The document discusses the solar interior and surface features. It explains that nuclear fusion in the core powers the sun, generating energy through the p-p chain reaction of converting hydrogen to helium. It also describes the solar neutrino problem, where fewer neutrinos are detected than models predict. The interior has different zones - the core, radiative zone, and convection zone. Surface features include sunspots, the 11-year sunspot cycle, prominences, and filaments.
What's So Interesting About AMO Phyiscs?Chad Orzel
A talk given at the 2011 meeting of the Division of Atomic, Molecular, and Optical Physics (DAMOP) of the American Physical Society, summarizing recent and exciting results in AMO physics being presented at the meeting.
The document traces the history of atomic theory from ancient Greece to modern times. It discusses the ideas of early philosophers like Democritus who hypothesized atoms as indivisible particles. Experimental discoveries throughout the 18th-19th centuries led to identifying elements through spectroscopy and discovering over 55 elements near volcanoes. Niels Bohr incorporated these findings into his 1913 model of the atom with electrons orbiting in discrete shells. John Dalton further refined atomic theory in 1808 by postulating that atoms are uniform, distinct, and combine to form compounds. Later, J.J. Thomson discovered the electron and Ernest Rutherford deduced the nuclear structure of atoms through deflection experiments.
The document discusses the gas giant planets Jupiter, Saturn, Uranus, and Neptune. It describes how the conditions in the early solar system led to their formation and composition primarily of hydrogen and helium. It explains what gives each planet its distinctive color through the composition of their clouds and atmospheres. Key details about the interiors, atmospheres, and cloud formations of each planet are provided.
The document provides information about outer solar system objects including Trans-Neptunian objects, Centaurs, Kuiper Belt objects, asteroids, comets, and dwarf planets. It discusses their classification, composition, formation processes, and what they reveal about the early solar system. Images show various outer solar system bodies like Pluto, Eris, asteroids, and comets, helping to illustrate their characteristics and relative sizes.
This document discusses a university course on nuclear physics and its goals of educating the public on basic nuclear concepts and issues. It outlines the course schedule which includes lectures on radiation properties, nuclear creation in the cosmos, applications of nuclear physics, and modern research frontiers. Laboratory sessions are planned to demonstrate radiation detection, half-life measurement, shielding, and source identification. The document also provides information on alpha, beta, gamma, and neutron radiation, and examples of isotope half-lives and their applications.
Dr. Kamal K. Ali's lecture discusses the structure of atoms and radioactivity. It covers topics like the atom structure, isotopes, radioactive decay mechanisms, and types of radiation. It also explains techniques used to measure isotopes like mass spectrometry. Mass spectrometry works by ionizing atoms, accelerating the ions, and separating them in a magnetic field based on their mass-to-charge ratio. This allows determining the relative abundances of isotopes in a sample.
This document provides an overview of several topics in astrophysics, including:
1. It discusses stars and their properties like mass, luminosity, temperature, and the proton-proton chain reaction.
2. It covers neutrinos and their characteristics.
3. It describes neutron stars and their properties, how they are formed in supernovas, and provides some details about Supernova 1987A.
4. It discusses pulsars and their discovery, and properties of neutron stars.
This document summarizes a study that used optical, infrared, and submillimeter data to examine star formation in the region surrounding the IC 348 star cluster and the nearby Flying Ghost Nebula. The study identified 13 protostars driving protostellar outflows in the region, including HH 211 which had not previously been detected at visible wavelengths. The region surrounding the Flying Ghost Nebula shows ongoing star formation with outflows similar to other areas of moderate star formation in Perseus. A candidate bent jet was also found, which may have been ejected from a multiple star system near IC 348.
What's So Interesting About AMO Phyiscs?Chad Orzel
A talk given at the 2011 meeting of the Division of Atomic, Molecular, and Optical Physics (DAMOP) of the American Physical Society, summarizing recent and exciting results in AMO physics being presented at the meeting.
The document traces the history of atomic theory from ancient Greece to modern times. It discusses the ideas of early philosophers like Democritus who hypothesized atoms as indivisible particles. Experimental discoveries throughout the 18th-19th centuries led to identifying elements through spectroscopy and discovering over 55 elements near volcanoes. Niels Bohr incorporated these findings into his 1913 model of the atom with electrons orbiting in discrete shells. John Dalton further refined atomic theory in 1808 by postulating that atoms are uniform, distinct, and combine to form compounds. Later, J.J. Thomson discovered the electron and Ernest Rutherford deduced the nuclear structure of atoms through deflection experiments.
The document discusses the gas giant planets Jupiter, Saturn, Uranus, and Neptune. It describes how the conditions in the early solar system led to their formation and composition primarily of hydrogen and helium. It explains what gives each planet its distinctive color through the composition of their clouds and atmospheres. Key details about the interiors, atmospheres, and cloud formations of each planet are provided.
The document provides information about outer solar system objects including Trans-Neptunian objects, Centaurs, Kuiper Belt objects, asteroids, comets, and dwarf planets. It discusses their classification, composition, formation processes, and what they reveal about the early solar system. Images show various outer solar system bodies like Pluto, Eris, asteroids, and comets, helping to illustrate their characteristics and relative sizes.
This document discusses a university course on nuclear physics and its goals of educating the public on basic nuclear concepts and issues. It outlines the course schedule which includes lectures on radiation properties, nuclear creation in the cosmos, applications of nuclear physics, and modern research frontiers. Laboratory sessions are planned to demonstrate radiation detection, half-life measurement, shielding, and source identification. The document also provides information on alpha, beta, gamma, and neutron radiation, and examples of isotope half-lives and their applications.
Dr. Kamal K. Ali's lecture discusses the structure of atoms and radioactivity. It covers topics like the atom structure, isotopes, radioactive decay mechanisms, and types of radiation. It also explains techniques used to measure isotopes like mass spectrometry. Mass spectrometry works by ionizing atoms, accelerating the ions, and separating them in a magnetic field based on their mass-to-charge ratio. This allows determining the relative abundances of isotopes in a sample.
This document provides an overview of several topics in astrophysics, including:
1. It discusses stars and their properties like mass, luminosity, temperature, and the proton-proton chain reaction.
2. It covers neutrinos and their characteristics.
3. It describes neutron stars and their properties, how they are formed in supernovas, and provides some details about Supernova 1987A.
4. It discusses pulsars and their discovery, and properties of neutron stars.
This document summarizes a study that used optical, infrared, and submillimeter data to examine star formation in the region surrounding the IC 348 star cluster and the nearby Flying Ghost Nebula. The study identified 13 protostars driving protostellar outflows in the region, including HH 211 which had not previously been detected at visible wavelengths. The region surrounding the Flying Ghost Nebula shows ongoing star formation with outflows similar to other areas of moderate star formation in Perseus. A candidate bent jet was also found, which may have been ejected from a multiple star system near IC 348.
Nuclear chemistry involves the study of radioactive decay, nuclear stability, and nuclear transformations. Radioactive decay occurs through alpha, beta, gamma, or positron emission, electron capture, or spontaneous fission. The rate of radioactive decay follows first order kinetics and is characterized by half-life. Radiometric dating uses radioactive decay to determine the age of materials. Nuclear stability depends on having an even number of protons and neutrons and being closest to the nuclear stability belt. Nuclear transformations can change the number of protons through various types of radioactive decay.
Apartes de la Charla: El Sol Cuántico. Sábado 8 de Julio_2017_JorgeIvanZuluagaSOCIEDAD JULIO GARAVITO
Apreciados Amigos de la Sociedad Julio Garavito, de la Astronomía y de las Ciencias Espaciales en general.
Reciban un cordial saludo.
El sábado 8 de Julio de 2017 desde las 11:00 Am hasta las 1:00 PM. se tuvo la reunión de la Sociedad Julio Garavito en el Auditorio del Planetario de Medellín "Jesús Emilio Ramírez González-Antioquia-Colombia con la Charla: "El Sol Cuántico"
Resumen:
El Sol es una gigantesca bola de plasma. Sería difícil asociarlo con la teoría cuántica, una teoría sobre el mundo microscópico. Sin embargo algunos de los secretos más increíbles sobre el Sol, su naturaleza y funcionamiento fueron posibles gracias a las curiosas consecuencias de esta teoría. En esta charla exploraremos la historia de cómo los astrofísicos "hackearon" los secretos que se esconden debajo de la superficie solar con la ayuda de la Física. Reacciones nucleares imposibles, neutrinos escurridizos y protones que nunca se encuentran pero mantienen encendida la "llama" solar, serán partes de esta increíble historia.
POR:
JORGE IVAN ZULUAGA
Profesor Asociado UdeA.
Nota: Estas charlas promovidas por la Sociedad Julio Garavito son de entrada libre sin costo alguno
La Sociedad Julio Garavito agradece a los Directivos del Parque Explora por permitirle realizar sus reuniones quincenales que han sido tradicionales por más de 42 años en un lugar que se ha convertido en un referente de Ciencia, Ingeniería, Tecnología e Industria AeroEspacial en la Ciudad de Medellín.
Por la atención prestada, muchas gracias.
Sinceramente:
Campo Elías Roldán.
Director Sociedad Julio Garavito para el Estudio de la Astronomía
Medellín-Antioquia
COLOMBIA.
campoelias.roldan@gmail.com
Characterizing Luminescent Properties of Thin Films by Farisch HanoemanFarisch Hanoeman
Thesis at Delft University of Technology. Fundamental Aspects of Materials and Energy (FAME), Radiation Science and Technology department, Faculty of Applied Sciences. Supervisor: dr. E. van der Kolk, co-reader: prof. dr. P. Dorenbos.
The document discusses the speed of light and why it appears as a constant in monotheism books. It explains that the speed of light is the same for all forces including light and electromagnetic waves like ultraviolet, infrared, radio, and TV. It is the upper limit speed in the universe and cannot be reached by matter due to the infinite energy needed. It then describes how analyzing the moon's motion in an isolated earth-moon system can be used to define the speed of light based on the moon's perfectly circular orbit and other orbital parameters in this system. Making these calculations precisely, the author determines that the speed of light defined from the isolated earth-moon system equations is 299,792.458 km/s, which matches
Big Questions, Small Particles and the Optimism of Curiosity discusses CERN's mission to push forward the frontiers of knowledge about the Big Bang and early universe by studying small particles using large particle accelerators. It summarizes CERN's goals of understanding fundamental physics, developing new technologies, and training scientists. The document outlines recent discoveries made with the Large Hadron Collider, including the 2012 discovery of the Higgs boson particle, and discusses many open questions that remain. It emphasizes that fundamental discoveries often raise more questions and that our understanding of nature is still evolving.
1. Nuclear fission is the splitting of atoms, usually large unstable atoms, which releases energy. Fission reactions have three steps: initiation, propagation, and termination.
2. Half-life is the time it takes for half of a radioactive sample to decay. The rate of radioactive decay depends only on the concentration of the radioactive isotope.
3. Nuclear fusion is the combining of small nuclei, such as two hydrogen nuclei fusing to form a helium nucleus. Fusion occurs in stars and is difficult to achieve on Earth.
A session about nuclear engineering, made for public to increase the public awareness about nuclear energy, radiation, nuclear waste, and nuclear accidents
1) The document is a chapter from an astronomy textbook about Mercury, Venus, Mars and the Moon. It contains multiple choice questions about characteristics of these bodies.
2) Mercury's surface most resembles the Moon's far side because they are both heavily cratered. Mercury is hard to observe from Earth because it is always close to the Sun.
3) Neither the Moon nor Mercury have atmospheres, contributing to their cratered surfaces. The lack of atmosphere also causes extreme temperature variations on Mercury.
This document presents observations of ACT-CL J0102−4915, a massive galaxy cluster discovered by the Atacama Cosmology Telescope (ACT) via its strong Sunyaev-Zeldovich signal. Optical and X-ray observations reveal that it is undergoing a major merger between components with a mass ratio of 2:1 at a redshift of 0.87. Chandra X-ray data show significant temperature variations across the cluster from 6.6 keV to 22 keV, indicating a hot, luminous system undergoing a merger. The cluster appears to be an excellent example of a "bullet cluster" system at high redshift.
Luc Patthey, leader of the research group of Spectroscopy on Novel Materials at the Synchrotron Radiation and Nanotechnology Laboratory at PSI, presents the Swiss Light Source and the future X-ray free electron laser, SwissFEL.
Fusion is the combination of smaller atoms into larger ones and requires temperatures over 10 million degrees to overcome electrostatic repulsion between protons. Stars generate heat and heavier elements through fusion in their cores. Fission is when atoms split into smaller atoms, releasing energy. It can be controlled for nuclear power generation or uncontrolled in atomic bombs. New elements can be artificially made through nuclear transmutation using particle accelerators to collide atoms together.
This document discusses radioactive dating and nuclear reactions. It begins by defining key terms like half-life, isotopes, and decay curves. It then explains how scientists use radioactive isotopes like carbon-14 to date fossils by comparing amounts of parent and daughter isotopes. The document also covers nuclear fission, fusion, and chain reactions. It includes examples of isotope pairs used for dating and discusses how nuclear power works through fission but produces dangerous waste.
This document summarizes key concepts from atomic theory:
1. Early atomic theories proposed by Democritus, Dalton, Thomson, and Rutherford attempted to explain the nature of atoms and subatomic particles. Rutherford's gold foil experiment led to the discovery of the atomic nucleus.
2. Niels Bohr combined Rutherford's nuclear model with Planck's quantum theory to explain atomic spectra. Electrons can only orbit at certain distances corresponding to specific energy levels.
3. Modern atomic theory incorporates quantum mechanics. Electrons do not have definite positions, but are described by orbital probabilities. The Heisenberg uncertainty principle limits the precision of measuring certain paired properties.
Nuclear chemistry involves three types of radiation emitted during radioactive decay: alpha, beta, and gamma rays. Alpha rays consist of helium nuclei, beta rays are electrons, and gamma rays have no charge. Radioactive substances decay through processes like alpha emission that can be represented by balanced nuclear equations. Nuclear reactions also occur through fission, fusion, and transmutation, releasing nuclear energy. Nuclear power plants utilize fission to generate electricity while minimizing waste, and radioisotopes have important medical applications.
ECE 413 Part10B Principles of Nuclear EnergyEugene Sebilo
The document summarizes basic principles of nuclear energy, including the discovery of nuclear fission in 1938. It discusses early nuclear reactors including the first self-sustaining nuclear reaction in 1942 and the first nuclear power plant in 1954. It also covers nuclear reactions such as alpha decay, beta decay, and gamma emission. The document explains concepts of isotopes, half-life, cross-section, fission and fission products. It notes the production of plutonium-239 from uranium-238 absorption of neutrons.
Space weather and potential impact on earth’s climate dec 19 10 v2Poramate Minsiri
This document discusses space weather and its potential impacts on Earth's climate and seismic activity. It provides an overview of the solar system and its dynamics, as well as how our solar system interacts with the Milky Way galaxy and larger universe. Recent observations have found evidence that the outer boundaries of our solar system are being compressed as we pass through Galactic clouds, allowing more cosmic rays and energetic particles to enter the inner solar system. This could affect Earth's climate and increase seismic activity. The document also discusses changes observed on other planets in our solar system, such as the growth of dark spots on Pluto and changes in cloud cover on Mars.
The document provides a summary of the history and development of Nuclear Magnetic Resonance (NMR) Spectroscopy. Some key points include:
1. NMR was first predicted in 1937 and first observed on bulk samples in 1946. Important early developments included 2D NMR in 1975 and NMR metabolomics in 1984.
2. NMR utilizes the magnetic properties of certain atomic nuclei to determine structural information about molecules. It provides information about the number and type of hydrogen atoms, as well as their electronic environment.
3. For a nucleus to be observable by NMR, it must have a non-zero spin quantum number and magnetic moment, and be spherical in shape. Common nuclei studied include 1H, 13C, 19
The document discusses various topics relating to nuclear reactions and radioactive decay:
1) It defines key terms like half-life, decay constant, and isotopes.
2) It describes the main types of radioactive decay - alpha, beta, electron capture, and gamma - and provides examples of equations for each.
3) It explains factors that contribute to nuclear stability and why only some isotopes are radioactive.
4) It provides a brief overview of fission, fusion, and chain reactions in nuclear power and weapons.
The document provides an introduction to stars, focusing on the sun. It discusses the layers of the sun's atmosphere and interior. The sun's core generates its enormous energy output through nuclear fusion. The solar wind consists of high-energy particles escaping the sun's gravity. The sun emits across the electromagnetic spectrum, including x-rays studied by orbital telescopes. The sun's total luminosity is calculated based on the energy received by a detector at Earth's distance. Sunspots occur in pairs of opposite magnetic fields and vary in a roughly 11-year solar cycle.
This very short document discusses the sun from beginning to end in a single sentence. It does not provide enough contextual information to generate a meaningful 3 sentence summary.
Nuclear chemistry involves the study of radioactive decay, nuclear stability, and nuclear transformations. Radioactive decay occurs through alpha, beta, gamma, or positron emission, electron capture, or spontaneous fission. The rate of radioactive decay follows first order kinetics and is characterized by half-life. Radiometric dating uses radioactive decay to determine the age of materials. Nuclear stability depends on having an even number of protons and neutrons and being closest to the nuclear stability belt. Nuclear transformations can change the number of protons through various types of radioactive decay.
Apartes de la Charla: El Sol Cuántico. Sábado 8 de Julio_2017_JorgeIvanZuluagaSOCIEDAD JULIO GARAVITO
Apreciados Amigos de la Sociedad Julio Garavito, de la Astronomía y de las Ciencias Espaciales en general.
Reciban un cordial saludo.
El sábado 8 de Julio de 2017 desde las 11:00 Am hasta las 1:00 PM. se tuvo la reunión de la Sociedad Julio Garavito en el Auditorio del Planetario de Medellín "Jesús Emilio Ramírez González-Antioquia-Colombia con la Charla: "El Sol Cuántico"
Resumen:
El Sol es una gigantesca bola de plasma. Sería difícil asociarlo con la teoría cuántica, una teoría sobre el mundo microscópico. Sin embargo algunos de los secretos más increíbles sobre el Sol, su naturaleza y funcionamiento fueron posibles gracias a las curiosas consecuencias de esta teoría. En esta charla exploraremos la historia de cómo los astrofísicos "hackearon" los secretos que se esconden debajo de la superficie solar con la ayuda de la Física. Reacciones nucleares imposibles, neutrinos escurridizos y protones que nunca se encuentran pero mantienen encendida la "llama" solar, serán partes de esta increíble historia.
POR:
JORGE IVAN ZULUAGA
Profesor Asociado UdeA.
Nota: Estas charlas promovidas por la Sociedad Julio Garavito son de entrada libre sin costo alguno
La Sociedad Julio Garavito agradece a los Directivos del Parque Explora por permitirle realizar sus reuniones quincenales que han sido tradicionales por más de 42 años en un lugar que se ha convertido en un referente de Ciencia, Ingeniería, Tecnología e Industria AeroEspacial en la Ciudad de Medellín.
Por la atención prestada, muchas gracias.
Sinceramente:
Campo Elías Roldán.
Director Sociedad Julio Garavito para el Estudio de la Astronomía
Medellín-Antioquia
COLOMBIA.
campoelias.roldan@gmail.com
Characterizing Luminescent Properties of Thin Films by Farisch HanoemanFarisch Hanoeman
Thesis at Delft University of Technology. Fundamental Aspects of Materials and Energy (FAME), Radiation Science and Technology department, Faculty of Applied Sciences. Supervisor: dr. E. van der Kolk, co-reader: prof. dr. P. Dorenbos.
The document discusses the speed of light and why it appears as a constant in monotheism books. It explains that the speed of light is the same for all forces including light and electromagnetic waves like ultraviolet, infrared, radio, and TV. It is the upper limit speed in the universe and cannot be reached by matter due to the infinite energy needed. It then describes how analyzing the moon's motion in an isolated earth-moon system can be used to define the speed of light based on the moon's perfectly circular orbit and other orbital parameters in this system. Making these calculations precisely, the author determines that the speed of light defined from the isolated earth-moon system equations is 299,792.458 km/s, which matches
Big Questions, Small Particles and the Optimism of Curiosity discusses CERN's mission to push forward the frontiers of knowledge about the Big Bang and early universe by studying small particles using large particle accelerators. It summarizes CERN's goals of understanding fundamental physics, developing new technologies, and training scientists. The document outlines recent discoveries made with the Large Hadron Collider, including the 2012 discovery of the Higgs boson particle, and discusses many open questions that remain. It emphasizes that fundamental discoveries often raise more questions and that our understanding of nature is still evolving.
1. Nuclear fission is the splitting of atoms, usually large unstable atoms, which releases energy. Fission reactions have three steps: initiation, propagation, and termination.
2. Half-life is the time it takes for half of a radioactive sample to decay. The rate of radioactive decay depends only on the concentration of the radioactive isotope.
3. Nuclear fusion is the combining of small nuclei, such as two hydrogen nuclei fusing to form a helium nucleus. Fusion occurs in stars and is difficult to achieve on Earth.
A session about nuclear engineering, made for public to increase the public awareness about nuclear energy, radiation, nuclear waste, and nuclear accidents
1) The document is a chapter from an astronomy textbook about Mercury, Venus, Mars and the Moon. It contains multiple choice questions about characteristics of these bodies.
2) Mercury's surface most resembles the Moon's far side because they are both heavily cratered. Mercury is hard to observe from Earth because it is always close to the Sun.
3) Neither the Moon nor Mercury have atmospheres, contributing to their cratered surfaces. The lack of atmosphere also causes extreme temperature variations on Mercury.
This document presents observations of ACT-CL J0102−4915, a massive galaxy cluster discovered by the Atacama Cosmology Telescope (ACT) via its strong Sunyaev-Zeldovich signal. Optical and X-ray observations reveal that it is undergoing a major merger between components with a mass ratio of 2:1 at a redshift of 0.87. Chandra X-ray data show significant temperature variations across the cluster from 6.6 keV to 22 keV, indicating a hot, luminous system undergoing a merger. The cluster appears to be an excellent example of a "bullet cluster" system at high redshift.
Luc Patthey, leader of the research group of Spectroscopy on Novel Materials at the Synchrotron Radiation and Nanotechnology Laboratory at PSI, presents the Swiss Light Source and the future X-ray free electron laser, SwissFEL.
Fusion is the combination of smaller atoms into larger ones and requires temperatures over 10 million degrees to overcome electrostatic repulsion between protons. Stars generate heat and heavier elements through fusion in their cores. Fission is when atoms split into smaller atoms, releasing energy. It can be controlled for nuclear power generation or uncontrolled in atomic bombs. New elements can be artificially made through nuclear transmutation using particle accelerators to collide atoms together.
This document discusses radioactive dating and nuclear reactions. It begins by defining key terms like half-life, isotopes, and decay curves. It then explains how scientists use radioactive isotopes like carbon-14 to date fossils by comparing amounts of parent and daughter isotopes. The document also covers nuclear fission, fusion, and chain reactions. It includes examples of isotope pairs used for dating and discusses how nuclear power works through fission but produces dangerous waste.
This document summarizes key concepts from atomic theory:
1. Early atomic theories proposed by Democritus, Dalton, Thomson, and Rutherford attempted to explain the nature of atoms and subatomic particles. Rutherford's gold foil experiment led to the discovery of the atomic nucleus.
2. Niels Bohr combined Rutherford's nuclear model with Planck's quantum theory to explain atomic spectra. Electrons can only orbit at certain distances corresponding to specific energy levels.
3. Modern atomic theory incorporates quantum mechanics. Electrons do not have definite positions, but are described by orbital probabilities. The Heisenberg uncertainty principle limits the precision of measuring certain paired properties.
Nuclear chemistry involves three types of radiation emitted during radioactive decay: alpha, beta, and gamma rays. Alpha rays consist of helium nuclei, beta rays are electrons, and gamma rays have no charge. Radioactive substances decay through processes like alpha emission that can be represented by balanced nuclear equations. Nuclear reactions also occur through fission, fusion, and transmutation, releasing nuclear energy. Nuclear power plants utilize fission to generate electricity while minimizing waste, and radioisotopes have important medical applications.
ECE 413 Part10B Principles of Nuclear EnergyEugene Sebilo
The document summarizes basic principles of nuclear energy, including the discovery of nuclear fission in 1938. It discusses early nuclear reactors including the first self-sustaining nuclear reaction in 1942 and the first nuclear power plant in 1954. It also covers nuclear reactions such as alpha decay, beta decay, and gamma emission. The document explains concepts of isotopes, half-life, cross-section, fission and fission products. It notes the production of plutonium-239 from uranium-238 absorption of neutrons.
Space weather and potential impact on earth’s climate dec 19 10 v2Poramate Minsiri
This document discusses space weather and its potential impacts on Earth's climate and seismic activity. It provides an overview of the solar system and its dynamics, as well as how our solar system interacts with the Milky Way galaxy and larger universe. Recent observations have found evidence that the outer boundaries of our solar system are being compressed as we pass through Galactic clouds, allowing more cosmic rays and energetic particles to enter the inner solar system. This could affect Earth's climate and increase seismic activity. The document also discusses changes observed on other planets in our solar system, such as the growth of dark spots on Pluto and changes in cloud cover on Mars.
The document provides a summary of the history and development of Nuclear Magnetic Resonance (NMR) Spectroscopy. Some key points include:
1. NMR was first predicted in 1937 and first observed on bulk samples in 1946. Important early developments included 2D NMR in 1975 and NMR metabolomics in 1984.
2. NMR utilizes the magnetic properties of certain atomic nuclei to determine structural information about molecules. It provides information about the number and type of hydrogen atoms, as well as their electronic environment.
3. For a nucleus to be observable by NMR, it must have a non-zero spin quantum number and magnetic moment, and be spherical in shape. Common nuclei studied include 1H, 13C, 19
The document discusses various topics relating to nuclear reactions and radioactive decay:
1) It defines key terms like half-life, decay constant, and isotopes.
2) It describes the main types of radioactive decay - alpha, beta, electron capture, and gamma - and provides examples of equations for each.
3) It explains factors that contribute to nuclear stability and why only some isotopes are radioactive.
4) It provides a brief overview of fission, fusion, and chain reactions in nuclear power and weapons.
The document provides an introduction to stars, focusing on the sun. It discusses the layers of the sun's atmosphere and interior. The sun's core generates its enormous energy output through nuclear fusion. The solar wind consists of high-energy particles escaping the sun's gravity. The sun emits across the electromagnetic spectrum, including x-rays studied by orbital telescopes. The sun's total luminosity is calculated based on the energy received by a detector at Earth's distance. Sunspots occur in pairs of opposite magnetic fields and vary in a roughly 11-year solar cycle.
This very short document discusses the sun from beginning to end in a single sentence. It does not provide enough contextual information to generate a meaningful 3 sentence summary.
Maybe too in-depth for most elementary students, but very good broad coverage for teacher background or more advanced students in elementary or middle school.
The document summarizes key information about the sun. It begins by stating that the sun is an average sized star, located at the center of the solar system, composed primarily of hydrogen and helium. It then describes the various layers of the sun, including the core, radiation layer, convection layer, photosphere, chromosphere, and corona. It explains that nuclear fusion in the core converts hydrogen into helium, releasing energy in the process. This energy eventually makes its way to the surface of the sun and radiates out into space.
This PowerPoint discusses the Sun at a high school level. It talks about characteristics, solar activities/events, how energy is created, and many more.
How much of the human body is made up of stardust,Does atoms age and what is ...Healthcare consultant
How much of the human body is made up of stardust,Does atoms age and what is the age of atoms. If an atom or molecule becomes electrically charged by gaining or losing one or more electrons, it becomes an ion. If the atom gains electrons, it has a negative charge. If it loses electrons, it has a positive charge.
The document summarizes key concepts about high mass stars and binary systems from sections 22.1, 22.2, and 23.5 of the textbook. It notes that high mass stars (>10 solar masses) end their lives as Type II supernovae, sometimes gamma-ray bursters. Binary systems produce novae, Type Ia supernovae, x-ray binaries, and x-ray bursters. All stars enrich the interstellar medium with heavier elements through their evolution and deaths. The goal is to answer fundamental questions about the universe and our origins.
Neutrinos are elementary particles that have no electric charge and interact very weakly with matter. There are three types of neutrinos related to electrons, muons, and tau particles. Neutrinos are abundantly produced in nature by the sun, stars, and nuclear reactions. They pass through the body without interacting but can be detected underground using large detectors composed of layers of iron and detectors that observe the curvature of charged particles produced during neutrino interactions, revealing information about the neutrinos' energy. The INO laboratory under construction in India will also study neutrinos.
Neutrinos: The Chameleon in the Elementary Particle ZooAlan Poon
Neutrinos are extremely lightweight elementary particles that are produced by nuclear reactions in the Sun. The document discusses the challenges of detecting neutrinos due to their very small interaction cross-section. It summarizes the discoveries made by Ray Davis Jr. using a large tank of cleaning fluid to detect solar neutrinos, as well as the Sudbury Neutrino Observatory which was able to detect neutrinos via three different reactions and demonstrated that neutrinos oscillate between flavors as they travel, indicating neutrinos have mass. The document provides background on neutrino sources, detection challenges, and important experiments that advanced the understanding of neutrino properties.
The document outlines a physics course covering topics related to astronomy and the structure of atoms and stars over 24 lessons. It provides learning objectives and activities for each lesson, including lessons on telescopes, the sun and planets, star distances and temperatures, galaxies, and the structure and behavior of atoms and gases.
Cobalt-60 is a radioactive isotope of cobalt that is used in medical and industrial applications. It undergoes beta decay, emitting high-energy photons. Cobalt-60 is produced artificially in nuclear reactors and is used in radiation therapy to treat cancer. It is also used for industrial sterilization and irradiation. Precautions must be taken when handling cobalt-60 due to its radioactivity and long half-life.
The document summarizes an experiment to measure the average lifespan of muons using a muon detector. The detector measured the time between a muon entering and decaying using a scintillation light and timing circuit. The average lifespan was calculated from the decay rate determined by the software. However, the calculated average lifespan was only 10% of the accepted value, indicating an error occurred during the experiment or calculations.
- There are two main systems for measuring radiation - the conventional US system and the International System of Units (SI).
- Radioactivity is measured in curies (Ci) in the US system and becquerels (Bq) in the SI system. 1 Ci equals 37 billion Bq.
- Exposure rate is measured in roentgens (R) per hour in the US system. The SI unit is the coulomb per kilogram (C/kg).
- Absorbed dose is measured in rads in the US system and grays (Gy) in the SI system. 1 Gy is equal to 100 rads.
1) The document provides reminders and information about upcoming assignments in science class, including corrections for Test #2 that are due today and signed by parents.
2) It summarizes key concepts from the Bohr and Schrodinger atomic models, including that Bohr believed electrons orbited the nucleus in fixed orbits like planets around the sun, while Schrodinger proposed that electrons vibrate around the nucleus and can only predict where they are most likely to be found.
3) The document reviews basic atomic structure, isotopes including examples for hydrogen, and how to identify metals, nonmetals and metalloids on the periodic table based on their location in the boxes.
1) The growth of the first stars was halted by ultraviolet radiation feedback from the stars themselves.
2) Radiation from the protostar evaporated the circumstellar accretion disk when the star's mass reached 43 times the mass of the Sun.
3) These massive primordial stars may help explain the lack of pair-instability supernovae signatures in ancient metal-poor stars.
The document discusses the structure of the atom. It describes how scientists like J.J. Thomson, Ernest Rutherford, and Niels Bohr contributed to developing atomic models through experiments and conclusions. Thomson proposed the "plum pudding" model where electrons were embedded in a uniform positively charged sphere. Rutherford's alpha particle scattering experiment showed that the positive charge and mass of atoms are concentrated in a small nucleus. Bohr incorporated Rutherford's nuclear model and proposed that electrons orbit in discrete energy levels, resolving issues with Rutherford's model. Later, Chadwick discovered the neutron in the nucleus and the modern understanding of atomic structure with protons, neutrons, and electrons was established.
Andy Stine's Thesis--Neutron Star ModelsAndy Stine
This document is Andrew Stine's thesis on modeling the structure of neutron stars through equations of state. It begins with an overview of neutron star formation and composition, outlining the different layers from the atmosphere to the core. It then discusses the history and theory behind different equations of state used to model neutron star interiors. The document presents Stine's 1D model of neutron stars using two equations of state, and includes the Python code and results. The model matches previous predictions for the maximum mass of neutron stars using these equations of state.
Here are the answers:
1. Aluminum
2. Helium
3. Palladium
4. Gold
5. Oxygen
6. Calcium has 20 protons
7. Silver has 47 protons
8. Neon has 10 protons
9. Potassium has 19 protons
10. Iron has 26 protons
11. (Draws a picture of a nitrogen nucleus with 7 protons)
Here are the answers:
1. Aluminum
2. Helium
3. Palladium
4. Gold
5. Oxygen
6. Calcium has 20 protons
7. Silver has 47 protons
8. Neon has 10 protons
9. Potassium has 19 protons
10. Iron has 26 protons
11. Nitrogen has 7 protons in its nucleus.
Physics in the news: Earthquakes, Tsunamis and Nuclear PowerDaniel Stillman
This document discusses various topics in physics including nuclear reactions, radioactive decay, stellar nucleosynthesis, nuclear fission and fusion, atomic structure, nuclear power and energy, plate tectonics, earthquakes, tsunamis, and wave mechanics. It provides explanations of physical phenomena like alpha, beta, and gamma radiation, conservation of nucleons, and conservation of energy. It also discusses choices and tradeoffs around different energy sources.
The document discusses the structure of atoms and the discovery of subatomic particles. It explains that:
1) Early experiments showed atoms were divisible and contained electrons and protons.
2) Rutherford's gold foil experiment showed atoms had a small, dense nucleus containing most of the mass.
3) Models were developed to explain the atom's structure, including Thomson's "plum pudding" model and Rutherford's nuclear model.
4) Later, the Bohr model incorporated allowed electron orbits, and neutrons were discovered in atomic nuclei.
Rutherford's experiment involved shooting alpha particles at a thin gold foil. He expected the particles to be slightly deflected, but instead observed that most passed through undeflected, some were slightly deflected, and a few were scattered backwards. This showed that the atom is mostly empty space, with a small, dense positively charged nucleus at the center surrounded by orbiting electrons. Further experiments revealed protons and neutrons in the nucleus. Isotopes of an element have the same number of protons but different numbers of neutrons, resulting in different atomic masses but the same chemical properties.
Here is a semi-log plot of the data with an exponential trendline:
The equation of the trendline is:
y = 12456e-0.4693x
Taking the natural log of both sides:
ln(y) = ln(12456) - 0.4693x
The slope is -0.4693
Using the equation:
t1/2 = 0.693/λ
λ = 0.4693
t1/2 = 0.693/0.4693 = 1.5
Therefore, the half-life of the isotope is 1.5 intervals, or 1.5 x 30 s = 45 seconds.
This document discusses the development of atomic structure models from ancient Greek philosophers through Rutherford's experiments. It describes Dalton's atomic theory that matter is made of atoms that cannot be divided further. Rutherford discovered that alpha particles fired at a gold foil occasionally bounced off at large angles, inconsistent with Thomson's uniform sphere model. This led to Rutherford's nuclear model with a small, dense nucleus containing positive charge and most mass, surrounded by electrons in empty space. Later, neutrons were discovered in atomic nuclei.
The document summarizes key information about the atmospheres of Venus, Earth, and Mars:
- Venus has a dense, 96% carbon dioxide atmosphere with a surface pressure of 90 bars and average temperature of 850°F, caused by a runaway greenhouse effect. Its clouds are composed of sulfuric acid.
- Earth has an atmosphere composed primarily of nitrogen and oxygen with a pressure of 1 bar and average temperature of 59°F. It hosts water clouds.
- Mars has a thin, 95% carbon dioxide atmosphere with a surface pressure of 0.007 bars and average temperature of -67°F, caused by a runaway refrigerator effect that stripped it of gases over time. It can host clouds of
The document summarizes key information about the geology of Venus. It states that Venus' surface is only about 500 million years old, as evidenced by impact craters, yet erosion rates are very low. Notable surface features include pancake-shaped volcanoes, coronae, and tectonic ridges and cracks. Venus has a slow 243-day rotation period that results in low wind speeds and erosion. Its atmosphere is extremely hot and dense.
The document provides information about Earth's moon, Luna. It discusses Luna's interior structure, including its crust, mantle, and core. It also describes Luna's surface features such as impact craters, maria (large dark plains), and regolith (loose rock and soil). Additionally, it discusses Luna's origin from a giant impact event about 4.5 billion years ago and its surface ages, with the highlands being the oldest at 4.4 billion years. The document also summarizes the Earth-Moon system, particularly how the Moon causes Earth's tides and is tide-locked in its orbit.
The document discusses the geology and evolution of Earth. It describes Earth's interior structure with a core, mantle, and crust. It explains tectonic plates, geological features like impact craters, and extinction events from impacts and climate change. It also summarizes the composition and evolution of Earth's atmosphere from early outgassing to today, including the role of greenhouse gases and life in transforming the atmosphere.
Early astronomers discovered and described key facts about the shape and size of the Earth and the structure of the solar system:
- Aristotle discovered that the Earth is round in 350 BC based on observations of lunar eclipses and changes in stars viewed from different locations.
- Eratosthenes estimated the circumference of the Earth to be about 25,000 miles in 240 BC by comparing shadows cast at different locations.
- Ptolemy proposed the geocentric model in 140 AD to explain the apparent retrograde motion of planets based on their orbits around the Earth.
- Copernicus proposed the heliocentric model in 1543 AD, placing the Sun at the center of the solar system with planets in
The document discusses factors involved in estimating the number of technological civilizations that may exist among stars using the Drake Equation. It examines each variable in the equation - R* (rate of formation of suitable stars), fp (fraction with planets), ne (number of planets suitable for life), fl (fraction where life appears), fi (fraction where intelligent life emerges), fc (fraction emitting detectable signals), and L (length of time signals emitted). It provides estimates and considerations for each variable based on current astronomical and biological understandings.
The document discusses the birth of the universe through several key topics:
1) Olber's Paradox - The question of why the night sky is dark if the universe contains an infinite number of stars. Explanations include a finite age universe and the expansion of space stretching light wavelengths.
2) Hubble's Law - The observation that more distant galaxies are moving away faster, indicating an expanding universe.
3) The Big Bang Theory - Proposed to explain the expansion of the universe and supported by evidence like the cosmic microwave background radiation. It provides an explanation for how the universe began from an extremely dense and hot initial state.
Galaxies are organized into clusters and superclusters that are separated by immense voids, creating a vast foam-like structure known as the "cosmic web". The largest known structure is the Sloan Great Wall, which is nearly 1.5 billion light years in length. Dark matter seems to come in standard clumps of about 30 million solar masses and 300 parsecs across, with a temperature of about 10,000 K. The cosmological principle assumes the universe is uniform on large enough scales, both homogeneous meaning no preferred locations and isotropic meaning no preferred directions.
Active galaxies can be categorized into three main types: Seyfert galaxies, radio galaxies, and quasars. Seyfert galaxies are active spiral galaxies with non-stellar spectra. Radio galaxies are active elliptical galaxies that also have non-stellar spectra and are strong radio emitters. Quasars are the most luminous active galaxies known, far brighter than normal galaxies, with non-stellar spectra. Centaurus A is the closest active galaxy and provides a unique laboratory for studying these powerful objects, showing evidence of a past merger that fuels activity at its center.
The document discusses different methods for measuring distances to galaxies. The Cepheid variable method can be used for galaxies in our Local Group. The Tully-Fisher relation uses the correlation between luminosity and rotational velocity of spiral galaxies to estimate distances to more distant spirals. Galaxy clusters and superclusters like the Local Supercluster provide context on larger scales of structure in the universe.
The document discusses the discovery of the Milky Way galaxy. It describes how in the early 20th century, Shapley and Curtis debated whether spiral nebulae were inside or outside our galaxy. Hubble later proved with Cepheid variables that they were actually other galaxies. The Milky Way is now understood to be a barred spiral galaxy about 30,000 light years wide, with a bulge, disk containing spiral arms, and halo of globular clusters. It formed from a cloud of gas that contracted under gravity and began rotating to form the spiral structure seen today.
Typical stellar evolution proceeds through several stages:
1. Red Giant Branch: Stars expand and cool as hydrogen fuses to helium in a shell around the core.
2. Horizontal Giant Branch: A helium flash occurs, followed by helium fusing to carbon in the core while hydrogen fuses in a shell.
3. Asymptotic Giant Branch: Helium and hydrogen shells alternately fuse heavier elements, causing the star to further expand and cool before ejecting its outer layers as a planetary nebula.
The document discusses the distance ladder, which is an attempt to determine astronomical distances by using a series of methods that build on one another. Within the Solar System, distances are measured using radar ranging. Within the galaxy, distances are measured using stellar parallax, main sequence fitting, and properties of Cepheid variable stars. Further out in the universe, distances are measured using the Tully-Fisher relation, Type Ia supernovae, brightest cluster galaxies, and Hubble's law. The document aims to answer fundamental questions about what exists in the universe and how large it is.
The document discusses the Hertzsprung–Russell diagram, which plots stars' spectral classifications and luminosity classes to show overall trends of stellar properties. It notes that spectral class indicates a star's temperature from hot (OBA) to cool (KM), while luminosity class reflects size from supergiants to dwarfs. The distribution of stars in the diagram relates their masses and lifetimes, with high-mass blue main sequence stars having short lives versus low-mass red main sequence stars with long lives. The diagram aims to understand what types of stars exist.
The document discusses asteroids and meteorites. Asteroids are remnants of planetary formation in the solar system. They are classified based on composition and location in relation to gravitational resonances with Jupiter. Ceres is the largest asteroid and is now classified as a dwarf planet. Meteorites provide information about early solar system conditions. They are classified based on composition as iron, stony, or stony-iron meteorites. Carbonaceous chondrites contain organic compounds and water, indicating the early solar system environment allowed these to form. Meteorites can also originate from the Moon or Mars.
The document discusses ring systems of the gas giant planets. It explains that ring systems are shaped by processes like the Roche limit and shepherding moons. It then provides details on the ring systems of Jupiter, Saturn, Uranus, and Neptune. Saturn's rings are the most extensive and are composed primarily of ice particles. The rings of the other planets are thinner and less is known about their compositions. Over time, ring systems evolve and may be temporary structures unless replenished.
The document discusses the moons of the gas giants Jupiter and Saturn, focusing on Jupiter's large Galilean moons (Io, Europa, Ganymede, and Callisto) and Saturn's moon Titan. It provides information about the surface conditions and geological features of these moons, including active volcanoes on Io, evidence that oceans may exist under the icy crusts of Europa and Ganymede, and liquid hydrocarbon seas on Titan. The document uses images from spacecraft like Galileo and Cassini to illustrate these characteristics and how they have been shaped by tidal interactions with the giant planets.
The document summarizes the formation of the solar system based on the nebular hypothesis. It describes how:
1) A giant cloud of dust and gas gravitationally contracted to form a solar nebula.
2) Condensation occurred within the solar nebula, with different materials condensing at different temperatures.
3) Accretion and differentiation led to the formation of planetesimals and eventually planets, with terrestrial planets like Earth forming near the sun and gas giants like Jupiter forming farther out where temperatures allowed hydrogen and helium to condense.
The document discusses optical telescopes, including refracting vs reflecting designs, and different types of reflecting telescopes like Newtonian and Cassegrain. It asks why telescopes are made big, and answers that it is to gather more light and achieve higher angular resolution, allowing dimmer and more distant objects to be observed. Bigger telescopes have larger light collecting areas. The document also notes that telescope technology aims to detect objects normally too dim for human vision and discusses using space-based and adaptive optics to overcome limitations from the atmosphere.
The document discusses electromagnetic radiation and its properties. It notes that EM radiation can be described as both a wave and particle. As a wave, it travels at the speed of light and is characterized by its frequency and wavelength. As a particle, it consists of individual quanta called photons. The document also discusses how spectroscopy can provide information about astronomical objects by examining the EM radiation they emit.
ISO/IEC 27001, ISO/IEC 42001, and GDPR: Best Practices for Implementation and...PECB
Denis is a dynamic and results-driven Chief Information Officer (CIO) with a distinguished career spanning information systems analysis and technical project management. With a proven track record of spearheading the design and delivery of cutting-edge Information Management solutions, he has consistently elevated business operations, streamlined reporting functions, and maximized process efficiency.
Certified as an ISO/IEC 27001: Information Security Management Systems (ISMS) Lead Implementer, Data Protection Officer, and Cyber Risks Analyst, Denis brings a heightened focus on data security, privacy, and cyber resilience to every endeavor.
His expertise extends across a diverse spectrum of reporting, database, and web development applications, underpinned by an exceptional grasp of data storage and virtualization technologies. His proficiency in application testing, database administration, and data cleansing ensures seamless execution of complex projects.
What sets Denis apart is his comprehensive understanding of Business and Systems Analysis technologies, honed through involvement in all phases of the Software Development Lifecycle (SDLC). From meticulous requirements gathering to precise analysis, innovative design, rigorous development, thorough testing, and successful implementation, he has consistently delivered exceptional results.
Throughout his career, he has taken on multifaceted roles, from leading technical project management teams to owning solutions that drive operational excellence. His conscientious and proactive approach is unwavering, whether he is working independently or collaboratively within a team. His ability to connect with colleagues on a personal level underscores his commitment to fostering a harmonious and productive workplace environment.
Date: May 29, 2024
Tags: Information Security, ISO/IEC 27001, ISO/IEC 42001, Artificial Intelligence, GDPR
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Training: ISO/IEC 27001 Information Security Management System - EN | PECB
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Article: https://pecb.com/article
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Main Java[All of the Base Concepts}.docxadhitya5119
This is part 1 of my Java Learning Journey. This Contains Custom methods, classes, constructors, packages, multithreading , try- catch block, finally block and more.
Thinking of getting a dog? Be aware that breeds like Pit Bulls, Rottweilers, and German Shepherds can be loyal and dangerous. Proper training and socialization are crucial to preventing aggressive behaviors. Ensure safety by understanding their needs and always supervising interactions. Stay safe, and enjoy your furry friends!
How to Fix the Import Error in the Odoo 17Celine George
An import error occurs when a program fails to import a module or library, disrupting its execution. In languages like Python, this issue arises when the specified module cannot be found or accessed, hindering the program's functionality. Resolving import errors is crucial for maintaining smooth software operation and uninterrupted development processes.
Strategies for Effective Upskilling is a presentation by Chinwendu Peace in a Your Skill Boost Masterclass organisation by the Excellence Foundation for South Sudan on 08th and 09th June 2024 from 1 PM to 3 PM on each day.
The simplified electron and muon model, Oscillating Spacetime: The Foundation...RitikBhardwaj56
Discover the Simplified Electron and Muon Model: A New Wave-Based Approach to Understanding Particles delves into a groundbreaking theory that presents electrons and muons as rotating soliton waves within oscillating spacetime. Geared towards students, researchers, and science buffs, this book breaks down complex ideas into simple explanations. It covers topics such as electron waves, temporal dynamics, and the implications of this model on particle physics. With clear illustrations and easy-to-follow explanations, readers will gain a new outlook on the universe's fundamental nature.
हिंदी वर्णमाला पीपीटी, hindi alphabet PPT presentation, hindi varnamala PPT, Hindi Varnamala pdf, हिंदी स्वर, हिंदी व्यंजन, sikhiye hindi varnmala, dr. mulla adam ali, hindi language and literature, hindi alphabet with drawing, hindi alphabet pdf, hindi varnamala for childrens, hindi language, hindi varnamala practice for kids, https://www.drmullaadamali.com
A Strategic Approach: GenAI in EducationPeter Windle
Artificial Intelligence (AI) technologies such as Generative AI, Image Generators and Large Language Models have had a dramatic impact on teaching, learning and assessment over the past 18 months. The most immediate threat AI posed was to Academic Integrity with Higher Education Institutes (HEIs) focusing their efforts on combating the use of GenAI in assessment. Guidelines were developed for staff and students, policies put in place too. Innovative educators have forged paths in the use of Generative AI for teaching, learning and assessments leading to pockets of transformation springing up across HEIs, often with little or no top-down guidance, support or direction.
This Gasta posits a strategic approach to integrating AI into HEIs to prepare staff, students and the curriculum for an evolving world and workplace. We will highlight the advantages of working with these technologies beyond the realm of teaching, learning and assessment by considering prompt engineering skills, industry impact, curriculum changes, and the need for staff upskilling. In contrast, not engaging strategically with Generative AI poses risks, including falling behind peers, missed opportunities and failing to ensure our graduates remain employable. The rapid evolution of AI technologies necessitates a proactive and strategic approach if we are to remain relevant.
Executive Directors Chat Leveraging AI for Diversity, Equity, and InclusionTechSoup
Let’s explore the intersection of technology and equity in the final session of our DEI series. Discover how AI tools, like ChatGPT, can be used to support and enhance your nonprofit's DEI initiatives. Participants will gain insights into practical AI applications and get tips for leveraging technology to advance their DEI goals.
Liberal Approach to the Study of Indian Politics.pdf
A1 15 Our Sun
1. The Solar Interior
LACC: §14.3, 15.2, 15.3
• Know what powers the sun
• Understand the Solar Neutrino Problem
• Know the Solar interior
An attempt to answer the “big questions”: what is
the sun? how does it effect us?
Thursday, April 15, 2010 1
2. The Sun: Wow! Sheet
Energy generated in the Sun's core takes a million years to reach its surface. Every
second 700 million tons (1/(3 billion billionth) of the sun’s total mass) of hydrogen are
converted into helium ash. In the process 5 million tons of pure energy is released;
therefore, as time goes on, the Sun is getting lighter.
Mass (tons) 2.19x1027
Mass (Earth = 1) 332,830 Principal chemistry (1.)
Equatorial radius (km) 695,000 Hydrogen 92.10%
Equatorial radius (Earth = 1) 108.97 Helium 7.80%
Mean density (gm/cm 3) 1.41 Oxygen 0.061%
Rotational period (days)! 25-36* Carbon 0.030%
Escape velocity (km/sec) 618.02 Nitrogen 0.084%
Luminosity (ergs/sec) 3.83x1033 Neon 0.076%
Magnitude (Vo) -26.8 Iron 0.0037%
Mean surface temperature! 10,800°F Silicon 0.0031%
Core temperature! 27,000,000°F Magnesium 0.0024%
Core density (gm/cm3) 150 Sulfur 0.0015%
Core pressure (atm) 340,000,000,000 All others 0.0015%
Age (billion years) 4.5 1. % by # of atoms abundances
* The Sun's period of rotation at the surface varies from approximately 25 days at the
equator to 36 days at the poles. Deep down, below the convective zone, everything
appears to rotate with a period of 27 days.
http://www.solarviews.com/eng/sun.htm
Thursday, April 15, 2010 2
3. The Proton-Proton Chain
http://astro.unl.edu/classaction/loader.html?filename=animations/sunsolarenergy/
fusion01.swf&movieid=fusion01&width=550&height=550&version=6.0.0
Thursday, April 15, 2010 3
4. The Atom, e.g. He 4
http://www.bio.miami.edu/~cmallery/150/chemistry/c8.2x5.helium.jpg
Thursday, April 15, 2010 4
5. Subatomic Particles of
Interest
Particle Symbols Charge Mass
Protons p, p+, 1H, H+ +1 1.0073
Neutrons n, n0 0 1.0087
Electrons e, e+, β+ -1 0.0005
Positron e- , β - +1 0.0005
Neutrino ν 0 0?
Gamma Ray γ 0 0
Alpha Particle α, 4He, He2+ +2 4.0015
Thursday, April 15, 2010 5
6. p-p Chain: Energy Production
The evidence is strong that the sun is "burning" H to make He:
4H + 2e- --> He4 + 2 neutrinos + 6 photons
In this reaction, the final particles have less internal energy than the
starting particles. Since energy is conserved, the extra energy is
released as energy of motion of the nuclei and electrons in the
solar gas, the production of photons [pure energy] and, finally, the
energy of the neutrinos, which just zip right out of the Sun. That is
the gas gets hotter and has lots of photons (and neutrinos). The
amount of energy involved is 26 MeV (26 million eV) each time the
reaction above happens. (By comparison, CH4 + 2O2 --> CO2 + 2H2O
results in 5.5 eV of energy.)
Why do we think that this is what goes on?
•
Energy output of millions of eV per reaction is needed if the Sun
has been producing energy at the observed rate over billions of years.
•
The reactions exist. (They have been studied in the laboratory.)
•
There is a consistent step-by-step theory for the reaction.
Davison E. Soper, Institute of Theoretical Science, University of Oregon, Eugene OR 97403 USA soper@bovine.uoregon.edu
http://zebu.uoregon.edu/~soper/Sun/fusion.html
Thursday, April 15, 2010 6
7. Solar Neutrino Problem
Super-
Kamiokande, a
neutrino
detector in
Japan, holds
50,000 tons of
ultrapure water
surrounded by
light tubes.
http://www.scidacreview.org/0601/html/astro.html
Thursday, April 15, 2010 7
8. Solar Neutrino Problem
Over the years scientists
have considered two
possible explanations of
the solar neutrino problem:
1. Perhaps we don't
understand the Sun
well enough. Maybe a
better theory of the
internal structure of the
Sun would predict fewer
neutrinos, in agreement
with the measurements.
2. Perhaps we don't
understand neutrinos
well enough; maybe
they have some
features beyond the
standard theory of
neutrinos that account
for the problem.
http://www.cora.nwra.com/~werne/eos/text/neutrino.html
Thursday, April 15, 2010 8
9. The Solar Neutrino
Problem
Particles in the Standard
Model of particle physics:
The Standard Model
contains 3 neutrinos of
definite flavor, and a set
of corresponding anti-
particles.
http://conferences.fnal.gov/lp2003/forthepublic/neutrinos/index.html
Thursday, April 15, 2010 9
10. Hydrostatic Equilibrium
http://physics.uoregon.edu/~jimbrau/astr122/Notes/Chapter16.html
Thursday, April 15, 2010 10
11. Solar Interior
http://sprg.ssl.berkeley.edu/%7Eabbett/sun1.html
Thursday, April 15, 2010 11
12. Solar Interior
The photons produced in nuclear reactions take about a million years to
move from the core to the surface. The photons scatter off the dense gas
particles in the interior and move about a centimeter between collisions. In each
collision they transfer some of their energy to the gas particles. By the time
photons reach the photosphere, the gamma rays have become photons of
much lower energy---visible light photons. Because the photons now reaching
the surface were produced about a million years ago, they tell us about the
conditions in the core as it was a million years ago. The other particle produced in
nuclear reactions has a less tortuous path out of the core.
A neutrino is a massless (or very nearly massless) particle that rarely interacts
with ordinary matter. Neutrinos travel extremely fast---the speed of light if they
have zero mass or very close to the speed of light if they have a small mass.
Because they travel so fast and interact so rarely with matter, neutrinos pass
from the core of the Sun to the surface in only two seconds. They
take less than 8.5 minutes to travel the distance from the Sun to the Earth. If you
could detect them, the neutrinos would tell you about the conditions in the Sun's
core as it was only 8.5 minutes ago (much more current information than the
photons!).
http://www.astronomynotes.com/starsun/s4.htm
Thursday, April 15, 2010 12
13. Solar Core
http://fas.org/irp/imint/docs/rst/Sect20/A5a.html
Thursday, April 15, 2010 13
14. Solar Interior
Core Radiation
• p-p chain occurs • photons travel
• convection • vacuum, gasses
Radiative zone Convection
• photon random walk • bulk fluid flow
• radiation • liquid, gasses
Convection zone Conduction
• convection cells • individual molecules collide
• convection • solids
Thursday, April 15, 2010 14
15. The Solar Interior
LACC: §14.3, 15.2, 15.3
• Know what powers the sun: Nuclear Fusion,
the p-p chain, 4H + 2e- --> He4 + 2 ν + 6 γ
• Understand the Solar Neutrino Problem: It
seems that neutrinos can change flavor
• Know the Solar interior: core, radiative zone,
convection zone, photosphere
An attempt to answer the “big questions”: what is
the sun? how does it effect us?
Thursday, April 15, 2010 15
16. HW: Franknoi, Morrison, and Wolff,
Voyages Through the Universe, 3rd ed.
• Ch 15, p354: #4
• Ch 14: Tutorial Quizzes accessible from: http://
www.brookscole.com/cgi-brookscole/course_products_bc.pl?
fid=M20b&product_isbn_issn=9780495017899&discipline_number=19
• Ch 15: Image Analysis Quizzes accessible
from: http://www.brookscole.com/cgi-brookscole/
course_products_bc.pl?
fid=M20b&product_isbn_issn=9780495017899&discipline_number=19
Due beginning of next class period.
Thursday, April 15, 2010 16
17. Solar Surface and Atmosphere
LACC: §14.3, 15.2, 15.3
• Know the sun’s atmosphere
• Know solar surface features
• Know how the sun affects the earth
An attempt to answer the “big questions”: what is
the sun? how does it effect us?
Thursday, April 15, 2010 17
18. Solar Atmosphere
K = Kelvin
°C = Celsius
°F = Fahrenheit
K = °C + 273.15
°F = 1.8°C + 32°
So, at high temperature,
°F ≅ 1.8°C
At very high temperatures,
°F ≅ 1.8K
http://rst.gsfc.nasa.gov/Sect20/A5a.html
Thursday, April 15, 2010 18
19. Solar Features
http://ircamera.as.arizona.edu/NatSci102/lectures/sun.htm
Thursday, April 15, 2010 19
20. Solar Features: Sunspots
http://www.astro.wisc.edu/
http://starchild.gsfc.nasa.gov/docs/
~sparke/ast103/
StarChild/questions/question17.html
lecture11.html
Granules are individual convection cells.
Thursday, April 15, 2010 20
21. Solar Features: Sunspots
Sunspots are dark, planet-sized regions that appear on
the "surface" of the Sun. Sunspots are "dark" because
they are cooler than their surroundings. A large
sunspot might have a central temperature of 4,000 K
(about 3,700° C or 6,700° F), much lower than the 5,800
K (about 5,500° C or 10,000° F) temperature of the
adjacent photosphere. Sunspots are only dark in
contrast to the bright face of the Sun. If you could cut an
average sunspot out of the Sun and place it elsewhere in
the night sky, it would be about as bright as a full moon.
Sunspots have a lighter outer section called the
penumbra, and a darker central region named the umbra.
Sunspots form over periods lasting from days to
weeks, and can persist for weeks or even months
http://www.windows.ucar.edu/
before dissipating. The average number of spots visible
tour/link=/sun/images/
on the face of the Sun is not constant, but varies in a
sunspots_earth_size_big_jpg_i
multi-year cycle. Historical records of sunspot counts,
mage.html&edu=high
which go back hundreds of years, verify that this sunspot
cycle has an average period of roughly eleven years.
http://www.windows.ucar.edu/tour/link=/sun/
atmosphere/sunspots.html&edu=high
Thursday, April 15, 2010 21
22. Solar Features:
Sunspot Cycle
Although astronomers have observed the fairly regular rise and fall of
sunspot counts in this 11-year cycle for several centuries, there have
also been disruptions in this pattern. The largest well-documented
disruption was an era that lasted from about 1645 to 1715 during which
almost no sunspots were seen. This long lull is known as the Maunder
Minimum. Curiously, Europe and parts of North America were struck by
spells of remarkably cold weather at roughly the same time.
http://www.windows.ucar.edu/tour/link=/sun/activity/solar_variation.html
Thursday, April 15, 2010 22
23. Solar Features:
Sunspots--Cause
Sunspots are magnetic -- they occur
in pairs where one is a north pole
while the other is a south pole.
Every 11 years, the more western parts
of sunspot pairs will change from
magnetic N to magnetic S (or vice
versa). (From Chaisson & McMillan,
Astronomy Today)
http://ircamera.as.arizona.edu/NatSci102/
lectures/sun.htm
Thursday, April 15, 2010 23
24. Solar Features:
Sunspots and Magnetism
Every 11 years the sun’s
magnetic field snaps back
to situation #1. But, when it
snaps back, the North and
South magnetic poles will be
reversed.
So the sunspot cycle is
every 11 years, but the solar
magnetic field cycle is every
22 years.
http://www.windows.ucar.edu/tour/link=/sun/atmosphere/
sunspot_form_jpg_image.html&edu=high
Thursday, April 15, 2010 24
25. Solar Features: Prominences
(and Filaments)
One of the most spectacular solar sights
is a prominence. A solar prominence is
a cloud of solar gas held above the
Sun's surface by the Sun's magnetic
field. Last month, NASA's Sun-orbiting
SOHO spacecraft imaged an
impressively large prominence hovering
over the surface, pictured above. The
Earth would easily fit under the hovering
curtain of hot gas. A quiescent
prominence typically lasts about a
month, and may erupt in a Coronal
Mass Ejection (CME) expelling hot gas
into the Solar System. Although
somehow related to the Sun's changing
magnetic field, the energy mechanism
that creates and sustains a Solar
prominence is still a topic of research.
http://apod.nasa.gov/apod/ap040330.html
Thursday, April 15, 2010 25
26. Solar Features: Prominences
(and Filaments)
Hot gas frequently erupts from the
Sun. One such eruption produced the
glowing filament pictured above,
which was captured in 2000 July by
the Earth-orbiting TRACE satellite.
The filament, although small
compared to the overall size of the
Sun, measures over 100,000
kilometers in height, so that the entire
Earth could easily fit into its
outstretched arms. Gas in the
filament is funneled by the complex
and changing magnetic field of the
Sun. After lifting off from the Sun's
surface, most of the filamentary gas
will eventually fall back.
http://antwrp.gsfc.nasa.gov/apod/ap040725.html
Thursday, April 15, 2010 26
27. Solar Features: Prominences
(and Filaments)
http://www.veoh.com/browse/videos/category/technology/watch/v2191746WPa6CtKC
Thursday, April 15, 2010 27
28. Flares vs Filament (Prominence)
Solar flare (171Å) Solar flare (1600Å) Solar flare (white light)
The two images on the left were
taken on 25 June 2000, around
07:37UT (the images were
rotated, so that north is to the
left). The image on the left
shows a filament in the process
of being ejected from the Sun,
with cool (dark) and hot (bright;
around 1.5 million degrees)
material at opposite ends of the
long, nearly vertical structure.
http://soi.stanford.edu/results/SolPhys200/Schrijver/TRACEpodoverview.html
Thursday, April 15, 2010 28
29. Solar Features: Flares
Solar flares are essentially huge explosions on the
Sun. Flares occur when intense magnetic fields on
the Sun become too tangled. Like a rubber band that
snaps when it is twisted too far, the tangled
magnetic fields release energy when they "snap".
Solar flares emit huge bursts of electromagnetic
radiation, including X-rays, ultraviolet radiation, visible
light, and radio waves. The energy emitted by a solar
flare is more than a million times greater than the
energy from a volcanic explosion on Earth!
Although solar flares can be visible in white light, they
are often more readily noticed via their bright X-ray
and ultraviolet emissions. Coronal mass ejections
often accompany solar flares, though scientists are
still trying to determine exactly how the two
phenomena are related. Solar flares burst forth from
the intense magnetic fields in the vicinity of active
regions on the Sun. Solar flares are most common
during times of peak solar activity, the "solar max"
years of the sunspot cycle.
http://www.windows.ucar.edu/tour/link=/
sun/atmosphere/solar_flares.html&edu=high
Thursday, April 15, 2010 29
30. Coronal Mass Ejection
http://www.windows.ucar.edu/tour/link=/sun/images/aug1980cme_jpg_image.html
Thursday, April 15, 2010 30
31. Coronal Mass Ejection
"Without warning, the relatively calm solar atmosphere can be torn asunder by
sudden outbursts of a scale unknown on Earth. Catastrophic events of
incredible energy...stretch up to halfway across the visible solar surface,
suddenly and unpredictably open up and expel their contents, defying the Sun's
enormous gravity." (Sun, Earth, and Sky by Kenneth R. Lang)
These catastrophic events that the author is speaking about are coronal mass
ejections (CME's).
Coronal mass ejections are explosions in the Sun's corona that spew out
solar particles. The CME's typically disrupt helmet streamers in the solar
corona. As much as 1x1013 (10 trillion) kilograms of material can be ejected into
the solar wind. Coronal mass ejections propagate out in the solar wind, where
they may encounter the Earth and influence geomagnetic activity.
CME's are believed to be driven by energy release from the solar magnetic
field. How this energy release occurs, and the relationship between different
types of solar activity, is one of the many puzzles facing solar physicists today.
http://www.windows.ucar.edu/tour/link=/sun/cmes.html&edu=high
Thursday, April 15, 2010 31
32. Magnetic Storms
CME's can seriously disrupt the Earth's environment. Intense radiation from the Sun,
which arrives only 8 minutes after being released, can alter the Earth's outer
atmosphere, disrupting long-distance radio communications and deteriorating satellite
orbits. Very energetic particles pushed along by the shock wave of the CME can
endanger astronauts or fry satellite electronics. These energetic particles arrive at the
Earth (or Moon) about an hour later. The actual coronal mass ejection arrives at the
Earth one to four days after the initial eruption, resulting in strong geomagnetic
storms, aurorae and electrical power blackouts.
"Thus, the Sun's sudden and
unexpected outbursts remain as
unpredictable as most human
passions. They just keep on
happening, and even seem to be
necessary to purge the Sun of pent-
up frustration and to relieve it of
twisted, contorted
magnetism." (Kenneth R. Lang, Sun,
Earth and Sky)
http://www.windows.ucar.edu/tour/
link=/sun/cmes.html&edu=high
http://ess.nrcan.gc.ca/rrnh-rran/proj3_e.php
Thursday, April 15, 2010 32
33. Solar Wind
The Sun is flinging 1 million tons of
matter out into space every second!
We call this material solar wind. Once
the solar wind is blown into space, the
particles travel at supersonic speeds of
200-800 km/sec! These particles travel
all the way past Pluto and do not slow
down until they reach the termination shock within the heliosphere. The Heliosphere is
the entire region of space influenced by the Sun.
The solar wind plasma is very thin. Near the Earth, the plasma is only about 6 particles
per cubic centimeter. So, even though the wind travels SUPER fast, it wouldn't even
ruffle your hair if you were to stand in it because it's so thin! But, it is responsible for
such unusual things as:
•
auroral lights
•
fueling magnetospheric storms
The particles of the solar wind, and the Sun's magnetic field (IMF) are stuck together,
therefore the solar wind carries the IMF (interplanetary magnetic field) with it into space.
http://www.windows.ucar.edu/tour/link=/sun/solar_wind.html&edu=mid
Thursday, April 15, 2010 33
34. Aurora
http://www.nasa.gov/centers/goddard/
news/topstory/2005/dueling_auroras.html
http://apod.nasa.gov/apod/ap060329.html
Thursday, April 15, 2010 34
35. Solar Surface and Atmosphere
LACC: §14.3, 15.2, 15.3
• Know the sun’s atmosphere: photosphere
(visible), chromosphere (reddish), corona (2
million Kelvin), solar wind (e- and p+’s)
• Know solar surface features: granules,
sunspots, prominences, flares, coronal mass
ejections
• Know how the sun affects the earth: CME
disruption of electronics, aurora
An attempt to answer the “big questions”: what is
the sun? how does it effect us?
Thursday, April 15, 2010 35
36. HW: Franknoi, Morrison, and Wolff,
Voyages Through the Universe, 3rd ed.
• Ch 14, p354: #5--Prominence, Flare, Coronal
Mass Ejection (mention energy, size, and time)
• Ch 15: Image Analysis Quizzes accessible
from: http://www.brookscole.com/cgi-brookscole/
course_products_bc.pl?
fid=M20b&product_isbn_issn=9780495017899&discipline_number=19
• 16, 17: Tutorial Quizzes accessible from: http://
www.brookscole.com/cgi-brookscole/course_products_bc.pl?
fid=M20b&product_isbn_issn=9780495017899&discipline_number=19
Due beginning of next class period.
Thursday, April 15, 2010 36