Download Warm- up Question Tell me what you know about The Big Bang

Essential Questions
1. I will be able to write an explain how
the sun converts matter into energy in
its core
2. I will be able to compare the radiative
and convective zones of the sun
3. When ask I will be able to describe
the 3 layers of the sun’s atmosphere
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describe how the planets developed
Vocabulary Chapter 28 section 1 & 2
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Radiative zone
Convective zone
Photosphere
Chromosphere
Corona
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Sunspots
Sunspot cycle
Prominences
Solar flare
Auroras
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Homework
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Vocabulary chapter 28, define and draw or
give meaning – due Friday
Read pages 571 – 575 answer review
questions on page 575 – due Wednesday
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Chapter 28.1 Objectives
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Explain how the sun converts matter into
energy in its core
Compare the Radiative and convection
zones of the sun
Describe the three layers of the sun’s
atmosphere
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Chapter 28 Standards
Astronomy and planetary exploration
reveal the solar system’s structure, scale,
and change over time.
1.
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Students know the Sun is a typical star and is
powered by nuclear reactions, primarily the
fusion of hydrogen to form helium
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Chapter 28.1 Notes
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Structure
of the sun
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Until recently most people thought
the sun energy was fire.
We now use spectroscopic analysis
of the sun’s rays
Have studied the inner layers of the
sun; the core, the inner zones and
the atmosphere
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Chapter 28.1 Notes
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The core
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The core is 15,000,000C and is
10% of the sun’s diameter of
1,300,000 km
Has 300,000 times our mass and
therefore more gravity
There is enough pressure in the
core to strip electrons from atoms
This creates plasma and allows
nuclear fusion to take place
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Chapter 28.1 Notes
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Hydrogen
Fusion
1.
2.
3.
4.
5.
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Two protons collide and fuse
One changes into a neutron
Another proton collide and fuse
with the neutron and proton
This collides with another nuclei of
the same
Two protons thrown off
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Chapter 28.1 Notes
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Mass
into
energy
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Einstein proposed that a small
amount of matter can create a large
amount of energy
E=mc2 is the theory of relativity that
show how much energy is created
from matter
The sun coverts 600 million tons of
Hydrogen a second
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Chapter 28.1 Notes
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The inner
zones
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The core 15,000,000C
 Radiative zone surrounds core
2,500,000C
 Convection zone
1,000,000C
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Chapter 28.1 Notes
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The Sun’s
Atmosphere
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Upper three layers of sun after
convection zone
Photosphere or light – energy
bubbles up here as light so we call
it the surface, 6,000C
The Chromosphere is a reddish
zone that seems to form jets off the
photosphere
Corona is the outer layer that
prevents energy loss
describe how the planets developed
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describe how the planets developed
Essential Questions
Explain how sunspots are related to
powerful magnetic fields on the sun
2. Compare prominences and solar flares
3. Describe how the solar wind can cause
auroras on the earth
When asked student should be able to
explain in writing or orally.
1.
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Chapter 28.2 Notes
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Solar
Activity
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Gravity and Fusion cause solar
materials to constantly rise and fall
Gas also moves because of the
solar rotation
The equator rotates in 25.3 days
The poles in 33 days
Average is 27 days
describe how the planets developed
Chapter 28.2 Notes
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Sun
Spots
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The up and down movement of the
gases cause strong magnetic fields
These magnetic fields cause the
convection currents to slow
Less material is raised to the
photosphere – cool spots form
3,000C
The sunspot cycle is a 11 year
period – most form at the equator –
last low was 2008
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Sunspots
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Chapter 28.2 Notes
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Prominences
and solar
flares
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The magnetic fields cause large
clouds of hot gas to arch high
above the sun’s surface
The arch follows the magnetic field
lines; can last a few days to a year
Solar flares a violent eruptions of
gas; can last several hours
Flares thrown into space; cause
magnetic storms on earth that can
effect radio communication
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Chapter 28.2 Notes
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Auroras
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Caused by magnetic storms from
the sun
Charged particles move along
earths magnetic fields and strike
gases in the atmosphere
The are 100km to 1,000km above
the surface
Sometimes called the northern or
southern lights
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Solar Wind Interaction with
Magnetosphere
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Essential Questions
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Explain the Nebular Theory of the origin of
the solar system
Describe how the planets developed
Describe the formation of the land, the
atmosphere, and the oceans of the earth
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Vocabulary Chapter 28 section 3
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Solar system
Planets
Nebular theory
Solar nebula
Planetesimals
Protoplanets
Moons
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Chapter 28.3 Notes – nebular theory
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Formation of the Sun & Planets
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Nebular Theory
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PlanetesimalsProtoplanets
Solar Nebula
5 Billion years ago…..
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Explosion of nearby supernova caused nebula to condense
and spin – SOLAR NEBULA
Planetesimals combined to form PROTOPLANETS – “preplanets”
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Origin of Elements
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Hydrogen & Helium
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Lithium  Iron
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found in nebulae
formed in core of stars
from fusion
Nickel  Plutonium
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formed during explosion
of supernovae and recondense in new nebula
Is the Earth an “Original
Planet?” Why?
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Origin of Elements
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Periodic Table of Elements
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Lecture 28.3 - Formation of the Earth
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3 Main sources of Residual HEAT
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Primordial Heat
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Left over heat from formation of Earth
Compression of outer layers
Radioactive Material in Core
3 Main Layers
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Dense Core of Nickel & Iron
Mantle
Crust of less dense materials
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Lecture 28.3 - Formation of the Earth
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The Solid Earth
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The Atmosphere
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Core-Mantle-Crust
Volcanic Outgassing of Oxygen & Carbon Dioxide
Reducing to Oxidizing Atmosphere through Cyanobacteria
production of Oxygen
The Oceans
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Rain formed oceans 3.5 Billion years ago
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The Atmosphere
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Original (FIRST) Atmosphere probably lost to solar winds
Present Atmosphere results from Outgassing
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Hydrogen & Helium abundant in Solar Nebula – where did water come
from?
Volcanic eruptions released MASSIVE amounts of carbon dioxide &
water
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Early Atmosphere
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Reducing  Oxidizing Atmosphere
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Sunlight caused Ammonia and water to form
NITROGEN GAS
Cyanobacteria & photosynthetic plants converted
nitrogen to energy making OXYGEN WASTE
PRODUCT
Oxygen reacted with sunlight to form OZONE –
PROTECTIVE LAYER
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With more ozone, life was able to thrive
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The Oceans
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3 to 3.5 BILLION years ago, the Earth
cooled enough to allow water to form from
steam
Rain fell and oceans formed in lower areas
Today’s atmosphere has been constant for
last 1.5 Billion years
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