upward in the bright cell centers and downward around the darker edges.
b
Two pieces of evidence for solar convection are the presence of granules on the solar surface, which are small convection cells visible in the photosphere, and solar oscillations caused by the motion of convection currents beneath the surface, which can be measured through helioseismology.
The grainieness is caused by convective cells at the sun's sufrace. Hooter material rises up at the centers of these "grains" (called granules) while less hot material sinks around their edges. Each granule is several hundred miles across.
The bubbling characteristic of the photosphere is called solar granulation. These granules are caused by the convective motion of plasma beneath the surface of the Sun, creating cells of rising hot plasma and sinking cooler plasma that appear as granules on the photosphere.
The surface of the sun is not actually grainy but i will give you a little insight into why it looks like that. If you have ever lit a large fire and let is burn down a little, when you look at the embers or deeper into the fire, you can see different colours, ranging from white through yellow, orange, red to black with varying degrees and shades. The Sun is similar to this but on a much more massive scale, when a snap shot is taken its looks grainy because of all the variations, but if you saw a motions movie of the suns surface it is an undulating mass of colours.Look at the related source videos and links below for comparison.
b
Two pieces of evidence for solar convection are the presence of granules on the solar surface, which are small convection cells visible in the photosphere, and solar oscillations caused by the motion of convection currents beneath the surface, which can be measured through helioseismology.
The grainieness is caused by convective cells at the sun's sufrace. Hooter material rises up at the centers of these "grains" (called granules) while less hot material sinks around their edges. Each granule is several hundred miles across.
The bubbling characteristic of the photosphere is called solar granulation. These granules are caused by the convective motion of plasma beneath the surface of the Sun, creating cells of rising hot plasma and sinking cooler plasma that appear as granules on the photosphere.
The surface of the sun is not actually grainy but i will give you a little insight into why it looks like that. If you have ever lit a large fire and let is burn down a little, when you look at the embers or deeper into the fire, you can see different colours, ranging from white through yellow, orange, red to black with varying degrees and shades. The Sun is similar to this but on a much more massive scale, when a snap shot is taken its looks grainy because of all the variations, but if you saw a motions movie of the suns surface it is an undulating mass of colours.Look at the related source videos and links below for comparison.
Churning Motions
A solar granule is typically around 1,500 kilometers (about 930 miles) in diameter. These granules are the tops of convective cells in the solar surface where hot plasma rises and cool plasma sinks, creating the granular pattern seen on the Sun's photosphere.
Granulation on the surface of the Sun is caused by convection currents carrying hot plasma from the interior to the surface. These rising currents of hot plasma create bright cells of gas at the surface, which appear as granules. The motion of these granules is evidence of the convective nature of the Sun's outer layers.
The surface of the sun, known as the photosphere, has an average temperature of about 5,500 degrees Celsius and is covered in granules caused by convection currents. It also exhibits features like sunspots, faculae, and solar flares.
The total solar irradiance would not necessarily increase with an increase in sunspot number. Sunspots are dark spots on the sun's surface that are cooler than the surrounding areas, so they can actually reduce the overall energy output of the sun.
sunspots prominence solar flares solar winds
The spectrum of a solar prominence reveals information about the elements present in the gas, the temperature, density, and motions of the material within the prominence, as well as magnetic fields influencing its behavior. By studying the spectrum, scientists can gain insights into the physical properties and processes occurring in solar prominences.