Formation Lab

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Astronomy

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Dec 6, 2023

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Abeyta – Kinnevy 1 Tearny Abeyta - Kinnevy AST 1110 October 10, 2022 Lab 6: Formation of the Solar System A. Time Periods a. Era 1: Phanerozoic i. In the Phanerozoic period, organisms rapidly expanded and evolved to cover all the available ecological niches. Continents drifted during the Phanerozoic, eventually forming Pangea, a single landmass that later disintegrated into the current continental landmasses (New World Encyclopedia).The development of plants with the ability to execute the photosynthetic system and, as a result, release unrestricted oxygen into the environment appears to have been the key to that amazing Phanerozoic expansion. Animals, in which energy transfers related to the process of breathing are vital, had not been able to grow because the atmosphere on Earth before that point contained small amounts of free oxygen. Earth gradually developed its current shape and physical characteristics during the Phanerozoic, including techniques like continental drift, mountain- building, and continental glaciation (Britannica). In light of the formation of the Earth's crust, the Phanerozoic Eon barely spans the last eight million years or thereabouts, yet its significance greatly outweighs this brief time span. The current state of the solar system predates that of earlier times. b. Era 2: Pre-solar nebula i. According to the nebular hypothesis, a piece of a huge molecular cloud was gravitationally forced to collapse, creating the Solar System

Abeyta - Kinnevy2 ( Geosciences ). The shards were around 1 parsec (3 and a quarter light- years) across whereas the cloud was about 20 parsec (65 light years) large. A new study suggests that the Earth's core is leaking helium 3, a rare isotope of helium gas. Since practically all helium-3 comes from the Big Bang, the gas leak provides support to the long-debated theory that Earth formed inside a solar nebula. The sun's birthplace was a molecular cloud formed by a vast collection of interstellar gas and dust that existed before the solar system. The gas began to condense and became increasingly denser as a result of the cold temperatures. With the help of a nearby stellar explosion, the densest portions of the cloud started to collapse due to gravity on their own, creating a vast number of protostars, which are newborn stars. As the young solar system continued to be compressed by gravity, a star and a disk of material, from which the planets would eventually form, were formed (Space). B. Forming the Planets a. A crucial component of the Solar System is the frost line. The frost line divides the Solar System in half. Below the frost line, it gets cold enough for volatiles to turn into ice grains. Examples of volatiles include water, ammonia, carbon dioxide, carbon monoxide, and methanol. The region below the frost line is heated by the Sun's radiation, which also breaks down the volatiles. They are then forced to exit the inner regions by the solar wind from the Sun. After they cross the frost line, they may become solid. As a result, the core is much drier and rockier while the surrounding cold areas are icier. All the rocky planets are below the frostline,

Abeyta - Kinnevy3 and all the gas giants are considerably below the mark, which causes the volatile components to condense and solidify due to a lack of suitable temperatures. b. Within the frost line, the surfaces that face the Sun are warm enough to melt or sublime icebergs, exposing granite like our Moon. In locations that are shaded or covered, such as the bottoms of deep craters, given the right combination of temperature and pressure, liquid water may endure, or ice may survive. Much like what we see on Earth. Like most outer solar system satellites, ice is stable outside of the frost line and can cling to most surfaces. The prominent outliers are once again the gas-covered large planets and Jupiter's moon, where water had been driven away by volcanic action. The bulk of surfaces' icy or rocky nature may, however, be reliably predicted by the frost line. When planetesimals include a volatile substance, such water, carbon dioxide, or methane, they will not be stable and evaporate, shrinking these things. The planets known as gas giants are located outside of the ice cap and are made of solidified carbon dioxide, methane, and water. These are found across the frostline. c. The distance from the sun when the temperature is so low that gaseous ammonia, methane, and water are evacuated, and solid shapes are visible is known as the frost line. Typically, planets below the frost line are gassed or vaporized, making them smaller than planets above the frost line. The ammonia solidified deposition layers, methane, and water on the planets outside the frost line give them an even larger size. Because of this, there exist tiny hot planets above the frost line.

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Abeyta - Kinnevy4 Planets created inside the outer portions of the Frost Line had a larger concentration of ice and gas due to the low pressure and temperature in that region. A few planets with more stony and metallic constituents are Mars onward to Mercury, which developed inside the inner reaches of the Frost Line. Because of less liquid water condensation and more solar exposure, this has happened. However, with the proper pressure and/or temperature circumstances, liquid water might still condense into ice. Due to the temperature of the early solar system, the inner planets are rocky, and the outer planets are gaseous. As the gases combined to form a protosun, the temperature of the solar system rose. d. There hasn't always been a frost line in the same spot. As the Solar System grew, the Sun pushed the frost line outside. This is as a result of the Sun's previous inactivity. The materials found in the solar nebula are often found in the Sun. Thus, causing the planets to be formed differently depending on the kinds of materials present inside and outside the frost line as well as where they were in relation to the frost line. The Sun's rays warmed the objects in the solar system, especially those inside the inner planets. The temperature was too high for light volatiles, like water and ammonia, to condense there. Additionally, solar wind particles pushed volatiles outside of the inner solar system. As the volatiles reached the chilly temperatures of the outer solar system, over an illusory barrier known as the frost line, they condensed onto the growing giant planets. Therefore, meaning that if the sun were hotter and some gas giants were within that border, the frost line would advance. The frost line travels towards the sun as the sun gets

Abeyta - Kinnevy5 colder, allowing the terrestrial planet to cross over and perhaps have these volatile compounds enclose its outer layer. Causing the outer planets to accumulate rocks, metals, and volatiles while the relatively warm, "windy" core region was emptied of all but the components with the highest density, such as rock and metal. e. Planetary Migration Research i. There are three ways that planetary migration is thought to happen: the first is a gas-driven process in which the planetary disk effectively pushes or pulls the planet to a new position; the second results from gravitational interactions between nearby bodies, where a large object can scatter a smaller one and thereby create an equal and opposite resulting force back onto itself; and the third is due to another gravitational effect, tidal forces (Planet Hunters). The largest planet in the Solar System, Jupiter, moved inward to start it all off. The gas giant, which weighs more than all the planets put together, is thought to have traveled all the way up to Mars' orbit, 1.5 AU from the Sun, before returning to its current location, which is nearly four times farther away. Fortunately for Mars, this happened about 600 million years into the Solar System's formation (about 4 billion years ago), when only four gas giants dominated the heavens. At this time, a dense disk of tiny, ice objects encircled Jupiter, Saturn, Uranus, and Neptune, which had considerably more constrained orbits. The first kind of planetary migration, which is gas driven and has varying effects depending on the mass of the planet, is what drew Jupiter toward the Sun.

Abeyta - Kinnevy6 The mechanism for low-mass planets, such as the Earth, happens when the planet's orbit disturbs the nearby gas or planetesimal disk, introducing spiral density waves. The planet may gain or lose angular momentum if there is an imbalance in the force of interaction with the spirals inside and beyond its orbit. The globe moves inside when angular momentum is lost, and outward when it is gained. High mass planets like Jupiter have significant gravitational pulls that cause a sizable gap in the disk to be cleared, stopping migration. It is believed that this migration mechanism explains why Jupiter is found in such close proximity to their stars in comparison to other planetary systems (Planet Hunter). Works Cited Courtland, R. (2009, February 25). Asteroid belt may bear scars of planets' migration. Retrieved July 16, 2020, from https://www.newscientist.com/article/dn16667-asteroid-belt-may- bear-scars-of-planets-migration/ Gupta, A., & Kalaria, A. (n.d.). Our Suns Planets . University of Michigan. Retrieved October 11, 2022, from http://websites.umich.edu/~gs265/planets.htm How Planets FormHow Planets Form. (2007, August). Retrieved July 16, 2020, from http://lasp.colorado.edu/outerplanets/solsys_planets.php howfarawayisit. (2020, June 13). Classroom aid - frost line . YouTube. Retrieved October 10, 2022, from https://www.youtube.com/watch?v=8N7VzHScNsE

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Abeyta - Kinnevy7 NASAWebbTelescope. (2010, October 19). Planetary formation: James Webb Space Telescope science . YouTube. Retrieved October 10, 2022, from https://www.youtube.com/watch? v=L2d7joOgVLg Overview of the Solar System . Overview of the solar system. (2006). Retrieved October 11, 2022, from http://ircamera.as.arizona.edu/Astr2016/lectures/solarsysovervw.htm#:~:text=The %20frost%20line%20for%20the,oxygen%2C%20but%20some%20hydrogen ). Phanerozoic . Visit the main page. (n.d.). Retrieved October 11, 2022, from https://www.newworldencyclopedia.org/entry/phanerozoic Phanerozoic Eon | Geochronology." Encyclopedia Britannica , www.britannica.com/science/Phanerozoic-Eon Simoes, C. (n.d.). Frost line or Snow line or ICE line in the solar system . Astronoo. Retrieved October 11, 2022, from http://www.astronoo.com/en/articles/frost-line.html Tillman, N. T. (2021, December 13). How did the solar system form? Space.com. Retrieved October 11, 2022, from https://www.space.com/35526-solar-system-formation.html The role of planetary migration in the evolution of the solar system . Planet Hunters. (2014, May 9). Retrieved October 11, 2022, from https://blog.planethunters.org/2014/05/09/the-role-of- planetary-migration-in-the-evolution-of-the-solar-system/ The Solar System . The solar system. (2018). Retrieved October 11, 2022, from http://astronomy.nmsu.edu/holtz/a110.fall08/a110notes/node5.html 8.2: Origin of the Solar System—the Nebular Hypothesis." Geosciences LibreTexts , 4 Nov. 2019,geo.libretexts.org/Bookshelves/Geology/Book %3A_An_Introduction_to_Geology_(Johnson_Affolter_Inkenbrandt_and_Mosher)/08%3A_Eart h_History/8.02%3A_Origin_of_the_Solar_SystemThe_Nebular_Hypothesis

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Formation Lab

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