1.1b classification of galaxies
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The document discusses the classification of galaxies into three main types: irregular galaxies, spiral galaxies, and elliptical galaxies. Irregular galaxies have no symmetrical structure and contain young stars and gas. Spiral galaxies have a central bulge, spiral disk, and halo, with the disk containing younger stars and arms. Elliptical galaxies are elongated spheres that decrease in brightness outward and have no axis of rotation.
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1.1b classification of galaxies
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Galaxies
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There are different types of galaxies including elliptical galaxies, spiral galaxies, and irregular galaxies. Elliptical galaxies do not have ongoing star formation while spiral galaxies do. Irregular galaxies do not fit into a defined shape category. The formation of galaxies is influenced by density - denser regions collapse first under gravity to form protogalaxies that then separate into cores and halos, with flatter structures forming when densities were highest.
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Materials RequiredComputer and internet accessCalcula.docx
Materials Required:
Computer and internet access
Calculator
Ruler
Pencils and pens, eraser
Digital camera and/or scanner
Print out
Galaxy Image
Prints document
Total Time Required:
Approximately 2-3 Hours
Part 1. The Local Group
In Table 1, you will find a list of most of the galaxies in the Local Group. This group is made up of our own galaxy, the Milky Way, and its closest neighbors. (Note: 1 kpc = 1 kiloparsec = 1000 parsec; 1 parsec = 3.26 light years)
Table 1. Galaxies of the Local Group
Name
Distance (kpc)
Diameter (kpc)
Name
Distance (kpc)
Diameter (kpc)
Milky Way
-
40.0
IC 1522
610
1.5
Sculptor
60
0.3
WLM
610
2.1
Large Magellanic Cloud (LMC)
60
6.1
Andromeda I
675
0.6
Carina
90
0.2
Andromeda II
675
0.6
Draco
90
0.2
Andromeda III
675
0.9
Ursa Minor
90
0.3
M32
675
1.5
Sextans I
90
0.9
NGC 185
675
1.8
Small Magellanic Cloud (SMC)
90
4.6
NGC 147
675
3.1
Fornax
150
0.9
NGC 205
675
3.1
Leo II
185
0.2
M31 (Andromeda Galaxy)
675
61
Leo I
185
0.3
IC 1613
765
3.7
NGC 6822
520
2.5
M33 (Triangulum Galaxy)
765
14.0
DDO 210
920
1.2
Below is a visual representation of our Local Group of galaxies. You can access and zoom into this image to see galaxies more clearly using this link
Local Group
.
Figure 1.
Local Group Visualization.
Type and label your answers to the below questions in your lab report.
Using Table 1 above and noting the diameters of the galaxies, which
five
galaxies in the Local Group are the largest? In a few sentences, compare the sizes of the other galaxies in the Local Group to the two largest ones.
Which
three
galaxies have the largest angular size (not including the Milky Way)? These galaxies are the ones that look the largest in the sky. Explain how you get your answer.
By hand and with pencil, create a
scale drawing
of the Milky Way and the Large Magellanic Cloud, showing their
relative sizes
and the
distance
between them in kiloparsecs (the galaxies can be represented by circles).
Write down the scale you use ,
and your calculations to find the scaled-down sizes and distance. (An example of a good scale to use would like something like: 5 mm = 10 kpc, also see this site
Basic-Mathematics.com
for more information on scaling.) You will photo your drawing and insert it into your lab report.
Figure 2.
Local Supercluster Print
Image courtesy of Palomar Sky Survey Photographs
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Materials RequiredComputer and internet accessCalcula.docx
Materials Required:
Computer and internet access
Calculator
Ruler
Pencils and pens, eraser
Digital camera and/or scanner
Print out
Galaxy Image
Prints document
Total Time Required:
Approximately 2-3 Hours
Part 1. The Local Group
In Table 1, you will find a list of most of the galaxies in the Local Group. This group is made up of our own galaxy, the Milky Way, and its closest neighbors. (Note: 1 kpc = 1 kiloparsec = 1000 parsec; 1 parsec = 3.26 light years)
Table 1. Galaxies of the Local Group
Name
Distance (kpc)
Diameter (kpc)
Name
Distance (kpc)
Diameter (kpc)
Milky Way
-
40.0
IC 1522
610
1.5
Sculptor
60
0.3
WLM
610
2.1
Large Magellanic Cloud (LMC)
60
6.1
Andromeda I
675
0.6
Carina
90
0.2
Andromeda II
675
0.6
Draco
90
0.2
Andromeda III
675
0.9
Ursa Minor
90
0.3
M32
675
1.5
Sextans I
90
0.9
NGC 185
675
1.8
Small Magellanic Cloud (SMC)
90
4.6
NGC 147
675
3.1
Fornax
150
0.9
NGC 205
675
3.1
Leo II
185
0.2
M31 (Andromeda Galaxy)
675
61
Leo I
185
0.3
IC 1613
765
3.7
NGC 6822
520
2.5
M33 (Triangulum Galaxy)
765
14.0
DDO 210
920
1.2
Below is a visual representation of our Local Group of galaxies. You can access and zoom into this image to see galaxies more clearly using this link
Local Group
.
Figure 1.
Local Group Visualization.
Type and label your answers to the below questions in your lab report.
Using Table 1 above and noting the diameters of the galaxies, which
five
galaxies in the Local Group are the largest? In a few sentences, compare the sizes of the other galaxies in the Local Group to the two largest ones.
Which
three
galaxies have the largest angular size (not including the Milky Way)? These galaxies are the ones that look the largest in the sky. Explain how you get your answer.
By hand and with pencil, create a
scale drawing
of the Milky Way and the Large Magellanic Cloud, showing their
relative sizes
and the
distance
between them in kiloparsecs (the galaxies can be represented by circles).
Write down the scale you use ,
and your calculations to find the scaled-down sizes and distance. (An example of a good scale to use would like something like: 5 mm = 10 kpc, also see this site
Basic-Mathematics.com
for more information on scaling.) You will photo your drawing and insert it into your lab report.
Figure 2.
Local Supercluster Print
Image courtesy of Palomar Sky Survey Photographs
As you have already seen, galaxies can vary a lot in size. Now, we will look at how their shapes are different. Two basic types of galaxies are the spiral galaxies and the elliptical galaxies. Spiral galaxies have a disk-like structure,and a central bulge. Our own Milky Way is a spiral galaxy. Elliptical galaxies appear round, looking a lot like a football .
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Materials RequiredComputer and internet accessCalcula.docx
Materials RequiredComputer and internet accessCalcula.docx
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2. Compaction and lithification - Under great pressure from overlying layers of sediment, loose particles are compressed into a solid mass. Their original structures may still be visible in the solidified rock. Over geologic time and increased pressure and cementation, the sediment lithifies and hardens into sedimentary rock.
2.1i earth's interior and plate tectonics review and enrichment lesson
This document provides information on plate tectonics including different types of plate boundaries and movements. It includes 3 video clips on plate tectonics, convergent boundaries, and transform boundaries. The text then defines key terms like lithosphere, asthenosphere, and magma and describes the three main types of plate boundaries: divergent where plates move apart, convergent where they move together, and transform where they scrape past one another.
2.1e asthenosphere and plate tectonics final printing of research
The document provides instructions for a PowerPoint presentation on asthenosphere and plate tectonics, asking the presenter to show their presentation, revise it if needed, print it, lay the slides out on poster paper, and hang the finished posters on the wall.
2.1d asthenosphere and plate tectonics research
The asthenosphere is the weak, hot, ductile layer of the upper mantle that lies below the lithosphere. Convection currents in the asthenosphere are driven by heat from the Earth's core and mantle, which causes the asthenosphere to slowly flow outward. Plate tectonics refers to the movement and interactions of the Earth's tectonic plates, which are driven by convection currents in the asthenosphere. Continental plates are less dense pieces of the Earth's crust that sit atop the asthenosphere and move slowly over time as the asthenosphere flows.
2.1c layers of the earth
The Earth is composed of four main layers from outermost to innermost:
1) The crust, which is the top solid rocky layer ranging from 5-70km thick.
2) The mantle, which makes up over 80% of the Earth's volume and is divided into the upper, middle, and lower mantle.
3) The outer core, which is liquid due to extreme heat and composed of nickel and iron.
4) The inner core, the hottest layer that is solid due to immense pressure from the layers above.
2.1b earth's interior and plate tectonics
The document summarizes the structure of the Earth and plate tectonics. It describes how the Earth initially formed as a molten ball that separated into layers over time, with denser materials like iron and nickel sinking to form the core. Less dense materials rose to form the crust. The crust and rigid upper mantle make up the lithosphere plates, which move atop the slowly flowing asthenosphere. Heat causes the asthenosphere to expand and push plates, resulting in their movement at boundaries in divergent or convergent patterns.
1.2e the sun and stars
This document defines key terms related to stars and their life cycles. It describes the evolution of massive stars from red giants to supergiants and their explosive deaths as supernovae, leaving behind neutron stars or black holes. Lower mass stars end as white dwarfs. The document also defines terms like photosphere, chromosphere, sunspots, and features of the Sun like coronal streamers, holes, and filaments.
1.2c nuclear fusion in stars
1) Nuclear fusion occurs inside the core of stars where extreme pressure and heat cause hydrogen atoms to fuse together, forming helium and releasing energy.
2) The temperature in a star's core is over 15 million kelvins and the density is over 150 times greater than water, creating the conditions for nuclear fusion.
3) During nuclear fusion, the nuclei of hydrogen atoms combine to form helium, releasing a large amount of energy in the process. This energy flows outward from the core, balancing the inward force of gravity in the star.
1.2a what are stars
Ancient Greeks thought stars were fixed to a celestial sphere and did not realize they were other suns. This view was incorrect because stars are actually enormous balls of hot, glowing gases that are extremely far away from Earth. A constellation is a recognizable pattern of stars in the night sky that forms an imaginary outline or picture and has been given a name, such as Orion or Ursa Major.
1.2a what are stars
Ancient Greeks thought stars were fixed to a celestial sphere and did not realize they were other suns. This view was incorrect because stars are actually enormous balls of hot, glowing gases that are extremely far away from Earth. A constellation is a recognizable pattern of stars in the night sky that forms an imaginary outline or picture and has been given a name, such as Orion or Ursa Major.
1.1f the origin and fate of the universe
The document discusses the origin and fate of the universe. It provides a timeline of cosmic events from the formation of hydrogen and helium nuclei shortly after the Big Bang to the formation of our solar system around 4.6 billion years ago. It also explains that the ultimate fate of the universe, whether it expands forever or contracts back into a "big crunch", depends on the total mass of the universe and its interaction with gravitational forces.
1.1e the origin of the universe - further investigation of the big bang theory
The document provides instructions for a classroom activity on the Big Bang Theory. Students are asked to complete a Frayer Model in their notebook about the Big Bang Theory, showing at least 4 ideas about it. They are also asked to give 4 things that were happening after the Big Bang, provide 4 proofs that the Big Bang really happened, and tell 3 new things they learned from the activity. The teacher emphasizes no excuses, just results, and reminds students to show up, engage, and produce meaningful work.
1.1e the origin of the universe - further investigation of the big bang theory
The Big Bang Theory proposes that the universe began approximately 13.8 billion years ago from the violent expansion of space and time starting from an extremely dense and hot state called a singularity. As the universe expanded and cooled, the first simple atomic elements like hydrogen and helium formed. Over millions of years, gravity caused matter to accumulate into dense clouds that collapsed and formed the first stars and galaxies. The early universe was dominated by hydrogen and helium, with heavier elements forming later in dying stars.
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2.2c convection currents drive the tectonics movement that drives vocanic ac...
2.2c convection currents drive the tectonics movement that drives vocanic ac...
2.1i earth's interior and plate tectonics review and enrichment lesson
2.1i earth's interior and plate tectonics review and enrichment lesson
2.1e asthenosphere and plate tectonics final printing of research
2.1e asthenosphere and plate tectonics final printing of research
1.1e the origin of the universe - further investigation of the big bang theory
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Cosa hanno in comune un mattoncino Lego e la backdoor XZ?
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みなさんこんにちはこれ何文字まで入るの？40文字以下不可とか本当に意味わからないけどこれ限界文字数書いてないからマジでやばい文字数いけるんじゃないの？えこ...
ここ3000字までしか入らないけどタイトルの方がたくさん文字入ると思います。
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1.1b classification of galaxies
- 1. Classification of Galaxies Chapter 16.1b No Excuses, Just Results! Show-up, Engage & Produce
- 2. ACHIEVE Activity – Direct Instruction Conversation – Voice Level 2. Limit to topic. Help – Raise hand until recognized. Integrity – If you go behind in note taking, raise your hand and ask for a “repeat or slow down.” Effort – Sit up eyes on screen, handout, or your notes. Write notes about material presented. Value – Presentation will help you more fully understand Galaxy Classificaton. Efficiency – Glue handouts and notes in notebook for easy access. No Excuses, Just Results! Show-up, Engage & Produce
- 3. Expectation Write down things on your notebook starting from the next available space. Poster is due today. If you need to review, visit my fusion page. Homework for today is in fusion page. Additional Resources are found in my fusion page. No Excuses, Just Results! Show-up, Engage & Produce
- 4. Irregular Galaxies Irregular galaxies have no regular or symmetrical structure. They have regions of elemental hydrogen gas, and many young stars. They have large amounts of dusts from which stars are born. No Excuses, Just Results! Show-up, Engage & Produce
- 5. Irregular Galaxies No Excuses, Just Results! Show-up, Engage & Produce
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- 9. Spiral Galaxies Spiral galaxies have three main components: a central bulge, disk, and halo No Excuses, Just Results! Show-up, Engage & Produce
- 10. Spiral Galaxies The bulge is a spherical structure found in the center of the galaxy. This feature mostly contains older stars. No Excuses, Just Results! Show-up, Engage & Produce
- 11. Spiral Galaxies The disk is made up of dust, gas, and younger stars. The disk forms arm structures. Our Sun is located in an arm of our galaxy, the Milky Way. No Excuses, Just Results! Show-up, Engage & Produce
- 12. Spiral Galaxies The halo of a galaxy is a loose, spherical structure located around the bulge and some of the disk. The halo contains old clusters of stars, known as globular clusters. No Excuses, Just Results! Show-up, Engage & Produce
- 13. Spiral Galaxies Globular clusters are spherical concentrations of stars typically 100 light years across and containing thousands of stars. Globular clusters 10 billion years old formed when the galaxy was still forming. No Excuses, Just Results! Show-up, Engage & Produce
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- 18. Elliptical Galaxies Elliptical galaxies are shaped like an elongated sphere. The light is smooth The surface brightness decreases as you go farther out from the center. Elliptical galaxies have no particular axis of rotation. No Excuses, Just Results! Show-up, Engage & Produce
- 19. Elliptical Galaxies No Excuses, Just Results! Show-up, Engage & Produce
- 20. Elliptical Galaxies No Excuses, Just Results! Show-up, Engage & Produce
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