Chasing the Auroras: Borealis & Polaris
•
0 likes•88 views
The auroras, also known as the northern and southern lights, are beautiful displays of light in the sky that occur when charged particles from the sun interact with gases in the Earth's atmosphere. These particles are dragged into the atmosphere by the Earth's magnetic field, traveling down magnetic field lines at the north and south poles to result in the aurora that can only be seen at night, though they occur throughout the day.
Report
Share
Report
Share
Download to read offline
Recommended
WHY ARE AURORAS FORMED ? 
For more such informative content, go to https://scifitechify.blogspot.com/. This video will give you the brief expanation as to why these colourful and wonderful auroras are formed in northern places. NEXT POST ON: WHAT IS A MIRAGE ?
The Aurora Borealis
The Northern Lights, or Aurora Borealis, are caused by interactions between the Earth's magnetic field and particles from the Sun. When solar storms eject electrons and protons from the Sun's surface, they travel through space and enter the Earth's atmosphere near the magnetic poles. There, the particles excite oxygen and nitrogen atoms in the atmosphere, causing them to glow in colorful patterns of light. These lights appear as veils, ribbons, or curtains and are centered around the magnetic north and south poles, extending further during times of strong solar activity. The temperature of the Sun's atmosphere reaches millions of degrees, causing hydrogen to break into electrons and protons. The solar wind carries this ionized plasma and the Sun's magnetic field outward into space
Aurora boreala
The Northern Lights, or Aurora Borealis, are caused by interactions between the Earth's magnetic field and particles from the Sun. When solar storms eject electrons and protons from the Sun's surface, they travel through space and enter the Earth's atmosphere near the magnetic poles. There, the particles excite oxygen and nitrogen atoms in the atmosphere, causing them to glow in colorful patterns of light. These lights appear as veils, ribbons, or curtains and are centered around the magnetic north and south poles, extending further during times of strong solar activity. The temperature of the Sun's atmosphere reaches millions of degrees, causing hydrogen to break into electrons and protons. The solar wind carries this ionized plasma and the Sun's magnetic field outward into space
The Aurora Borealis
The Northern Lights, or Aurora Borealis, are caused by interactions between the Earth's magnetic field and particles from the Sun. When solar storms eject electrons and protons from the Sun's surface, they travel through space and enter the Earth's atmosphere near the magnetic poles. There, the particles excite oxygen and nitrogen atoms in the atmosphere, causing them to glow in colorful patterns of light known as the Northern Lights. The size and shape of the Aurora is determined by the level of activity on the Sun - more active periods result in a larger and more extended light display.
The Aurora Borealis
The Northern Lights, or Aurora Borealis, are caused by interactions between the Earth's magnetic field and particles from the Sun. When solar storms eject electrons and protons from the Sun's surface, they travel through space and enter the Earth's atmosphere near the magnetic poles. There, the particles excite oxygen and nitrogen atoms in the atmosphere, causing them to glow in colorful patterns of light in the sky. The location and size of the light displays depend on the level of activity on the Sun's surface. During periods of high solar activity, the auroral oval expands and the Northern Lights can be seen further from the poles.
Aurora boreala -muzica
The document discusses the Aurora Borealis (Northern Lights). It explains that the lights are caused by charged particles from the sun interacting with the earth's magnetic field. During solar storms, electrons and protons from the sun enter the earth's atmosphere where they cause nitrogen and oxygen atoms to become energized and glow in colorful patterns. The particles are guided by the magnetic field to the magnetic poles, appearing as lights near the north and south poles. The size and shape of the lights depends on the level of solar activity.
Aurora Presentation by Syed Hashir
The document discusses auroras, which are displays of light in the night sky caused by collisions between the solar wind and Earth's magnetosphere. When solar wind particles interact with oxygen and nitrogen atoms in Earth's upper atmosphere, the atoms become excited and emit photons of light in colors like green, red, and blue. Auroras are typically seen near Earth's magnetic poles as the solar wind is guided there by Earth's magnetic field. Other planets like Jupiter and Saturn also have auroras caused by similar mechanisms, while planets without magnetospheres like Venus and Mars do not show the phenomenon. Auroras are important to study as the charged particles and currents they produce can interfere with communication systems and satellites.
Venus
Venus can be seen from Earth and looks like the morning star before sunrise and the evening star after sunset. It orbits the sun every 225 days, compared to Earth's 365 day orbit. Venus is similar in size to Earth but is the hottest planet due to its dense carbon dioxide atmosphere and greenhouse effect, with surface temperatures over 800°F. The first spacecraft to land on Venus in 1975 sent back images, providing the first photos from the surface.
Recommended
WHY ARE AURORAS FORMED ?
For more such informative content, go to https://scifitechify.blogspot.com/. This video will give you the brief expanation as to why these colourful and wonderful auroras are formed in northern places. NEXT POST ON: WHAT IS A MIRAGE ?
The Aurora Borealis
The Northern Lights, or Aurora Borealis, are caused by interactions between the Earth's magnetic field and particles from the Sun. When solar storms eject electrons and protons from the Sun's surface, they travel through space and enter the Earth's atmosphere near the magnetic poles. There, the particles excite oxygen and nitrogen atoms in the atmosphere, causing them to glow in colorful patterns of light. These lights appear as veils, ribbons, or curtains and are centered around the magnetic north and south poles, extending further during times of strong solar activity. The temperature of the Sun's atmosphere reaches millions of degrees, causing hydrogen to break into electrons and protons. The solar wind carries this ionized plasma and the Sun's magnetic field outward into space
Aurora boreala
The Northern Lights, or Aurora Borealis, are caused by interactions between the Earth's magnetic field and particles from the Sun. When solar storms eject electrons and protons from the Sun's surface, they travel through space and enter the Earth's atmosphere near the magnetic poles. There, the particles excite oxygen and nitrogen atoms in the atmosphere, causing them to glow in colorful patterns of light. These lights appear as veils, ribbons, or curtains and are centered around the magnetic north and south poles, extending further during times of strong solar activity. The temperature of the Sun's atmosphere reaches millions of degrees, causing hydrogen to break into electrons and protons. The solar wind carries this ionized plasma and the Sun's magnetic field outward into space
The Aurora Borealis
The Northern Lights, or Aurora Borealis, are caused by interactions between the Earth's magnetic field and particles from the Sun. When solar storms eject electrons and protons from the Sun's surface, they travel through space and enter the Earth's atmosphere near the magnetic poles. There, the particles excite oxygen and nitrogen atoms in the atmosphere, causing them to glow in colorful patterns of light known as the Northern Lights. The size and shape of the Aurora is determined by the level of activity on the Sun - more active periods result in a larger and more extended light display.
The Aurora Borealis
The Northern Lights, or Aurora Borealis, are caused by interactions between the Earth's magnetic field and particles from the Sun. When solar storms eject electrons and protons from the Sun's surface, they travel through space and enter the Earth's atmosphere near the magnetic poles. There, the particles excite oxygen and nitrogen atoms in the atmosphere, causing them to glow in colorful patterns of light in the sky. The location and size of the light displays depend on the level of activity on the Sun's surface. During periods of high solar activity, the auroral oval expands and the Northern Lights can be seen further from the poles.
Aurora boreala -muzica
The document discusses the Aurora Borealis (Northern Lights). It explains that the lights are caused by charged particles from the sun interacting with the earth's magnetic field. During solar storms, electrons and protons from the sun enter the earth's atmosphere where they cause nitrogen and oxygen atoms to become energized and glow in colorful patterns. The particles are guided by the magnetic field to the magnetic poles, appearing as lights near the north and south poles. The size and shape of the lights depends on the level of solar activity.
Aurora Presentation by Syed Hashir
The document discusses auroras, which are displays of light in the night sky caused by collisions between the solar wind and Earth's magnetosphere. When solar wind particles interact with oxygen and nitrogen atoms in Earth's upper atmosphere, the atoms become excited and emit photons of light in colors like green, red, and blue. Auroras are typically seen near Earth's magnetic poles as the solar wind is guided there by Earth's magnetic field. Other planets like Jupiter and Saturn also have auroras caused by similar mechanisms, while planets without magnetospheres like Venus and Mars do not show the phenomenon. Auroras are important to study as the charged particles and currents they produce can interfere with communication systems and satellites.
Venus
Venus can be seen from Earth and looks like the morning star before sunrise and the evening star after sunset. It orbits the sun every 225 days, compared to Earth's 365 day orbit. Venus is similar in size to Earth but is the hottest planet due to its dense carbon dioxide atmosphere and greenhouse effect, with surface temperatures over 800°F. The first spacecraft to land on Venus in 1975 sent back images, providing the first photos from the surface.
Meteors, Comets, and Asteroids
Comets are icy, dusty objects that orbit the Sun. They are composed of ice, dust, and small rocky particles. When a comet approaches the Sun, its ice warms and sublimates into gas, forming a coma - a fuzzy cloud around the comet. Solar wind and radiation pressure cause the coma to form two tails - a blue ion tail and a white dust tail. Comets can be short-period or long-period depending on the shape and size of their orbits.
Facts about planets
The document provides information about the planets in our solar system. It describes key facts about each planet such as their size, composition, rotation, and orbital periods. The Sun is described as the closest star to Earth, with temperatures reaching 15 million degrees Celsius. Mercury is the smallest planet and orbits the Sun every 88 Earth days. Venus rotates in the opposite direction of other planets and has surface temperatures over 400 degrees Celsius.
Mars Atmosphere Stripped by Solar Winds
The Martian atmosphere was stripped away by solar winds over time. NASA's MAVEN spacecraft discovered that during solar storms, the rate at which atoms were knocked out of Mars' atmosphere was 10-20 times higher than normal, with up to 5 pounds of atmosphere escaping every second. Without a global magnetic field to deflect solar winds like Earth, auroras occurred across Mars, further contributing to the loss of its atmosphere and liquid water over millions of years.
Solar promineneces rapp
Solar prominences are arcs of ionized solar gas that erupt from the sun's surface and extend hundreds of thousands of miles into the sun's atmosphere. They are held in place by the sun's magnetic field but are not static, lasting anywhere from hours to months before floating away. Solar prominences form because the sun's hot, magnetized interior churns in convective bubbles, tangling the magnetic field and causing large loops to burst through the surface into the atmosphere.
The Sun: Not Just Our Star
The sun is a huge glowing ball of gas at the center of our solar system that provides light, heat, and energy to Earth. It is made up primarily of hydrogen and helium and has a radius about 109 times that of Earth. The sun was formed around 4.6 billion years ago and will remain stable for another 5 billion years before expanding into a red giant. It emits electromagnetic radiation across the spectrum, including visible light and infrared that we experience as heat and light. Nuclear fusion in the sun's core converts hydrogen to helium and releases enormous amounts of energy.
Astronomy 4.1 Energy formation and layers of the Sun - IT6230
The document provides information about the sun, including that it is an average sized star located in one arm of the Milky Way galaxy. It is made up primarily of hydrogen and helium. The sun is very important to Earth as it provides heat, light and keeps Earth and other planets in orbit. It undergoes a solar cycle every 11 years where its magnetic field flips.
Mercury by Raghad
Mercury is the planet closest to the Sun and has extreme temperature variations. It has no atmosphere due to its small size and weak gravity. Mercury orbits the Sun very quickly, giving it the shortest year and day length of any planet in our solar system.
the sun!
The sun is a star at the center of our solar system that produces an immense amount of energy. It holds 98.8% of the total mass of the solar system and has a diameter 109 times that of Earth. The sun was born approximately 4.6 billion years ago from the collapse of a large cloud of dust and gases under the force of gravity, forming a hot, dense center that became the sun surrounded by planets. Sunspots, which are darker and cooler than surrounding areas, are caused by powerful magnetic fields emerging from below the sun's surface. Sometimes large eruptions from sunspots called solar storms can reach Earth and disrupt communication systems. Without the sun providing energy, life on Earth would not be possible as plants
4.1 The Sun is our Local Star
The document discusses the structure and composition of the Sun. It has 6 layers: the core, where fusion occurs at 15 million degrees Celsius; the radiative zone, where energy moves by radiation; the convection zone, where hot gas currents transfer energy; the photosphere, the visible surface; the chromosphere, a thin pinkish layer; and the corona, the outermost low density layer. The Sun is mostly made of hydrogen and helium and produces energy through the fusion of hydrogen into helium. It contains over 99% of the mass in the solar system and has prominent features like sunspots and solar winds.
Our universe
Planets of the Solar System. Star and a Planet, Amazing facts of different planets, Asteroids, Constellations
The sun
The sun is the largest object in the solar system, containing over 99% of its mass. It emits light and heat that support life on Earth and influence all solar system objects. The sun has various internal layers, including the core where energy is produced through nuclear fusion, and an outer atmosphere. Sunspots, solar flares, and other features periodically appear on its surface. In a few billion years, the sun will expand and grow hotter, eventually making Earth uninhabitable.
Earth’s Magnetism
The document discusses the Earth's magnetism. It explains that the Earth behaves like a giant bar magnet with a north and south magnetic pole. These magnetic poles are different from the geographic north and south poles and move about 10 km each year. The Earth's core is made of iron, a magnetic material, and its liquid outer core circulating around generates the planet's magnetic field through a process called the dynamo theory. The Earth's magnetic field protects the atmosphere from the sun's charged particles and is responsible for the northern and southern lights by trapping and directing solar particles toward the poles.
Simmi ppt 1
This document provides information about the solar system and its key components. It lists the nine planets in our solar system, from the Sun to Pluto. It explains that the solar system formed from a giant cloud of gas and dust in space that was disturbed by a supernova explosion, causing it to squeeze and form the Sun and planets. It provides details about each planet's characteristics, sizes and conditions. It also describes the Sun as the center of the system containing 98% of the mass, and notes Earth's moon Luna's proximity and surface features like mountains and craters.
Earth's Magnetic Field
This Powerpoint presentation shows the Magnetic Field of Earth. It also shows the parts of the Earth's Magnetic Field.
The Sun: Our Star
The Sun is made up of hot plasma and provides heat and light to our solar system. It is over 1000 times more massive than all the planets combined. The Sun has an interior of a core, radiation zone and convection zone where nuclear fusion occurs. It also has an atmosphere of a photosphere, chromosphere and corona. The different layers have varying temperatures, from over 15 million Kelvin in the core to around 6,000 Kelvin in the photosphere. The Sun also produces solar wind, prominences and flares.
WHY COMETS HAVE TAILS ?
For more such informative content, go to https://scifitechify.blogspot.com/. This video will give you brief information as to why comets have tials and how is it formed. NEXT POST ON: WHY ARE AURORAS FORMED ?
Our Closest Star, the Sun
Exploring our closest star, the Sun, its makeup, evolution, its place in the universe, and its significance to life on earth.
The layers of the atmosphere pontius
This document summarizes the layers of Earth's atmosphere. It describes 5 main layers - the troposphere, stratosphere, mesosphere, thermosphere, and exosphere. Each layer is defined by changes in temperature and the types of gases present. The troposphere contains around 78% nitrogen and 21% oxygen and extends 4-12 miles above the surface. The stratosphere contains ozone and temperature increases with height. The document compares Earth's atmosphere to those of other planets like Venus, Mars, and Saturn. It notes how Earth's atmosphere protects us and allows life to exist.
The Solar System
The Solar System consists of the Sun and eight planets as well as moons, asteroids, comets and dwarf planets. The planets in order from the Sun are Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus and Neptune. Each planet has unique characteristics such as Mercury having extreme temperature variations and Venus having hurricane-force winds and lightning. Earth is the only known planet capable of supporting life.
Astronomy unit 2011 SUN EARTH MOON SYSTEM acloutier copyright
The document provides an overview of concepts in astronomy including:
1) It describes Earth's rotation, the moon's effect on Earth, and how this impacts seasons and timekeeping.
2) It explains how the tilt of the Earth's axis and its orbit around the sun cause the seasons and equinoxes and solstices.
3) It discusses technology that has expanded our ability to observe space like telescopes, interferometry, and photography.
Multicultural Literacy
Literacy: Multiculturalism
The presentation contains animation.
Email for a copy:jesuitas.maryfrance3@gmail.com
More Related Content
What's hot
Meteors, Comets, and Asteroids
Comets are icy, dusty objects that orbit the Sun. They are composed of ice, dust, and small rocky particles. When a comet approaches the Sun, its ice warms and sublimates into gas, forming a coma - a fuzzy cloud around the comet. Solar wind and radiation pressure cause the coma to form two tails - a blue ion tail and a white dust tail. Comets can be short-period or long-period depending on the shape and size of their orbits.
Facts about planets
The document provides information about the planets in our solar system. It describes key facts about each planet such as their size, composition, rotation, and orbital periods. The Sun is described as the closest star to Earth, with temperatures reaching 15 million degrees Celsius. Mercury is the smallest planet and orbits the Sun every 88 Earth days. Venus rotates in the opposite direction of other planets and has surface temperatures over 400 degrees Celsius.
Mars Atmosphere Stripped by Solar Winds
The Martian atmosphere was stripped away by solar winds over time. NASA's MAVEN spacecraft discovered that during solar storms, the rate at which atoms were knocked out of Mars' atmosphere was 10-20 times higher than normal, with up to 5 pounds of atmosphere escaping every second. Without a global magnetic field to deflect solar winds like Earth, auroras occurred across Mars, further contributing to the loss of its atmosphere and liquid water over millions of years.
Solar promineneces rapp
Solar prominences are arcs of ionized solar gas that erupt from the sun's surface and extend hundreds of thousands of miles into the sun's atmosphere. They are held in place by the sun's magnetic field but are not static, lasting anywhere from hours to months before floating away. Solar prominences form because the sun's hot, magnetized interior churns in convective bubbles, tangling the magnetic field and causing large loops to burst through the surface into the atmosphere.
The Sun: Not Just Our Star
The sun is a huge glowing ball of gas at the center of our solar system that provides light, heat, and energy to Earth. It is made up primarily of hydrogen and helium and has a radius about 109 times that of Earth. The sun was formed around 4.6 billion years ago and will remain stable for another 5 billion years before expanding into a red giant. It emits electromagnetic radiation across the spectrum, including visible light and infrared that we experience as heat and light. Nuclear fusion in the sun's core converts hydrogen to helium and releases enormous amounts of energy.
Astronomy 4.1 Energy formation and layers of the Sun - IT6230
The document provides information about the sun, including that it is an average sized star located in one arm of the Milky Way galaxy. It is made up primarily of hydrogen and helium. The sun is very important to Earth as it provides heat, light and keeps Earth and other planets in orbit. It undergoes a solar cycle every 11 years where its magnetic field flips.
Mercury by Raghad
Mercury is the planet closest to the Sun and has extreme temperature variations. It has no atmosphere due to its small size and weak gravity. Mercury orbits the Sun very quickly, giving it the shortest year and day length of any planet in our solar system.
the sun!
The sun is a star at the center of our solar system that produces an immense amount of energy. It holds 98.8% of the total mass of the solar system and has a diameter 109 times that of Earth. The sun was born approximately 4.6 billion years ago from the collapse of a large cloud of dust and gases under the force of gravity, forming a hot, dense center that became the sun surrounded by planets. Sunspots, which are darker and cooler than surrounding areas, are caused by powerful magnetic fields emerging from below the sun's surface. Sometimes large eruptions from sunspots called solar storms can reach Earth and disrupt communication systems. Without the sun providing energy, life on Earth would not be possible as plants
4.1 The Sun is our Local Star
The document discusses the structure and composition of the Sun. It has 6 layers: the core, where fusion occurs at 15 million degrees Celsius; the radiative zone, where energy moves by radiation; the convection zone, where hot gas currents transfer energy; the photosphere, the visible surface; the chromosphere, a thin pinkish layer; and the corona, the outermost low density layer. The Sun is mostly made of hydrogen and helium and produces energy through the fusion of hydrogen into helium. It contains over 99% of the mass in the solar system and has prominent features like sunspots and solar winds.
Our universe
Planets of the Solar System. Star and a Planet, Amazing facts of different planets, Asteroids, Constellations
The sun
The sun is the largest object in the solar system, containing over 99% of its mass. It emits light and heat that support life on Earth and influence all solar system objects. The sun has various internal layers, including the core where energy is produced through nuclear fusion, and an outer atmosphere. Sunspots, solar flares, and other features periodically appear on its surface. In a few billion years, the sun will expand and grow hotter, eventually making Earth uninhabitable.
Earth’s Magnetism
The document discusses the Earth's magnetism. It explains that the Earth behaves like a giant bar magnet with a north and south magnetic pole. These magnetic poles are different from the geographic north and south poles and move about 10 km each year. The Earth's core is made of iron, a magnetic material, and its liquid outer core circulating around generates the planet's magnetic field through a process called the dynamo theory. The Earth's magnetic field protects the atmosphere from the sun's charged particles and is responsible for the northern and southern lights by trapping and directing solar particles toward the poles.
Simmi ppt 1
This document provides information about the solar system and its key components. It lists the nine planets in our solar system, from the Sun to Pluto. It explains that the solar system formed from a giant cloud of gas and dust in space that was disturbed by a supernova explosion, causing it to squeeze and form the Sun and planets. It provides details about each planet's characteristics, sizes and conditions. It also describes the Sun as the center of the system containing 98% of the mass, and notes Earth's moon Luna's proximity and surface features like mountains and craters.
Earth's Magnetic Field
This Powerpoint presentation shows the Magnetic Field of Earth. It also shows the parts of the Earth's Magnetic Field.
The Sun: Our Star
The Sun is made up of hot plasma and provides heat and light to our solar system. It is over 1000 times more massive than all the planets combined. The Sun has an interior of a core, radiation zone and convection zone where nuclear fusion occurs. It also has an atmosphere of a photosphere, chromosphere and corona. The different layers have varying temperatures, from over 15 million Kelvin in the core to around 6,000 Kelvin in the photosphere. The Sun also produces solar wind, prominences and flares.
WHY COMETS HAVE TAILS ?
For more such informative content, go to https://scifitechify.blogspot.com/. This video will give you brief information as to why comets have tials and how is it formed. NEXT POST ON: WHY ARE AURORAS FORMED ?
Our Closest Star, the Sun
Exploring our closest star, the Sun, its makeup, evolution, its place in the universe, and its significance to life on earth.
The layers of the atmosphere pontius
This document summarizes the layers of Earth's atmosphere. It describes 5 main layers - the troposphere, stratosphere, mesosphere, thermosphere, and exosphere. Each layer is defined by changes in temperature and the types of gases present. The troposphere contains around 78% nitrogen and 21% oxygen and extends 4-12 miles above the surface. The stratosphere contains ozone and temperature increases with height. The document compares Earth's atmosphere to those of other planets like Venus, Mars, and Saturn. It notes how Earth's atmosphere protects us and allows life to exist.
The Solar System
The Solar System consists of the Sun and eight planets as well as moons, asteroids, comets and dwarf planets. The planets in order from the Sun are Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus and Neptune. Each planet has unique characteristics such as Mercury having extreme temperature variations and Venus having hurricane-force winds and lightning. Earth is the only known planet capable of supporting life.
Astronomy unit 2011 SUN EARTH MOON SYSTEM acloutier copyright
The document provides an overview of concepts in astronomy including:
1) It describes Earth's rotation, the moon's effect on Earth, and how this impacts seasons and timekeeping.
2) It explains how the tilt of the Earth's axis and its orbit around the sun cause the seasons and equinoxes and solstices.
3) It discusses technology that has expanded our ability to observe space like telescopes, interferometry, and photography.
What's hot (20)
Astronomy 4.1 Energy formation and layers of the Sun - IT6230
Astronomy 4.1 Energy formation and layers of the Sun - IT6230
Astronomy unit 2011 SUN EARTH MOON SYSTEM acloutier copyright
Astronomy unit 2011 SUN EARTH MOON SYSTEM acloutier copyright
More from Mary France Jesuitas
Multicultural Literacy
Literacy: Multiculturalism
The presentation contains animation.
Email for a copy:jesuitas.maryfrance3@gmail.com
Curriculum Evaluation & Curriculum Improvement
This document provides an overview of curriculum evaluation, including reasons for evaluation, types of evaluation, and models of evaluation. It also discusses levels and approaches to curriculum improvement. Specifically, it outlines that curriculum evaluation establishes strengths and weaknesses, provides feedback for improvement, and informs strategic decisions. The two main types of evaluation are formative, which provides ongoing feedback, and summative, which measures outcomes. Several models of curriculum evaluation are also presented, including Tyler's objective-centered model, Stufflebeam's CIPP model, Taba's antecedents-transactions-outcomes model, Stake's responsive model, and Kirkpatrick's reaction-learning-behavior-results model.
RA 7796: TESDA ACT OF 1994
This agency was sign into law under the Republic Act No. 7796, known as the TESDA Act of 1994.
The presentation contains animation.
Email for a copy:jesuitas.maryfrance3@gmail.com
Negative Effects of Teaching Profession
Teaching Profession in the Philippines
The presentation contains animation.
Email for a copy:jesuitas.maryfrance3@gmail.com
Rocks and Minerals pt.2
Different Types of Rocks: Earth Science
It contains animations and videos.
Email for a copy:jesuitas.maryfrance3@gmail.com
Cooperative Learning
This document discusses cooperative learning, which is an educational approach that organizes classroom activities into academic and social learning experiences. There are five key elements of cooperative learning: positive interdependence, face-to-face interaction, group processing, individual and group accountability, and interpersonal skills. The document outlines several techniques used in cooperative learning, such as Think-Pair-Share, Jigsaw, and STAD. It also notes the advantages of cooperative learning in improving academic achievement and social skills, while the disadvantages can include teachers lacking understanding of the methods.
Rocks and Minerals pt.1
Earth's Minerals: Earth Science
The presentation contains animations and videos.
Email for a copy:jesuitas.maryfrance3@gmail.com
More from Mary France Jesuitas (8)
Recently uploaded
The binding of cosmological structures by massless topological defects
Assuming spherical symmetry and weak field, it is shown that if one solves the Poisson equation or the Einstein field
equations sourced by a topological defect, i.e. a singularity of a very specific form, the result is a localized gravitational
field capable of driving flat rotation (i.e. Keplerian circular orbits at a constant speed for all radii) of test masses on a thin
spherical shell without any underlying mass. Moreover, a large-scale structure which exploits this solution by assembling
concentrically a number of such topological defects can establish a flat stellar or galactic rotation curve, and can also deflect
light in the same manner as an equipotential (isothermal) sphere. Thus, the need for dark matter or modified gravity theory is
mitigated, at least in part.
Bob Reedy - Nitrate in Texas Groundwater.pdf
Presented at June 6-7 Texas Alliance of Groundwater Districts Business Meeting
THEMATIC APPERCEPTION TEST(TAT) cognitive abilities, creativity, and critic...
THEMATIC APPERCEPTION TEST(TAT) cognitive abilities, creativity, and critic...Abdul Wali Khan University Mardan,kP,Pakistan
hematic appreciation test is a psychological assessment tool used to measure an individual's appreciation and understanding of specific themes or topics. This test helps to evaluate an individual's ability to connect different ideas and concepts within a given theme, as well as their overall comprehension and interpretation skills. The results of the test can provide valuable insights into an individual's cognitive abilities, creativity, and critical thinking skillsCytokines and their role in immune regulation.pptx
This presentation covers the content and information on "Cytokines " and their role in immune regulation .
Nucleic Acid-its structural and functional complexity.
This presentation explores a brief idea about the structural and functional attributes of nucleotides, the structure and function of genetic materials along with the impact of UV rays and pH upon them.
Thornton ESPP slides UK WW Network 4_6_24.pdf
ESPP presentation to EU Waste Water Network, 4th June 2024 “EU policies driving nutrient removal and recycling
and the revised UWWTD (Urban Waste Water Treatment Directive)”
原版制作(carleton毕业证书)卡尔顿大学毕业证硕士文凭原版一模一样
原版纸张【微信：741003700 】【(carleton毕业证书)卡尔顿大学毕业证】【微信：741003700 】学位证，留信认证（真实可查，永久存档）offer、雅思、外壳等材料/诚信可靠,可直接看成品样本，帮您解决无法毕业带来的各种难题！外壳，原版制作，诚信可靠，可直接看成品样本。行业标杆！精益求精，诚心合作，真诚制作！多年品质 ,按需精细制作，24小时接单,全套进口原装设备。十五年致力于帮助留学生解决难题，包您满意。
本公司拥有海外各大学样板无数，能完美还原海外各大学 Bachelor Diploma degree, Master Degree Diploma
1:1完美还原海外各大学毕业材料上的工艺：水印，阴影底纹，钢印LOGO烫金烫银，LOGO烫金烫银复合重叠。文字图案浮雕、激光镭射、紫外荧光、温感、复印防伪等防伪工艺。材料咨询办理、认证咨询办理请加学历顾问Q/微741003700
留信网认证的作用:
1:该专业认证可证明留学生真实身份
2:同时对留学生所学专业登记给予评定
3:国家专业人才认证中心颁发入库证书
4:这个认证书并且可以归档倒地方
5:凡事获得留信网入网的信息将会逐步更新到个人身份内，将在公安局网内查询个人身份证信息后，同步读取人才网入库信息
6:个人职称评审加20分
7:个人信誉贷款加10分
8:在国家人才网主办的国家网络招聘大会中纳入资料，供国家高端企业选择人才
Remote Sensing and Computational, Evolutionary, Supercomputing, and Intellige...
Remote Sensing and Computational, Evolutionary, Supercomputing, and Intellige...University of Maribor
Slides from talk:
Aleš Zamuda: Remote Sensing and Computational, Evolutionary, Supercomputing, and Intelligent Systems.
11th International Conference on Electrical, Electronics and Computer Engineering (IcETRAN), Niš, 3-6 June 2024
Inter-Society Networking Panel GRSS/MTT-S/CIS Panel Session: Promoting Connection and Cooperation
https://www.etran.rs/2024/en/home-english/The use of Nauplii and metanauplii artemia in aquaculture (brine shrimp).pptx
Although Artemia has been known to man for centuries, its use as a food for the culture of larval organisms apparently began only in the 1930s, when several investigators found that it made an excellent food for newly hatched fish larvae (Litvinenko et al., 2023). As aquaculture developed in the 1960s and ‘70s, the use of Artemia also became more widespread, due both to its convenience and to its nutritional value for larval organisms (Arenas-Pardo et al., 2024). The fact that Artemia dormant cysts can be stored for long periods in cans, and then used as an off-the-shelf food requiring only 24 h of incubation makes them the most convenient, least labor-intensive, live food available for aquaculture (Sorgeloos & Roubach, 2021). The nutritional value of Artemia, especially for marine organisms, is not constant, but varies both geographically and temporally. During the last decade, however, both the causes of Artemia nutritional variability and methods to improve poorquality Artemia have been identified (Loufi et al., 2024).
Brine shrimp (Artemia spp.) are used in marine aquaculture worldwide. Annually, more than 2,000 metric tons of dry cysts are used for cultivation of fish, crustacean, and shellfish larva. Brine shrimp are important to aquaculture because newly hatched brine shrimp nauplii (larvae) provide a food source for many fish fry (Mozanzadeh et al., 2021). Culture and harvesting of brine shrimp eggs represents another aspect of the aquaculture industry. Nauplii and metanauplii of Artemia, commonly known as brine shrimp, play a crucial role in aquaculture due to their nutritional value and suitability as live feed for many aquatic species, particularly in larval stages (Sorgeloos & Roubach, 2021).
Deep Behavioral Phenotyping in Systems Neuroscience for Functional Atlasing a...
Functional Magnetic Resonance Imaging (fMRI) provides means to characterize brain activations in response to behavior. However, cognitive neuroscience has been limited to group-level effects referring to the performance of specific tasks. To obtain the functional profile of elementary cognitive mechanisms, the combination of brain responses to many tasks is required. Yet, to date, both structural atlases and parcellation-based activations do not fully account for cognitive function and still present several limitations. Further, they do not adapt overall to individual characteristics. In this talk, I will give an account of deep-behavioral phenotyping strategies, namely data-driven methods in large task-fMRI datasets, to optimize functional brain-data collection and improve inference of effects-of-interest related to mental processes. Key to this approach is the employment of fast multi-functional paradigms rich on features that can be well parametrized and, consequently, facilitate the creation of psycho-physiological constructs to be modelled with imaging data. Particular emphasis will be given to music stimuli when studying high-order cognitive mechanisms, due to their ecological nature and quality to enable complex behavior compounded by discrete entities. I will also discuss how deep-behavioral phenotyping and individualized models applied to neuroimaging data can better account for the subject-specific organization of domain-general cognitive systems in the human brain. Finally, the accumulation of functional brain signatures brings the possibility to clarify relationships among tasks and create a univocal link between brain systems and mental functions through: (1) the development of ontologies proposing an organization of cognitive processes; and (2) brain-network taxonomies describing functional specialization. To this end, tools to improve commensurability in cognitive science are necessary, such as public repositories, ontology-based platforms and automated meta-analysis tools. I will thus discuss some brain-atlasing resources currently under development, and their applicability in cognitive as well as clinical neuroscience.
Randomised Optimisation Algorithms in DAPHNE
Slides from talk:
Aleš Zamuda: Randomised Optimisation Algorithms in DAPHNE .
Austrian-Slovenian HPC Meeting 2024 – ASHPC24, Seeblickhotel Grundlsee in Austria, 10–13 June 2024
https://ashpc.eu/
20240520 Planning a Circuit Simulator in JavaScript.pptx
Evaporation step counter work. I have done a physical experiment.
(Work in progress.)
Phenomics assisted breeding in crop improvement
As the population is increasing and will reach about 9 billion upto 2050. Also due to climate change, it is difficult to meet the food requirement of such a large population. Facing the challenges presented by resource shortages, climate
change, and increasing global population, crop yield and quality need to be improved in a sustainable way over the coming decades. Genetic improvement by breeding is the best way to increase crop productivity. With the rapid progression of functional
genomics, an increasing number of crop genomes have been sequenced and dozens of genes influencing key agronomic traits have been identified. However, current genome sequence information has not been adequately exploited for understanding
the complex characteristics of multiple gene, owing to a lack of crop phenotypic data. Efficient, automatic, and accurate technologies and platforms that can capture phenotypic data that can
be linked to genomics information for crop improvement at all growth stages have become as important as genotyping. Thus,
high-throughput phenotyping has become the major bottleneck restricting crop breeding. Plant phenomics has been defined as the high-throughput, accurate acquisition and analysis of multi-dimensional phenotypes
during crop growing stages at the organism level, including the cell, tissue, organ, individual plant, plot, and field levels. With the rapid development of novel sensors, imaging technology,
and analysis methods, numerous infrastructure platforms have been developed for phenotyping.
Deep Software Variability and Frictionless Reproducibility
Deep Software Variability and Frictionless ReproducibilityUniversity of Rennes, INSA Rennes, Inria/IRISA, CNRS
The ability to recreate computational results with minimal effort and actionable metrics provides a solid foundation for scientific research and software development. When people can replicate an analysis at the touch of a button using open-source software, open data, and methods to assess and compare proposals, it significantly eases verification of results, engagement with a diverse range of contributors, and progress. However, we have yet to fully achieve this; there are still many sociotechnical frictions.
Inspired by David Donoho's vision, this talk aims to revisit the three crucial pillars of frictionless reproducibility (data sharing, code sharing, and competitive challenges) with the perspective of deep software variability.
Our observation is that multiple layers — hardware, operating systems, third-party libraries, software versions, input data, compile-time options, and parameters — are subject to variability that exacerbates frictions but is also essential for achieving robust, generalizable results and fostering innovation. I will first review the literature, providing evidence of how the complex variability interactions across these layers affect qualitative and quantitative software properties, thereby complicating the reproduction and replication of scientific studies in various fields.
I will then present some software engineering and AI techniques that can support the strategic exploration of variability spaces. These include the use of abstractions and models (e.g., feature models), sampling strategies (e.g., uniform, random), cost-effective measurements (e.g., incremental build of software configurations), and dimensionality reduction methods (e.g., transfer learning, feature selection, software debloating).
I will finally argue that deep variability is both the problem and solution of frictionless reproducibility, calling the software science community to develop new methods and tools to manage variability and foster reproducibility in software systems.
Exposé invité Journées Nationales du GDR GPL 2024
Sharlene Leurig - Enabling Onsite Water Use with Net Zero Water
Sharlene Leurig - Enabling Onsite Water Use with Net Zero WaterTexas Alliance of Groundwater Districts
Presented at June 6-7 Texas Alliance of Groundwater Districts Business MeetingMicronuclei test.M.sc.zoology.fisheries.
Current Ms word generated power point presentation covers major details about the micronuclei test. It's significance and assays to conduct it. It is used to detect the micronuclei formation inside the cells of nearly every multicellular organism. It's formation takes place during chromosomal sepration at metaphase.
8.Isolation of pure cultures and preservation of cultures.pdf
Isolation of pure culture, its various method.
Recently uploaded (20)
The binding of cosmological structures by massless topological defects
The binding of cosmological structures by massless topological defects
THEMATIC APPERCEPTION TEST(TAT) cognitive abilities, creativity, and critic...
THEMATIC APPERCEPTION TEST(TAT) cognitive abilities, creativity, and critic...
Cytokines and their role in immune regulation.pptx
Cytokines and their role in immune regulation.pptx
Nucleic Acid-its structural and functional complexity.
Nucleic Acid-its structural and functional complexity.
Remote Sensing and Computational, Evolutionary, Supercomputing, and Intellige...
Remote Sensing and Computational, Evolutionary, Supercomputing, and Intellige...
The use of Nauplii and metanauplii artemia in aquaculture (brine shrimp).pptx
The use of Nauplii and metanauplii artemia in aquaculture (brine shrimp).pptx
Deep Behavioral Phenotyping in Systems Neuroscience for Functional Atlasing a...
Deep Behavioral Phenotyping in Systems Neuroscience for Functional Atlasing a...
20240520 Planning a Circuit Simulator in JavaScript.pptx
20240520 Planning a Circuit Simulator in JavaScript.pptx
Deep Software Variability and Frictionless Reproducibility
Deep Software Variability and Frictionless Reproducibility
mô tả các thí nghiệm về đánh giá tác động dòng khí hóa sau đốt
mô tả các thí nghiệm về đánh giá tác động dòng khí hóa sau đốt
Sharlene Leurig - Enabling Onsite Water Use with Net Zero Water
Sharlene Leurig - Enabling Onsite Water Use with Net Zero Water
8.Isolation of pure cultures and preservation of cultures.pdf
8.Isolation of pure cultures and preservation of cultures.pdf
Chasing the Auroras: Borealis & Polaris
- 1. The auroras occur throughout the day, but can only be seen by the naked eye by night. Energy and small particles travel down the magnetic field lines at the north and south poles. Particles interact with gases in our atmosphere resulting in beautiful displays of light in the sky. Charged particles from the sun are dragged into the atmosphere by the Earth's magnetic field. Sun burps out a huge bubble of electrified gas that can travel through space at high speeds. AURORA AURORA Earth’s atmosphere gives off when they are