Class presentation for UNT's Emergency Management degree program. Accompanying detailed paper available here:
https://goo.gl/OUAV4F
This PowerPoint was created for educational purposes only.
The document provides information about the global energy budget and how NASA studies it using satellite data. It includes guiding questions about energy absorption, reflection, and radiation from Earth. Students will perform experiments on how different surfaces absorb heat from a lamp to understand how Earth "spends" the energy it receives from the Sun. They will also learn that the global energy budget works like a monetary budget, with most energy absorbed by land and oceans, while some is reflected by clouds, atmosphere, and Earth's surface.
This document summarizes key concepts about Earth's atmosphere including its composition, structure, and the factors that influence weather and climate. The atmosphere is made up primarily of nitrogen and oxygen, with trace amounts of other gases like carbon dioxide and water vapor. Solar radiation interacts with the atmosphere and Earth's surface in complex ways, heating the atmosphere through absorption, conduction, convection, and the greenhouse effect. Temperature varies based on factors like latitude, altitude, proximity to water, and cloud cover. Together these atmospheric dynamics help determine global and regional weather patterns and climates over time.
Natural disasters can be categorized into three main groups: geological, hydrological, and meteorological. Geological disasters include volcanic eruptions which cause widespread destruction from lava and ash, as well as earthquakes which originate from underground focuses and have epicenters on the surface. Hydrological disasters contain avalanches, which are sudden rapid flows of snow down slopes.
The document discusses various factors that influence air temperature, including solar radiation, greenhouse gases, conduction, convection, and latitude. It explains that air temperature results from complex interactions between these factors, such as different surfaces absorbing radiation differently, greenhouse gases trapping outgoing radiation, and rising air cooling through expansion.
The document discusses Earth's heat budget and the factors that influence it. It explains that Earth receives energy from the sun and loses energy through radiation and that these energy inputs and outputs must balance annually for Earth's overall heat budget. However, there are imbalances at different latitudes that drive winds and ocean currents to redistribute heat globally. Key concepts covered include the greenhouse effect, mechanisms of heat transfer like conduction and radiation, and how gases in the atmosphere impact heating.
This document summarizes the five main layers of Earth's atmosphere - troposphere, stratosphere, mesosphere, thermosphere, and exosphere. It describes key features of each layer such as how temperature varies with altitude and the gases present. The document then discusses topics like the greenhouse effect, how greenhouse gases trap the sun's energy and cause global warming, and how chlorofluorocarbons contribute to ozone depletion in the stratosphere.
Fiji Times article - Energy to destroy 06-04-2015Ashneel Chandra
Tropical cyclones form when sea surface temperatures exceed 26°C to a depth of 60m, particularly near the equator. While increasing temperatures are expected to worsen cyclone conditions over time, other factors like wind shear also influence cyclone formation, so their frequency may not rise consistently. Future cyclones could be more intense as oceans hold more energy, but not necessarily more common. Research is analyzing lightning and wind patterns within cyclones to better predict intensification.
The document provides information about the global energy budget and how NASA studies it using satellite data. It includes guiding questions about energy absorption, reflection, and radiation from Earth. Students will perform experiments on how different surfaces absorb heat from a lamp to understand how Earth "spends" the energy it receives from the Sun. They will also learn that the global energy budget works like a monetary budget, with most energy absorbed by land and oceans, while some is reflected by clouds, atmosphere, and Earth's surface.
This document summarizes key concepts about Earth's atmosphere including its composition, structure, and the factors that influence weather and climate. The atmosphere is made up primarily of nitrogen and oxygen, with trace amounts of other gases like carbon dioxide and water vapor. Solar radiation interacts with the atmosphere and Earth's surface in complex ways, heating the atmosphere through absorption, conduction, convection, and the greenhouse effect. Temperature varies based on factors like latitude, altitude, proximity to water, and cloud cover. Together these atmospheric dynamics help determine global and regional weather patterns and climates over time.
Natural disasters can be categorized into three main groups: geological, hydrological, and meteorological. Geological disasters include volcanic eruptions which cause widespread destruction from lava and ash, as well as earthquakes which originate from underground focuses and have epicenters on the surface. Hydrological disasters contain avalanches, which are sudden rapid flows of snow down slopes.
The document discusses various factors that influence air temperature, including solar radiation, greenhouse gases, conduction, convection, and latitude. It explains that air temperature results from complex interactions between these factors, such as different surfaces absorbing radiation differently, greenhouse gases trapping outgoing radiation, and rising air cooling through expansion.
The document discusses Earth's heat budget and the factors that influence it. It explains that Earth receives energy from the sun and loses energy through radiation and that these energy inputs and outputs must balance annually for Earth's overall heat budget. However, there are imbalances at different latitudes that drive winds and ocean currents to redistribute heat globally. Key concepts covered include the greenhouse effect, mechanisms of heat transfer like conduction and radiation, and how gases in the atmosphere impact heating.
This document summarizes the five main layers of Earth's atmosphere - troposphere, stratosphere, mesosphere, thermosphere, and exosphere. It describes key features of each layer such as how temperature varies with altitude and the gases present. The document then discusses topics like the greenhouse effect, how greenhouse gases trap the sun's energy and cause global warming, and how chlorofluorocarbons contribute to ozone depletion in the stratosphere.
Fiji Times article - Energy to destroy 06-04-2015Ashneel Chandra
Tropical cyclones form when sea surface temperatures exceed 26°C to a depth of 60m, particularly near the equator. While increasing temperatures are expected to worsen cyclone conditions over time, other factors like wind shear also influence cyclone formation, so their frequency may not rise consistently. Future cyclones could be more intense as oceans hold more energy, but not necessarily more common. Research is analyzing lightning and wind patterns within cyclones to better predict intensification.
The document summarizes key concepts about the Earth's energy balance. It explains that the atmosphere absorbs and scatters some incoming solar radiation while allowing visible light to pass through, and greenhouse gases like carbon dioxide and water vapor in the atmosphere absorb outgoing infrared radiation from the Earth's surface, enhancing the greenhouse effect and warming the planet. The Earth's temperature remains relatively constant over time as the gains and losses of radiant energy are balanced on a global scale, though human activities can affect these energy flows and potentially disrupt this balance.
This document discusses how energy from the sun interacts with the atmosphere and Earth's surface. Solar radiation enters the atmosphere and is scattered, refracted, reflected, or absorbed. Atmospheric gases and particles influence these processes. Absorbed radiation is transferred within the atmosphere and at the surface via conduction, convection, and radiation. Greenhouse gases in the atmosphere and clouds contribute to the greenhouse effect by trapping infrared radiation emitted from the surface. The surface and atmospheric energy budgets describe the distribution of solar energy after it passes through the atmosphere and reaches the Earth's surface.
The atmosphere consists of 78% nitrogen, 21% oxygen and trace amounts of other gases that make life possible on Earth. It protects the planet from harmful rays and meteorites. Weather occurs in the lower layer of the atmosphere, the troposphere, which extends up to 12 miles high and where temperatures decrease with altitude. Higher layers include the stratosphere, mesosphere, thermosphere and outermost exosphere. Climate is associated with a place and includes daily, seasonal and yearly variations in elements like temperature, precipitation, humidity, pressure and wind. Factors influencing climate include latitude, altitude, land and ocean distribution, barriers and currents.
Atmosphere & surface energy balanceNagina Nighat
The document discusses concepts related to solar radiation and Earth's energy balance. It begins by describing how the Sun generates energy through nuclear fusion and emits it as electromagnetic waves. It then defines insolation as the amount of solar radiation reaching a given area, noting it varies by location and time. Finally, it explains that Earth's climate is powered by solar energy and achieves radiative equilibrium when the amount of incoming solar energy balances the amount radiated back to space, keeping global temperatures stable.
All energy from the sun that reaches Earth is converted to thermal energy or heat. The amount of heat absorbed at the surface varies by location and time due to factors like the sun's angle, cloud cover, Earth's distance from the sun, and greenhouse gases trapping heat in the atmosphere. This trapped heat maintains Earth's temperature through the greenhouse effect, resembling the way a greenhouse warms an environment for plants. Different surfaces like land, water, and air heat up differently via radiation, convection, and conduction.
Earth's Energy Budget and solar radiation (with Animations)Sameer baloch
about earth's Energy budget. how much coming and how much radiation leaving from our surface to atmosphere from atmo to space with animated picture.
it clears your concept by animated gif photos
The document discusses solar flares, including how they occur due to magnetic reconnection on the sun's surface, their stages of development, their recorded effects on Earth including disrupting telegraph systems in 1859, potential impacts such as damaging electronics and electrical infrastructure, challenges predicting them, and recommendations for preparing like having backup power sources and fuel.
This document discusses electromagnetic radiation (EMR) and its interaction with the atmosphere. It covers the following key points:
1) EMR can be described as waves with different wavelengths that determine their energy content. Shorter wavelengths like gamma rays have higher energy.
2) The atmosphere only allows certain wavelengths to pass through in "atmospheric windows" while absorbing others. Gases like oxygen, nitrogen, ozone, carbon dioxide and water vapor are significant absorbers.
3) Factors like albedo, scattering, temperature inversions, and cloud cover influence the transmission and absorption of EMR and impact atmospheric temperatures.
Solar storms are known as called solar flares. The solar magnetic field causes solar activities. It is an intense burst of radiation that is generated due to the release of magnetic energy from the sunspots. These are the biggest explosive events in our solar system. The solar storm looks like a bright spot in the sun, lasting from a few minutes to a few hours.
This document discusses various topics relating to physical geography and temperature, including:
- The electromagnetic spectrum and how different wavelengths of light refract differently.
- The greenhouse effect and how gases like carbon dioxide and methane trap heat.
- The various controls on temperature, including latitude, proximity to water, cloud cover, urbanization and more.
- How water moderates temperature through processes like evaporation and its higher specific heat.
- Different types of heat transfer and how phase changes in water absorb or release heat.
The document discusses the Earth's radiation balance and how human activity is impacting it through increased greenhouse gas emissions, leading to global warming. It explains that the Earth maintains a temperature balance through absorbing and emitting radiation. Increased greenhouse gases like carbon dioxide and methane absorb more outgoing radiation, disrupting this balance and causing warming. It outlines various impacts of global warming like melting ice caps, more extreme weather, and discusses efforts to reduce emissions and mitigate further impacts.
The document summarizes how energy from the sun is transferred within the Earth's atmosphere and surfaces. It explains that some solar energy is reflected by gases and particles in the atmosphere, while some is absorbed by the land and water, warming the Earth's surface. It also describes the different methods by which heat is transferred, including radiation from the sun or fires, conduction between touching substances, and convection through fluid movements like air currents.
Solar flares are violent eruptions on the Sun's surface that can release energy equivalent to millions of hydrogen bombs and last a few minutes. During flares, material is ejected into space at up to 1000 km/s in coronal mass ejections, which produce bursts in the solar wind that influence the solar system, including Earth by causing increased auroras and activity days later. Flares are associated with the Sun's magnetic field and occur more frequently near solar maximum when interactions between opposing magnetic fields are more common due to increased solar activity and sunspots.
Earth's energy budget refers to the tracking of how much energy is flowing into and out of the Earth's climate, where the energy is going, and if the energy coming in balances with the energy going out. The Earth receives energy from the Sun, and it also reflects and radiates energy back into space. All of the energy that warms the atmosphere, oceans and land must be radiated back into space in order to maintain our current climate. If the amount of energy radiating back into space is decreased by even a very small amount, it can lead to warming. It is believed that increasing levels of carbon dioxide in the atmosphere has a 'greenhouse effect' of reducing the amount of energy radiated into space.
The document discusses the key factors that influence weather and climate on Earth, including heat from the sun, atmospheric gases, and their interactions. It explains that the sun provides visible light, ultraviolet radiation, and infrared radiation that warm the Earth's surface and atmosphere. Gases like carbon dioxide in the atmosphere contribute to the greenhouse effect by trapping heat. The amount of solar energy reaching different locations on Earth depends on latitude and time of year due to variations in the sun's angle and the spread of its energy across larger areas.
The document discusses how solar radiation interacts with the Earth's atmosphere and maintains the planet's energy balance. It explains that the sun radiates energy in the form of electromagnetic waves, which interact with gases in the atmosphere through scattering, absorption, and transmission. Some solar energy is scattered back into space by particles, while some reaches the Earth's surface. Gases like ozone, carbon dioxide, and water vapor absorb radiation at different wavelengths. Together with radiation laws like Stefan-Boltzmann and Planck's law, this governs the spectrum of solar radiation that reaches the Earth and is re-radiated back to space, maintaining the planet's temperature.
1) An atmosphere is a layer of gas that surrounds a world and can be obtained through comet impacts, outgassing during planetary differentiation and volcanism, and ongoing volcanic outgassing.
2) Atmospheric properties like temperature and composition vary with altitude due to interactions with sunlight.
3) Key atmospheric processes include gaining gases through volcanism and impacts and losing them through escape and surface interactions, while the greenhouse effect traps heat from the sun.
1) Even small variations in the sun's output, such as the 0.1% change over the sun's 11-year solar cycle, can significantly impact Earth's climate through complex interactions between the atmosphere and ocean.
2) The sun's extreme ultraviolet radiation varies by much larger factors of 10 over the solar cycle, strongly affecting the chemistry and temperature of the upper atmosphere in ways that can influence surface weather patterns.
3) Recent studies provide evidence that solar variability leaves an imprint on regional climates like the Pacific Ocean through both "top-down" and "bottom-up" atmospheric and oceanic mechanisms.
Volcanic Eruptions Are Awesome Manifestations Of Heat Flowing Non-Explosively As A Result Of Mantle Hot Spots (E.G., Hawaii And Iceland) Or Erupting Explosively (e.g., The Pacific Rim, Atlantic Ridge). Volcano Hazards Can Have Far Reaching Impacts Lava Flows: Lahars (Can Bury Villages); Earthquakes (Related To Movement Of magma); “volcanic Winter” (Causing Famine And Mass Extinctions). The Reasons For A Disaster To Occur: The Community Is Un-Prepared For What Will Likely Happen, Not To Mention The Low-Probability Of Occurrence—high-Probability-Of-Adverse- Consequences Event. The Community Has No Disaster Planning Scenario Or Warning System In Place As A Strategic Framework For Early Threat Identification And Coordinated Local, National, Regional, And International Countermeasures. The Community Is Inefficient During Recovery And Reconstruction Because It Has Not Learned From Either The Current Experience Or The Cumulative Prior Experiences. The Keys To Resilience: 1) Know The Eruptive History Of Your Region’s Volcanoes, 2) Be Prepared (e.g., exposure analysis (it is not enough to analyse the hazard) and then systematically analyse vulnerability/fragility of the exposed elements. 3) Have A Warning System 4) Evacuate 5) Learn From The Experience And Start Over. Presentation courtesy of Dr Walter Hays, Global Alliance for Disaster Reduction
The volcano Eyjafjallajökull in Iceland erupted twice in 2010, disrupting air traffic across Northern Europe. The April 2010 eruption was ten to twenty times more powerful than the March eruption. Eyjafjallajökull is a 1,666 meter tall volcano covered by a glacier, and has erupted frequently since the last ice age, with its most recent eruption before 2010 being from 1821 to 1823. The crater of the volcano has a diameter of 3-4 kilometers and the glacier covers an area of about 100 square kilometers.
The volcano Eyjafjallajökull in Iceland erupted twice in 2010, in March and April. The April eruption was ten to twenty times more powerful than the March event and caused massive disruption to air traffic across Northern Europe. The volcano, which is covered by a glacier, has erupted frequently since the last Ice Age, with its most recent eruption before 2010 occurring between 1821 and 1823.
The document summarizes key concepts about the Earth's energy balance. It explains that the atmosphere absorbs and scatters some incoming solar radiation while allowing visible light to pass through, and greenhouse gases like carbon dioxide and water vapor in the atmosphere absorb outgoing infrared radiation from the Earth's surface, enhancing the greenhouse effect and warming the planet. The Earth's temperature remains relatively constant over time as the gains and losses of radiant energy are balanced on a global scale, though human activities can affect these energy flows and potentially disrupt this balance.
This document discusses how energy from the sun interacts with the atmosphere and Earth's surface. Solar radiation enters the atmosphere and is scattered, refracted, reflected, or absorbed. Atmospheric gases and particles influence these processes. Absorbed radiation is transferred within the atmosphere and at the surface via conduction, convection, and radiation. Greenhouse gases in the atmosphere and clouds contribute to the greenhouse effect by trapping infrared radiation emitted from the surface. The surface and atmospheric energy budgets describe the distribution of solar energy after it passes through the atmosphere and reaches the Earth's surface.
The atmosphere consists of 78% nitrogen, 21% oxygen and trace amounts of other gases that make life possible on Earth. It protects the planet from harmful rays and meteorites. Weather occurs in the lower layer of the atmosphere, the troposphere, which extends up to 12 miles high and where temperatures decrease with altitude. Higher layers include the stratosphere, mesosphere, thermosphere and outermost exosphere. Climate is associated with a place and includes daily, seasonal and yearly variations in elements like temperature, precipitation, humidity, pressure and wind. Factors influencing climate include latitude, altitude, land and ocean distribution, barriers and currents.
Atmosphere & surface energy balanceNagina Nighat
The document discusses concepts related to solar radiation and Earth's energy balance. It begins by describing how the Sun generates energy through nuclear fusion and emits it as electromagnetic waves. It then defines insolation as the amount of solar radiation reaching a given area, noting it varies by location and time. Finally, it explains that Earth's climate is powered by solar energy and achieves radiative equilibrium when the amount of incoming solar energy balances the amount radiated back to space, keeping global temperatures stable.
All energy from the sun that reaches Earth is converted to thermal energy or heat. The amount of heat absorbed at the surface varies by location and time due to factors like the sun's angle, cloud cover, Earth's distance from the sun, and greenhouse gases trapping heat in the atmosphere. This trapped heat maintains Earth's temperature through the greenhouse effect, resembling the way a greenhouse warms an environment for plants. Different surfaces like land, water, and air heat up differently via radiation, convection, and conduction.
Earth's Energy Budget and solar radiation (with Animations)Sameer baloch
about earth's Energy budget. how much coming and how much radiation leaving from our surface to atmosphere from atmo to space with animated picture.
it clears your concept by animated gif photos
The document discusses solar flares, including how they occur due to magnetic reconnection on the sun's surface, their stages of development, their recorded effects on Earth including disrupting telegraph systems in 1859, potential impacts such as damaging electronics and electrical infrastructure, challenges predicting them, and recommendations for preparing like having backup power sources and fuel.
This document discusses electromagnetic radiation (EMR) and its interaction with the atmosphere. It covers the following key points:
1) EMR can be described as waves with different wavelengths that determine their energy content. Shorter wavelengths like gamma rays have higher energy.
2) The atmosphere only allows certain wavelengths to pass through in "atmospheric windows" while absorbing others. Gases like oxygen, nitrogen, ozone, carbon dioxide and water vapor are significant absorbers.
3) Factors like albedo, scattering, temperature inversions, and cloud cover influence the transmission and absorption of EMR and impact atmospheric temperatures.
Solar storms are known as called solar flares. The solar magnetic field causes solar activities. It is an intense burst of radiation that is generated due to the release of magnetic energy from the sunspots. These are the biggest explosive events in our solar system. The solar storm looks like a bright spot in the sun, lasting from a few minutes to a few hours.
This document discusses various topics relating to physical geography and temperature, including:
- The electromagnetic spectrum and how different wavelengths of light refract differently.
- The greenhouse effect and how gases like carbon dioxide and methane trap heat.
- The various controls on temperature, including latitude, proximity to water, cloud cover, urbanization and more.
- How water moderates temperature through processes like evaporation and its higher specific heat.
- Different types of heat transfer and how phase changes in water absorb or release heat.
The document discusses the Earth's radiation balance and how human activity is impacting it through increased greenhouse gas emissions, leading to global warming. It explains that the Earth maintains a temperature balance through absorbing and emitting radiation. Increased greenhouse gases like carbon dioxide and methane absorb more outgoing radiation, disrupting this balance and causing warming. It outlines various impacts of global warming like melting ice caps, more extreme weather, and discusses efforts to reduce emissions and mitigate further impacts.
The document summarizes how energy from the sun is transferred within the Earth's atmosphere and surfaces. It explains that some solar energy is reflected by gases and particles in the atmosphere, while some is absorbed by the land and water, warming the Earth's surface. It also describes the different methods by which heat is transferred, including radiation from the sun or fires, conduction between touching substances, and convection through fluid movements like air currents.
Solar flares are violent eruptions on the Sun's surface that can release energy equivalent to millions of hydrogen bombs and last a few minutes. During flares, material is ejected into space at up to 1000 km/s in coronal mass ejections, which produce bursts in the solar wind that influence the solar system, including Earth by causing increased auroras and activity days later. Flares are associated with the Sun's magnetic field and occur more frequently near solar maximum when interactions between opposing magnetic fields are more common due to increased solar activity and sunspots.
Earth's energy budget refers to the tracking of how much energy is flowing into and out of the Earth's climate, where the energy is going, and if the energy coming in balances with the energy going out. The Earth receives energy from the Sun, and it also reflects and radiates energy back into space. All of the energy that warms the atmosphere, oceans and land must be radiated back into space in order to maintain our current climate. If the amount of energy radiating back into space is decreased by even a very small amount, it can lead to warming. It is believed that increasing levels of carbon dioxide in the atmosphere has a 'greenhouse effect' of reducing the amount of energy radiated into space.
The document discusses the key factors that influence weather and climate on Earth, including heat from the sun, atmospheric gases, and their interactions. It explains that the sun provides visible light, ultraviolet radiation, and infrared radiation that warm the Earth's surface and atmosphere. Gases like carbon dioxide in the atmosphere contribute to the greenhouse effect by trapping heat. The amount of solar energy reaching different locations on Earth depends on latitude and time of year due to variations in the sun's angle and the spread of its energy across larger areas.
The document discusses how solar radiation interacts with the Earth's atmosphere and maintains the planet's energy balance. It explains that the sun radiates energy in the form of electromagnetic waves, which interact with gases in the atmosphere through scattering, absorption, and transmission. Some solar energy is scattered back into space by particles, while some reaches the Earth's surface. Gases like ozone, carbon dioxide, and water vapor absorb radiation at different wavelengths. Together with radiation laws like Stefan-Boltzmann and Planck's law, this governs the spectrum of solar radiation that reaches the Earth and is re-radiated back to space, maintaining the planet's temperature.
1) An atmosphere is a layer of gas that surrounds a world and can be obtained through comet impacts, outgassing during planetary differentiation and volcanism, and ongoing volcanic outgassing.
2) Atmospheric properties like temperature and composition vary with altitude due to interactions with sunlight.
3) Key atmospheric processes include gaining gases through volcanism and impacts and losing them through escape and surface interactions, while the greenhouse effect traps heat from the sun.
1) Even small variations in the sun's output, such as the 0.1% change over the sun's 11-year solar cycle, can significantly impact Earth's climate through complex interactions between the atmosphere and ocean.
2) The sun's extreme ultraviolet radiation varies by much larger factors of 10 over the solar cycle, strongly affecting the chemistry and temperature of the upper atmosphere in ways that can influence surface weather patterns.
3) Recent studies provide evidence that solar variability leaves an imprint on regional climates like the Pacific Ocean through both "top-down" and "bottom-up" atmospheric and oceanic mechanisms.
Volcanic Eruptions Are Awesome Manifestations Of Heat Flowing Non-Explosively As A Result Of Mantle Hot Spots (E.G., Hawaii And Iceland) Or Erupting Explosively (e.g., The Pacific Rim, Atlantic Ridge). Volcano Hazards Can Have Far Reaching Impacts Lava Flows: Lahars (Can Bury Villages); Earthquakes (Related To Movement Of magma); “volcanic Winter” (Causing Famine And Mass Extinctions). The Reasons For A Disaster To Occur: The Community Is Un-Prepared For What Will Likely Happen, Not To Mention The Low-Probability Of Occurrence—high-Probability-Of-Adverse- Consequences Event. The Community Has No Disaster Planning Scenario Or Warning System In Place As A Strategic Framework For Early Threat Identification And Coordinated Local, National, Regional, And International Countermeasures. The Community Is Inefficient During Recovery And Reconstruction Because It Has Not Learned From Either The Current Experience Or The Cumulative Prior Experiences. The Keys To Resilience: 1) Know The Eruptive History Of Your Region’s Volcanoes, 2) Be Prepared (e.g., exposure analysis (it is not enough to analyse the hazard) and then systematically analyse vulnerability/fragility of the exposed elements. 3) Have A Warning System 4) Evacuate 5) Learn From The Experience And Start Over. Presentation courtesy of Dr Walter Hays, Global Alliance for Disaster Reduction
The volcano Eyjafjallajökull in Iceland erupted twice in 2010, disrupting air traffic across Northern Europe. The April 2010 eruption was ten to twenty times more powerful than the March eruption. Eyjafjallajökull is a 1,666 meter tall volcano covered by a glacier, and has erupted frequently since the last ice age, with its most recent eruption before 2010 being from 1821 to 1823. The crater of the volcano has a diameter of 3-4 kilometers and the glacier covers an area of about 100 square kilometers.
The volcano Eyjafjallajökull in Iceland erupted twice in 2010, in March and April. The April eruption was ten to twenty times more powerful than the March event and caused massive disruption to air traffic across Northern Europe. The volcano, which is covered by a glacier, has erupted frequently since the last Ice Age, with its most recent eruption before 2010 occurring between 1821 and 1823.
The document discusses Iceland's unique position astride the Mid-Atlantic Ridge tectonic plate boundary. Iceland experiences frequent volcanic eruptions from divergent tectonic activity, with a recent eruption in 2010 from the Eyjafjallajökull volcano. Iceland's volcanism, while less destructive than convergent boundaries, helps form new land as the plates pull apart and magma rises to fill the gaps. The island nation has a population of over 300,000, with 92% living in urban areas and the economy dependent on fishing and geothermal/hydropower energy.
There are several main types of volcanoes classified based on their shape, eruptive behavior, and composition. Composite volcanoes, also known as stratovolcanoes, are conical mountains built up by viscous lava flows and explosive eruptions, examples being Mount St. Helens and Mount Pinatubo. Shield volcanoes are larger and less steeply sloped, constructed by fluid basaltic lava flows like those of Hawaii. Small cinder cones form from explosive eruptions of pyroclastic material. Fissure eruptions produce fluid lava flows from cracks in the crust along zones of weakness.
WHAT IS HAPPENING? AIRLINES ON RED ALERT AFTER VOLCANIC ERUPTION IN ICELAND. After a week of seismic activity rattled the uninhabited area 200 miles (320 kilometers) east of the capital of Reykjavik with thou-sands of earthquakes, Iceland's Bardarbunga volcano began erupting Saturday (Aug. 23rd) under the country's largest glacier. An Iceland volcanologist said it was not clear when, or if, the eruption would melt through the ice — which is between 100 and 400 meters (330 feet and 1,300 feet) thick — and send steam and ash into the air. On Saturday, Icelandic authorities declared a no-fly zone of 100 nautical miles by 140 nautical miles around the eruption, but did not shut the country's airspace. An eruption at the Katla volcano could be disastrous, both for Iceland and other nations. Presentation courtesy of Dr. Walter Hays, Global Alliance for Disaster Reduction
This document lists several volcanoes in Iceland and websites about volcanoes. It discusses Krafla volcano which last erupted in 1984 and is 650m high. It also mentions the recent eruptions of Eyjafjallajökull and Fimmvörðuháls volcanoes. Several Icelandic and international websites about volcanoes, geology, and natural disasters in Iceland are listed, including those run by the Icelandic Earth Sciences Institute and the Global Volcanism Program.
Alaska has high volcanic activity with over 90 historically active volcanoes due to its position along the Pacific Ring of Fire. These volcanoes pose hazards such as ash falls, lava flows, pyroclastic flows, and tsunamis. The U.S. Geological Survey monitors Alaskan volcanoes using seismic, GPS, gas, and visual data to analyze unrest and eruptive activity in order to provide warnings to communities and aviation.
The document summarizes an expedition to Mt. Etna in Sicily to measure and compare energy levels near the active volcano to levels near the Ionian Sea. An advanced scientific instrument measured significantly higher energy levels at Mt. Etna (7.68) than at the sea (4.84). Standard deviation readings also spiked at Mt. Etna, correlating with a seismic burst. The findings suggest volcanic areas have higher energy and this technology may help predict earth-related signals.
Geography Project on Volcanoes, made by a 14 year old student as his school submission work, has almost all the required information about the Volcanoes and includes case studies & maps of major volcanic regions of the world, active volcanoes of the world, Volcanic eruptions in the modern times.
Copyright (c) 2021-2022 Ishan Ketan Bhavsar
TO BE USED FOR EDUCATIONAL PURPOSES ONLY
This presentation provides an overview of volcanoes, including their formation from plate tectonics or hotspots, the different types of volcanic features and erupted materials, classifications of volcanic activity, and notable examples. Volcanic activity can have effects on global climate through emissions into the stratosphere and impacts soil through added nutrients.
The document discusses Eyjafjallajökull, a glacier volcano located in Iceland. It describes how in 2010 Eyjafjallajökull erupted twice, with the second eruption spewing ash kilometers into the atmosphere and causing major flight disruptions across Europe. The eruption also caused flooding from melted glacier water. The document notes that past eruptions of Eyjafjallajökull have preceded eruptions of the nearby and more powerful Katla volcano, raising concerns that Katla may erupt soon.
Volcanoes form when molten rock escapes through openings in the earth's crust. There are over 500 active volcanoes worldwide, with 75% located on the Ring of Fire around the Pacific Ocean. The main types of volcanoes are cinder cones, composite volcanoes, shield volcanoes, and lava domes, which vary based on the viscosity of the erupted lava and shape of the volcanic feature. Cinder cones are small and steep, while shield volcanoes are broad and gently sloping due to highly fluid lava flows. Composite and lava dome volcanoes have more explosive eruptions of viscous magma.
Natural disasterPPT-Volcanoes made by Agastya DhanorkarAgastya Dhanorkar
This PPT consists slides and matter on Volcanoes please coment below if you liked this. This is my first upload. thank you...... ALSO my youtube channel is Agastya Dhanorkar
Similar to Ice & Fire: The Volcano Eruption of Eyjafjallajökull (15)
Sexuality - Issues, Attitude and Behaviour - Applied Social Psychology - Psyc...PsychoTech Services
A proprietary approach developed by bringing together the best of learning theories from Psychology, design principles from the world of visualization, and pedagogical methods from over a decade of training experience, that enables you to: Learn better, faster!
Candidate young stellar objects in the S-cluster: Kinematic analysis of a sub...Sérgio Sacani
Context. The observation of several L-band emission sources in the S cluster has led to a rich discussion of their nature. However, a definitive answer to the classification of the dusty objects requires an explanation for the detection of compact Doppler-shifted Brγ emission. The ionized hydrogen in combination with the observation of mid-infrared L-band continuum emission suggests that most of these sources are embedded in a dusty envelope. These embedded sources are part of the S-cluster, and their relationship to the S-stars is still under debate. To date, the question of the origin of these two populations has been vague, although all explanations favor migration processes for the individual cluster members. Aims. This work revisits the S-cluster and its dusty members orbiting the supermassive black hole SgrA* on bound Keplerian orbits from a kinematic perspective. The aim is to explore the Keplerian parameters for patterns that might imply a nonrandom distribution of the sample. Additionally, various analytical aspects are considered to address the nature of the dusty sources. Methods. Based on the photometric analysis, we estimated the individual H−K and K−L colors for the source sample and compared the results to known cluster members. The classification revealed a noticeable contrast between the S-stars and the dusty sources. To fit the flux-density distribution, we utilized the radiative transfer code HYPERION and implemented a young stellar object Class I model. We obtained the position angle from the Keplerian fit results; additionally, we analyzed the distribution of the inclinations and the longitudes of the ascending node. Results. The colors of the dusty sources suggest a stellar nature consistent with the spectral energy distribution in the near and midinfrared domains. Furthermore, the evaporation timescales of dusty and gaseous clumps in the vicinity of SgrA* are much shorter ( 2yr) than the epochs covered by the observations (≈15yr). In addition to the strong evidence for the stellar classification of the D-sources, we also find a clear disk-like pattern following the arrangements of S-stars proposed in the literature. Furthermore, we find a global intrinsic inclination for all dusty sources of 60 ± 20◦, implying a common formation process. Conclusions. The pattern of the dusty sources manifested in the distribution of the position angles, inclinations, and longitudes of the ascending node strongly suggests two different scenarios: the main-sequence stars and the dusty stellar S-cluster sources share a common formation history or migrated with a similar formation channel in the vicinity of SgrA*. Alternatively, the gravitational influence of SgrA* in combination with a massive perturber, such as a putative intermediate mass black hole in the IRS 13 cluster, forces the dusty objects and S-stars to follow a particular orbital arrangement. Key words. stars: black holes– stars: formation– Galaxy: center– galaxies: star formation
Signatures of wave erosion in Titan’s coastsSérgio Sacani
The shorelines of Titan’s hydrocarbon seas trace flooded erosional landforms such as river valleys; however, it isunclear whether coastal erosion has subsequently altered these shorelines. Spacecraft observations and theo-retical models suggest that wind may cause waves to form on Titan’s seas, potentially driving coastal erosion,but the observational evidence of waves is indirect, and the processes affecting shoreline evolution on Titanremain unknown. No widely accepted framework exists for using shoreline morphology to quantitatively dis-cern coastal erosion mechanisms, even on Earth, where the dominant mechanisms are known. We combinelandscape evolution models with measurements of shoreline shape on Earth to characterize how differentcoastal erosion mechanisms affect shoreline morphology. Applying this framework to Titan, we find that theshorelines of Titan’s seas are most consistent with flooded landscapes that subsequently have been eroded bywaves, rather than a uniform erosional process or no coastal erosion, particularly if wave growth saturates atfetch lengths of tens of kilometers.
PPT on Sustainable Land Management presented at the three-day 'Training and Validation Workshop on Modules of Climate Smart Agriculture (CSA) Technologies in South Asia' workshop on April 22, 2024.
SDSS1335+0728: The awakening of a ∼ 106M⊙ black hole⋆Sérgio Sacani
Context. The early-type galaxy SDSS J133519.91+072807.4 (hereafter SDSS1335+0728), which had exhibited no prior optical variations during the preceding two decades, began showing significant nuclear variability in the Zwicky Transient Facility (ZTF) alert stream from December 2019 (as ZTF19acnskyy). This variability behaviour, coupled with the host-galaxy properties, suggests that SDSS1335+0728 hosts a ∼ 106M⊙ black hole (BH) that is currently in the process of ‘turning on’. Aims. We present a multi-wavelength photometric analysis and spectroscopic follow-up performed with the aim of better understanding the origin of the nuclear variations detected in SDSS1335+0728. Methods. We used archival photometry (from WISE, 2MASS, SDSS, GALEX, eROSITA) and spectroscopic data (from SDSS and LAMOST) to study the state of SDSS1335+0728 prior to December 2019, and new observations from Swift, SOAR/Goodman, VLT/X-shooter, and Keck/LRIS taken after its turn-on to characterise its current state. We analysed the variability of SDSS1335+0728 in the X-ray/UV/optical/mid-infrared range, modelled its spectral energy distribution prior to and after December 2019, and studied the evolution of its UV/optical spectra. Results. From our multi-wavelength photometric analysis, we find that: (a) since 2021, the UV flux (from Swift/UVOT observations) is four times brighter than the flux reported by GALEX in 2004; (b) since June 2022, the mid-infrared flux has risen more than two times, and the W1−W2 WISE colour has become redder; and (c) since February 2024, the source has begun showing X-ray emission. From our spectroscopic follow-up, we see that (i) the narrow emission line ratios are now consistent with a more energetic ionising continuum; (ii) broad emission lines are not detected; and (iii) the [OIII] line increased its flux ∼ 3.6 years after the first ZTF alert, which implies a relatively compact narrow-line-emitting region. Conclusions. We conclude that the variations observed in SDSS1335+0728 could be either explained by a ∼ 106M⊙ AGN that is just turning on or by an exotic tidal disruption event (TDE). If the former is true, SDSS1335+0728 is one of the strongest cases of an AGNobserved in the process of activating. If the latter were found to be the case, it would correspond to the longest and faintest TDE ever observed (or another class of still unknown nuclear transient). Future observations of SDSS1335+0728 are crucial to further understand its behaviour. Key words. galaxies: active– accretion, accretion discs– galaxies: individual: SDSS J133519.91+072807.4
JAMES WEBB STUDY THE MASSIVE BLACK HOLE SEEDSSérgio Sacani
The pathway(s) to seeding the massive black holes (MBHs) that exist at the heart of galaxies in the present and distant Universe remains an unsolved problem. Here we categorise, describe and quantitatively discuss the formation pathways of both light and heavy seeds. We emphasise that the most recent computational models suggest that rather than a bimodal-like mass spectrum between light and heavy seeds with light at one end and heavy at the other that instead a continuum exists. Light seeds being more ubiquitous and the heavier seeds becoming less and less abundant due the rarer environmental conditions required for their formation. We therefore examine the different mechanisms that give rise to different seed mass spectrums. We show how and why the mechanisms that produce the heaviest seeds are also among the rarest events in the Universe and are hence extremely unlikely to be the seeds for the vast majority of the MBH population. We quantify, within the limits of the current large uncertainties in the seeding processes, the expected number densities of the seed mass spectrum. We argue that light seeds must be at least 103 to 105 times more numerous than heavy seeds to explain the MBH population as a whole. Based on our current understanding of the seed population this makes heavy seeds (Mseed > 103 M⊙) a significantly more likely pathway given that heavy seeds have an abundance pattern than is close to and likely in excess of 10−4 compared to light seeds. Finally, we examine the current state-of-the-art in numerical calculations and recent observations and plot a path forward for near-future advances in both domains.
PPT on Direct Seeded Rice presented at the three-day 'Training and Validation Workshop on Modules of Climate Smart Agriculture (CSA) Technologies in South Asia' workshop on April 22, 2024.
Anti-Universe And Emergent Gravity and the Dark UniverseSérgio Sacani
Recent theoretical progress indicates that spacetime and gravity emerge together from the entanglement structure of an underlying microscopic theory. These ideas are best understood in Anti-de Sitter space, where they rely on the area law for entanglement entropy. The extension to de Sitter space requires taking into account the entropy and temperature associated with the cosmological horizon. Using insights from string theory, black hole physics and quantum information theory we argue that the positive dark energy leads to a thermal volume law contribution to the entropy that overtakes the area law precisely at the cosmological horizon. Due to the competition between area and volume law entanglement the microscopic de Sitter states do not thermalise at sub-Hubble scales: they exhibit memory effects in the form of an entropy displacement caused by matter. The emergent laws of gravity contain an additional ‘dark’ gravitational force describing the ‘elastic’ response due to the entropy displacement. We derive an estimate of the strength of this extra force in terms of the baryonic mass, Newton’s constant and the Hubble acceleration scale a0 = cH0, and provide evidence for the fact that this additional ‘dark gravity force’ explains the observed phenomena in galaxies and clusters currently attributed to dark matter.
Microbial interaction
Microorganisms interacts with each other and can be physically associated with another organisms in a variety of ways.
One organism can be located on the surface of another organism as an ectobiont or located within another organism as endobiont.
Microbial interaction may be positive such as mutualism, proto-cooperation, commensalism or may be negative such as parasitism, predation or competition
Types of microbial interaction
Positive interaction: mutualism, proto-cooperation, commensalism
Negative interaction: Ammensalism (antagonism), parasitism, predation, competition
I. Mutualism:
It is defined as the relationship in which each organism in interaction gets benefits from association. It is an obligatory relationship in which mutualist and host are metabolically dependent on each other.
Mutualistic relationship is very specific where one member of association cannot be replaced by another species.
Mutualism require close physical contact between interacting organisms.
Relationship of mutualism allows organisms to exist in habitat that could not occupied by either species alone.
Mutualistic relationship between organisms allows them to act as a single organism.
Examples of mutualism:
i. Lichens:
Lichens are excellent example of mutualism.
They are the association of specific fungi and certain genus of algae. In lichen, fungal partner is called mycobiont and algal partner is called
II. Syntrophism:
It is an association in which the growth of one organism either depends on or improved by the substrate provided by another organism.
In syntrophism both organism in association gets benefits.
Compound A
Utilized by population 1
Compound B
Utilized by population 2
Compound C
utilized by both Population 1+2
Products
In this theoretical example of syntrophism, population 1 is able to utilize and metabolize compound A, forming compound B but cannot metabolize beyond compound B without co-operation of population 2. Population 2is unable to utilize compound A but it can metabolize compound B forming compound C. Then both population 1 and 2 are able to carry out metabolic reaction which leads to formation of end product that neither population could produce alone.
Examples of syntrophism:
i. Methanogenic ecosystem in sludge digester
Methane produced by methanogenic bacteria depends upon interspecies hydrogen transfer by other fermentative bacteria.
Anaerobic fermentative bacteria generate CO2 and H2 utilizing carbohydrates which is then utilized by methanogenic bacteria (Methanobacter) to produce methane.
ii. Lactobacillus arobinosus and Enterococcus faecalis:
In the minimal media, Lactobacillus arobinosus and Enterococcus faecalis are able to grow together but not alone.
The synergistic relationship between E. faecalis and L. arobinosus occurs in which E. faecalis require folic acid
2. Eyjafjallajökull [ˈeɪjaˌfjatlaˌjœːkʏtl̥]
• Pronounced: AY-yah-fyad-layer-kuh-tel
• “Eyjafjallajökull” translates as “Island Mountain Glacier”, and actually
refers to the glacier on top of the volcano
• The volcano itself is named “Eyjafjöll”
• Elevation of volcano is 5,466 feet
• Located on Mid-Atlantic Ridge, which runs through the island
5. Major eruptions begin, plume reaches 26,000 ft, seen here mixed with lightning (Reuters/Lucas Jackson).
6. Ash Cloud Elevation
NASA/CNES elevation data using Cloud-Aerosol Lidar and Infrared Pathfinder Satellite
Observations (CALIPSO) imagery. The yellow layer under volcanic plume is air pollution in Paris.
Ash Cloud
• 6,000-21,000 feet in altitude
• Some traces reached 30,000 feet
CALIPSO
• Uses pulsating lasers aimed at
ground from satellites
• Measures particles/aerosols such
as dust, smoke, and pollution
• Creates a vertical profile of the
atmosphere