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On April 8, 2024, volunteers participating in NASA’s Eclipse Megamovie citizen science project all around the United States hurried to photograph the solar eclipse with the latest, greatest equipment, capturing groundbreaking images of the Sun’s corona.

Now, the Eclipse Megamovie team has released the remarkable new dataset that resulted from this effort — the first-ever, white-light eclipse dataset with calibration frames, spanning more than a cumulative hour and a half of observations of the solar corona. This data, which includes 52,469 total photographs uploaded by project volunteers, is now live: https://eclipsemegamovie.org/database. The data include contributions from 143 unique, mobile, volunteer-led “observatories” – people with cameras charged with taking precise images of the eclipse, taking extra steps to allow the painstaking calibration required to reveal how the corona evolves from one person’s view to the next. Researchers around the world can now use these observations to identify solar jets leaving the Sun’s surface and study how solar plumes grow and develop. The public can also peruse and download all of this data, which is highly accessible and searchable by observatory name and location.

“Thank you for all you do and have done for us,” said Eclipse Megamovie volunteer Jessi McKenna. “Everyone in the group has been amazingly supportive of each other. And those who are running things are always so obviously appreciative of everyone who has contributed to the project.” 

The files include data at three different levels of processing, from raw (level 1) data to calibrated (level 3) data, in a format called FITS, or Flexible Image Transport System. It is the standard astronomical data format used by NASA and the International Astronomical Union. Of the 143 unique observatories involved, 28 observatories had clear skies, sufficient calibration frames, and enough unique exposure times to create calibrated level 3 images.

The Eclipse Megamovie team at Sonoma State University and the University of California, Berkeley and collaborators at NASA’s Goddard Space Flight Center began working together long before the eclipse to construct this database, together with EdEon STEM (Science, Technology, Engineering, & Mathematics) Learning programmer Troy Wilson. But crucially, Eclipse Megamovie 2024 was made possible because of hundreds of volunteers who journeyed into the path of the April 8, 2024 total solar eclipse with their cameras, patience, and curiosity.

Learn More and Get Involved

Eclipse Megamovie 2024

Measuring the motion of these plumes could help scientists understand the nature of the corona: what makes it so hot, and how it creates space weather. But these plumes can only be directly observed during an eclipse.

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NASA’s James Webb Space Telescope provided the first vertical view of Uranus’s ionosphere in this image released on Feb. 19, 2026, revealing auroras shaped by its tilted magnetic field.

Getting a look at the structure of the region where the atmosphere interacts strongly with the planet’s magnetic field is giving us the most detailed portrait yet of where its auroras form, how the magnetic field influences them, and also data on how Uranus’s atmosphere has continued to cool since the 1990s.

Uranus has the strangest magnetosphere in the Solar System. It is tilted and offset from the planet’s rotation axis (and this planet already rolls around the Sun nearly on its side), which means auroras move across the surface in complex ways. Better understanding Uranus will give us insight into ice-giant planets and help us better characterize giant planets outside our Solar System.

Read more about this image.

Image credit: ESA/Webb, NASA, CSA, STScI, P. Tiranti, H. Melin, M. Zamani (ESA/Webb)

Groundbreaking “camera-on-a-chip” technology that was originally developed at NASA’s Jet Propulsion Laboratory (JPL) for use in space missions is currently employed in billions of devices like cell phones that are used daily by people worldwide.

In the 1980s, sensors used to produce high-quality images for space science (including the amazing images from NASA’s Hubble Space Telescope) and other applications employed charge coupled device (CCD) technology. Dr. Eric Fossum was originally hired at JPL in 1990 to advance CCD technology for use in interplanetary space missions, but he ended up advancing another technology called complementary metal-oxide semiconductor (CMOS) technology for that purpose and much more. While at JPL, Fossum took advantage of a technique commonly used for CCDs and applied it to CMOS sensors to develop the first CMOS active pixel image sensor. This development began a chain of events that led to the present use of CMOS technology not only in space science missions, but also in billions of cameras in smartphones, webcams, automobiles, and medical devices used worldwide.

A new technology emerges…

In 1990, CCDs were the primary technology used to generate high-quality images. CCD sensors consist of arrays of pixels that convert light into electric charges. The charge from each pixel is transferred step-by-step to an output amplifier at the corner of the sensor and converted to a voltage that represents the brightness of the light received at the corresponding pixel. The data from all the pixels is then aggregated to generate an image. While CCD cameras can produce very high-quality images that are suitable for scientific use, they require a lot of power and an efficient charge transfer process to be effective.

CMOS sensors, on the other hand, have signal amplifiers within each pixel and signals can be read directly from each pixel instead of being transferred long distances to an amplifier for conversion. CMOS sensors therefore require less voltage to operate than CCDs and issues with the charge transfer process such as radiation susceptibility are greatly reduced. Although CMOS sensors existed in the 1990s, they produced too much noise to produce high-quality images required for science applications.

To reduce the signal noise typical of CMOS sensors at that time, Fossum applied a technique that was often used in CCD devices. This technique—called “intra-pixel charge transfer with correlated double sampling”—enables a double measurement of a pixel’s voltage without and with the light-generated charge. Subtracting the values of these two samples enables noise to be suppressed, improving the signal-to-noise ratio.

The next steps

Soon several companies signed Technology Cooperation Agreements with JPL and partnered with Fossum and his colleagues to develop the promising new technology. In 1995, Fossum and co-worker Dr. Sabrina Kemeny licensed the technology from CalTech and founded a company called Photobit to develop CMOS sensors. In 1996, Fossum left JPL to work at Photobit full time. The Photobit, team further refined the CMOS technology to get it closer to CCD capabilities, reduce power requirements, and make manufacturing cheaper.

Shortly thereafter, CMOS cameras started to be used in webcams, “pill cams” (small, swallowable devices that incorporate a tiny camera to take thousands of high-resolution images of the digestive tract), and other applications. In 2001 Photobit was acquired by Micron Technology, a larger company that devoted even more resources to development of CMOS technology. With the subsequent explosion of the cell phone industry, by 2013 more than a billion CMOS sensors were manufactured each year, and today that number has grown to about seven billion per year.

Where are these sensors now?

The CMOS technology Dr. Fossum originally developed has not only enabled space science, it has been infused into devices we depend on every day, dramatically and positively transforming many aspects of our lives. Virtually all digital still and video cameras, including those on cell phones, employ them. In addition, CMOS technology is used in automotive electronics, webcams, sports cameras, industrial equipment, security cameras including doorbells, and cinematography cameras, and for medical and dental imaging, among many other applications.

In addition to dominating the commercial and consumer market, CMOS imagers have been used as engineering cameras to enable the entry, descent, and landing of NASA’s Perseverance Mars rover, in the camera onboard the OCO-3 (Orbiting Carbon Observatory-3) mission that monitors the distribution of carbon dioxide on Earth, and as scientific imagers on NASA’s Parker Solar Probe mission that is revolutionizing our understanding of the Sun. CMOS imagers are on their way to Jupiter’s moon, Europa, on the agency’s Europa Clipper mission, and a delta-doped ultraviolet version with tailored response is under development for use on the upcoming UVEX (UltraViolet EXplorer) mission that will provide insight into how galaxies and stars evolve.

CMOS imagers are routinely used in monitoring the launch and deployment of CubeSats and SmallSats. They were recently used to monitor the deployment of Pandora, a small satellite that will characterize exoplanet atmospheres and their host stars; BLACKCAT (the Black Hole Coded Aperture Telescope), a small X-ray telescope; and the SPARCS (Star-Planet Activity Research CubeSat) mission designed to monitor and characterize the stellar flares of low-mass stars in ultraviolet to provide context for the habitability of exoplanets in their system. NASA is also developing descendants of this technology for use in missions that will search for life beyond Earth like its Habitable Worlds Observatory.

In recognition of the impact this CMOS technology has had, the National Academy of Engineering (NAE) has named Dr. Fossum the recipient of the 2026 Charles Stark Draper Prize for Engineering “for innovation, development, and commercialization of the complementary metal-oxide semiconductor (CMOS) active pixel image sensor ‘camera-on-a-chip.’” The NAE bestows this award biennially to honor an engineer “whose accomplishment has significantly impacted society by improving the quality of life, providing the ability to live freely and comfortably, and/or permitting the access to information.”

Sponsoring Organizations: The original efforts at JPL to develop this CMOS technology were funded by JPL and NASA.

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The tallest point in South Korea is not located in the Taebaek Mountains that run along the country’s eastern coast. Rather, it is found atop a volcanic peak on Jeju Island, about 100 kilometers (60 miles) south of the Korean Peninsula. In winter 2026, winds blew past the island in just the right way to send clouds spinning in its wake.

The MODIS (Moderate Resolution Imaging Spectroradiometer) on NASA’s Terra satellite captured this image of swirling clouds—and colorful, turbulent water—near Jeju Island on February 19, 2026. The island rises about 1,950 meters (6,400 feet) above the sea surface. At its center is Hallasan, a shield volcano that last erupted in the 11th century and contains a notable network of lava tubes.

The trailing, staggered spirals, called von Kármán vortex streets, form when a fluid passes a tall, isolated, stationary object. If winds are too weak, clouds simply flow smoothly past, and if winds are too strong, vortices cannot maintain their shape. In the sweet spot, with winds between 18 and 54 kilometers (11 and 34 miles) per hour, clouds trace the airflow in patterns of counterrotating vortices. Though the underlying physics is the same, the appearance of the vortices can vary: sometimes they look wispy, as they do here, and other times they form more sharply defined, parallel rows, as they did at the same location the previous day.

The seas, as well as the atmosphere, were turbulent near Jeju Island in mid-February. To the west, a large plume of sediment coming off the coast of China’s Jiangsu province turned waters murky. While brown, sediment-laden water is present in the shallow nearshore area year-round, expansive plumes like this one are common during winter. Research suggests that seasonal changes in currents and vertical mixing of the water column may account for the large winter plumes.

NASA Earth Observatory image by Michala Garrison, using MODIS data from NASA EOSDIS LANCE and GIBS/Worldview. Story by Lindsey Doermann.

Downloads

February 19, 2026

JPEG (2.74 MB)

References & Resources

• Global Volcanism Program, Halla. Accessed February 23, 2026.
• NASA Earth Observatory (2024, February 24) Sediment Fans Out Over the Yangtze Bank. Accessed February 23, 2026.
• NASA Earth Observatory (2008, November 16) Cheju Island, South Korea. Accessed February 23, 2026.
• UNESCO World Heritage Convention (2018) Jeju Volcanic Island and Lava Tubes. Accessed February 23, 2026.
• Weather Underground (2019, December) Whirls, Curls, and Little Swirls: The Science Behind Von Karman Vortices. Accessed February 23, 2026.

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Young ‘Sun’ Caught Blowing Bubbles by NASA’s Chandra

For the first time, a much younger version of the Sun has been caught red-handed blowing bubbles in the galaxy, by astronomers using NASA’s Chandra X-ray Observatory.

HD 61005 in X-ray, infrared, and optical light

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Image Details

These images show the star HD 61005 with X-rays from the Chandra X-ray Observatory as well as infrared data from Hubble Space Telescope. A view in optical light from a telescope in Chile shows the larger field that HD 61005 is located in. Astronomers recently used Chandra to discover an “astrosphere,” a wind-blown bubble, around HD 61005, the first seen around a star like the Sun.

The bubble – called an “astrosphere” – completely surrounds the juvenile star. Winds from the star’s surface are blowing up the bubble and filling it with hot gas as it expands into much cooler galactic gas and dust surrounding the star. The Sun has a similar bubble around it, which scientists call the heliosphere, created by the solar wind. It extends far beyond the planets in our solar system and protects Earth from cosmic radiation.

This is the first image of an astrosphere astronomers have obtained around a star similar to the Sun. It shows slightly extended emission, rather than a single point of light as seen for other such stars.

“We have been studying our Sun’s astrosphere for decades, but we can’t see it from the outside,” said Carey Lisse of Johns Hopkins University in Baltimore, who led the study, which published [day of week] in the Astrophysical Journal. “This new Chandra result about a similar star’s astrosphere teaches us about the shape of the Sun’s, and how it has changed over billions of years as the Sun evolves and moves through the galaxy.”

The star is called HD 61005 and is located about 120 light-years from Earth, making it relatively close. HD 61005 has roughly the same mass and temperature as the Sun, but it is much younger with an age of about 100 million years, compared to the Sun’s age of about 5 billion years.

Because it is so young, HD 61005 has a much stronger wind of particles blowing from its surface that travels about 3 times faster and is about 25 times denser than the wind from the Sun. This amplifies the process of astrosphere bubble-blowing and mimics how our Sun was behaving several billion years ago.

“We are impacted by the Sun every day, not only through the light it gives off, but also by the wind it sends out into space that can affect our satellites and potentially astronauts traveling to the Moon or Mars,” said co-author Scott Wolk of the Center for Astrophysics | Harvard & Smithsonian (CfA). “This image of the astrosphere around HD 61005 gives us important information about what the Sun’s wind may have been like early in its evolution.”

Astronomers have nicknamed the HD 61005 star system the “Moth” because it is surrounded by large amounts of dust patterned similarly to the shape of a moth’s wings when viewed through infrared telescopes. The wings are formed from material left behind after the formation of the star, similar to the Kuiper Belt in our own solar system. Observations of these wings with NASA’s Hubble Space Telescope showed that the interstellar matter surrounding HD 61005 is about a thousand times denser than that around the Sun.

Since the 1990s, astronomers have been trying to capture an image of an astrosphere around a Sun-like star. Chandra was able to detect the astrosphere around HD 61005 because it is producing X-rays as the stellar wind runs into cooler local interstellar medium dust and gas that surrounds the star. The dense local galactic environment, combined with Chandra’s high-resolution X-ray vision, the strong stellar wind, and the star’s proximity, all helped create a strong X-ray signal, allowing discovery of an astrosphere around HD 61005. It has a diameter about 200 times the distance from Earth to the Sun.

“There’s a saying about a moth being drawn to a flame,” said co-author Brad Snios, formerly of CfA and now at MITRE, a non-profit that participates in federally funded research. “In the case of HD 61005, the ‘Moth’ can’t easily escape from the flame because it was born around it and might be sustained by a disk around it.”

The Sun not only likely passed through a phase of development similar to HD 61005 when it was younger, it also likely traveled through a denser region of dust and gas than where the Sun is currently located, strengthening the connection with HD 61005.

“It is amazing to think that our protective heliosphere would only extend out to the orbit of Saturn if we were in the part of the galaxy where the Moth is located, or, conversely, that the Moth would have an astrosphere 10 times wider larger than the Sun’s if it were located here,” Lisse said.

HD 61005 is not visible from Earth with the unaided eye, but it is close enough that skywatchers could see it using binoculars.

The first hints of X-ray emission from the Moth’s central star were based on a brief, one-hour-long Chandra observation of HD 61005 in 2014. In 2021, astronomers observed HD 61005 for almost 19 hours, which allowed the detection of the extended astrospheric structure.

NASA’s Marshall Space Flight Center manages the Chandra program. The Smithsonian Astrophysical Observatory’s Chandra X-ray Center controls science operations from Cambridge, Massachusetts, and flight operations from Burlington, Massachusetts.

Image credit: X-ray: NASA/CXC/John Hopkins Univ./C.M. Lisse et al.; Infrared: NASA/ESA/STIS; Optical: NSF/NoirLab/CTIO/DECaPS2; Image Processing: NASA/CXC/SAO/N. Wolk

To learn more about Chandra, visit:

https://science.nasa.gov/chandra

Read more from NASA’s Chandra X-ray Observatory

Learn more about the Chandra X-ray Observatory and its mission here:

https://www.nasa.gov/chandra

https://chandra.si.edu

Visual Description

This release contains three main images, each offering a different take on the astrosphere surrounding a young star called HD 61005. An astrosphere is a wind-blown bubble full of gas and dust particles that encases a star as it pushes through interstellar space.

In this release, an optical image from the Cerro Tololo Inter-American Observatory in Chile shows HD 61005 in the context of its star field. Here, the star in question appears as a glowing, gleaming white dot surrounded by other glowing dots of similar and smaller sizes. The image is utterly packed with specks of light in shades of blue, white, gold, green, and red. At this distance, in an optical observation, the star’s astrosphere is not discernible.

The second image is a composite, which presents a close-up of HD 61005 using infrared data from Hubble, and X-ray data from the Chandra X-ray Observatory. Here, the spherical star has a brilliant core bursting with white X-ray light. Ringing the white core is a neon purple glow; the astrosphere surrounding the star. A distinguishing feature of HD 61005 is a white, wedge-shaped tail with neon blue tips, which trails the fast-moving star. This tail is dusty material left behind after the star’s formation. The wedge, or wing shape of the tail has earned the star the nickname ‘Moth’ by astronomers spying it through infrared telescopes.

The third image in this release is an artist’s illustration of an astrosphere in action. Here, a large, pale purple ball soars from our right toward our left, into a misty brown cloud. The purple ball appears to be protected by a blue force field, which pushes the brown cloud aside as the ball dives in. In this illustration, the purple ball represents the astrosphere surrounding a star and the brown cloud is interstellar gas. The blue force field is a bow shock, a curved free-floating shock wave, similar to the sonic boom that travels in front of a supersonic plane. The bow shock is caused by the motion of the star and its astrosphere hurtling through space. This illustration features a series of faint lines representing wind patterns from HD 61005, but does not show the tail of debris found behind and beside HD 61005.

News Media Contact

Megan Watzke
Chandra X-ray Center
Cambridge, Mass.
617-496-7998
mwatzke@cfa.harvard.edu

Joel Wallace
Marshall Space Flight Center, Huntsville, Alabama
256-544-0034
joel.w.wallace@nasa.gov

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