The Red Giant The red giant is a star that has a large mass and heat

Diagram of planets This diagram shows the different sizes of planets and stars.

Blue Giant A blue giant is a giant blue star that is very hot and Also very great in mass.

NEBULAS These are some of the different nebulas in our universe. These nebulas are all very unique in their own way. Also they are very big

Atoms and Molecules These atoms and molecules are going through fusion

HERE IS THE AWSOME LOOKING BLACK HOLE !!!!!!!! BLACK HOLES ARE KNOWN TO FORM AFTER SUPER NOVA AND WE DO HAVE A FEW IN OUR UNIVERSE BUT NOT CLOSE ENOUGH TO US TO WERE WE WILL ALL DIE BY GETTING SUCKED IN BY ITS SWERRILING VORTEX OF DOOM HAHAHAHAHA!!!!!!!!!!!!!!!!!!!!!

WHITE DWARF White dwarfs are stars that are formed after the main sequence and also they look really cool cause they are bright. ROFLROFLROFL

Brown dwarf Brown dwarfs are very cool and are the size of a planet so yeah there kind of big.

PROTOSTAR A PROTSTAR IS A BABY STAR THAT IS FORMING INTO A BIG STAR AND ALSO IS KIND OF LIKE A FETUS.

MAIN SEQUENCE The main sequence is a continuous and distinctive band of stars that appear on plots of stellar color versus brightness. These color- magnitude plots are known as Hertzsprung- Russell diagrams after their co-developers, Ejnar Hertzsprung and Henry Norris Russell. Stars on this band are known as main- sequence stars or "dwarf" stars.

Hydrogen fusion In nuclear physics and nuclear chemistry, nuclear fusion is the process by which multiple like-charged atomic nuclei join together to form a heavier nucleus. It is accompanied by the release or absorption of energy, which allows matter to enter a plasma state.

Helium Fusion Helium fusion is a kind of nuclear fusion, with the nuclei involved being helium. The fusion of helium-4 nuclei (alpha particles) is known as the triple-alpha process, because fusion of just two helium nuclei only produces beryllium-8, which is unstable and breaks back down to two helium nuclei with a half life of 1×10 −16 to 2.6×10 −16 seconds. If the core temperature of a star exceeds 100 million kelvins (100 megakelvins), as may happen in the later phase of red giants and red supergiants, then a third helium nucleus has a significant chance of fusing with the beryllium-8 nucleus before it breaks down, thus forming carbon-12. Depending upon the temperature and density, an additional helium nucleus may fuse with carbon-12 to form oxygen-16, and at very high temperatures, additional fusions of helium to oxygen and heavier nuclei may occur (see alpha process).

Planetary nebula A planetary nebula is an emission nebula consisting of a glowing shell of gas and plasma formed by certain types of stars when they die. The name originated in the 18th century because of their similarity in appearance to giant planets when viewed through small optical telescopes, and is unrelated to the planets of the solar system. [ They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years. [

Black Dwarf A 'black dwarf' is a white dwarf that has cooled down enough that it no longer emits light.

Massive main sequence The more massive a main sequence star, the brighter and bluer it is. For example, Sirius, the dog star, located to the lower left of the constellation Orion, is more massive than the Sun, and is noticeably bluer. On the other hand, Proxima Centauri, our nearest neighbor, is less massive than the Sun, and is thus redder and less luminous.

Red Supergiant When all the hydrogen in the core of an intermediate- mass star has fused into helium, the star changes rapidly. Because the core no longer produces fusion energy, gravity immediately crushes matter down upon it. The resulting compression quickly heats the core and the region around it. The temperature becomes so high that hydrogen fusion begins in a thin shell surrounding the core. This fusion produces even more energy than had been produced by hydrogen fusion in the core. The extra energy pushes against the star's outer layers, and so the star expands enormously.

Supernova A supernova is an exploding star that can become billions of times as bright as the sun before gradually fading from view. At its maximum brightness, the exploded star may outshine an entire galaxy. The explosion throws a large cloud of dust and gas into space. The mass of the expelled material may exceed 10 times the mass of the sun. Astronomers recognize two types of supernovae -- Type I and Type II. Type I supernovae probably occur in certain binary stars. A binary star is a pair of stars that are close together and orbit about each other. A Type I probably occurs in binaries in which one of the stars is a small, dense star called a white dwarf. If the two stars are close enough to each other, the gravitational pull of the white dwarf draws mass from the larger companion. When the white dwarf reaches a mass about 1.4 times that of the sun, it collapses and then explodes.

Neutron Star A neutron star forms when a massive star explodes as a supernova, leaving behind an ultradense core. Most known neutron stars emit regular pulsations that are powered by rapid spins. Astronomers have found nearly 1,800 of these so-called pulsars in our galaxy. Pulsars have incredibly strong magnetic fields by Earthly standards, but a dozen of them — slow rotators known as magnetars — actually derive their energy from incredibly powerful magnetic fields, the strongest known in the universe. These fields can stress the neutron star’s solid crust past the breaking point, triggering starquakes that snap magnetic-field lines, producing violent and sporadic X-ray bursts.

Nasa.com & Wikipedia.com All this info is from wikipedia and Nasa.com