures form. This image shows one example of a light bridge in remarkable detail. Umbra: Dark, central region of a sunspot where the magnetic field is strongest. Penumbra: The brighter, surrounding region of a sunspot’s umbra characterized by bright filamentary structures.
A detailed example of a light bridge crossing a sunspot’s umbra. In this picture, the presence of convection cells surrounding the sunspot is also evident. Hot solar material (plasma) rises in the bright centers of these surrounding “cells,” cools off, and then sinks below the surface in dark lanes in a process known as convection. The detailed image shows complex light bridge and convection cell structures on the Sun’s surface or photosphere. Light bridge: A bright solar feature that spans across an umbra from one penumbra to the other. It is a complex structure, taking different forms and phases, and is believed to be the signature of the start of a decaying sunspot. Umbra: Dark, central region of a sunspot where the magnetic field is strongest.
A detailed example of a light bridge crossing a sunspot’s umbra. In this picture, the presence of convection cells surrounding the sunspot is also evident. Hot solar material (plasma) rises in the bright centers of these surrounding “cells,” cools off, and then sinks below the surface in dark lanes in a process known as convection. The detailed image shows complex light bridge and convection cell structures on the Sun’s surface or photosphere. Light bridge: A bright solar feature that spans across an umbra from one penumbra to the other. It is a complex structure, taking different forms and phases, and is believed to be the signature of the start of a decaying sunspot. Umbra: Dark, central region of a sunspot where the magnetic field is strongest.
A sunspot is identifiable by its dark, central umbra and surrounding filamentary-structured penumbra. A closer look reveals the presence of nearby umbral fragments – essentially, a sunspot that’s lost its penumbra. These fragments were previously a part of the neighboring sunspot, suggesting that this may be the “end phase” of a sunspot’s evolution. While this image shows the presence of umbral fragments, it is extraordinarily rare to capture the process of a penumbra forming or decaying. Umbra: Dark, central region of a sunspot where the magnetic field is strongest. Penumbra: The brighter, surrounding region of a sunspot’s umbra characterized by bright filamentary structures.
A sunspot is identifiable by its dark, central umbra and surrounding filamentary-structured penumbra. A closer look reveals the presence of nearby umbral fragments – essentially, a sunspot that’s lost its penumbra. These fragments were previously a part of the neighboring sunspot, suggesting that this may be the “end phase” of a sunspot’s evolution. While this image shows the presence of umbral fragments, it is extraordinarily rare to capture the process of a penumbra forming or decaying. Umbra: Dark, central region of a sunspot where the magnetic field is strongest. Penumbra: The brighter, surrounding region of a sunspot’s umbra characterized by bright filamentary structures.

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