All About The Cartwheel Galaxy Analysis

In line with its already established reputation, Hubble (http://hubblesite.org/the_telescope/) , along with the Herschel (https://herschel.jpl.nasa.gov/) space telescope, was recently used to peer back in time in order to provide astronomers with an idea of how galaxies within the vast expanse of the Universe have undergone dramatic trasnforsatioms over the last eight billion years ro so.

Scientists using NASA's Hubble Space Telescope have discovered that the i halo of gas enveloping the Andromeda galaxy, our nearest massive neighbor, is about six times larger and 1,000 times more massive than previously measured. The dark, nearly invisible halo stretches about a million light-years from its host galaxy, halfway to our own Milky Way galaxy. One of the most common types of galaxies in the universe.

Mayall’s object (also known as Arp 148) is the stunning result of an encounter between two galaxies resulting in a ring-shaped galaxy and a long-tailed companion, located almost 465 million light-years away within the constellation Ursa Major. The pair extends across 80 thousand light-years.

Cygnus A is a radio galaxy, and one of the strongest radio sources in the sky. It was discovered byGrote Reber in 1939. In 1951, Cygnus A, along with Cassiopeia A, and Puppis A were the first "radio stars" identified with an optical source. Of these, Cygnus A became the first radio galaxy; the other two being nebulae inside the Milky Way.[3] In 1953 Roger Jennison and M K Das Gupta showed it to be a double source.[4] Like all radio galaxies, it contains an active galactic nucleus.

A planet located further from the Sun rotates slower, following the curve labelled A in the graph below. However, Vera Rubin showed instead that stars in a spinning galaxy followed curve B. This was as if the stars were not rotating around the visible centre of the galaxy but around many unknown centres, all providing additional

Corona Borealis Galaxy Cluster (Abell 2065) is highly concentrated with galaxies. About 400,000,000 galaxies are in this.

The solar nebula theory stated that the solar system started with a grain of dust. From that grain of dust, our solar system expanded through three processes; condensation, accretion, and gravitational collapse. Through condensation particles add matter from gas. In the process of accretion, particles stick together forming masses. These masses collided at low velocities creating protoplanets. The larger the protoplanet, the greater the gravitational pull, thus attracting more matter growing larger. The third process, gravitational collapse occurred when gas from the nebula accumulated quickly.

You have probably heard about galaxies, whether it was in school, a book, a television show, or movie, you've most likely heard about them. If you're wondering, "what exactly are galaxies?" fret not, friend, for I will help you figure out this question.

The Milky Way was first determined by Galileo Galilei with his telescope in 1610. Thanks to Galileo because before the use of his telescope, the formation of stars was a confusion to most astronomers. With the use of a telescope, Galileo studied the Milky Way and discovered that it was composed of a huge number of faint stars. There was a confusion on stars. Until 1920, astronomers thought that all stars were contained inside of the Milky Way. After Galileo’s telescope, other astronomers became more creative on understanding that the Milky Way is just one of many galaxies now known to be billions. The Milky Way contains more than one planet like the solar system which is located within the disk. The solar system is located on the constellation of “gas and dust called the Orion Arm” (Wikipedia contributors). We are located in the Orion arm of the Milky Way

In our universe, collisions or interactions between galaxies are often observed and can be predicted too. This colossal phenomenon occurs due to the large gravitational fields of the galaxies which attract other galaxies or are attracted by the fields of the other galaxies. The force of gravity is exerted when two galaxies are extremely close to each other. Near misses and crashes between any two galaxies are generally referred to as “interactions”. Collision may lead to merging and the galaxies may also bend out of shape, which is the case in most of the interactions. Dr Chris Power of International Centre for Radio Astronomy Research explained, ‘As the galaxies come together, mutual gravity leads to gas and stars being flung out in the form of tidal arms’. Some major galaxy interactions which happened in the past were between the Mice galaxies and the Antennae galaxies. The collision between the former went up to the second

"As galaxies fall through these larger halos, the superheated intergalactic plasma between them removes their gas in a fast-acting

To explain how the origins of galaxies and stars, we must go back to the previous threshold: the big bang. Gravity was one of the four fundamental forces that came from the big bang, and as a result, plays a central role in the formation of stars and galaxies as it has the ability to change something else. Gravity holds the ability to garner more mass when there is more mass involved and vice versa, this leads to a different effect of different areas depending on mass. Like stars, stars begin very small, just particles in vast clouds of dust and gas. These ‘nebulae’ remain cold for ages until an external force come through and causes a disturbance. As the force moves through the cloud, particles collide and clump together. These clumps then gain more mass, and as I mentioned above, a stronger gravitational pull, attracting, even more, particles. as these clumps grow, the center grows denser and hotter. This is a long process, it takes a few million years before it moves onto the next stage: the protostar. This process will continue as the protostar grows until the center becomes too hot, then its hydrogen atoms begin to fuse which produce an influx of helium and energy. This reaction is called nuclear fusions, and while it may sound as the changing factor, but this outflux of energy is still weaker than the inward pull of gravity. The turning point of a protostar into a star is when there is too much material being fed into the protostar. Is enough mass increases into the

NGC 1672, a barred spiral galaxy located in the direction of the southern constellation Dorado lies more than 60 million light-years away. This is a spiral galaxy that’s composed of stars in a central bar-shaped design. NGC 1672 is a member of the Seyfert galaxy, which was named after famous astronomer, Carl Keenan Seyfert, who extensively studied galaxies with active nuclei in the 1940s. In the middle of NGC 1672’s galaxy, it contains a high surface brightness bar from which four wire-like spiral arms extend outwards. This galaxy’s symmetrical look is mainly formed by the four extending arms of which are bordered with the most spectacular dust lines that extend out from the center. Unlike the normal galaxies, NGC 1672’s arms do not fully spiral all the way to the center. The arms are actually connected to both ends of a linear-like bar of stars encompassing the nucleus. In fact, the arms extending from the middle of this galaxy is the main reason I was drawn to this image. The arms with the beautiful pinkish purple rays look like an Eastern Redbud blossoming in the months of April-May, which have always caught my eye since I was a little kid. Visible from the Southern Hemisphere, NGC 1672 shows extraordinary regions of star formations. Near the edges of this galaxy’s galactic bar, the greatest clustering of star formations can be found. The picture taken of NGC 1672 above was photographed with Hubble’s Advanced Camera for a survey in August of 2005. This image is composed

The prominent bar in the LMC suggests that it may have previously existed as a barred spiral galaxy.3 The LMC’s notably off-center bar was studied by Subramaniam and

The third and final type of galaxy is categorized as irregular because of their lack of global structure. These galaxies are basically all the odd-ones-out, because they cannot be defined as either elliptical of spiral. These galaxies usually have abounding amounts of interstellar dust, gas, and are home to a variety of younger and older stars. An interesting characteristic about these galaxies is the fact that they shine very bright, and also are among the smallest galaxies. Due to the fact that these galaxies are made up of so many different kinds,