1. The document describes the motions of objects in the sky and our location in the universe, including a description of the Milky Way galaxy and our solar system.
2. Key concepts covered include the coordinate systems used to locate celestial objects, precession of the Earth, and the causes of the seasons due to the tilt of the Earth's axis.
3. Motions of objects like the sun and stars are explained, including how the sun appears to move along the ecliptic and causes the seasons as the Earth orbits around it.
Unit I: Force, Motion and Energy
Module 2 – Work and Energy
· Definition and Calculation of Work
· Kinetic Energy
· Potential Energy
· Work, Energy and Power Relations
Planet Earth and its properties necessary to support lifeSimple ABbieC
Department of Education | Senior High School
Topic: Planet Earth and its properties necessary to support life.
Learning Competency:
Earth and Life Science: Recognize the uniqueness of Earth, being the only planet in the Solar System with properties necessary to support life.
Earth Science (for STEM): Describe the characteristics of Earth that are necessary to support life.
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Facebook: https://www.facebook.com/Simple-ABbieC-131584525051378/
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Learn about meteors, meteoroids, and meteorites. What's the difference? What are they made of? How do they move? Find out, from the University of Arizona, where we've discovered 52% of all known near-Earth objects.
Unit I: Force, Motion and Energy
Module 2 – Work and Energy
· Definition and Calculation of Work
· Kinetic Energy
· Potential Energy
· Work, Energy and Power Relations
Planet Earth and its properties necessary to support lifeSimple ABbieC
Department of Education | Senior High School
Topic: Planet Earth and its properties necessary to support life.
Learning Competency:
Earth and Life Science: Recognize the uniqueness of Earth, being the only planet in the Solar System with properties necessary to support life.
Earth Science (for STEM): Describe the characteristics of Earth that are necessary to support life.
Please LIKE / FOLLOW and SHARE my other social media accounts.
Facebook: https://www.facebook.com/Simple-ABbieC-131584525051378/
-----------------------------------------------------------------------
Youtube:
http://tiny.cc/SimpleABbieC
-----------------------------------------------------------------------
Slideshare:
https://www.slideshare.net/AbbieMahinay
-----------------------------------------------------------------------
Blogger:
https://simpleabbiec.blogspot.com/?m=1
Learn about meteors, meteoroids, and meteorites. What's the difference? What are they made of? How do they move? Find out, from the University of Arizona, where we've discovered 52% of all known near-Earth objects.
Astronomy - State of the Art - GalaxiesChris Impey
Astronomy - State of the Art is a course covering the hottest topics in astronomy. In this section, the properties of galaxies are discussed, including supermassive black holes and dark matter.
A lecture I'd given on spiral galaxies, barred spirals, mass of galaxies, Sgr A, Elliptical galaxies, standard candles, dark matter, composition of the universe, back in my university days.
You probably need to download the file for the animations to work.
E teaching- Smart Classes, Online Teaching, WebcastingBabu Appat
Now the profession of teaching is undergoing drastic changes. A person who is not having enough computer knowledge is considered to be illiterate in the modern times. A teacher who is not having enough technical knowledge to acquire, update, and effectively present his acumen to the right group of students at its right time cannot be considered a good teacher. This session is to familiarise you with some modern tools of teaching.
factor responsible for nutrient in soil and their contribution to soil fertility. importance of soil fertility, processes involved in sustaining soil productivity
Astronomy- State of the art is a course covering the hottest topics in astronomy. In this section, the exotic end states of stars are discussed, including pulsars, neutron stars, and black holes.
Astronomy Impact
Astronomy Essay
Astronomy Essay
Astronomy Essay
Astronomy Essay
Essay about Telescopes in Astronomy
Socrates On Astronomy
Ancient Greek Astronomy Essay
History of Astronomy
Multiple Representations And Misconceptions In Science Instructional Materials, originally presented at a high school Science Teacher Forum, January 2006.
Cristina Giosue proposes Donkey Milk for Italy--includes fascinating analyses of milk's energy content and systematic feedback analysis of animal husbandry.
Epistemic Interaction - tuning interfaces to provide information for AI supportAlan Dix
Paper presented at SYNERGY workshop at AVI 2024, Genoa, Italy. 3rd June 2024
https://alandix.com/academic/papers/synergy2024-epistemic/
As machine learning integrates deeper into human-computer interactions, the concept of epistemic interaction emerges, aiming to refine these interactions to enhance system adaptability. This approach encourages minor, intentional adjustments in user behaviour to enrich the data available for system learning. This paper introduces epistemic interaction within the context of human-system communication, illustrating how deliberate interaction design can improve system understanding and adaptation. Through concrete examples, we demonstrate the potential of epistemic interaction to significantly advance human-computer interaction by leveraging intuitive human communication strategies to inform system design and functionality, offering a novel pathway for enriching user-system engagements.
GraphRAG is All You need? LLM & Knowledge GraphGuy Korland
Guy Korland, CEO and Co-founder of FalkorDB, will review two articles on the integration of language models with knowledge graphs.
1. Unifying Large Language Models and Knowledge Graphs: A Roadmap.
https://arxiv.org/abs/2306.08302
2. Microsoft Research's GraphRAG paper and a review paper on various uses of knowledge graphs:
https://www.microsoft.com/en-us/research/blog/graphrag-unlocking-llm-discovery-on-narrative-private-data/
Software Delivery At the Speed of AI: Inflectra Invests In AI-Powered QualityInflectra
In this insightful webinar, Inflectra explores how artificial intelligence (AI) is transforming software development and testing. Discover how AI-powered tools are revolutionizing every stage of the software development lifecycle (SDLC), from design and prototyping to testing, deployment, and monitoring.
Learn about:
• The Future of Testing: How AI is shifting testing towards verification, analysis, and higher-level skills, while reducing repetitive tasks.
• Test Automation: How AI-powered test case generation, optimization, and self-healing tests are making testing more efficient and effective.
• Visual Testing: Explore the emerging capabilities of AI in visual testing and how it's set to revolutionize UI verification.
• Inflectra's AI Solutions: See demonstrations of Inflectra's cutting-edge AI tools like the ChatGPT plugin and Azure Open AI platform, designed to streamline your testing process.
Whether you're a developer, tester, or QA professional, this webinar will give you valuable insights into how AI is shaping the future of software delivery.
Smart TV Buyer Insights Survey 2024 by 91mobiles.pdf91mobiles
91mobiles recently conducted a Smart TV Buyer Insights Survey in which we asked over 3,000 respondents about the TV they own, aspects they look at on a new TV, and their TV buying preferences.
Builder.ai Founder Sachin Dev Duggal's Strategic Approach to Create an Innova...Ramesh Iyer
In today's fast-changing business world, Companies that adapt and embrace new ideas often need help to keep up with the competition. However, fostering a culture of innovation takes much work. It takes vision, leadership and willingness to take risks in the right proportion. Sachin Dev Duggal, co-founder of Builder.ai, has perfected the art of this balance, creating a company culture where creativity and growth are nurtured at each stage.
Neuro-symbolic is not enough, we need neuro-*semantic*Frank van Harmelen
Neuro-symbolic (NeSy) AI is on the rise. However, simply machine learning on just any symbolic structure is not sufficient to really harvest the gains of NeSy. These will only be gained when the symbolic structures have an actual semantics. I give an operational definition of semantics as “predictable inference”.
All of this illustrated with link prediction over knowledge graphs, but the argument is general.
DevOps and Testing slides at DASA ConnectKari Kakkonen
My and Rik Marselis slides at 30.5.2024 DASA Connect conference. We discuss about what is testing, then what is agile testing and finally what is Testing in DevOps. Finally we had lovely workshop with the participants trying to find out different ways to think about quality and testing in different parts of the DevOps infinity loop.
Accelerate your Kubernetes clusters with Varnish CachingThijs Feryn
A presentation about the usage and availability of Varnish on Kubernetes. This talk explores the capabilities of Varnish caching and shows how to use the Varnish Helm chart to deploy it to Kubernetes.
This presentation was delivered at K8SUG Singapore. See https://feryn.eu/presentations/accelerate-your-kubernetes-clusters-with-varnish-caching-k8sug-singapore-28-2024 for more details.
Accelerate your Kubernetes clusters with Varnish Caching
Milky Way physics 101
1. Astronomy 101 1. Where we are in the Universe 2. Motions on the sky
2. 200 billion stars Milky Way Galaxy 1 pc = 3.26 ly Galactic year = 225 million yr Our sun is 4.6 billion yr old 25,000 light years, Or ~ 8 kpc
3. The parallax angle p Define 1 parsec as a distance to a star whose parallax is 1 arcsec d (in parsecs) = 1/ p 1 pc = 206265 AU = 3.26 ly Small-angle formula:
4. “ Milky Way” – a milky patch of stars that rings the Earth Galactos = milk in Greek
6. Galaxy M31 in Andromeda – similar to the Milky Way Galaxy 1 Mpc from us
7. ~ 100 billion galaxies in the observable Universe 10 day exposure photo! Over 1500 galaxies in a spot 1/30 the diameter of the Moon Farthest and oldest objects are 13 billion light years away! Hubble Deep Field Hubble Space telescope
10. The Galactic Center Wide-angle optical view of the GC region Galactic center Our view (in visible light) towards the galactic center (GC) is heavily obscured by gas and dust Extinction by 30 magnitudes Only 1 out of 10 12 optical photons makes its way from the GC towards Earth!
11. If one looks at this region with big telescopes and near-infrared cameras one can see lots of stars. If one takes pictures every year it seems that some stars are moving very fast (up to 1500 kilometers per second). The fastest stars are in the very center - the position marked by the radio nucleus Sagittarius A* (cross). Distance between stars is less that 0.01 pc
12. A Black Hole at the Center of Our Galaxy? By following the orbits of individual stars near the center of the Milky Way, the mass of the central black hole could be determined to ~ 2.6 million solar masses
13. Radio observations with Very Long Baseline Interferometry (VLBI) that are thousands of times more precise than optical observations (good enough to easily pin-point a source the size of a pea in New York when sitting in Paris)
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16. Size ~ 1 AU (12 Schwarzschild Radii) Density ~ 7x10 21 M sun /pc 3 Recent VLBI observations (latest issue of Nature)
19. The Kuiper Belt – home for short-period comets?? Starting in 1992, astronomers have become aware of a vast population of small bodies orbiting the sun beyond Neptune. There are at least 70,000 "trans-Neptunians" with diameters larger than 100 km in the radial zone extending outwards from the orbit of Neptune (at 30 AU) to 50 AU.
23. Launched in 1977 Voyager 1 is now 95 AU from the Sun! (13 light-hours, or 14 billion km) The most distant human-made object in the Universe Speed 17.2 km/sec (3.6 AU per year) Voyagers 1 and 2
24. Proxima Centauri (Alpha Centauri C) Closest star (4.2 light-years from the Sun) It would take ~ 80,000 years for Voyager 1 to reach a neighboring star Plutonium battery will be dead by 2020 Mission may be shut down by 11/2005 Golden record
25. Local Bubble Density ~ 0.05 atoms/cm 3 Temperature ~ 10 5 K Remnant of supernova explosion?
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27. Distance scale Looking through space = travel in time! 10 7 m planets 10 9 m Sun 10 17 m = 3 pc distance between stars 10 21 m = 10 kpc galaxy 10 11 m = 1 AU Solar System 10 25 m = 100 Mpc Largest structure 10 26 m = Gpc Hubble radius
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29. The constellations are an ancient heritage handed down for thousands of years as celebrations of great heroes and mythical creatures. Here Sagittarius and Scorpius hang above the southern horizon.
30. Constellations In ancient times, constellations only referred to the brightest stars that appeared to form groups, representing mythological figures.
31. Constellations (2) Today, constellations are well-defined regions on the sky, irrespective of the presence or absence of bright stars in those regions.
32. Names and Standard Abbreviations of Constellations The following list of constellation names and abbreviations is in accordance with the resolutions of the International Astronomical Union (Trans. IAU, 1, 158; 4, 221; 9, 66 and 77). The boundaries of the constellations are listed by E. Delporte, on behalf of the IAU, in, Delimitation scientifique des constellations (tables et cartes), Cambridge University Press, 1930; they lie along the meridians of right ascension and paralleIs of declination for the mean equator and equinox of 1875.0. http://www.iau.org/IAU/Activities/nomenclature/const.html International Astronomical Union (IAU) 88 constellations Librae Lib Libra Aquilae Aql Aquila Leporis Lep Lepus Aquarii Aqr Aquarius Leonis Minoris LMi Leo Minor Apodis Aps Apus Leonis Leo Leo Antliae Ant Antlia Lacertae Lac Lacerta Andromedae And Andromeda Genitive Nominative Genitive Nominative
36. Hipparchus of Rhodes Born: 190 BC in Nicaea (now Iznik), Bithynia (now Turkey) Died: 120 BC in probably Rhodes, Greece Catalogue of 850 stars Discovered precession of the Earth’s orbit Determined the distance to the moon Compiled trigonometric tables For thousands of years, discoveries in math and science were driven by astronomical observations!
40. OFFICIAL STAR-NAMING PROCEDURES Bright stars from first to third magnitude have proper names that have been in use for hundreds of years. Most of these names are Arabic. Examples are Betelgeuse , the bright orange star in the constellation Orion , and Dubhe , the second-magnitude star at the edge of the Big Dipper's cup ( Ursa Major ). A few proper star names are not Arabic. One is Polaris , the second-magnitude star at the end of the handle of the Little Dipper ( Ursa Minor ). Polaris also carries the popular name, the North Star. A second system for naming bright stars was introduced in 1603 by J. Bayer of Bavaria. In his constellation atlas, Bayer assigned successive letters of the Greek alphabet to the brighter stars of each constellation. Each Bayer designation is the Greek letter with the genitive form of the constellation name. Thus Polaris is Alpha Ursae Minoris . Occasionally, Bayer switched brightness order for serial order in assigning Greek letters. An example of this is Dubhe as Alpha Ursae Majoris, with each star along the Big Dipper from the cup to handle having the next Greek letter. Faint stars are designated in different ways in catalogs prepared and used by astronomers. One is the Bonner Durchmusterung , compiled at Bonn Observatory starting in 1837. A third of a million stars are listed by "BD numbers." The Smithsonian Astrophysical Observatory (SAO) Catalogue , the Yale Star Catalog , and The Henry Draper Catalog published by Harvard College Observatory are all widely used by astronomers. The Supernova of 1987 (Supernova 1987a), one of the major astronomical events of this century, was identified with the star named SK -69 202 in the very specialized catalog, the Deep Objective Prism Survey of the Large Magellanic Cloud , published by the Warner and Swasey Observatory. These procedures and catalogs accepted by the International Astronomical Union are the only means by which stars receive long-lasting names.
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43. The celestial sphere The entire sky appears to turn around imaginary points in the northern and southern sky once in 24 hours. This is termed the daily or diurnal motion of the celestial sphere, and is in reality a consequence of the daily rotation of the earth on its axis. The diurnal motion affects all objects in the sky and does not change their relative positions: the diurnal motion causes the sky to rotate as a whole once every 24 hours. Superposed on the overall diurnal motion of the sky is "intrinsic" motion that causes certain objects on the celestial sphere to change their positions with respect to the other objects on the celestial sphere. These are the "wanderers" of the ancient astronomers: the planets, the Sun, and the Moon.
44. We can define a useful coordinate system for locating objects on the celestial sphere by projecting onto the sky the latitude-longitude coordinate system that we use on the surface of the earth. The stars rotate around the North and South Celestial Poles . These are the points in the sky directly above the geographic north and south pole, respectively. The Earth's axis of rotation intersects the celestial sphere at the celestial poles. Fortunately, for those in the northern hemisphere, there is a fairly bright star real close to the North Celestial Pole (Polaris or the North star). Another important reference marker is the celestial equator: an imaginary circle around the sky directly above the Earth's equator. It is always 90 degrees from the poles. All the stars rotate in a path that is parallel to the celestial equator . The celestial equator intercepts the horizon at the points directly east and west anywhere on the Earth.
45.
46. Equatorial coordinates Right ascension (similar to longitude) Declination (similar to latitude) Counted from Vernal Equinox Measured in hours, minutes, seconds Full circle is 24 hours Counted from celestial equator Measured in degrees etc.
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49. The arc that goes through the north point on the horizon, zenith, and south point on the horizon is called the meridian . The positions of the zenith and meridian with respect to the stars will change as the celestial sphere rotates and if the observer changes locations on the Earth, but those reference marks do not change with respect to the observer's horizon. Any celestial object crossing the meridian is at its highest altitude (distance from the horizon) during that night (or day). During daylight, the meridian separates the morning and afternoon positions of the Sun. In the morning the Sun is ``ante meridiem'' (Latin for ``before meridian'') or east of the meridian, abbreviated ``a.m.''. At local noon the Sun is right on the meridian. At local noon the Sun is due south for northern hemisphere observers and due north for southern hemisphere observers. In the afternoon the Sun is ``post meridiem'' (Latin for ``after meridian'') or west of the meridian, abbreviated ``p.m.''.
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51. If you are in the northern hemisphere, celestial objects north of the celestial equator are above the horizon for more than 12 hours because you see more than half of their total 24-hour path around you. Celestial objects on the celestial equator are up 12 hours and those south of the celestial equator are above the horizon for less than 12 hours because you see less than half of their total 24-hour path around you. The opposite is true if you are in the southern hemisphere. Notice that stars closer to the NCP are above the horizon longer than those farther away from the NCP. Those stars within an angular distance from the NCP equal to the observer's latitude are above the horizon for 24 hours---they are circumpolar stars. Also, those stars close enough to the SCP (within a distance = observer's latitude) will never rise above the horizon. They are also called circumpolar stars.
55. Precession (1) The Sun’s gravity is doing the same to Earth. The resulting “wobbling” of Earth’s axis of rotation around the vertical w.r.t. the Ecliptic takes about 26,000 years and is called precession . At left, gravity is pulling on a slanted top. => Wobbling around the vertical.
56. Precession (2) As a result of precession, the celestial north pole follows a circular pattern on the sky, once every 26,000 years. It will be closest to Polaris ~ A.D. 2100. There is nothing peculiar about Polaris at all (neither particularly bright nor nearby etc.) ~ 12,000 years from now, it will be close to Vega in the constellation Lyra.
57. The Sun and Its Motions Earth’s rotation is causing the day/night cycle.
58.
59. The Ecliptic The Sun’s apparent path on the sky is called the Ecliptic . Equivalent: The Ecliptic is the projection of Earth’s orbit onto the celestial sphere. Due to Earth’s revolution around the sun, the sun appears to move through the zodiacal constellations. Sun travels 360 o /365.25 days ~ 1 o /day
60. The Seasons Earth’s axis of rotation is inclined vs. the normal to its orbital plane by 23.5 ° , which causes the seasons .
65. The ecliptic and celestial equator intersect at two points: the vernal (spring) equinox and autumnal (fall) equinox . The Sun crosses the celestial equator moving northward at the vernal equinox around March 21 and crosses the celestial equator moving southward at the autumnal equinox around September 22. When the Sun is on the celestial equator at the equinoxes, everybody on the Earth experiences 12 hours of daylight and 12 hours of night for those two days (hence, the name ``equinox'' for ``equal night''). The day of the vernal equinox marks the beginning of the three-month season of spring on our calendar and the day of the autumn equinox marks the beginning of the season of autumn (fall) on our calendar. On those two days of the year, the Sun will rise in the exact east direction, follow an arc right along the celestial equator and set in the exact west direction.
67. Since the ecliptic is tilted 23.5 degrees with respect to the celestial equator, the Sun's maximum angular distance from the celestial equator is 23.5 degrees. This happens at the solstices. For observers in the northern hemisphere, the farthest northern point above the celestial equator is the summer solstice , and the farthest southern point is the winter solstice . The word ``solstice'' means ``sun standing still'' because the Sun stops moving northward or southward at those points on the ecliptic. The Sun reaches winter solstice around December 21 and you see the least part of its diurnal path all year---this is the day of the least amount of daylight and marks the beginning of the season of winter for the northern hemisphere. On that day the Sun rises at its furthest south position in the southeast, follows its lowest arc south of the celestial equator, and sets at its furthest south position in the southwest. The Sun reaches the summer solstice around June 21 and you see the greatest part of its diurnal path above the horizon all year---this is the day of the most amount of daylight and marks the beginning of the season of summer for the northern hemisphere. On that day the Sun rises at its furthest north position in the northeast, follows its highest arc north of the celestial equator, and sets at its furthest north position in the northwest.
77. As a result, the flux of solar radiation received by the Earth oscillates with different periodicities and amplitudes This triggers changes in climate Our Earth makes a complicated motion through space , like a crazy spaceship
78. f1 f2 f3 Adding oscillations with different phases and incommensurate frequencies f1 = sin[2 t + 1] f2 = 0.7 sin[3.1 t + 2.4] f3 = 1.3 sin[4.5 t + 0.3] f1+f2 f1+f2+f3
79. Adding Milankovitch cycles of solar irradiation for 65 degree North latitude (Berger 1991) Note the last peak 9,000 years ago when the last large ice sheet melted
81. Are these effects enough to explain the Ice Ages??? Other factors? Volcanic winters, impacts, … 71,000 yr ago: eruption of Mount Toba (Sumatra) 2,800 km 3 of material thrown in the atmosphere Instant ice age? Meteorite impacts; Mass extinctions
82. 150 known impact sites on Earth Diameters from 50-70 m to 200 km
83. Barringer crater, Arizona 49,000 yr old Iron meteorite of size 50 m, mass 300,000 ton Impact velocity 11 km/sec
84. 65 million years ago a huge meteorite of 10 km size hit the Earth
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88. Our Moon could have been formed in a giant collision 4.5 billion years ago