A Spiral Galaxy

More and more is being learned about the Kuiper Belt showing us that it is an interesting part of our galaxy that may help us better understand how our solar system was formed.

To explain the change, scientists have come up with two possible hypotheses. The first attributes theformatioan of the oval galaxies to the a merging event, in which two disc-shaped clusters that happen to move to close to each come together due to gravity. The other explanation relates to stars in a “round, lfat galazxy, migrate towards the core to produce the same rough oval.

Stars start off as clouds of gas that are usually in the spinning “arms” of a galaxy

According to the International Astronomical Union (IAU) to classify an object as a planet it must have three qualities. One it must orbit a Sun or Star of some kind. Second it must big enough for gravity to compress it into a big round ball. And lastly it must be big enough to pull neighboring objects into the planet itself or sling-shot them around the planet and shoot them off into outer space. The place for my planet is in the Triangulum Galaxy. The Triangulum Galaxy is a spiral galaxy about 2.7 million light years (25761569076837520000km)away from Earth. The solar mass of the Triangulum Galaxy is 50 billion Mʘ (standard unit of mass in Astronomy). This galaxy has about 40 billion stars which is 1/5th of how many there are in the Milky Way Galaxy. And 1/25th 's of the Andromeda Galaxy. The name of my planet is Frigusodayin (Cold Air)(Latin, Armenian). The first rule of classifying a planet states that it must orbit a Sun or Star. The Sun my planet will orbit is called WASP-56. Some properties of WASP-56 are that this star has an apparent magnitude of 11.48. Apparent magnitude is the brightness of an object as seen from Earth. The higher the apparent magnitude the brighter it is (Our Sun 's is 26.7). This star is a G6 star which is part of the G-Type main-sequence star group. The G-Type main-sequence star is a main sequence star of spectral type G and luminosity level V. These types of stars have about 0.8 to 1.2 solar masses. Solar masses being the mass of a sun or star

Curtis correctly noted that spectral lines could be seen within the spiral nebulae, and that they were generally consistent with the nebulae in the form of large assembled star clusters. These clusters supported Curtis's argument that these were in fact stellar systems, which are comparable to our Milky Way

Texture: It feels like a wash sponge,but a little more softer and kind of gooey.

The autumn constellations Andromeda and Perseus, along with Cetus, Pegasus, Cassiopeia and Cepheus, are richly intertwined in mythology, but are vastly diverse in the objects they present to astronomers. While Perseus lies along the Milky Way, and offers many dazzling open star clusters and diffuse nebulae, Andromeda lies away from our galaxy's plane, and introduces us to the inhabitants of intergalactic space. Some of the finest celestial objects reside in these constellations, and it is well worth braving cool autumn nights to observe them.

Parenago 1802, a member of the ∼1 Myr Orion Nebula Cluster, is a double-lined, detached eclipsing binary in a 4.674 d orbit, with equal-mass components (M2/M1=0.985±0.029). Here we present extensive V IC JHKS light curves spanning ∼15 yr, as well as a Keck/HIRES optical spectrum. The light curves evince a third light source that is variable with a period of 0.73 d, and is also manifested in the high-resolution spectrum, strongly indicating the presence of a third star in the system, probably a rapidly rotating classical T Tauri star. We incorporate this third light into our radial velocity and light curve modeling of the eclipsing pair, measuring accurate masses (M1=0.391±0.032, M2=0.385±0.032 M⊙), radii (R1=1.73±0.02, R2=1.62±0.02 R⊙), and temperature ratio (Teff,1/Teff,2=1.0924±0.0017). Thus the radii of the eclipsing stars differ by 6.9±0.8%, the temperatures differ by 9.2±0.2%, and consequently the luminosities differ by 62±3%, despite having masses equal to within 3%. This could be indicative of an age difference of ∼ 3 × 105 yr between the two eclipsing stars, perhaps a vestige of the binary formation history. We find that the eclipsing pair is in an orbit that has not yet fully circularized,

Oh dreamer, gone are the days your eyes refused to stop kissing the curiosity that ignited within the atoms of outer space.

One astronomer, named Harlow Shapley, believed that the Milky Way, which is the region of space in which our planet is located, was much larger than previously thought. However, he thought that because it was so big, there were no other regions of space similar to our Milky Way. Another astronomer, named Heber Curtis, believed that the Milky Way was much smaller, but that there were other regions of space similar to it. Shapley ended up being right that the Milky Way was much larger than previously estimated, however, he was wrong about it being the only region of space, also known as a galaxy. Curtis was correct that there were other regions of space, or galaxies, other than our Milky Way.

Simulations of galaxy formation based on the Lambda Cold Dark matter (ΛCDM) cosmological model predict that a large galaxy such as the Milky Way should have many (~ 200) dwarf satellite galaxies. However, only about 20 or 30 have been identified. Where are the rest? Warm dark matter, constituting of sterile neutrinos, is lighter and since dwarf galaxies consisting mainly of dark matter are so difficult to find by visible light, there could be enough of them to reconcile the large number of dwarf galaxies that simulations predict to exist with the small number actually observed. We are looking for a weak unidentified emission line at E = (3.55−3.57) ±0.03 keV in a stacked XMM-Newton spectrum of Dwarf galaxies, which are the satellite galaxies of our Milky Way.

The Orion Nebula contains one of the brightest star clusters in the night sky. With a magnitude of 4, this nebula is easily visible from the Northern Hemisphere during the winter months. It is surprising, therefore, that this region was not documented until 1610 by a French lawyer named Nicholas-Claude Fabri de Peiresc. On March 4, 1769, Charles Messier inducted the Orion Nebula, M42, into his list of stellar objects. Then, in 1771, Messier released his list of objects for its first publication in Memoires de l'Academie.1

The stage was set for a “Great Debate” that occurred at the National Academy of Sciences in Washington in 1920. At issue were the fuzzy “spiral nebulae” (which today we call galaxies): Were they close enough to be part of our own Milky Way, or were they sufficiently distant to be whole galaxies unto themselves? Shapley held that, given that his research had revised an increase in theinupward the size of the Milky Way, the spiral nebulae must be part of our own Galaxy. His opponent, Heber Curtis of California’s Lick Observatory, while incorrectly rejecting the great size of our Galaxy, correctly argued that the spirals were removed aggregates of stars similar to the Milky Way. Both men presented other scientific arguments supporting their views,

Have you ever wondered how it would feel to experience life on a space mission? Now you have the opportunity to have gravity pull you in and to come along through a journey into space on Galaxy Impact! You’ll be faced with top speeds of 75 miles per hour with an overall time of 60 seconds on Galaxy Impact. This ride features the newest technology including several virtual reality screens; therefore, simulating an incredibly real scenario. Jump onto our surround sound cars that hold 32 people at a time. In these inverted seats you’ll be able to pull the harness over and down until it can’t possibly continue any further, and as a result, you’ll be immaculately secure. With the design of these cars, you will feel as if you are floating

A galaxy, also called a nebula, consists of billions of stars, interstellar gas, dust, and dark matter which are all bound to form a massive cloud in which we live in. Although it cannot be very well explained, dark matter makes up at least 90% of a galaxy’s mass.