The chromosphere of the sun - high res photo.

The chromosphere is the thin middle layer of the Sun's atmosphere, located just above the visible surface (photosphere) and below the outer atmosphere (corona). It comes from the Greek word chroma, meaning color, because it shines with a bright red glow during total solar eclipses. The red color comes from glowing hydrogen gas, specifically the hydrogen-alpha (H-alpha) light wavelength. It extends roughly 2,000 to 4,000 kilometers (about 1,200 to 2,500 miles) above the solar surface. Unlike inner layers, it gets hotter as you move outward, rising from about 4,000 K near the bottom to 10,000 K (or higher) at the top. Possible to see/photograph: Spicules: Narrow, grass-like jets of plasma that shoot upwards from the bottom layer before falling back down.

Prominences and filaments: Huge, cool loops and clouds of gas held above the surface by magnetic fields. Visibility: It is normally hidden by the blinding brightness of the photosphere below, but it is visible during total solar eclipses or through special solar filters.

Photo taken with several photos stitched together as a high res photo of the sun.

Sunny Days

On sunny days, you want to take the opportunity to photograph the sun, which is quite active now with nice prominences on the edge of the sun and quite a lot of activity on the solar surface as well. All images from the Carpe Noctem Observatory and taken with a Ha solar filter.

The sun is the undisputed powerhouse of our solar system. Constantly fusing hydrogen into helium in its core, it radiates a staggering \(3.8 \times 10^{26}\) Joules of energy every single second. This output completely dwarfs human energy consumption, providing a nearly limitless engine for life on Earth

Solar Prominence

In solar physics, a prominence, sometimes referred to as a filament,[a] is a large plasma and magnetic field structure extending outward from the Sun's surface, often in a loop shape. Prominences are anchored to the Sun's surface in the much brighter photosphere, and extend outwards into the solar corona. While the corona consists of extremely hot plasma, prominences contain much cooler plasma, similar in composition to that of the chromosphere. Prominences form over timescales of about a day and may persist in the corona for several weeks or months, looping hundreds of thousands of kilometers into space. Some prominences may give rise to coronal mass ejections. Exact mechanism of prominence generation is an ongoing target of scientific research. A typical prominence extends over many thousands of kilometers; the largest on record was estimated at over 800,000 km (500,000 mi) long, roughly of solar radius. Photos taken back in 2022 using my Ha Solar filter and telescope.

Sun, Aurora and the Moon