The Sun is a middle-aged, average sized yellow star that is made up mostly of hydrogen and helium. It is about 4.6 billion years old and located 93 million miles from Earth. The Sun generates heat and light through nuclear fusion reactions in its core that convert hydrogen into helium. It is the center of our Solar System and contains over 99% of the mass in the entire system. The Solar System also includes eight official planets that orbit the Sun, along with dwarf planets, moons, asteroids, comets, and other small bodies.
The solar system is made up of the Sun, the planets that orbit the Sun, their satellites, dwarf planets and many, many small objects, like asteroids and comets. All of these objects move and we can see these movements. We notice the Sun rises in the eastern sky in the morning and sets in the western sky in the evening. We observe different stars in the sky at different times of the year.
The solar system is made up of the Sun, the planets that orbit the Sun, their satellites, dwarf planets and many, many small objects, like asteroids and comets. All of these objects move and we can see these movements. We notice the Sun rises in the eastern sky in the morning and sets in the western sky in the evening. We observe different stars in the sky at different times of the year.
The Solar System slideshow gives solid yet general notes on our solar system. It defines geocentric and heliocentric models and explains why the planets orbit the sun. It tells where our solar system is within the universe. It gives a general overview of each planet denoting the differences of inner planets and outer planets. It is an excellent introduction to any solar system unit.
To download the pdf file or download the guided notes to accompany this slideshow, visit this post. https://thehomeschooldaily.com/free-solar-system-unit/
Thanks for looking!
Acetabularia Information For Class 9 .docxvaibhavrinwa19
Acetabularia acetabulum is a single-celled green alga that in its vegetative state is morphologically differentiated into a basal rhizoid and an axially elongated stalk, which bears whorls of branching hairs. The single diploid nucleus resides in the rhizoid.
Palestine last event orientationfvgnh .pptxRaedMohamed3
An EFL lesson about the current events in Palestine. It is intended to be for intermediate students who wish to increase their listening skills through a short lesson in power point.
Read| The latest issue of The Challenger is here! We are thrilled to announce that our school paper has qualified for the NATIONAL SCHOOLS PRESS CONFERENCE (NSPC) 2024. Thank you for your unwavering support and trust. Dive into the stories that made us stand out!
Francesca Gottschalk - How can education support child empowerment.pptxEduSkills OECD
Francesca Gottschalk from the OECD’s Centre for Educational Research and Innovation presents at the Ask an Expert Webinar: How can education support child empowerment?
The Roman Empire A Historical Colossus.pdfkaushalkr1407
The Roman Empire, a vast and enduring power, stands as one of history's most remarkable civilizations, leaving an indelible imprint on the world. It emerged from the Roman Republic, transitioning into an imperial powerhouse under the leadership of Augustus Caesar in 27 BCE. This transformation marked the beginning of an era defined by unprecedented territorial expansion, architectural marvels, and profound cultural influence.
The empire's roots lie in the city of Rome, founded, according to legend, by Romulus in 753 BCE. Over centuries, Rome evolved from a small settlement to a formidable republic, characterized by a complex political system with elected officials and checks on power. However, internal strife, class conflicts, and military ambitions paved the way for the end of the Republic. Julius Caesar’s dictatorship and subsequent assassination in 44 BCE created a power vacuum, leading to a civil war. Octavian, later Augustus, emerged victorious, heralding the Roman Empire’s birth.
Under Augustus, the empire experienced the Pax Romana, a 200-year period of relative peace and stability. Augustus reformed the military, established efficient administrative systems, and initiated grand construction projects. The empire's borders expanded, encompassing territories from Britain to Egypt and from Spain to the Euphrates. Roman legions, renowned for their discipline and engineering prowess, secured and maintained these vast territories, building roads, fortifications, and cities that facilitated control and integration.
The Roman Empire’s society was hierarchical, with a rigid class system. At the top were the patricians, wealthy elites who held significant political power. Below them were the plebeians, free citizens with limited political influence, and the vast numbers of slaves who formed the backbone of the economy. The family unit was central, governed by the paterfamilias, the male head who held absolute authority.
Culturally, the Romans were eclectic, absorbing and adapting elements from the civilizations they encountered, particularly the Greeks. Roman art, literature, and philosophy reflected this synthesis, creating a rich cultural tapestry. Latin, the Roman language, became the lingua franca of the Western world, influencing numerous modern languages.
Roman architecture and engineering achievements were monumental. They perfected the arch, vault, and dome, constructing enduring structures like the Colosseum, Pantheon, and aqueducts. These engineering marvels not only showcased Roman ingenuity but also served practical purposes, from public entertainment to water supply.
Macroeconomics- Movie Location
This will be used as part of your Personal Professional Portfolio once graded.
Objective:
Prepare a presentation or a paper using research, basic comparative analysis, data organization and application of economic information. You will make an informed assessment of an economic climate outside of the United States to accomplish an entertainment industry objective.
Synthetic Fiber Construction in lab .pptxPavel ( NSTU)
Synthetic fiber production is a fascinating and complex field that blends chemistry, engineering, and environmental science. By understanding these aspects, students can gain a comprehensive view of synthetic fiber production, its impact on society and the environment, and the potential for future innovations. Synthetic fibers play a crucial role in modern society, impacting various aspects of daily life, industry, and the environment. ynthetic fibers are integral to modern life, offering a range of benefits from cost-effectiveness and versatility to innovative applications and performance characteristics. While they pose environmental challenges, ongoing research and development aim to create more sustainable and eco-friendly alternatives. Understanding the importance of synthetic fibers helps in appreciating their role in the economy, industry, and daily life, while also emphasizing the need for sustainable practices and innovation.
4. Our Sun
–A middle-aged, average
sized, Yellow star
–Made of mostly Hydrogen
& Helium
–99.8% of the mass in our
Solar System
–4.6 billion years old
–93 million miles from the
Earth
5. Our Sun
• A giant sphere of hot glowing
gas, called plasma
• Shines because it is hot:
– Surface Temp ~5500 C
– Mostly Visible, UV & IR light
• Kept hot by nuclear fusion in
its core:
– Builds Helium from Hydrogen
fusion.
– Will shine for ~12 billion years
6. Sunspots
• Dark areas on the Sun’s surface.
• cooler than the surrounding area
• The number of sunspots and location are
changing in a regular, 11 year cycle.
7. Solar flaresSolar flares
Powerful erruptions of
particles that shoot into
space
Powerful erruptions of
particles that shoot into
space
The erupting particles
strengthen the solar wind,
which is made of fast-
moving gases that travel
through space.
The erupting particles
strengthen the solar wind,
which is made of fast-
moving gases that travel
through space.
8. Solar WindSolar Wind
Fast moving gases that can travel in spaceFast moving gases that can travel in space
9. Solar Winds cause AurorasSolar Winds cause Auroras
The solar wind can
disrupt radio waves and
cause auroras.
The solar wind can
disrupt radio waves and
cause auroras.
Aurora seen
from space
11. Energy from the SunEnergy from the Sun
4 hydrogen nuclei fuse to form 1 helium nucleus4 hydrogen nuclei fuse to form 1 helium nucleus
Huge energy
release
12. Nuclear Fusion
In the early 1900’s, Albert Einstein discovered that matter
and energy are interchangeable.
Matter can be converted to energy as demonstrated by
E = mc2
Where E is energy, m is mass and c is the speed of light.
13. Energy from the SunEnergy from the Sun
Uneven heating
affects weather
Uneven heating
affects weather
Powers the
water cycle
14. Energy from the SunEnergy from the Sun
Uneven heating
causes winds
Uneven heating
causes winds
Provides energy
for living things
producers
15. Life Cycle of StarsLife Cycle of Stars
A star forms
from rotating
clouds and dust
called a
nebula
11
16. Life Cycle of StarsLife Cycle of Stars
Gravity and
other forces
cause the nebula
to collapse.
Clouds begin to
glow as the
temperature
rises forming a
Protostar
22
17. HL Tauri — a star system that is
just being born.
The proto-planetary disk
surrounding a young star 450 light-
years away. The concentric rings
cutting through the glowing gas
and dust are tracks etched out by
planets being spawned inside the
disk.
baby planets forming around a star -
18. Life Cycle of StarsLife Cycle of Stars
When gas
pressure inside
the star equals
gravity, the star
becomes stable
and forms a
Main-
sequence
Star
33
Nuclear fusion begins when
the temperature reaches 10 million C
19. Life Cycle of StarsLife Cycle of Stars
The outer part
of the star
expands over
time, while the
core contracts
forming a
Red Giant
44
Red giants are very bright,
but cooler star.
Very large red giant stars
are known as Super Giants.
Very large red giant stars
are known as Super Giants.
20. Life Cycle of StarsLife Cycle of Stars
The outer
layers of the
star are
released
forming a
Planetary
Nebula
55
21. Life Cycle of StarsLife Cycle of Stars
66
Over time the
star shrinks
forming a
White
Dwarf
22. Life Cycle of StarsLife Cycle of Stars
Out of nuclear
fuel, the star
eventually
fades into a
Black
Dwarf
77
24. Alternate Life Cycle of Huge StarsAlternate Life Cycle of Huge Stars
44
Very large red giants stars are known as Super GiantsVery large red giants stars are known as Super Giants
25. Alternate Life Cycle of Huge StarsAlternate Life Cycle of Huge Stars
5
And
6
5
And
6
A Supernova is an explosion of a star accompanied by
emission of radiation and light.
A Supernova is an explosion of a star accompanied by
emission of radiation and light.
26. Alternate Life Cycle of Huge StarsAlternate Life Cycle of Huge Stars
77
Both cycles end with a Black DwarfBoth cycles end with a Black Dwarf
27. Astronomy – the study of planets, our moon, stars
(including our sun) and the universe.
Constellation – a group of stars that forms a pattern
Star chart – a map of the night sky
36. Terrestrial Planets
• Mercury, Venus, Earth & Mars
– “Earth-Like” Rocky Planets
– Largest is Earth
– Only in the inner solar system
• Rocky Planets:
– Solid Surfaces
– Mostly Silicates and Iron
– High Density: (rock & metal)
– Earth, Venus, & Mars have atmospheres
38. The Jovian Planets
• Jupiter, Saturn, Uranus & Neptune
– Largest Planets: at least 15 times mass of Earth.
– Only in the outer solar system (5 to 30 AU)
– No solid surfaces (mostly atmosphere)
– Low density
• Gas Giants: (Jupiter & Saturn)
– Thick H/He atmosphere, liquid hydrogen mantle, ice core
• Ice Giants: (Uranus & Neptune)
– Ice/rock core & mantle, thin H/He atmosphere
41. Dwarf Planets
• Defined by the IAU in 2006
• Dwarf Planets:
– Ceres: first of the Asteroids, discovered in 1801
– Pluto: trans-Neptunian object discovered in
1930
– Eris: trans-Neptunian object discovered in 2005
– Haumea (trans-Neptunian, suspected)
– Makemake (trans-Neptunian, suspected)
43. The Giant Moons
• Moon: any natural satellite orbiting a planet or
dwarf planet
• Giant Moons:
– Earth: The Moon (Luna)
– Jupiter: Io, Europa, Ganymede, & Callisto
– Saturn: Titan – has an atmosphere
– Neptune: Triton – has an atmosphere
• Many smaller moons, both rocky & icy.
• Only Mercury & Venus have no moons.
44. The Giant Moons
• Moon: any natural satellite orbiting a planet or
dwarf planet
• Giant Moons:
– Earth: The Moon (Luna)
– Jupiter: Io, Europa, Ganymede, & Callisto
– Saturn: Titan – has an atmosphere
– Neptune: Triton – has an atmosphere
• Many smaller moons, both rocky & icy.
• Only Mercury & Venus have no moons.
47. Kuiper Belt
• Class of icy bodies orbiting beyond Neptune.
– Found only in the outer Solar System (>30AU)
– Astronomical Units, AU. One AU is the average
distance between the Earth and the Sun, 93 million
miles, or 150 million kilometres.
• Examples:
– Pluto & Eris (icy dwarf planets)
– Kuiper Belt Objects (30-50AU)
– Charon, Pluto’s large moon
– Sedna & Quaor: distant large icy bodies
49. Oort Cloud
• Spherical cloud of comets.
– Extends out to almost 50,000 AU (1 light-year)
– May contain trillions of comets
– The outer edge is the farthest reach of the Sun’s
gravitational pull.
– There are no confirmed observations – its
existence is theoretical only.
51. The Leftovers (small bodies)
• Asteroids:
– Made of rock & metal (density 2-3 g/cc)
– Sizes: Few 100km to large boulders
– Most are found in the Main Belt (2.1-3.2 AU)
• Meteoroids:
– Bits of rock and metal
– Sizes: grains of sand to boulders
• Comets:
– Composite rock & ice “dirty snowballs”
– Longs tails of gas & dust are swept off them when
they pass near the Sun.
56. Is Pluto a Planet?
What to consider?
• Size?
• Shape?
• Orbit?
• What is it made
of?
57. IAU Definition of a Planet
In 2006, the International Astronomical Union
(IAU) came up with the following definition of
a planet:
orbits the Sun
has sufficient mass for its self-gravity to overcome
rigid body forces so that it assumes a hydrostatic
equilibrium shape (i.e., it is spherical),
has cleared the neighborhood around its orbit,
is not a satellite
58. IAU Definition of a Dwarf Planet
In 2006, the International Astronomical Union
(IAU) came up with the following definition of
a dwarf planet:
orbits the Sun
has sufficient mass for its self-gravity to overcome
rigid body forces so that it assumes a hydrostatic
equilibrium shape (i.e., it is spherical),
has not cleared the neighborhood around its orbit,
is not a satellite
Editor's Notes
The circulation of gases within the sun produces magnetic fields that reach out into space.
The magnetic fields slow down activity in the convective zone.
This causes areas of the photosphere to be cooler than others.
Welcome to HL Tauri — a star system that is just being born and the target of one of the most mind-blowing astronomical observations ever made.
Observed by the powerful Atacama Large Millimeter/submillimeter Array (ALMA) in Chile, this is the most detailed view of the proto-planetary disk surrounding a young star 450 light-years away. And those concentric rings cutting through the glowing gas and dust? Those, my friends, are tracks etched out by planets being spawned inside the disk.
When gas pressure inside the star equals gravity, the star attains a stable state and begins entering the main sequence phase. It attains a temperature of about 15,000,000 °C. Nuclear fusion occurs and it begins to glow.
Read more at Buzzle: http://www.buzzle.com/articles/life-cycle-of-a-star.html
When gas pressure inside the star equals gravity, the star attains a stable state and begins entering the main sequence phase. It attains a temperature of about 15,000,000 °C. Nuclear fusion occurs and it begins to glow.
Read more at Buzzle: http://www.buzzle.com/articles/life-cycle-of-a-star.html
When gas pressure inside the star equals gravity, the star attains a stable state and begins entering the main sequence phase. It attains a temperature of about 15,000,000 °C. Nuclear fusion occurs and it begins to glow.
Read more at Buzzle: http://www.buzzle.com/articles/life-cycle-of-a-star.html
When gas pressure inside the star equals gravity, the star attains a stable state and begins entering the main sequence phase. It attains a temperature of about 15,000,000 °C. Nuclear fusion occurs and it begins to glow.
Read more at Buzzle: http://www.buzzle.com/articles/life-cycle-of-a-star.html
When gas pressure inside the star equals gravity, the star attains a stable state and begins entering the main sequence phase. It attains a temperature of about 15,000,000 °C. Nuclear fusion occurs and it begins to glow.
Read more at Buzzle: http://www.buzzle.com/articles/life-cycle-of-a-star.html
When gas pressure inside the star equals gravity, the star attains a stable state and begins entering the main sequence phase. It attains a temperature of about 15,000,000 °C. Nuclear fusion occurs and it begins to glow.
Read more at Buzzle: http://www.buzzle.com/articles/life-cycle-of-a-star.html
When gas pressure inside the star equals gravity, the star attains a stable state and begins entering the main sequence phase. It attains a temperature of about 15,000,000 °C. Nuclear fusion occurs and it begins to glow.
Read more at Buzzle: http://www.buzzle.com/articles/life-cycle-of-a-star.html
When gas pressure inside the star equals gravity, the star attains a stable state and begins entering the main sequence phase. It attains a temperature of about 15,000,000 °C. Nuclear fusion occurs and it begins to glow.
Read more at Buzzle: http://www.buzzle.com/articles/life-cycle-of-a-star.html
When gas pressure inside the star equals gravity, the star attains a stable state and begins entering the main sequence phase. It attains a temperature of about 15,000,000 °C. Nuclear fusion occurs and it begins to glow.
Read more at Buzzle: http://www.buzzle.com/articles/life-cycle-of-a-star.html