# What Happens When You Zoom Into the Sun The scientific details of a virtual journey into the Sun's depths. - **Source:** [CNET (YouTube)](https://brifing.si/source/d98fed98-60b0-44b1-9469-4438fc7d13f9) - **Published:** 2026-08-23 - **Topic:** [Business](https://brifing.si/c/business) - **Original article:** - **On Brifing:** https://brifing.si/s/1ed34b6c-9937-4dd7-8372-50ea2c3a7ca9 ## The Sun's Layers The Sun consists of core, radiative zone, convective zone, photosphere, chromosphere, and corona from inside out. The core is where nuclear fusion occurs at 15 million °C. In the radiative zone, energy travels as photons. The convective zone is where energy transfer happens through convection currents. ## Photosphere and Visible Surface The photosphere is the yellow-orange surface we see, with temperatures around 5,500°C. Sunspots and solar flares can be observed here. Layers below the photosphere cannot be observed directly, only through indirect methods. This visible layer is about 500 km thick. ## Chromosphere and Corona The chromosphere lies above the photosphere, about 20,000 km thick with temperatures ranging from 4,000°C to 25,000°C. The corona is the Sun's outermost layer reaching 1-3 million °C, a phenomenon scientists still struggle to explain. These layers are visible during solar eclipses. ## Magnetic Field Effects The Sun's magnetic field affects all its layers. Tangled magnetic field lines cause solar flares and coronal mass ejections. These events can disrupt Earth's satellite systems and power grids. Sunspots are also manifestations of magnetic activity, appearing as cooler areas on the surface. ## Virtual Zoom Simulations Computer simulations allow virtual journeys into the Sun's inner layers. These models help understand nuclear fusion processes and energy transfer mechanisms. Data comes from NASA's Solar Dynamics Observatory and Parker Solar Probe missions. Such simulations advance our stellar physics knowledge. ## Solar Winds and Impacts Charged particles streaming from coronal holes form solar winds, reaching speeds of 1.6 million km/h. When interacting with Earth's magnetosphere, they create auroras. Intense solar storms can disrupt communication systems. The solar wind shapes the heliosphere, protecting us from cosmic rays. ## The Sun's Future Our Sun is midway through its life, with about 5 billion years of hydrogen fuel remaining. It will eventually expand into a red giant, potentially engulfing Earth. Finally, it will collapse into a white dwarf and slowly cool. This stellar evolution mirrors other similar-sized stars. ## Importance of Solar Research Understanding the Sun helps us comprehend other stars. Solar activity directly affects Earth's climate and technology. Space weather forecasts are crucial for satellite and astronaut safety. Solar energy technology development also benefits from this research, advancing renewable energy solutions. ## Sources covering this story - https://www.youtube.com/watch?v=ivjX5zVeSdA — --- _Summary written by Brifing from the original reporting. Copyright in the original article belongs to its publisher; read the full piece at the link above._