PROJECT: HELIOS V2

SOLARIS

A cinematic exploration into the thermonuclear core of our home star and the interactive flow of its plasma fields.

SCROLL TO ORBIT

CORE TEMP 15,700,000 K

RADIATION LEVEL 3.8 × 10²⁶ W

SOLAR FLUX INDEX 142.7 SFU

THERMONUCLEAR CORE

At the sun's heart, gravity compresses hydrogen into helium under pressures of 260 billion atmospheres. Every second, 600 million tons of hydrogen fuse, generating pure photons that take 100,000 years to reach the surface.

CORE ACTIVITY

STABLE

CONVECTION FIELDS

Giant boiling cells of plasma rise and fall like liquid metal. Heated from below, cells the size of continents bubble up to the surface, cool, and sink back down, generating magnetic field loops that breach the solar atmosphere.

CONVECTION CELLS

9,420 / MIN

CORONAL LOOPS

Glowing arches of plasma trace out magnetic paths, soaring thousands of miles into space. These hot structural loops contain gas superheated to 1,000,000 Kelvin, radiating heavily in extreme ultraviolet wavelengths.

MAGNETIC TENSION

4.2 TESLA

HELIOSPHERIC SHIELD

The solar wind expands outward in a bubble of charged particles, encapsulating all planets in our solar system and shielding us from intense interstellar cosmic radiation. It represents the Sun's final line of cosmic domain.

SHIELD BOUNDARY

120 AU

LIVE SIMULATION

THE SOLAR WIND

Interact with the stream of charged particles flowing from the sun. Hover to bend the magnetic lines. Click to release coronal mass energy and disperse particles.

PARTICLE COUNT 12,000

VELOCITY 450 KM/S

INTERACTION MODE MAGNETIC DEFLECTION

SOLAR ARCHIVES

PHENOMENON CATALOG

SOLAR FLARES

Sudden flashes of brightness near the sun's surface releasing equivalent power of billions of megatons of TNT.

EXPAND ARCHIVE

SOLAR FLARES

A solar flare is an intense localized eruption of electromagnetic radiation in the Sun's atmosphere.

Flares occur in active regions and are often, but not always, accompanied by coronal mass ejections, solar particle events, and other solar phenomena. The radiation is emitted across virtually the entire electromagnetic spectrum, from radio waves to gamma rays. They are powered by the sudden release of magnetic energy stored in the corona.

ENERGY RELEASE: 10²⁵ Joules

SPEED OF EMISSION: Speed of Light

IMPACT TIME TO EARTH: 8.3 Minutes

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AURORA BOREALIS

Celestial light displays occurring at high-latitude regions, triggered by solar particles colliding with Earth's magnetosphere.

EXPAND ARCHIVE

AURORA BOREALIS

The Northern Lights are natural light displays in Earth's sky, predominantly seen in high-latitude regions.

Auroras are the result of disturbances in the magnetosphere caused by solar wind. These disturbances alter the trajectories of charged particles in the galactic wind, cosmic rays, and solar wind, causing them to precipitate into the upper atmosphere, where they ionize and excite atmospheric constituents, emitting light of varying colors.

PRIMARY COLORS: Green, Violet, Red

ALTITUDE RANGE: 80km to 640km

TRIGGER: Geomagnetic Storms

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CORONAL HOLES

Areas where the Sun's corona is colder and darker, letting high-speed solar wind escape easily into interplanetary space.

EXPAND ARCHIVE

CORONAL HOLES

Temporary regions of lower-density plasma where magnetic field lines open up directly into space.

Because these magnetic lines do not loop back to the solar surface, solar plasma can flow outward freely, escaping as high-speed streams of solar wind. This wind causes geomagnetic activity when it collides with Earth. They look darker because they contain less hot material.

WIND VELOCITY: 800 KM/S

TEMPERATURE DIFF: -500,000 K

LIFESPAN: Weeks to Months

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