Journey To The Edge of The Universe [PDF]

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Journey to the Edge of the Universe National Geographic introduces the first precise non-stop journey from Earth to the Galaxy center with a single unbroken image of spectacular CGI technology. ‘Journey to the Edge of the Universe' is a film on National Geographic and the Discovery Channel, a documentary broadcast. It represents a simulated voyage from Land to the Universe's edge. Establishing images captured from the Hubble space telescope Journey to the Universe explores science and history in the solar system behind faraway celestial bodies (Ananthaswamy 2010). This spectacular and epic journey through the cosmos leads us to the closest stars, nebulas, and galaxies, from the Earth, from the night sky and our adjacent planets, and from our solar system to the far end of the Universe. The documentary uncovers what we would discover if we could travel across our Universe. As Neil Armstrong's footsteps were still screened at the moon, the notable rise onto Mercury via the brightly illuminated Venus, which was almost entirely made of iron, might be the left remains of a far more giant planet. Mars is an outer planet with tornadoes, volcanoes, and canyons, as opposed to anything seen in the world, while the always-present Red tempest of Jupiter is three times the size and lasting centuries. We find Land that closely resembles Earth when reaching the moon of Saturn Titan, but the rivers, oceans, and lakes of Titan are made of water but liquid methane (Ananthaswamy 2010). Is life here able to exist? Over 90 trillion kilometers from Earth, spectators enter into a star system in Epsilon Eridani, where our solar system's form is similar to forming a spectacular ring of dust and ice 4,5 billion years ago. Gliese 581, around the same era as our Sun, is just the perfect distance to life with a biosphere. Throughout those wolves, one can see great stars that bring glow and perhaps life to the Universe, deep in the pillars of creation.



Formation of Stars and Determining Masses and Sizes of Stars



A star is an excessive entity composed of an individually gravitated, luminous plasma spheroid. The Sun is the closest star in the world. Many other stars appear naked at night; however, they occur as fixed light points in the sky due to their massive distance from Earth. The leading stars are clustered into celestial bodies and asterisms, and most of the shining stars have names of their own. Stars have not always been around, like our own Sun (Reina-Campos et al., 2019). Stars have come into existence and die for thousands or billions of years. When dust and gas regions collapse in the Galaxy due to gravity, stars form. Stars would not develop without such dust and gas. These stars develop from a buildup of gas and powder that crumbles the force of gravity and becomes stars. The star-building process takes about a million decades from the beginning of the gas cloud until the principal is built and glows like the Sun. The material remaining from the beginning of the star is utilized to produce planets and objects orbiting the central star. It is challenging to observe star formation as the residue is not translucent to visible light. However, these dim stellar nurseries can be observed on radio waves because waves of radio travel freely to our radio observatories and ourselves. Measuring fundamental stellar physical parameters, particularly the mass and radius of our stellar evolution, is paramount. However, different physical prescriptions currently anticipate different radii and temperatures in stellar models, such as winds, mass-loss and convective overflow in the same mass, age, and metallicity of the stars. Similarly, even if they have the same weight and total metal abundance, stars with different elementary abundance ratios will have substantially



different pathways (Stassun et al., 2017). Thus, it is essential to place specific restrictions on these parameters to limit the wide variety of possible stellar development models. The stars' volumes can be obtained by analyzing the binary-star orbit—two stars around a prominent mass center. Two stars can be observed independently in a telescope in visual binaries, while only two stars can be observed in the spectroscopic binary ((Stassun et al., 2017). The stellar masses vary between 1:12 and 100 times as much as the Sun's size (in uncommon instances, they range 250 times as much as the volume of the Sun Sun-brown dwarfs called objects with the mass from 1:12 to 1:100. Planets are objects that cannot produce nuclear reactions. In most cases, the most prominent stars are also luminescent, and this causative link is called the relationship between mass-luminosity.



Galaxies, Cosmology, Large Scale Structure How big is the Milky Way in light years? The Milky Way is around 1,000,000,000,000,000,000 km (around 100,000 light years away or around 30 kpc) wide. How massive is the Milky Way in solar masses? Astronomers reported that in March, in a radius of approximately 129,000 light-years, the Milky Way galaxy volume amounted to 1.5 billion solar masses, over twice as many as previously determined, and about 90% of the Galaxy's mass was dark. What type of Galaxy is the Milky Way? Spiral galaxy. The Milky Way is an enormous collection of stars, pollution, and gas. It is called a galaxy of spirals because it would appear like a whirling pinwheel if you can see it from the



edge or the ground. The Sun is situated about 25,000 light-years from the galactic center in one of the vortex galaxies' arms. Which spiral arm of the Milky Way is our solar system in? The Orion Arm. The Orion Arm is a small vortex branch of the Milky Way galaxy with a length of 3,500 light-years (1,100 pars.) and about 10,000 light-years (3,100 pars.) a galaxy, including Earth. How long does it take the Sun to orbit the Milky Way? 225–250 million years approximately. How far out from the center of our Galaxy is our solar system? 25,000 light-years approximately. Around 25,000 light-years away from galactic and 25,000 light-years far from the border is the Galaxy (and Earth). We would have been the point about halfway between center and edge if you considered the Andromeda Galaxy as a massive record. Why can’t we take a picture of our Milky Way galaxy and see its complete spiral shape as we have done of the Andromeda and other distant galaxies? We cannot take pictures from the edge "above" the Galaxy because we are inside the Milky Way. Only the system of the edge-on Milky Way can be seen from within instead. What is the Local Group (i.e. Local Cluster)? The Local Group comprises the Milky Way galaxy group. The Andromeda Galaxy and its antenna systems form one lobe, and the Andromeda and its sates constitute the other. It consists of two catalogs of galaxies of "dumbbell" shape. How big is the Local Group in light years? Five million light-years How many galaxies are in the Local Group?



Thirty Galaxies. What supercluster is the Local Group in? The Supercluster of Virgo Describe the Hercules Cluster of galaxies (i.e. distance, number of galaxies, and in which supercluster is it?) Hercules' Cluster comprises approximately 200 galaxies in the Hercules constellation, around 500 million light-years away. Rich in spiral galaxies, it has many universes that interact. The cluster is a component of Hercules' broader supercluster, which itself forms a portion of the much wider superstructure of the Great Wall. Describe the Virgo Cluster of galaxies (i.e. distance, number of galaxies, and in which supercluster is it?) Virgo Cluster is a vast galaxy cluster centered in the Virgo Constellation with a distance of (16.5 ± 0.1 Mpc) 53.8 ± 0.3 Mly. The collection is the core of a large Virgo Supercluster, of whatever group (including our Milky Way galaxy) the local group, comprising about 1,300 galaxies (and probably up to 2000). What is the Virgo Supercluster? The Virgo Supercluster is a mass of galaxies that contains the Virgo Cluster and the Local Supercluster group that includes the Milky Way and Supernovae galaxies. At least 100 groups and groups of galaxies are within 33 megaparsecs of diameter. How big is the Virgo Supercluster in light years? Fifty-five million light-years How many clusters are in the Virgo Supercluster? One thousand five hundred clusters.



What larger supercluster is the Virgo supercluster part of? Supercluster of Laniakea What are voids and what are filaments in the large-scale structure of the Universe? The most significant known universe structures are galaxy filaments. It is Massive, thread-like, typically 50 to 80 megaparsecs long (or 200 to 500 million light-years) form borders between considerable voids in the Universe. Cosmic voids are vast space between filaments, which contain only a few or no galaxies, the most significant structures in the Universe. Voids are typically from ten to a hundred megaparsecs in diameter, and enormous voids called super voids, defined by the absence of rich superclusters. What is the Big Bang? How many years ago do astronomers believe it happened? also, Write out this number in scientific notation? Researchers, astronomers, and cosmologists have agreed to the fact that the Universe, as we know, it has been formed in a massive explosion that has created not only the majority but also the physical laws governing our ever-expanding cosmos. That is the Big Bang Theory. The big bang theory says that all the past and current material in the Universe existed simultaneously approximately 13.8 billion years ago. How old do astronomers think the Universe is? 13.8 billion years. How big is the entire observable Universe? There is an estimated radius of around 46.5 billion light-years in the observable Universe, with a diameter of approximately 28.5 gigaparsecs equivalent to 880 yottameters. Why is the size of the Universe in light years a bigger number than the age of the Universe in years?



When the world first "stopped" about 13.75 billion years ago, space-time itself started to expand at velocities faster than light speed. This time, known as inflation, is vital to explain far more than the size of the Universe.



References Ananthaswamy, A. (2010). The Edge of Physics: A Journey to Earth's Extremes to Unlock the Secrets of the Universe. HMH. Reina-Campos, M., Kruijssen, J. D., Pfeffer, J. L., Bastian, N., & Crain, R. A. (2019). Formation histories of stars, clusters, and globular clusters in the E-MOSAICS simulations. Monthly Notices of the Royal Astronomical Society, 486(4), 5838-5852. Stassun, K. G., Corsaro, E., Pepper, J. A., & Gaudi, B. S. (2017). Empirical accurate masses and radii of single stars with TESS and Gaia. The Astronomical Journal, 155(1), 22.