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Aurora is also known as the northern lights. This is caused by collisions between fast moving particles from space and the oxygen and nitrogen gas in our atmosphere. The electrons are in the magnetosphere, which is the region of space that is controlled by the magnetic field of Earth. As these particles fall into the atmosphere, they impart energy to oxyen and nitrogen molecules and they become excited. As these particles return to a normal state, they release small bursts of energy in the form of light, called photons.
https://pwg.gsfc.nasa.gov/polar/telecons/archive/PR_E-PO/Aurora_flyer/aurora-flyer_p2.doc.pdf

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A solar flare is a sudden, rapid, and intense variation in brightness. A flare occurs when built up magnetic energy is suddenly released. When this happens, radiation is released across the entire electromagnetic spectrum.
https://hesperia.gsfc.nasa.gov/sftheory/flare.htm

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Solar prominence is a large, bright feature that extends from the surface of the Sun. A prominence forms in about 24 hours and may persist for many months and can be thousands of miles long. The looped material is plasma, which is a gas composed of electrically charges hydrogen and helium.
https://www.nasa.gov/content/goddard/what-is-a-solar-prominence

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Sunsports are cooler areas on the surface of the sun that appear darker in color. The temperature of the sunspots is about 3,500 degrees C compared to the photospheres temperature of 5,500 degrees C. Sunspots are cause by interactions with the Sun's magnetic field, which is not fully understood. They occur over regions with intense magnetic activity. When energy is released, solar flares and a big storm erupts, call a coronal mass ejections, will erupt from sunspots.
https://www.space.com/14736-sunspots-sun-spots-explained.html

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The Corona is the outer atmosphere of the Sun. It is visible during total eclipses, and seems to give the Sun a white crown. Many features can be seen in the corona including streamers, plumes, and loops, which can change from each eclipse. The shape of the corona changes with the sunspot cycle.
https://solarscience.msfc.nasa.gov/corona.shtml

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The chromosphere is an irregular layer that is located above the photosphere. The temperature here ranges from 6,000 degrees C to 20,000 degrees C. Because of the higher temperatures, hydrogen emits light that have a red color, which is an H-alpha emission. This is where the chromosphere gets its name, color-sphere.
https://solarscience.msfc.nasa.gov/chromos.shtml

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The photosphere is the visible part of the Sun that everyone is mostly familiar with. This is not a solid surface, since the Sun is just a ball of gas. On the photosphere you can see dark sunspots, bright faculae, and granules. The flow of the photosphere can be measured using the Doppler effect. The measurements can reveal more features such as supergranules, large scale flows, and a pattern of waves. The rotation of the sun can be detected by observing the motion of sunspots.
https://solarscience.msfc.nasa.gov/surface.shtml

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This is the outer-most layer of the interior Sun. The temperature here is about 2,000,000 degrees C, and is cool enough for ions such as carbon, nitrogen, oxygen, calcium, and iron to hold onto their electrons. This makes the material more opaque, causing it to be harder for radiation to get through, trapping the heat and making the fluid unstable and even boil.
https://solarscience.msfc.nasa.gov/interior.shtml

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This zone extends from the outer edge of the core to the convection zone. This is where most of the energy that is created by the core is carried by light (photons) that bounces off particles through the radiative zone. Photons take about a million years to finally reach the inerface layer due to the rapid bouncing between particles. The density ranges from 20 grams per centimeter cubed to 0.2 grams per centimeter cubed and the temperature ranges from 7,000,000 degrees C to 2,000,000 degrees C.
https://solarscience.msfc.nasa.gov/interior.shtml

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The core of the Sun is where nuclear reactions consume hydrogen and helium. The reactions release energy that leaves the surface as visable light. The temperature of the core is about 27,000,000 degrees F, with a density of about 150 grams per centimeter cubed.
https://solarscience.msfc.nasa.gov/interior.shtml