The document provides information about the Moon:
- The Moon has 1/80 the mass and 1/4 the diameter of Earth. Its orbit is nearly circular with a mean distance of 384,000 km from Earth.
- The Moon causes Earth's tides and the slowing of Earth's rotation over time. The Moon's surface shows impact craters and lacks atmosphere or liquid water.
- Samples returned by Apollo astronauts show the Moon has a similar composition to Earth's mantle but is deficient in iron and volatiles like water, suggesting it formed from mantle material ejected during an ancient giant impact.
The document summarizes the evolution of Earth from its formation to present day. It describes how:
- Dust and gas coalesced from the solar nebula to form planetesimals and eventually Earth around 4.5 billion years ago.
- Early Earth was mostly molten due to heavy bombardment and radioactive decay. The heat allowed the planet to differentiate into a core, mantle, and crust.
- As Earth cooled, water and an atmosphere formed. Photosynthetic life evolved and increased oxygen in the atmosphere around 2.4 billion years ago.
- Plate tectonics and volcanism have continuously recycled Earth's crust and regulated temperatures and atmospheric gases through geologic time.
The document summarizes key concepts about the sun and Earth's formation. It describes how the sun generates energy through nuclear fusion in its core, and how this energy reaches the surface in about 8 minutes. It also explains how Earth formed from the accretion of planetesimals, and how its core, mantle and crust layers developed as denser materials sank to the center. The oceans formed from early rainfall, and continents gradually emerged and shifted positions over billions of years.
The document summarizes theories about how our solar system formed from a collapsing cloud of gas and dust. It describes how:
1) Our solar system likely began from a giant interstellar cloud that collapsed under gravity and formed a rotating disk, with a dense center that became the Sun and a surrounding disk that formed the planets.
2) The solar nebula disk varied in temperature by distance from the Sun, allowing different elements to condense into planetary cores near and far from the Sun, forming the terrestrial and gas giant planets.
3) Asteroids and comets are remnants from solar system formation and provide clues about its early history through observations and analysis of their composition and orbits.
- The document discusses key features of Earth and the Moon, including their formation and interactions.
- It describes how plate tectonics leads to geological activity at plate boundaries like earthquakes and volcanoes.
- It also explains how tidal forces from the Moon cause Earth's ocean tides and how the Moon synchronously rotates to always show the same face to Earth due to tidal locking during its formation.
The solar system formed 4.6 billion years ago from a giant cloud of dust and gas called a solar nebula. As the cloud contracted under gravity, the proto-Sun formed at the center and a disk of dust and ice particles formed around it. These particles collided and merged to become planetesimals and eventually the planets. The inner planets like Earth are rocky due to higher temperatures in the inner solar system, while outer planets are gaseous. The Moon formed from debris ejected during a giant impact between Earth and a Mars-sized planet. Life on Earth began as single-celled organisms and changed the atmosphere through photosynthesis over billions of years.
(figure 15.18 The planets drawn to scale.)diameter of Neptu.docxjoyjonna282
(
figure 15.18
The planets drawn to scale.
)diameter of Neptune (the smallest Jovian planet) is three times larger than the diameter of Earth or Venus. Further, Neptune's mass is 17 times greater than that of Earth or Venus (figure 15.18).
Other properties that differ include densities, chemical compositions, orbital periods, and numbers of satellites. Variations in the chemical composition of planets are largely responsible for their density differences. Specifically, the average density of the terrestrial planets is about five times the density of water, whereas the average density of the Jovian planets is only 1.5 times that of water. Saturn has a density only 0.7 times that of water, which means that it would float if placed in a large enough tank of water. The outer planets are also characterized by long orbital periods and numerous satellites.
Internal Structures
Shortly after Earth formed, the segregation of material resulted in the formation of three major layers defined by their chemical composition—the crust, mantle, and core. This type of chemical separation occurred in the other planets as well. However, because the terrestrial planets are compositionally different than the Jovian planets, the nature of these layers differs between these two groups (figure is. i 9).
The terrestrial planets are dense, having relatively large cores of iron and iron compounds. From their centers outward, the amount of metallic iron decreases while the amount of rocky silicate minerals increase. The outer cores of Earth and Mercury are liquid, whereas the cores of Venus and Mars are thought to be partially molten. This difference is attributable to Venus and Mars having lower internal temperatures than those of Earth and Mercury. Silicate minerals and other lighter compounds make up the mantles of the terrestrial planets. Finally, the silicate crusts of terrestrial planets are relatively thin compared to their mantles.
The two largest Jovian planets, Jupiter and Saturn, have small metallic inner cores consisting of iron compounds at extremely high temperatures and pressures. The outer cores of these two giants are thought to be liquid metallic hydrogen, whereas the mantles are comprised of liquid hydrogen and helium. The outermost layers are gases and ices of hydrogen, helium, water, ammonia, and methane—which account for the low densities of these planets. Uranus and Neptune also have small metallic cores but their mantles are likely hot dense water and ammonia. Above their mantles, the amount of hydrogen and helium increases, but exists in much lower concentrations than those of Jupiter and Saturn.
The Atmospheres of the Planets
The Jovian planets have very thick atmospheres composed mainly of hydrogen and helium, with lesser amounts of water, methane, ammonia, and other hydrocarbons. The Jovian atmospheres are so thick that they do not show a clear boundary between "atmosphere" and "planet." By contrast, the terrestrial planets, including Earth, h ...
The document summarizes key aspects of how scientists believe the universe began and evolved based on two major theories - the Big Bang theory and the Solar Nebula theory. It provides details on each theory, including that the Big Bang occurred approximately 13.75 billion years ago and resulted in the rapid expansion and cooling of an extremely hot and dense early universe. The Solar Nebula theory proposes that our solar system formed from a collapsing cloud of gas and dust that gave rise to the sun and orbiting bodies.
The document provides information about the Moon:
- The Moon has 1/80 the mass and 1/4 the diameter of Earth. Its orbit is nearly circular with a mean distance of 384,000 km from Earth.
- The Moon causes Earth's tides and the slowing of Earth's rotation over time. The Moon's surface shows impact craters and lacks atmosphere or liquid water.
- Samples returned by Apollo astronauts show the Moon has a similar composition to Earth's mantle but is deficient in iron and volatiles like water, suggesting it formed from mantle material ejected during an ancient giant impact.
The document summarizes the evolution of Earth from its formation to present day. It describes how:
- Dust and gas coalesced from the solar nebula to form planetesimals and eventually Earth around 4.5 billion years ago.
- Early Earth was mostly molten due to heavy bombardment and radioactive decay. The heat allowed the planet to differentiate into a core, mantle, and crust.
- As Earth cooled, water and an atmosphere formed. Photosynthetic life evolved and increased oxygen in the atmosphere around 2.4 billion years ago.
- Plate tectonics and volcanism have continuously recycled Earth's crust and regulated temperatures and atmospheric gases through geologic time.
The document summarizes key concepts about the sun and Earth's formation. It describes how the sun generates energy through nuclear fusion in its core, and how this energy reaches the surface in about 8 minutes. It also explains how Earth formed from the accretion of planetesimals, and how its core, mantle and crust layers developed as denser materials sank to the center. The oceans formed from early rainfall, and continents gradually emerged and shifted positions over billions of years.
The document summarizes theories about how our solar system formed from a collapsing cloud of gas and dust. It describes how:
1) Our solar system likely began from a giant interstellar cloud that collapsed under gravity and formed a rotating disk, with a dense center that became the Sun and a surrounding disk that formed the planets.
2) The solar nebula disk varied in temperature by distance from the Sun, allowing different elements to condense into planetary cores near and far from the Sun, forming the terrestrial and gas giant planets.
3) Asteroids and comets are remnants from solar system formation and provide clues about its early history through observations and analysis of their composition and orbits.
- The document discusses key features of Earth and the Moon, including their formation and interactions.
- It describes how plate tectonics leads to geological activity at plate boundaries like earthquakes and volcanoes.
- It also explains how tidal forces from the Moon cause Earth's ocean tides and how the Moon synchronously rotates to always show the same face to Earth due to tidal locking during its formation.
The solar system formed 4.6 billion years ago from a giant cloud of dust and gas called a solar nebula. As the cloud contracted under gravity, the proto-Sun formed at the center and a disk of dust and ice particles formed around it. These particles collided and merged to become planetesimals and eventually the planets. The inner planets like Earth are rocky due to higher temperatures in the inner solar system, while outer planets are gaseous. The Moon formed from debris ejected during a giant impact between Earth and a Mars-sized planet. Life on Earth began as single-celled organisms and changed the atmosphere through photosynthesis over billions of years.
(figure 15.18 The planets drawn to scale.)diameter of Neptu.docxjoyjonna282
(
figure 15.18
The planets drawn to scale.
)diameter of Neptune (the smallest Jovian planet) is three times larger than the diameter of Earth or Venus. Further, Neptune's mass is 17 times greater than that of Earth or Venus (figure 15.18).
Other properties that differ include densities, chemical compositions, orbital periods, and numbers of satellites. Variations in the chemical composition of planets are largely responsible for their density differences. Specifically, the average density of the terrestrial planets is about five times the density of water, whereas the average density of the Jovian planets is only 1.5 times that of water. Saturn has a density only 0.7 times that of water, which means that it would float if placed in a large enough tank of water. The outer planets are also characterized by long orbital periods and numerous satellites.
Internal Structures
Shortly after Earth formed, the segregation of material resulted in the formation of three major layers defined by their chemical composition—the crust, mantle, and core. This type of chemical separation occurred in the other planets as well. However, because the terrestrial planets are compositionally different than the Jovian planets, the nature of these layers differs between these two groups (figure is. i 9).
The terrestrial planets are dense, having relatively large cores of iron and iron compounds. From their centers outward, the amount of metallic iron decreases while the amount of rocky silicate minerals increase. The outer cores of Earth and Mercury are liquid, whereas the cores of Venus and Mars are thought to be partially molten. This difference is attributable to Venus and Mars having lower internal temperatures than those of Earth and Mercury. Silicate minerals and other lighter compounds make up the mantles of the terrestrial planets. Finally, the silicate crusts of terrestrial planets are relatively thin compared to their mantles.
The two largest Jovian planets, Jupiter and Saturn, have small metallic inner cores consisting of iron compounds at extremely high temperatures and pressures. The outer cores of these two giants are thought to be liquid metallic hydrogen, whereas the mantles are comprised of liquid hydrogen and helium. The outermost layers are gases and ices of hydrogen, helium, water, ammonia, and methane—which account for the low densities of these planets. Uranus and Neptune also have small metallic cores but their mantles are likely hot dense water and ammonia. Above their mantles, the amount of hydrogen and helium increases, but exists in much lower concentrations than those of Jupiter and Saturn.
The Atmospheres of the Planets
The Jovian planets have very thick atmospheres composed mainly of hydrogen and helium, with lesser amounts of water, methane, ammonia, and other hydrocarbons. The Jovian atmospheres are so thick that they do not show a clear boundary between "atmosphere" and "planet." By contrast, the terrestrial planets, including Earth, h ...
The document summarizes key aspects of how scientists believe the universe began and evolved based on two major theories - the Big Bang theory and the Solar Nebula theory. It provides details on each theory, including that the Big Bang occurred approximately 13.75 billion years ago and resulted in the rapid expansion and cooling of an extremely hot and dense early universe. The Solar Nebula theory proposes that our solar system formed from a collapsing cloud of gas and dust that gave rise to the sun and orbiting bodies.
The document discusses the greenhouse effect on Earth and the factors that allow liquid water to exist, including the greenhouse gases in our atmosphere like water vapor and carbon dioxide. It also explains how Earth's carbon dioxide cycle acts as a natural thermostat to regulate the planet's temperature over millions of years. Plate tectonics and life, through photosynthesis, have also played important roles in maintaining conditions suitable for water and habitability.
This chapter discusses the origin and evolution of the Earth and the solar system. It begins with an overview of the Big Bang theory for the origin of the universe and then describes the nebular hypothesis for the formation of the solar system from a primordial cloud of gas and dust. Key points include the differentiation of the Earth into a core, mantle and crust due to melting after accretion and the abundance of iron in the Earth's core versus the crust. The chapter also provides details about the different types of planets, asteroids, comets and meteorites that make up the solar system.
This document provides a summary of key concepts in astronomy, including the universe, galaxies, stars, planets in our solar system, and important historical astronomers like Ptolemy, Copernicus, and Galileo. It describes how stars are born from nebulae and die, as well as concepts like nuclear fusion, main sequence, and how our sun will eventually die. Important terms are defined like nebulae, constellations, blue giants, and red dwarfs. Historical figures that advanced our understanding of astronomy are also summarized.
The greenhouse effect causes Earth's atmosphere to be slightly warmer than if it were only heated by solar radiation. Greenhouse gases like water vapor, carbon dioxide, and methane absorb and re-emit infrared radiation from the planet's surface to the atmosphere, increasing temperatures. Over long time periods, natural processes like volcanoes, weathering, and plate tectonics have regulated Earth's climate through fluctuations in atmospheric carbon dioxide.
The document summarizes the formation of the Solar System according to the Nebular Theory. It explains that 4.6 billion years ago, a giant cloud of gas and dust collapsed due to gravity and began spinning, forming a disk with the Sun at the center. As the cloud contracted and the protosun heated up, planets formed from accretion of planetesimals in the disk. Closer planets are rocky due to high temperatures, while outer planets are gas giants which formed in the cooler outer regions and captured hydrogen and helium. The asteroids, comets, and Kuiper Belt are remnants of the original planetesimal formation.
Planetesimal ejection describes how leftover debris from the formation of the planets was captured as moons or ended up in the asteroid belt, Kuiper belt, or Oort cloud. Asteroids and meteoroids are small rocky or metallic objects found primarily in the inner solar system, with asteroids larger than 100 meters and meteoroids smaller. They orbit near the plane of the solar system in regions like the asteroid belt. When these objects enter the Earth's atmosphere, they appear as meteors and some survive impact as meteorites. Larger impacts are rarer but can cause global effects like the extinction of dinosaurs.
In this presentation, I focused on the geomorphological aspect of earthquake which means tectonic plates. Additionally, we also included the origin of the Universe and tectonic plates. And also the Nepal and Taiwan earthquakes of 2015 was also described here in perspective with tectonic plates.
The Moon and Mercury are both characterized as dead worlds with little to no atmosphere or magnetic field. The Moon has almost no magnetic field while Mercury does have a weak global magnetic field, implying it has a molten iron core. Both bodies are heavily cratered but Mercury has some smooth volcanic plains. The interior of the Moon is only partially differentiated while Mercury's core likely contains iron and iron sulfides. Limited past missions have provided data about the features and conditions on these two bodies, but more exploration is still needed to understand their formation and evolution.
There are two basic groups of planets in the solar system - terrestrial and jovian. Terrestrial planets are small and rocky like Mercury, Venus, Earth, and Mars. Jovian planets are large and gaseous, consisting of Jupiter, Saturn, Uranus, and Neptune. Mars has the largest volcano and canyon in the solar system. Jupiter's clouds move in east-west bands and Saturn has a large ring system with gaps. Uranus and Neptune are similar in size and interior composition. Comets have long elliptical orbits and contain ice that evaporates when passing close to the sun. Meteoroids enter the atmosphere and burn up, appearing as meteors, with some larger pieces surviving
The Sun is a normal main-sequence G2 star located at the center of our solar system. It contains over 99% of the mass in the system and is about 4.6 billion years old. It has a diameter of 1.39 million km and a surface temperature of around 5,800 K. The Sun is composed primarily of hydrogen and helium and will likely exist for another 5 billion years before exhausting its nuclear fuel. It supports eight planets, including Earth, and numerous smaller objects in orbit through its strong gravitational pull and emission of heat and light.
This document provides a summary of key topics in space exploration including:
1) Early space probes and manned missions that explored space starting in the 1950s and 1960s including Sputnik 1, Vostok 1, Mercury, and Apollo missions.
2) Components of rockets such as the launch vehicle, control module, service module, and lunar module.
3) Properties of the inner planets Mercury, Venus, Earth, and Mars including their atmospheres, temperatures, moons, and geological features.
4) Formation and characteristics of the moon including its dark surface, lack of erosion, and differences between the highlands and maria regions.
Asteroids are rocky objects that orbit the Sun, mostly located in a belt between Mars and Jupiter. Their irregular shapes indicate they have not undergone geological processes like planets. Some large asteroids even have their own moons. Most meteorites originate from asteroids. Comets are icy objects that originate much further from the Sun in the Kuiper belt and Oort cloud. When heated as they approach the Sun, comets grow dust and plasma tails. Pluto and other large Kuiper belt objects are classified as dwarf planets rather than planets due to their small size and icy composition. Evidence suggests a large asteroid or comet impact was responsible for the mass extinction that killed the dinosaurs 65 million years ago.
The document discusses the greenhouse effect on Earth and how it contributes to suitable conditions for liquid water. It notes that Earth's atmosphere is slightly warmer than expected due to greenhouse gases like water vapor and carbon dioxide trapping infrared radiation emitted from the surface. A mild greenhouse effect prevents temperatures from being too hot or cold for water to remain liquid. It also discusses how water vapor is the most abundant greenhouse gas and is important for regulating Earth's temperature through a feedback loop with carbon dioxide.
The document summarizes key aspects of the greenhouse effect on Earth and how it enables liquid water to exist on the planet's surface. It describes how greenhouse gases like water vapor and carbon dioxide trap infrared radiation in the atmosphere, warming it and maintaining temperatures suitable for water. The greenhouse effect is mild, avoiding temperatures that are too hot or cold. The document also discusses the carbon dioxide and water cycles that regulate Earth's climate over long timescales.
This document summarizes the differentiation of the Earth. It discusses how the Earth initially formed as a molten mass and over time separated into layers with the heavier materials sinking to the center to form the core. The two main theories for this differentiation are homogeneous and heterogeneous accretion. Evidence from the Moon supports the Earth differentiating into layers early in its formation history around 4.5 billion years ago. The Earth is now composed of concentric layers that decrease in density from the iron-nickel core, to the silicate mantle, and finally the crust at the surface.
The document summarizes the layers of the Sun and what they are composed of. It discusses that the core of the Sun undergoes nuclear fusion, combining hydrogen into helium. This reaction powers the Sun and releases energy. The energy moves outward through the radiative zone by radiation and then the convective zone carries the energy to the surface by convection currents. The visible surface is the photosphere, which has a temperature of around 6000 Kelvin and emits light.
The four terrestrial planets - Mercury, Venus, Earth, and Mars - are similar in size and structure. They orbit in the inner solar system and are too small to retain thick hydrogen atmospheres. Mercury is the smallest and hottest planet, with extensive volcanic plains and impact craters. Venus has a dense, toxic atmosphere that causes a strong greenhouse effect and maintains surface temperatures over 400°C. Mars has the largest volcano in the solar system, Olympus Mons, and polar ice caps that vary in size with the seasons.
The document summarizes the formation of the solar system based on the nebular hypothesis. It explains that the solar system formed from the gravitational collapse of a giant gas and dust cloud about 4.6 billion years ago. As the cloud collapsed and spun faster, the heavier elements collected in the center to form the inner terrestrial planets, while the outer parts formed the outer gaseous jovian planets. Over time, small particles collided and merged to form larger bodies called planetesimals, which eventually formed the planets.
Main Java[All of the Base Concepts}.docxadhitya5119
This is part 1 of my Java Learning Journey. This Contains Custom methods, classes, constructors, packages, multithreading , try- catch block, finally block and more.
The document discusses the greenhouse effect on Earth and the factors that allow liquid water to exist, including the greenhouse gases in our atmosphere like water vapor and carbon dioxide. It also explains how Earth's carbon dioxide cycle acts as a natural thermostat to regulate the planet's temperature over millions of years. Plate tectonics and life, through photosynthesis, have also played important roles in maintaining conditions suitable for water and habitability.
This chapter discusses the origin and evolution of the Earth and the solar system. It begins with an overview of the Big Bang theory for the origin of the universe and then describes the nebular hypothesis for the formation of the solar system from a primordial cloud of gas and dust. Key points include the differentiation of the Earth into a core, mantle and crust due to melting after accretion and the abundance of iron in the Earth's core versus the crust. The chapter also provides details about the different types of planets, asteroids, comets and meteorites that make up the solar system.
This document provides a summary of key concepts in astronomy, including the universe, galaxies, stars, planets in our solar system, and important historical astronomers like Ptolemy, Copernicus, and Galileo. It describes how stars are born from nebulae and die, as well as concepts like nuclear fusion, main sequence, and how our sun will eventually die. Important terms are defined like nebulae, constellations, blue giants, and red dwarfs. Historical figures that advanced our understanding of astronomy are also summarized.
The greenhouse effect causes Earth's atmosphere to be slightly warmer than if it were only heated by solar radiation. Greenhouse gases like water vapor, carbon dioxide, and methane absorb and re-emit infrared radiation from the planet's surface to the atmosphere, increasing temperatures. Over long time periods, natural processes like volcanoes, weathering, and plate tectonics have regulated Earth's climate through fluctuations in atmospheric carbon dioxide.
The document summarizes the formation of the Solar System according to the Nebular Theory. It explains that 4.6 billion years ago, a giant cloud of gas and dust collapsed due to gravity and began spinning, forming a disk with the Sun at the center. As the cloud contracted and the protosun heated up, planets formed from accretion of planetesimals in the disk. Closer planets are rocky due to high temperatures, while outer planets are gas giants which formed in the cooler outer regions and captured hydrogen and helium. The asteroids, comets, and Kuiper Belt are remnants of the original planetesimal formation.
Planetesimal ejection describes how leftover debris from the formation of the planets was captured as moons or ended up in the asteroid belt, Kuiper belt, or Oort cloud. Asteroids and meteoroids are small rocky or metallic objects found primarily in the inner solar system, with asteroids larger than 100 meters and meteoroids smaller. They orbit near the plane of the solar system in regions like the asteroid belt. When these objects enter the Earth's atmosphere, they appear as meteors and some survive impact as meteorites. Larger impacts are rarer but can cause global effects like the extinction of dinosaurs.
In this presentation, I focused on the geomorphological aspect of earthquake which means tectonic plates. Additionally, we also included the origin of the Universe and tectonic plates. And also the Nepal and Taiwan earthquakes of 2015 was also described here in perspective with tectonic plates.
The Moon and Mercury are both characterized as dead worlds with little to no atmosphere or magnetic field. The Moon has almost no magnetic field while Mercury does have a weak global magnetic field, implying it has a molten iron core. Both bodies are heavily cratered but Mercury has some smooth volcanic plains. The interior of the Moon is only partially differentiated while Mercury's core likely contains iron and iron sulfides. Limited past missions have provided data about the features and conditions on these two bodies, but more exploration is still needed to understand their formation and evolution.
There are two basic groups of planets in the solar system - terrestrial and jovian. Terrestrial planets are small and rocky like Mercury, Venus, Earth, and Mars. Jovian planets are large and gaseous, consisting of Jupiter, Saturn, Uranus, and Neptune. Mars has the largest volcano and canyon in the solar system. Jupiter's clouds move in east-west bands and Saturn has a large ring system with gaps. Uranus and Neptune are similar in size and interior composition. Comets have long elliptical orbits and contain ice that evaporates when passing close to the sun. Meteoroids enter the atmosphere and burn up, appearing as meteors, with some larger pieces surviving
The Sun is a normal main-sequence G2 star located at the center of our solar system. It contains over 99% of the mass in the system and is about 4.6 billion years old. It has a diameter of 1.39 million km and a surface temperature of around 5,800 K. The Sun is composed primarily of hydrogen and helium and will likely exist for another 5 billion years before exhausting its nuclear fuel. It supports eight planets, including Earth, and numerous smaller objects in orbit through its strong gravitational pull and emission of heat and light.
This document provides a summary of key topics in space exploration including:
1) Early space probes and manned missions that explored space starting in the 1950s and 1960s including Sputnik 1, Vostok 1, Mercury, and Apollo missions.
2) Components of rockets such as the launch vehicle, control module, service module, and lunar module.
3) Properties of the inner planets Mercury, Venus, Earth, and Mars including their atmospheres, temperatures, moons, and geological features.
4) Formation and characteristics of the moon including its dark surface, lack of erosion, and differences between the highlands and maria regions.
Asteroids are rocky objects that orbit the Sun, mostly located in a belt between Mars and Jupiter. Their irregular shapes indicate they have not undergone geological processes like planets. Some large asteroids even have their own moons. Most meteorites originate from asteroids. Comets are icy objects that originate much further from the Sun in the Kuiper belt and Oort cloud. When heated as they approach the Sun, comets grow dust and plasma tails. Pluto and other large Kuiper belt objects are classified as dwarf planets rather than planets due to their small size and icy composition. Evidence suggests a large asteroid or comet impact was responsible for the mass extinction that killed the dinosaurs 65 million years ago.
The document discusses the greenhouse effect on Earth and how it contributes to suitable conditions for liquid water. It notes that Earth's atmosphere is slightly warmer than expected due to greenhouse gases like water vapor and carbon dioxide trapping infrared radiation emitted from the surface. A mild greenhouse effect prevents temperatures from being too hot or cold for water to remain liquid. It also discusses how water vapor is the most abundant greenhouse gas and is important for regulating Earth's temperature through a feedback loop with carbon dioxide.
The document summarizes key aspects of the greenhouse effect on Earth and how it enables liquid water to exist on the planet's surface. It describes how greenhouse gases like water vapor and carbon dioxide trap infrared radiation in the atmosphere, warming it and maintaining temperatures suitable for water. The greenhouse effect is mild, avoiding temperatures that are too hot or cold. The document also discusses the carbon dioxide and water cycles that regulate Earth's climate over long timescales.
This document summarizes the differentiation of the Earth. It discusses how the Earth initially formed as a molten mass and over time separated into layers with the heavier materials sinking to the center to form the core. The two main theories for this differentiation are homogeneous and heterogeneous accretion. Evidence from the Moon supports the Earth differentiating into layers early in its formation history around 4.5 billion years ago. The Earth is now composed of concentric layers that decrease in density from the iron-nickel core, to the silicate mantle, and finally the crust at the surface.
The document summarizes the layers of the Sun and what they are composed of. It discusses that the core of the Sun undergoes nuclear fusion, combining hydrogen into helium. This reaction powers the Sun and releases energy. The energy moves outward through the radiative zone by radiation and then the convective zone carries the energy to the surface by convection currents. The visible surface is the photosphere, which has a temperature of around 6000 Kelvin and emits light.
The four terrestrial planets - Mercury, Venus, Earth, and Mars - are similar in size and structure. They orbit in the inner solar system and are too small to retain thick hydrogen atmospheres. Mercury is the smallest and hottest planet, with extensive volcanic plains and impact craters. Venus has a dense, toxic atmosphere that causes a strong greenhouse effect and maintains surface temperatures over 400°C. Mars has the largest volcano in the solar system, Olympus Mons, and polar ice caps that vary in size with the seasons.
The document summarizes the formation of the solar system based on the nebular hypothesis. It explains that the solar system formed from the gravitational collapse of a giant gas and dust cloud about 4.6 billion years ago. As the cloud collapsed and spun faster, the heavier elements collected in the center to form the inner terrestrial planets, while the outer parts formed the outer gaseous jovian planets. Over time, small particles collided and merged to form larger bodies called planetesimals, which eventually formed the planets.
Main Java[All of the Base Concepts}.docxadhitya5119
This is part 1 of my Java Learning Journey. This Contains Custom methods, classes, constructors, packages, multithreading , try- catch block, finally block and more.
This document provides an overview of wound healing, its functions, stages, mechanisms, factors affecting it, and complications.
A wound is a break in the integrity of the skin or tissues, which may be associated with disruption of the structure and function.
Healing is the body’s response to injury in an attempt to restore normal structure and functions.
Healing can occur in two ways: Regeneration and Repair
There are 4 phases of wound healing: hemostasis, inflammation, proliferation, and remodeling. This document also describes the mechanism of wound healing. Factors that affect healing include infection, uncontrolled diabetes, poor nutrition, age, anemia, the presence of foreign bodies, etc.
Complications of wound healing like infection, hyperpigmentation of scar, contractures, and keloid formation.
How to Fix the Import Error in the Odoo 17Celine George
An import error occurs when a program fails to import a module or library, disrupting its execution. In languages like Python, this issue arises when the specified module cannot be found or accessed, hindering the program's functionality. Resolving import errors is crucial for maintaining smooth software operation and uninterrupted development processes.
How to Make a Field Mandatory in Odoo 17Celine George
In Odoo, making a field required can be done through both Python code and XML views. When you set the required attribute to True in Python code, it makes the field required across all views where it's used. Conversely, when you set the required attribute in XML views, it makes the field required only in the context of that particular view.
This slide is special for master students (MIBS & MIFB) in UUM. Also useful for readers who are interested in the topic of contemporary Islamic banking.
This presentation was provided by Steph Pollock of The American Psychological Association’s Journals Program, and Damita Snow, of The American Society of Civil Engineers (ASCE), for the initial session of NISO's 2024 Training Series "DEIA in the Scholarly Landscape." Session One: 'Setting Expectations: a DEIA Primer,' was held June 6, 2024.
Beyond Degrees - Empowering the Workforce in the Context of Skills-First.pptxEduSkills OECD
Iván Bornacelly, Policy Analyst at the OECD Centre for Skills, OECD, presents at the webinar 'Tackling job market gaps with a skills-first approach' on 12 June 2024
What is Digital Literacy? A guest blog from Andy McLaughlin, University of Ab...
About earth.ppt
1. The Earth as a Planet
Basic Properties
(size, density, composition)
Interior structure
Interior dynamics
Atmosphere
Formation and Evolution
2. How to find the basic parameters?
We find that the bulk density of the Earth is
much higher than that of surface rocks. It
must have something denser inside.
3. Why is the Earth still hot?
The heat was generated by the violent accumulation of planetesimals
which created the Earth. Further heat is added by decay of
radioactive elements. The main source is the crystallization of our
iron core from liquid to solid. The heat has trouble getting out
because of the large volume to surface area ratio. Smaller planets
cool faster.
Heat is carried out from
the interior by
“convection”. Hot rock
rises up to the surface
where it radiates its
energy and cools,
sinking back down.
This causes the
dynamics on our crust.
4. Structure of the Earth’s Interior
We can use seismic waves
generated by earthquakes to “see”
inside the Earth. We find that it has
a “liquid” iron/nickel core,
surrounded by a “plastic” mantle.
The crust of solid rock is thinner
than an eggshell in relative terms.
Thus, the Earth is still basically a
molten ball.
The denser stuff is in
the middle because
it sunk there –
“differentiation”.
6. The Earth’s Atmosphere
Our atmosphere is about
80% molecular nitrogen
and 20% molecular
oxygen, with water and
carbon dioxide in small
amounts. The temperature
changes direction several
times as you go up.
7. The Greenhouse Effect
1) In equilibrium, a planet
must re-radiate all the
energy it absorbs.
2) Solar energy tends to be
converted from visible to
infrared radiation.
3) Some gases are
transparent to visible
radiation, but opaque to
infrared radiation.
4) When radiation is
blocked, you need a
bigger temperature
gradient to push the
energy through.
8. Carbon Dioxide is a critical factor
Without subduction and water, the atmosphere and climate on the
Earth would have been very different. A little more conversion of
CO2 to rock, or lack of subduction and vulcanism, and we would
have “snowball Earth”. Less conversion could make us more like
Venus (human greenhouse gases not really enough for that). Life
has played an important role by using
CO2 in plant respiration and production
of shells which sink to the ocean bottom.
10. The Ozone Hole is Different (and less critical)
Slide 21 Fig. 6-11b, p.105
Ozone blocks solar UV, which causes tans and skin cancer. The hole is
due to CFCs (a chemical) which is now being controlled. The
atmosphere should recover in about 50 years (we hope).
11. The Origin and History of the Moon
The surface of the
Moon has craters,
highlands, and
“maria” (dark
lava basins). Its
composition is
similar to that of
the Earth’s
mantle, with little
or no iron core.
12. Craters on the Moon
The craters on the Moon are almost all
impact craters. They tell of an early
violent history, one which is also
recorded around the rest of the Solar
System. The first half-billion years
were filled with flying debris (some of
it planet-sized).
13. Getting Ages from Half-lives
Start
1 half-life
2 half-lives
3 half-lives
If you know the starting composition of a material, and
you know the time it takes for half of it to change into a
decay product, you can figure out how old it is by
measuring the ratio of original material to decay product.
16. Why Tides Happen
Tides are caused by the difference in
the pull of gravity from one body on
the near and far side of another (1/r3).
They are important in all kinds of
astronomical contexts. They cause the
Earth to slow down and the Moon to
recede.
18. Where to find the Moon in the Sky
The angle between the Sun and the Moon determines its phase.
A crescent Moon must be near
the Sun
A half Moon (first or last
quarter) must be overhead when
the Sun is rising or setting
The full Moon must rise when
the Sun sets, and be on the
meridian near midnight
The waning Moon will tend to
be seen in the daytime
20. Lunar Eclipses
A lunar eclipse occurs when the Moon
goes into the Earth’s shadow.
Everyone who can see the Moon then
sees the eclipse. It looks red because
sunlight is refracted through our air.
The Moon must be full.
21. Solar Eclipses
Solar eclipses happen when the
Moon passes between us and
the Sun. The eclipse can only be
seen where the alignment is
perfect. The sky goes dark, the
stars come out, and the solar
corona becomes visible. It only
lasts a few minutes in any given
spot. Although there are 1 or 2
per year, any given place has a
long wait to see one.
The Moon must be new.
22. ShadowDance
Eclipses usually don’t happen, because the Moon’s orbit is tilted.
The Moon just happens to have about the same angular size as the Sun.
This is a coincidence of the present, the distant past and future will not
get perfect solar eclipses because the Moon’s distance is growing.
23. Astro Quiz
Under which condition below would there be a
total solar eclipse every month?
1) The moon’s orbit crosses the ecliptic at 12 points.
2) The moon’s orbit appears to move along the ecliptic.
3) The moon’s orbit is perpendicular to the celestial equator.
