Europe Goes Dark August 12th: What to Expect During the 2026 Total Solar Eclipse

Europe’s First Total Eclipse Since 1999

The total solar eclipse of August 12, 2026, represents a highly anticipated celestial event for the global astronomical community, offering a rare intersection of favorable orbital geometry, dynamic solar activity, and unique terrestrial viewing conditions. Sweeping across the Arctic, Greenland, Iceland, the Atlantic Ocean, and the Iberian Peninsula, the event provides the first total solar eclipse visible from mainland Europe since 1999¹. Furthermore, it marks the beginning of an exceptional astronomical sequence for the Iberian Peninsula, which will experience a triad of eclipses: the total eclipse in 2026, a subsequent total eclipse in August 2027, and an annular eclipse in January 2028³. Beyond its visual spectacle, the 2026 eclipse serves as a critical natural laboratory. It presents opportunities to observe the solar corona during the declining phase of Solar Cycle 25, study the thermodynamics of the Earth's atmospheric boundary layer, and resolve lingering spectroscopic anomalies related to low-altitude atmospheric scattering⁵.

This research report provides a comprehensive analysis of the August 2026 eclipse, deconstructing the orbital mechanics of its Saros cycle, the climatological variables along the path of totality, the heliophysical implications of the solar corona, and the transient atmospheric gravity waves induced by the lunar shadow.

Orbital Mechanics and the Evolution of Solar Saros 126

Solar eclipses are not isolated cosmic accidents but rather predictable manifestations of orbital commensurability. The August 2026 eclipse belongs to Solar Saros 126, a specific family of eclipses governed by the alignment of three distinct lunar orbital periods. The first is the synodic month, which is the interval between consecutive new moons, lasting approximately 29.53 days⁸. The second is the draconic month, defined as the time it takes for the Moon to return to the same orbital node relative to the Sun, lasting 27.21 days⁸. The third is the anomalistic month, the time required for the Moon to travel from perigee to perigee, lasting 27.55 days⁸.

A single Saros cycle aligns these periods almost perfectly every 6,585.3 days, which equates to 18 years, 11 days, and 8 hours⁸. This interval aligns exactly 223 synodic months, 242 draconic months, and 239 anomalistic months⁸. Because these periods align so closely, consecutive eclipses in a Saros series occur at the same lunar node, with the Moon at a comparable distance from Earth, and during the exact same season of the year⁸.

The Northward Migration of the Lunar Shadow

Because Saros 126 is an even-numbered series, its eclipses occur exclusively at the Moon's descending node⁸. A slight mathematical mismatch in the lunar periods stems from lunar precession and Earth's orbital dynamics, dictating that the Moon's orbital plane shifts gradually relative to Earth over successive cycles⁸. This geometry forces the lunar shadow to migrate progressively northward across the Earth's surface over the lifespan of the series, which spans 1,280 years and comprises 72 individual eclipses⁸.

The progression of the shadow is tracked using the gamma parameter, which measures the minimum distance from the axis of the lunar shadow to the center of the Earth, expressed in Earth radii. A gamma value of zero indicates that the shadow axis passes directly through the center of the Earth, while positive and negative values indicate a shift north or south, respectively⁸.

The Saros 126 series initiated on March 10, 1179, with a minor partial eclipse near the Antarctic, recording a highly negative gamma of negative 1.53⁸. As the series progressed, the shadow axis moved closer to the Earth's center. This geometric shift generated a long sequence of 28 annular eclipses between 1323 and 1810⁸. The longest annular eclipse of the series occurred on June 26, 1359, lasting an impressive 6 minutes and 30 seconds across the southern hemisphere⁸. By the mid-19th century, the Moon's proximity to Earth during these nodal crossings allowed the umbra, the dark inner core of the shadow, to reach the Earth's surface. This triggered a cluster of 13 central umbral events, comprising 3 hybrid eclipses and 10 total eclipses⁸. The longest total eclipse in this sequence took place on July 10, 1972, featuring a totality of 2 minutes and 36 seconds⁸.

The August 12, 2026 eclipse represents the 58th event in the series and one of its final total eclipses. It possesses a gamma of 0.8977 and a magnitude of 1.0386, placing the core shadow in the high northern latitudes⁸. Following the subsequent total eclipse in August 2044, which will have a gamma of 0.9613, the gamma parameter will exceed 1.0, lifting the umbral shadow completely off the Earth's surface⁸. The series will then revert to partial eclipses, finally concluding in the year 2459⁸.

Table 1: Evolutionary Phases of Solar Saros 126

Phase	Date Range	Number of Eclipses	Gamma Range	Characteristics
Initial Partial	1179 - 1305	8	-1.53 to -1.06	Shadow axis misses Earth to the south; visible only in Antarctic regions.
Annular	1323 - 1810	28	-0.98 to 0.10	Moon appears smaller than the Sun; progression from south to equator.
Hybrid	1828 - 1864	3	0.14 to 0.26	Transitional eclipses varying between annular and total along the path.
Total	1882 - 2044	10	0.32 to 0.96	Moon fully occults the Sun; paths migrate from the equator to the Arctic.
Final Partial	2062 - 2459	23	1.01 to 1.51	Shadow axis misses Earth to the north; visible only in Arctic regions.

Geographic Trajectory and Observational Climatology

The physical path of the eclipse is dictated by the orbital motion of the Moon, which travels from west to east at roughly 3,700 kilometers per hour, far exceeding the rotational speed of the Earth⁹. On August 12, 2026, the umbra will first touch down at sunrise over a remote region of northern Siberia, near the Taymyr Peninsula and the Laptev Sea¹¹. Because the event occurs during the Arctic summer, the eclipsed Sun will hover just above the northern horizon, providing an 85-second totality in a region experiencing 24-hour continuous daylight¹².

The shadow will then sweep rapidly across the Arctic Ocean, passing within a single degree of the North Pole, before making landfall in northeastern Greenland¹¹. From there, it will cross the Denmark Strait to Iceland, traverse the North Atlantic Ocean, and finally bisect the Iberian Peninsula¹¹. The umbra will lift off the Earth's surface at sunset in the Balearic Sea, creating a unique atmospheric and visual phenomenon for observers in the Mediterranean¹¹.

Table 2: Key Locations and Totality Parameters for August 12, 2026

Country	Location	Totality Start (Local)	Duration	Sun Altitude
Greenland	Vandreblok	16:35 UTC	1 min 15 sec	~20 degrees
Iceland	Látrabjarg (West)	17:44 UTC	2 min 12 sec	~25 degrees
Iceland	Reykjavik	17:48 UTC	0 min 57 sec	~24 degrees
Spain	A Coruña	20:27 CEST	1 min 16 sec	~12 degrees
Spain	Oviedo	20:27 CEST	1 min 48 sec	~10 degrees
Spain	Burgos	20:28 CEST	1 min 44 sec	~8 degrees
Spain	Palma de Mallorca	20:31 CEST	1 min 36 sec	~2 degrees

Climatological Variables and Cloud Cover Predictions

Obtaining clear views of the solar corona relies heavily on localized microclimates and synoptic weather patterns. The High Arctic and the North Atlantic are notoriously cloudy during August, driven by cool, easily saturated air masses and persistent low-pressure systems¹⁴. Average cloud cover over the Arctic Ocean during this period hovers around 75 percent, severely limiting the probability of a clear observation in the earliest stages of the eclipse¹⁴.

However, the coastal fjords of Greenland, particularly Scoresby Sund, present unique microclimatic advantages. Cold, dry air descending from the Greenlandic icecap creates katabatic winds that warm and dry as they drop into the fjords¹¹. This localized phenomenon effectively suppresses cloud formation. Satellite data from the past two decades indicates an 80 percent probability of at least partial visibility within these specific fjords¹⁴.

In Iceland, weather patterns are heavily influenced by the windward and leeward dynamics of the island's topography. The island sits directly in the North Atlantic storm track near the semi-permanent Icelandic Low, resulting in an average cloud cover of 70 to 80 percent¹⁴. Observers must navigate based on real-time wind data; on sunny days, convective clouds tend to build over the interior of the western peninsulas, leaving the immediate coastlines relatively clear¹⁴.

The Iberian Peninsula offers the most statistically favorable weather conditions, though it presents unique topographical challenges. The path of totality crosses northern and eastern Spain, traversing regions like Galicia, Asturias, Castile and León, Aragon, and the Balearic Islands⁴. While the overall probability of clear skies in the central plateaus ranges from 70 to 85 percent, the intense summer heat of August frequently triggers afternoon convective thunderstorms¹³. Heating along the dark slopes of the Sistema Ibérico and the Sierra de Guadarrama can initiate convective cells by mid-morning, maturing into massive thunderheads by the late afternoon¹⁴. Because the eclipse occurs roughly an hour before sunset, these high-level anvil clouds can easily obscure the western horizon¹⁴. Furthermore, the low solar altitude in Spain, which drops from 10 degrees in the northwest to a mere 2 degrees in the Balearic Islands, means that even distant mountains, buildings, or low-lying coastal haze can completely obstruct the view of totality⁴.

Heliophysics: The Corona in the Declining Phase of Solar Cycle 25

A total solar eclipse provides an unparalleled opportunity to study the Sun's inner and middle corona, a superheated envelope of plasma that is normally rendered invisible by the overwhelming glare of the photosphere¹⁶. The August 2026 eclipse is particularly significant because it occurs shortly after the peak of Solar Cycle 25, during a highly active period known as the declining phase⁵.

Solar magnetic activity operates on an 11-year cycle, known as the Schwabe-Wolf cycle, which transitions from a solar minimum characterized by quiet, highly ordered magnetic fields to a solar maximum defined by chaotic, entangled magnetic fields¹⁸. These 11-year cycles exist against the backdrop of longer-term fluctuations, such as the 22-year Hale cycle and the 100-year Gleissberg cycle¹⁸. Solar Cycle 25 reached its maximum between early 2024 and 2025, producing numerous sunspots and intense extreme ultraviolet emissions¹⁹. Historically, the declining phase of a solar cycle, spanning the one to three years post-maximum, yields some of the most powerful and complex solar events⁵. The breakdown of the complex magnetic structures often results in massive X-class flares and highly energetic coronal mass ejections⁵.

Coronal Structure and Thermodynamic Mysteries

The shape of the white-light corona is highly dependent on the phase of the solar cycle. During a solar minimum, the corona appears highly asymmetric; the plasma is confined to the equatorial regions by closed magnetic loops, while the polar regions feature distinct, brush-like plumes that trace open magnetic field lines extending into interplanetary space¹⁷. During a solar maximum and its immediate aftermath, the magnetic field is highly complex, resulting in a symmetric, star-burst corona with helmet streamers protruding at all latitudes¹⁷. Observations during the 2026 eclipse will likely reveal a highly dynamic, globally distributed corona, potentially capturing active prominences or the early stages of a coronal mass ejection.

A primary focus of heliophysics during this eclipse is the coronal heating problem. While the visible surface of the Sun rests at roughly 5,500 degrees Celsius, the corona burns at several million degrees²². The mechanisms responsible for this extreme temperature inversion remain a subject of intense research. Recent eclipse observations have identified complex turbulent structures within the corona, including vortex rings and wave-like rolling motions²⁴. These turbulent features often originate near the boundary of solar prominences, which are dense, relatively cool structures rooted in the photosphere. The steep temperature and density gradients between the cool prominences and the surrounding superheated coronal plasma create unstable conditions, triggering turbulent waves²⁴. These waves transfer immense amounts of thermal energy outward into the corona, contributing to the extreme heating and subsequently accelerating the solar wind²⁴.

Citizen Science, Polarimetric Measurements, and Orbital Vantage Points

The relatively short duration of totality during the 2026 eclipse necessitates highly coordinated observational campaigns. The Network for Astronomical Training and Education (NATE) project, a massive collaboration between the Instituto de Astrofísica de Canarias, the National Solar Observatory, and the Mohammed VI Polytechnic University in Morocco, will utilize the 2026 eclipse as a critical training ground²⁵. Ten automated telescope stations will be deployed across Palencia, Spain²⁵.

While the short duration, lasting just under two minutes, and the low solar altitude in Spain are not optimal for long-exposure deep-space coronal imaging, the event serves as a vital rehearsal for the subsequent 2027 total solar eclipse in North Africa²⁵. During the 2027 event, totality will last over six minutes in locations like Luxor and Morocco¹. Programs like NATE utilize advanced polarimetric imaging to measure the orientation of oscillating light waves in the corona²³. Because coronal light is generated by photospheric photons scattering off highly agitated electrons, measuring the polarization angle across different coronal regions provides a direct, high-resolution map of electron density and the underlying magnetic field architecture¹⁷.

Furthermore, the 2026 eclipse will be analyzed alongside orbital data reconstructions. Using software platforms like SunPy, researchers can reconstruct solar observations from various vantage points in space. For instance, prior reconstructions of the Artemis II Orion spacecraft trajectory allowed scientists to project coronagraph data from satellites into the exact coordinate frame of an astronaut's viewpoint²⁷. Similar computational techniques will be applied to the 2026 eclipse, allowing ground-based community observations across Europe to be directly correlated with simultaneous space-based solar observations, providing a three-dimensional understanding of coronal dynamics²⁷.

Atmospheric Physics: The Terrestrial Response to the Lunar Shadow

The sudden interruption of solar insolation during a total solar eclipse exerts an intense, transient forcing on the Earth's atmosphere. This rapid shift acts as a natural laboratory to study the thermodynamics of the planetary boundary layer and the generation of atmospheric gravity waves⁶.

Boundary Layer Thermodynamics and the "Eclipse Wind"

As the Moon's shadow races across the Earth, it drastically curtails downwelling shortwave radiation, resulting in the rapid cooling of the surface air. Depending on the local environment, temperature drops can range from a modest 0.3 degrees Celsius over open oceans to as much as 6.8 degrees Celsius in inland regions⁶. The reduction in temperature typically lags the point of maximum eclipse by 10 to 15 minutes due to the thermal inertia of the soil and lower atmosphere²⁹. Coastal regions and marine atmospheric boundary layers exhibit higher thermal inertia, which moderates the temperature decrease compared to dry, inland environments³⁰.

This rapid cooling fundamentally alters the structure of the atmospheric boundary layer. On a normal summer afternoon, solar heating generates an unstable boundary layer characterized by robust thermal updrafts and intense turbulent mixing²⁹. As the eclipse progresses, the surface cools much faster than the air aloft, creating a micro-inversion that stabilizes the lower atmosphere²⁹.

This stabilization suppresses turbulent kinetic energy and vertical mixing, leading to a noticeable deceleration in near-surface wind speeds⁶. However, this overall calming effect is often interrupted by anomalous wind shifts historically termed the "eclipse wind" or "eclipse cyclone"⁶. The sudden temperature gradient between the chilled air within the umbra and the warm air in the surrounding sunlit regions generates a localized pressure perturbation⁶. High-resolution meteorological modeling and advanced sonic anemometer measurements have demonstrated that this pressure gradient can induce a weak, transient circulation pattern⁶. This often manifests as a counterclockwise rotation in wind direction and a brief, localized surge in wind speed just outside the center of the shadow boundary⁶.

Atmospheric Gravity Waves and Ionospheric Bow Waves

Perhaps the most profound atmospheric phenomenon induced by a solar eclipse is the generation of internal gravity waves. As the lunar umbra moves at supersonic speeds, frequently exceeding Mach 2, across the atmosphere, the rapid, localized cooling of the ozone layer and troposphere creates a moving pressure anomaly³³.

Much like a fast-moving boat displacing water and creating a V-shaped wake, the supersonic cooling spot generates atmospheric bow waves³³. These are not acoustic sound waves, but rather buoyancy oscillations known as gravity waves. In this mechanism, air parcels are displaced vertically by the sudden pressure shift and are subsequently pulled back down by gravity, creating a rhythmic oscillation³⁵. These waves propagate upward and outward from the eclipse path, expanding in amplitude as they reach the thinner air of the upper atmosphere³³.

The characteristics of these waves have been successfully mapped during recent eclipses. During the annular solar eclipse of 2023 over Brazil, researchers utilized reverse ray-tracing methods and all-sky imagers to track gravity waves in the mesosphere and lower thermosphere³⁴. They identified medium-scale waves with horizontal wavelengths of 174 kilometers, and large-scale waves reaching wavelengths of 1,523 kilometers traveling at phase speeds of 218 meters per second³⁴. By tracing the trajectories of these waves backward, scientists confirmed they originated precisely at stratospheric altitudes where the Moon's shadow intersected the atmosphere, proving they were triggered by eclipse-induced cooling rather than local convective storms³⁴.

When these gravity waves reach the ionosphere, a layer of charged particles located 50 to 1,000 kilometers above the surface, they interact with the local plasma, creating traveling ionospheric disturbances³³. During eclipses, dense networks of Global Navigation Satellite System receivers have successfully detected these ionospheric bow waves by measuring fluctuations in the total electron content³³. The August 2026 eclipse will allow atmospheric physicists to track these disturbances across the North Atlantic and Europe, further validating the models that link thermospheric anomalies directly back to the sudden stratospheric cooling initiated by the lunar shadow³⁴.

Low-Altitude Optics and Spectroscopic Anomalies

The geometry of the 2026 eclipse over the Iberian Peninsula provides a unique environment for studying atmospheric optics. Because the event occurs just before sunset, the eclipsed Sun will sit extremely low on the western horizon⁴.

Rayleigh Scattering and Coronal Reddening

When light from the solar corona passes through the Earth's atmosphere at a low angle, it traverses a significantly thicker slice of air than it would if the Sun were directly overhead³⁷. This long atmospheric path profoundly intensifies the effects of Rayleigh scattering. Rayleigh scattering is the physical process by which air molecules and small aerosols scatter shorter wavelengths of light, such as blue and violet, much more efficiently than longer wavelengths like red and orange³⁷.

During the 2026 eclipse in Spain, the blue light emitted by the corona will be heavily depleted by scattering before reaching the observer. As a result, the lower portion of the sky will take on a distinct reddish or dirty orange hue, and the white-light corona itself may appear uncharacteristically warm, golden, or red³⁷. Furthermore, the sky directly overhead at the zenith will appear an unusually deep blue. This occurs because the primary sunlight is blocked, and the only light reaching the zenith is secondary scattered light originating from high altitudes outside the shadow zone³⁷.

The darkening of the sky also dramatically alters the visual range across the landscape. The contrast between dark objects on the ground and the horizon increases significantly because the ratio of nearby scattered air light to distant air light is reduced. This reduction in atmospheric haze within the umbra effectively extends the daytime visual range, allowing observers to see distant topography much more clearly during the brief window of totality³⁸.

The Helium 1083 nm Origin Debate

This intense low-altitude atmospheric scattering is at the heart of an ongoing spectroscopic debate within the heliophysics community. During several previous eclipses, astronomers detected strong emissions of the neutral Helium atomic line, specifically He I at 1083.0 nanometers, extending several solar radii into the corona⁷.

The presence of neutral helium in the middle corona is physically baffling. The corona's ambient temperature is several million degrees Celsius, meaning that nearly all helium should be fully ionized; neutral helium should theoretically be destroyed instantly in this environment⁷. Two opposing hypotheses have emerged over the decades to explain this anomaly. The first hypothesis suggests that the signal originates from the Sun itself, positing that cool, dense material from solar prominences is somehow dispersed and magnetically shielded within the superheated coronal plasma, allowing neutral helium to survive⁷.

The second hypothesis argues that the signal is entirely a terrestrial optical illusion. According to this theory, strong chromospheric light, which naturally contains He I 1083 emissions from the lower, cooler layers of the Sun, is Rayleigh-scattered by the Earth's atmosphere⁷. This scattering artificially projects the chromospheric signal into the dark space around the eclipsed Sun, making it appear as though the corona itself is emitting the neutral helium signature⁷.

High-resolution spectroscopic measurements taken during the April 2024 total solar eclipse provided strong evidence for the terrestrial hypothesis. Researchers demonstrated that the line width and intensity of the He I 1083 signal, alongside the chromospheric Paschen-gamma line, mirrored Rayleigh scattering models rather than matching the thermal signatures expected from true coronal emission⁷. The 2026 eclipse over Spain, with its extreme atmospheric path length and enhanced scattering conditions, will serve as a definitive test bed to confirm the terrestrial origin of these diffuse coronal signals once and for all⁷.

Coinciding Astronomical Phenomena

The scientific and observational value of August 12, 2026, is further amplified by a coinciding celestial event. A solar eclipse can only occur during the new moon phase, a period when the lunar hemisphere facing Earth is completely unilluminated³⁹. This precise alignment guarantees an exceptionally dark night sky immediately following the daytime eclipse³⁹.

By celestial coincidence, the evening of August 12 and the early morning of August 13 align perfectly with the peak of the Perseid meteor shower³⁹. The Perseids, which originate from the vast debris stream left behind by Comet Swift-Tuttle, are renowned for producing dozens of bright meteors per hour, including frequent, highly luminous fireballs known as bolides⁴⁰. When these larger fragments of comet debris strike the Earth's atmosphere at high speeds, they compress and heat the air in front of them, causing the surrounding gases to glow brightly and occasionally fragment in spectacular bursts of light⁴⁰.

Moonlight is typically the greatest hindrance to meteor observation, as the glare washes out the fainter streaks and diminishes the contrast of the night sky³⁹. The complete absence of lunar glare on the night of the eclipse will provide pristine, ideal conditions for astronomical observation. This effectively creates a rare 24-hour window of extreme celestial activity, seamlessly transitioning from observing complex coronal physics during the day to witnessing dramatic atmospheric meteoroid ablation at night³⁹.

The total solar eclipse of August 12, 2026, transcends a mere visual phenomenon; it represents a profound multi-disciplinary forcing event. The northward migration of the lunar shadow, driven by the rigid mechanics of Solar Saros 126, brings the umbra into a highly specific atmospheric and climatic regime. For the heliophysics community, the timing of the eclipse within the declining phase of Solar Cycle 25 offers a crucial glimpse into the turbulent thermodynamics and magnetic complexity that dictate space weather. Simultaneously, the shadow's supersonic transit will trigger rapid boundary layer stabilization and launch atmospheric gravity waves that disrupt the ionosphere. Finally, the extreme low-altitude geometry over the Iberian Peninsula will exacerbate Rayleigh scattering, providing the necessary conditions to resolve long-standing spectroscopic anomalies. By coordinating observations across these diverse domains, researchers can utilize the 2026 eclipse to refine both solar atmospheric models and terrestrial meteorological algorithms, ultimately enhancing our broader understanding of the interconnected mechanics of the Earth-Sun system.

Works cited

1. Planning a route to the total solar eclipses of 2026 and 2027 - Universe Space Tech, https://universemagazine.com/en/planning-a-route-to-the-total-solar-eclipses-of-2026-and-2027/

2. How to see the 12 August 2026 partial solar eclipse - Royal Museums Greenwich, https://www.rmg.co.uk/stories/space-astronomy/how-see-12-august-2026-partial-solar-eclipse

3. ESA - Total solar eclipse 12 August 2026 – Global map - European Space Agency, https://www.esa.int/ESA_Multimedia/Images/2026/05/Total_solar_eclipse_12_August_2026_Global_map

4. Total solar eclipse, August 12, 2026 - Astronomía IGN, https://astronomia.ign.es/en/eclipses-de-sol-y-luna/eclipse-total-sol-de-12-de-agosto-2026

5. We're not done yet! | SIDC - Solar Influences Data Analysis Center, https://www.sidc.be/article/were-not-done-yet

6. Ensemble-Averaging Resolves Rapid Atmospheric Response to the 2017 Total Solar Eclipse - Frontiers, https://www.frontiersin.org/journals/earth-science/articles/10.3389/feart.2019.00198/full

7. Detection of “diffuse” coronal He 1 1083 during the April 8 2024 Solar Eclipse: evidence for terrestrial atmospheric scattering origin - arXiv, https://arxiv.org/html/2501.01009v1

8. Solar Saros 126 - Grokipedia, https://grokipedia.com/page/solar_saros_126

9. Map of the August 12, 2026, Total Solar Eclipse - NASA SVS, https://svs.gsfc.nasa.gov/5647

10. Total Solar Eclipse of August 12, 2026: Complete Information - TheSkyLive, https://theskylive.com/solar-eclipse?id=2026-08-12

11. 2026 August 12 — Eclipse Atlas, http://www.eclipseatlas.com/2026-august-12

12. Where can I see the total solar eclipse on Aug. 12, 2026? - Space, https://www.space.com/where-to-see-total-solar-eclipse-2026-maps

13. Total Solar Eclipse of August 12, 2026 in Spain: Where, When and How to See It, https://spainroutes.com/en/total-solar-eclipse-spain-august-12-2026/

14. Total Solar Eclipse 2026 August 12 - Eclipsophile, https://eclipsophile.com/tse2026/

15. The Solar Eclipse — Stories | Swisspath Yachting, https://swisspath-yachting.com/story/the-solar-eclipse

16. August 12, 2026 Solar Eclipse Map - NSO, https://nso.edu/for-public/eclipse-map-2026/

17. Revealing the True Solar Corona | American Scientist, https://www.americanscientist.org/article/revealing-the-true-solar-corona

18. Rybov et al. Radio Astronomical and Magnetometric Monitoring of Space Weather - PoS - Proceeding of science, https://pos.sissa.it/520/009/pdf

19. Solar Cycle Progression | NOAA / NWS Space Weather Prediction Center, https://www.spaceweather.gov/products/solar-cycle-progression

20. Solar Cycle 25 Peak: Extreme Solar Flares Captured by NASA | Zendar Universe, https://zendaruniverse.com/updates/extreme-solar-flares-nasa-sdo-captures-solar-cycle-25-peak/

21. (PDF) EVOLUTION OF CHANGES IN THE STRUCTURE OF THE SOLAR CORONA WITH THE PHASE OF SOLAR ACTIVITY - ResearchGate, https://www.researchgate.net/publication/408248638_EVOLUTION_OF_CHANGES_IN_THE_STRUCTURE_OF_THE_SOLAR_CORONA_WITH_THE_PHASE_OF_SOLAR_ACTIVITY

22. What Is the Sun's Corona? | NASA Space Place – NASA Science for Kids, https://spaceplace.nasa.gov/sun-corona/en/

23. SwRI-led eclipse projects shed new light on solar corona | Southwest Research Institute, https://www.swri.org/newsroom/press-releases/swri-led-eclipse-projects-shed-new-light-solar-corona

24. UH eclipse research finds turbulent times in the Sun's corona - University of Hawaii System, https://www.hawaii.edu/news/2026/02/17/eclipse-research-suns-corona/

25. NATE: Science that brings people together under the eclipses, https://www.iac.es/en/projects/nate-science-brings-people-together-under-eclipses

26. The “NATE” educational program on the August eclipse was presented in Palencia, https://www.iac.es/en/outreach/news/nate-educational-program-august-eclipse-was-presented-palencia

27. Reconstructing an Artemis II Solar Eclipse with SunPy, https://uksolphys.org/education-and-public-outreach/reconstructing-an-artemis-ii-solar-eclipse-with-sunpy/

28. Atmospheric changes from solar eclipses - Royal Society Publishing, https://royalsocietypublishing.org/rsta/article/374/2077/20150217/40810/Atmospheric-changes-from-solar-eclipsesAtmospheric

29. The effect of the total solar eclipse of 29 March 2006 on meteorological variables in Greece - Copernicus ACP, https://acp.copernicus.org/articles/7/5543/2007/acp-7-5543-2007.pdf

30. Surface temperature drop at various sites of different obscuration... - ResearchGate, https://www.researchgate.net/figure/Surface-temperature-drop-at-various-sites-of-different-obscuration-during-the-eclipse_tbl2_26634540

31. Regression-based gap-filling methods show air temperature reductions and wind pattern changes during the 2019 total eclipse in Chile - PMC, https://pmc.ncbi.nlm.nih.gov/articles/PMC9095667/

32. Diagnosing eclipse-induced wind changes | Proceedings A | The Royal Society, https://royalsocietypublishing.org/rspa/article/468/2143/1839/83389/Diagnosing-eclipse-induced-wind-changesDiagnosing

33. Solar eclipse caused bow waves in Earth's atmosphere - MIT News, https://news.mit.edu/2018/solar-eclipse-caused-bow-waves-earths-atmosphere-0119

34. Atmospheric gravity waves observed in Brazil on 14 October 2023 - EGUsphere, https://egusphere.copernicus.org/preprints/2026/egusphere-2025-6571/egusphere-2025-6571.pdf

35. On the detection and attribution of gravity waves generated by the 20 March 2015 solar eclipse - PMC, https://pmc.ncbi.nlm.nih.gov/articles/PMC5004052/

36. Investigation of the Ionospheric Effects of the Solar Eclipse of April 8, 2024 Using Multi-Instrument Measurements - MDPI, https://www.mdpi.com/2073-4433/16/2/161

37. Sky color near the horizon during a total solar eclipse - Optica Publishing Group, https://opg.optica.org/ao/fulltext.cfm?uri=ao-14-12-2831

38. Extended visual range during solar eclipses - Optica Publishing Group, https://opg.optica.org/ao/upcoming_pdf.cfm?id=315615

39. One day, two spectacular sky events: Solar eclipse and Perseid meteor shower to align on August 12, 2026, https://timesofindia.indiatimes.com/science/one-day-two-spectacular-sky-events-solar-eclipse-and-perseid-meteor-shower-to-align-on-august-12-2026/articleshow/132259431.cms

40. Meteor Showers | Scott's Astronomy Page, https://scottsastropage.com/category/meteor-showers/