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Genetic variation, classification and race

Genetic variation, classification and ‘race’

Lynn B Jorde & Stephen P Wooding

Department of Human Genetics, University of Utah School of Medicine, Salt Lake City, Utah 84112, USA

Nature Genetics 36, S28 – S33 (2004)  Published online: ; | doi:10.1038/ng1435

New genetic data has enabled scientists to re-examine the relationship between human genetic variation and ‘race’. We review the results of genetic analyses that show that human genetic variation is geographically structured, in accord with historical patterns of gene flow and genetic drift.

Analysis of many loci now yields reasonably accurate estimates of genetic similarity among individuals, rather than populations. Clustering of individuals is correlated with geographic origin or ancestry. These clusters are also correlated with some traditional concepts of race, but the correlations are imperfect because genetic variation tends to be distributed in a continuous, overlapping fashion among populations. Therefore, ancestry, or even race, may in some cases prove useful in the biomedical setting, but direct assessment of disease-related genetic variation will ultimately yield more accurate and beneficial information.

Figure 1: A neighbor-joining network of population similarities, based on the frequencies of 100 Alu insertion polymorphisms.

The network is rooted using a hypothetical ancestral group that lacks the Alu insertions at each locus. Bootstrap values are shown (as percentages) for main internal branches. (Because of the relatively small sample sizes of some individual populations, bootstrap values for terminal branches within main groups are usually smaller than those of the main branches, indicating less statistical support for terminal branches.)

The population groups and their sample sizes are as follows:

Africans (152): Alur, 12; Biaka Pygmy, 5; Hema, 18; Coriell Mbuti Pygmy, 5; a second sample of Mbuti Pygmy from the Democratic Republic of the Congo, 33; Nande, 17; Nguni, 14; Sotho/Tswana, 22; Kung (San), 15; Tsonga, 14. East Asians (61):

Cambodian, 12; Chinese, 17; Japanese, 17; Malay, 6; Vietnamese, 9. Europeans (118): northern Europeans, 68; French, 20; Poles, 10; Finns, 20. South Indians (365): upper caste Brahmin, Kshatriya and Vysya, 81; middle caste Kapu and Yadava, 111; lower caste Relli, Mala and Madiga, 74; tribal Irula, Khonda Dora, Maria Gond and Santal, 99.

Figure 2

A neighbor-joining tree of individual similarities, based on 60 STR polymorphisms, 100 Alu insertion polymorphisms, and 30 restriction site polymorphisms.

The percentage of shared alleles was calculated for all possible pairs of individuals, and a neighbor-joining tree was formulated using the PHYLIP software package. African individuals are shown in blue, European individuals in green and Asian individuals in orange.

Figure 3

(a) Results of applying the structure program to 100 Alu insertion polymorphisms typed in 107 sub-Saharan Africans, 67 East Asians and 81 Europeans. Individuals are shown as dots in the diagram.

Three clusters appear in this diagram; a cluster membership posterior probability of 100% would place an individual at an extreme corner of the diagram.

(b) A second application of the structure program, using the individuals shown in a as well as 263 members of caste populations from South India. Adapted from ref. 32.

Figure 4

A neighbor-joining tree formulated using the same methods as in Figure 2, based on polymorphisms in the 14.4-kb gene AGT.

A total of 246 sequence variants, including 100 singletons, were observed. The 368 European, Asian and African individuals are described further in ref. 54.

Author’s conclusion: “Race remains an inflammatory issue, both socially and scientifically. Fortunately, modern human genetics can deliver the salutary message that human populations share most of their genetic variation and that there is no scientific support for the concept that human populations are discrete, nonoverlapping entities.

Furthermore, by offering the means to assess disease-related variation at the individual level, new genetic technologies may eventually render race largely irrelevant in the clinical setting. Thus, genetics can and should be an important tool in helping to both illuminate and defuse the race issue.”

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Note by RK about -> ” there is no scientific support for the concept that human populations are discrete, nonoverlapping entities.”

– Outside of racist groups, no scientist even makes such a claim. This article does not debunk the idea that biological groups for humans exists: It clearly shows that such groups exist, in precise detail. However, this data debunk claims made from people using non-scientific definitions of  words.

When scientists use words like “race”, “population” or “clade”, these words need to have precise meanings. Every discovery in biology and evolution over the last 200 years shows that biological groups has to exist. That is to say,  all life has a family tree that can be represented by cladograms. Those cladograms show evolutionary phylogenies.

“A clade is a grouping that includes a common ancestor and all the descendants (living and extinct) of that ancestor. Using a phylogeny, it is easy to tell if a group of lineages forms a clade. Imagine clipping a single branch off the phylogeny — all of the organisms on that pruned branch make up a clade.”

See Clades and phylogenies and clades rotate = equivalent phylogenies.

Related articles

The Importance of Race and Ethnic Background in Biomedical Research and Clinical Practice

The New England Journal of Medicine, Vol. 348, p. 1170-1175, 2003

Esteban González Burchard, M.D., Elad Ziv, M.D., Natasha Coyle, Ph.D., Scarlett Lin Gomez, Ph.D., Hua Tang, Ph.D., Andrew J. Karter, Ph.D., Joanna L. Mountain, Ph.D., Eliseo J. Pérez-Stable, M.D., Dean Sheppard, M.D., and Neil Risch, Ph.D.

The Genomic Challenge to the Social Construction of Race

By Jiannbin Lee Shiao, Thomas Bode, Amber Beyer et al, Sociological Theory, Vol 30, Issue 2, 2012

Race in biology, genetics and cladistics. Wikipedia.

The Whole Side of It—An Interview with Neil Risch. By Jane Gitschier

Evolution of cereals and grasses

What are cereals and grains, and where do they come from?

A cereal is any grass – yes you read that correctly, grass – cultivated for the edible components of its grain.

Common grasses that produce these wonderful grains are wheat, rye, millet, oat, barley, rice, and corn.

Types of Grains found on Recipematic

Wheat is the most common grain producing grass.

(botanically, a type of fruit called a caryopsis), composed of the endosperm, germ, and bran.

The term may also refer to the resulting grain itself (specifically “cereal grain”).

Cereal grain crops are grown in greater quantities and provide more food energy worldwide than any other type of crop[1] and are therefore staple crops. Edible grains from other plant families, such as buckwheat, quinoa and chia, are referred to as pseudocereals.

From the Health happens at Home website

All of the grains that we eat have been genetically modified by thousands of years of artificial selection. This includes all wheat, barley, rye, spelt and oats.

Paper 1: “Wheat: The Big Picture”, The Bristol Wheat Genomics site, School of Biological Sciences, University of Bristol

Wheat: The Big Picture – the evolution of wheat

Evolution wheat barley sorghum rice

Figure 2. Phylogenetic tree showing the evolutionary relationship between some of the major cereal grasses. Brachypodium is a small grass species that is often used in genetic studies because of its small and relatively simple genome.

Paper 2: Increased understanding of the cereal phytase complement for better mineral bio-availability and resource management

Article (PDF Available) in Journal of Cereal Science 59(3) · January 2013 with 244 Reads
DOI: 10.1016/j.jcs.2013.10.003

Fig-1-Phylogenetic tree of cereals selected grasses PAPhy gene copy numbers

Fig. 1. Phylogenetic tree of cereals and selected grasses. PAPhy gene copy numbers are given for each species and key evolutionary events are indicated.

Paper 2
Genome-wide characterization of the biggest grass, bamboo, based on 10,608 putative full-length cDNA sequences.
Peng Z, Lu T, Li L, Liu X, Gao Z, Hu T, Yang X, Feng Q, Guan J, Weng Q, Fan D, Zhu C, Lu Y, Han B, Jiang Z – BMC Plant Biol. (2010)

Phylogeny of grasses inferred from concatenated alignment of 43 putative orthologous cDNA sequences

Figure 2: Phylogeny of grasses inferred from concatenated alignment of 43 putative orthologous cDNA sequences. (A) Tree inferred from maximal likelihood method. Bayes inference yielded the same topology. (B) Tree inferred from neighbor joining method. Branch length is proportional to estimated sequence divergence measured by scale bars. Numbers associated with branches are bootstrap percentages. Arabidopsis was used as outgroup. Subfamily affiliation of the grasses is indicated at right.

Paper 3 Evolution of corn

The evolution of maize (corn)

Figure 1: The evolutionary stages of domestication and diversification.
From Evolution of crop species: genetics of domestication and diversification, Rachel S. Meyer & Michael D. Purugganan, Nature Reviews Genetics 14, 840–852 (2013) doi:10.1038/nrg3605

http://www.nature.com/nrg/journal/v14/n12/fig_tab/nrg3605_F1.html

Paper 4 text

Brachypodium distachyon: making hay with a wild grass, Magdalena Opanowicz, Philippe Vain, John Draper, David Parker, John H. Doonan
DOI: http://dx.doi.org/10.1016/j.tplants.2008.01.007

Phylogenetic Brachypodium and cereals

This next image is from Setaria viridis as a Model System to Advance Millet Genetics and Genomics.

By Huang, Pu & Shyu, Christine & Coelho, Carla & Cao, Yingying & Brutnell, Thomas. (2016) Frontiers in Plant Science. 7. 10.3389/fpls.2016.01781.

Cladogram phylogenetic rice wheat teff millet corn sorghum

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Sonar and ultrasound

Sonar (SOund Navigation And Ranging)

The use of sound to navigate, communicate with, or detect objects – on or under the surface of the water – such as another vessel.

Old Navy Sub sonar GIF

Active sonar uses a sound transmitter and a receiver.

Active sonar creates a pulse of sound, often called a “ping”, and then listens for reflections (echo) of the pulse.

Active sonar Wikipedia

Several animals developed sonar through evolution by natural selection.

Example: whales

Example: dolphins

echolocation of a dolphin wikipedia

Example: bats

Aquaman uses sonar! (Superfriends, 1970s, ABC)

How do we know what the ocean floor looks like?

Figure 6.8: A ship sends out sound waves to create a picture of the seafloor below it.

The echo sounder has many beams of sound. It creates a three dimensional map of the seafloor beneath the ship.

Early echo sounders had only a single beam and only created a line of depth measurements.

Boston Harbor

Boston Harbor Bathymetry ocean floor

Data from USGS Construction of Digital Bathymetry for the Gulf of Maine

What would it look like if we could use sonar to map out the entire Atlantic ocean?

Mid atlantic ridge NOAA

National Oceanic and Atmospheric Administration (NOAA), ETOPO1 Global Relief Model, http://www.virginiaplaces.org/geology/rocksdui4.html

Ultrasound

Medical ultrasound – a diagnostic imaging technique using ultrasound.

Used to see internal body structures such as tendons, muscles, joints, vessels and internal organs.

The practice of examining pregnant women using ultrasound is called obstetric ultrasound.

Ultrasound is sound waves with frequencies which are higher than those audible to humans (>20,000 Hz).

Ultrasonic images also known as sonograms are made by sending pulses of ultrasound into tissue using a probe.

The sound echoes off the tissue; with different tissues reflecting varying degrees of sound. These echoes are recorded and displayed as an image to the operator.

Medical ultrasound (Wikipedia)

Ultrasound human heart 4 chambers Wikipedia

“Amniocentesis is a prenatal test in which a small amount of amniotic fluid is removed from the sac surrounding the fetus for testing. The sample of amniotic fluid (less than one ounce) is removed through a fine needle inserted into the uterus through the abdomen, under ultrasound guidance.”

“The fluid is then sent to a laboratory for analysis. Different tests can be performed on a sample of amniotic fluid, depending on the genetic risk and indication for the test.”

Amniocentesis: WebMD

Amniocentesis image006

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Doppler effect

The Doppler effect

Named after Austrian physicist Christian Doppler who proposed it in 1842.

You hear the high pitch of an approaching ambulance’s siren – and then notice that its pitch drops as it passes you. That’s the Doppler effect.

Listen to the Doppler effect! A passing car beeps its horn

Doppler effect Acela express train

Doppler effect racetrack

The Big Bang Theory – The Doppler Effect

Doppler effect YouTube example 1

Doppler effect YouTube example 2

sound frequency increases during the approach,
is identical as it passes by,
and decreases during the recession.
(Adapted from Wikipedia.)

Watch the spacing of the sound waves, when the car is at rest, and when it is in motion. How does motion change the spacing of the waves?

http://www.acs.psu.edu/drussell/Demos/doppler/doppler.html

doppler-effect-car-frequency

Step 1: Staying at rest

In the center is a stationary sound source.
It produces sound waves.
The wavefronts propagate symmetrically away from the source,
at a constant speed

stationary-sound-source-produces-sound-waves-doppler

 

Step 2: Now the source is moving quickly.

Since the source is moving, the centre of each new wavefront
is slightly displaced to the right.

As a result, the wave-fronts begin to bunch up in front of,
and spread further apart behind, the source.

So an observer in front of the source will hear a higher frequency.

doppler-effect-source-moving-right-mach-0-7

We can see this in water: Doppler effect of water flow around a swan

doppler-effect-of-water-flow-around-a-swan

 

Doppler effect applet

Doppler applet (with sound)

Doppler effect and sonic booms

MCAS problems

By the end of our unit on waves we should be able to do MCAS Physics exam: sample wave problems

 

Learning Standards

2016 Massachusetts Science and Technology/Engineering Curriculum Framework

HS-PS4-1. Use mathematical representations to support a claim regarding relationships among the frequency, wavelength, and speed of waves traveling within various media. Recognize that electromagnetic waves can travel through empty space (without a medium) as compared to mechanical waves that require a medium

SAT subject test in Physics: Waves and optics

• General wave properties, such as wave speed, frequency, wavelength, superposition, standing wave diffraction, and Doppler effect
• Reflection and refraction, such as Snell’s law and changes in wavelength and speed
• Ray optics, such as image formation using pinholes, mirrors, and lenses
• Physical optics, such as single-slit diffraction, double-slit interference, polarization, and color

Code.Org lessons

Hit the ground running: Coding lessons from Code.Org

We’re using Blockly, a visual coding language.

code-org-puzzle-coding-example

 

What are “conditionals”?  “On One Condition” If-then-else conditional flowchart lesson

Course 2. Stage 3: Angry Birds coding the path through the maze.

Course 2, Stage 6: Maze Loops

Course 2, Stage 7. Artist loops

Course 2, Stage 8. Bee Loops.

Course 2, Stage 10. Bee Debugging.

Course 2, Stage 11. Artist debugging.

Course 2, Stage 13. Bee Conditionals.

Course 2, Stage 16. Flappy Birds

Code.org Stage 19 Artist – nested loops

Code.Org: Course 4 Intro to programming

Course 4: Stage 6, Artist variables

Course 4, Stage 7 : Play Lab variables

Course 4, Stage 9. Bee “For” loops, and counters

Course 4, Stage 10. Artist. “For” Loops.

Course 4. Stage 11. Play Lab “For” loops

Course 4. Stage 12. Artist Functions
Homework: Write a paragraph explaining how loops work, how WHILE loops work,
and how DO…WHILE loops work.

Tutorialspoint: Loops and Chapter 8: Loops. Introduction to Programming

Course 4. Stage 14. Artist with parameters

Course 4. Stage 16. Bees – Functions with parameters
Homework: What is a “Hello, World!” program?

Excelwithbusiness.com: Say “Hello, world!”.
How would  we tell a computer to write “Hello, World!” in Blockly?

PCAdvisor How to code-with-google-blockly

Course 4, Stage 19: variables super challenge
Homework :Go to TutorialsPoint (link below) Choose “programming environment”.
(1) What’s the purpose of a text editor?
(2) What’s the purpose of a compiler?
(3) What’s the purpose of  an interpreter?
Tutorialspoint.com lessons

Course 4. Stage 20. For Loops Super Challenge: Can you get Skrat to his acorn using as few blocks as possible?

Course 4. Stage 21. Super Challenge – Functions and Parameters

Course 4. Stage 2. EXTREME CHALLENGE. No rules. No clues. Just the challenge!

Hour of code programs

tba

Resources

Code.Org: Course 2 Intro to programming

Accelerated Intro to Computer Science: Code.Org

Hexadecimal

The hexadecimal numeral system, hex, is a numeral system made up of 16 symbols (base 16).

Your standard numeral system is called decimal (base 10) and uses ten symbols: 0,1,2,3,4,5,6,7,8,9.

Hexadecimal uses the decimal numbers and six extra symbols, from the English alphabet: A, B, C, D, E and F.

Hexadecimal A = decimal 10, and hexadecimal F = decimal 15.

We mostly use the decimal system. This is because humans have ten fingers (ten digits). Computers however, only have on and off, called a binary digit (or bit, for short). A binary number is just a string of zeros and ones: 11011011, for example.

For convenience, engineers working with computers tend to group bits together. In earlier days, such as the 1960’s, they would group 3 bits at a time (much like large decimal numbers are grouped in threes, like the number 123,456,789).

Three bits, each being on or off, can represent the eight numbers from 0 to 7: 000 = 0; 001 = 1; 010 = 2; 011 = 3; 100 = 4; 101 = 5; 110 = 6 and 111 = 7. This is called octal.

As computers got bigger, it was more convenient to group bits by four, instead of three. The additional bit can be either on or off, a 0 or a 1. So this doubles the numbers that the symbol would represent. This is 16 numbers.

Hex = 6 and Decimal = 10, so it is called hexadecimal.

Four bits is called a nibble (sometimes spelled nybble). A nibble is one hexadecimal digit, and is written using a symbol 0-9 or A-F.

Two nibbles is a byte (8 bits). Most computer operations use the byte, or a multiple of the byte (16 bits, 24, 32, 64, etc.).

Hexadecimal makes it easier to write these large binary numbers.
To avoid confusion with decimal, octal or other numbering systems, hexadecimal numbers are sometimes written with a “h” after the number. For example, 63h means 63 hexadecimal. Software developers quite often use 0x before the number (0x63).

Adapted from https://simple.wikipedia.org/wiki/Hexadecimal_numeral_system

How to Convert from Decimal to Hexadecimal: WikiHow

 

Light pollution

dark-sky-power-outage-los-angeles-call-911

Source: http://www.pbs.org/seeinginthedark/astronomy-topics/light-pollution.html

This is what we see on a night without clouds, if there was no light pollution:

Some camera lens filters can filter out some of the glare.

dark-sky-with-astronomik-filter-by-frank-hollis

Enter a caption

from http://photography-on-the.net/forum/showthread.php?t=1063821

Here are the various levels of polluted vs dark skies:

dark-sky-various-levels

This video from Sunchaser Pictures shows what LA night skies could look like without light pollution.

“An experimental timelapse created for SKYGLOWPROJECT.COM, a crowdfunded quest to explore the effects and dangers of urban light pollution in contrast with some of the most incredible Dark Sky Preserves in North America. Visit the site for more!
Inspired by the “Darkened Cities” stills project by Thierry Cohen, this short film imagines the galaxy over the glowing metropolis of Los Angeles through composited timelapse and star trail astrophotography. Shot by Gavin Heffernan (SunchaserPictures.com) and Harun Mehmedinovic (Bloodhoney.com). SKYGLOW is endorsed by the International Dark Sky Association”

Also see:

____________________________________________

This lesson is from http://darksky.org/light-pollution/

Less than 100 years ago, everyone could look up and see a spectacular starry night sky. Now, millions of children across the globe will never experience the Milky Way where they live.

The increased and widespread use of artificial light at night is not only impairing our view of the universe, it is adversely affecting our environment, our safety, our energy consumption and our health.

What is Light Pollution?

Most of us are familiar with air, water, and land pollution, but did you know that light can also be a pollutant?

The inappropriate or excessive use of artificial light – known as light pollution – can have serious environmental consequences for humans, wildlife, and our climate. Components of light pollution include:

  • Glare – excessive brightness that causes visual discomfort

  • Skyglow – brightening of the night sky over inhabited areas

  • Light trespass – light falling where it is not intended or needed

  • Clutter – bright, confusing and excessive groupings of light sources

Light pollution is a side effect of industrial civilization. Its sources include building exterior and interior lighting, advertising, commercial properties, offices, factories, streetlights, and illuminated sporting venues.

The fact is that much outdoor lighting used at night is inefficient, overly bright, poorly targeted, improperly shielded, and, in many cases, completely unnecessary. This light, and the electricity used to create it, is being wasted by spilling it into the sky, rather than focusing it on to the actual objects and areas that people want illuminated.

Glossary of Lighting Terms

How Bad is Light Pollution?

With much of the Earth’s population living under light-polluted skies, over lighting is an international concern. If you live in an urban or suburban area all you have to do to see this type of pollution is go outside at night and look up at the sky.

According to the 2016 groundbreaking “World Atlas of Artificial Night Sky Brightness,” 80 percent of the world’s population lives under skyglow.

In the United States and Europe 99 percent of the public can’t experience a natural night!

2003-blackout-ontario-canada-by-todd-carlson

If you want to find out how bad light pollution is where you live, use this interactive map created from the”World Atlas” data or the NASA Blue Marble Navigator for a bird’s eye view of the lights in your town. Google Earth users can download an overlay also created from the “World Atlas” data. And don’t forget to check out the Globe at Night interactive light pollution map data created with eight years of data collected by citizen scientists.

Effects of Light Pollution

For three billion years, life on Earth existed in a rhythm of light and dark that was created solely by the illumination of the Sun, Moon and stars. Now, artificial lights overpower the darkness and our cities glow at night, disrupting the natural day-night pattern and shifting the delicate balance of our environment. The negative effects of the loss of this inspirational natural resource might seem intangible. But a growing body of evidence links the brightening night sky directly to measurable negative impacts including

Light pollution affects every citizen. Fortunately, concern about light pollution is rising dramatically. A growing number of scientists, homeowners, environmental groups and civic leaders are taking action to restore the natural night. Each of us can implement practical solutions to combat light pollution locally, nationally and internationally.

You Can Help!

The good news is that light pollution, unlike many other forms of pollution, is reversible and each one of us can make a difference! Just being aware that light pollution is a problem is not enough; the need is for action. You can start by minimizing the light from your own home at night. You can do this by following these simple steps.

  • Learn more. Check out our Light Pollution blog posts

  • Only use lighting when and where it’s needed

  • If safety is concern, install motion detector lights and timers

  • Properly shield all outdoor lights

  • Keep your blinds drawn to keep light inside

  • Become a citizen scientist and helping to measure light pollution

Learn more about Outdoor Lighting Basics

Then spread the word to your family and friends and tell them to pass it on. Many people either don’t know or don’t understand a lot about light pollution and the negative impacts of artificial light at night. By being an ambassador and explaining the issues to others you will help bring awareness to this growing problem and inspire more people to take the necessary steps to protect our natural night sky.

IDA has many valuable resources to help you including Public Outreach Materials, How to Talk to Your Neighbor, Lighting Ordinances and Residential and Business Lighting.

Want to do more? Get Involved Now

dark-sky-galaxy-viewed-without-light-pollution

Big Bang Nucleosynthesis

This lesson is copyright © Michael Richmond. This work is licensed under a Creative Commons License.

The Big Bang Model

Let’s review the observational evidence:

  • Distance/velocity relationship: distant galaxies are moving away from us, with speeds which increase linearly with distance

  • Chemistry: the universe is almost entirely hydrogen and helium, in a mixture of roughly 12 H atoms to 1 He atom

  • Cosmic Microwave Background: no matter where we look in the universe, we see radio waves which look like those radiated by a blackbody at about 2.7 degrees above absolute zero. There are tiny (one part in 10,000) variations in the brightness of this radiation on scales of a degree or so

Is there any way to tie all these pieces of data together? Yes! One model which can explain them all is called the Big Bang model. The name was coined by a scientist who didn’t like the theory and tried to make it sound silly.


Fundamentals of the Big Bang Model

The Big Bang is built upon three main tenets:

  1. the universe used to be very hot

  2. the universe used to be very dense

  3. the universe is expanding (which is why it isn’t so hot or dense anymore)

Note that the basic Big Bang Model does NOT say anything about the following questions:

  • will the universe collapse again, or expand forever?

  • is space curved or flat?

  • how old is the universe?

  • what is the matter density in the universe?

  • what about dark matter?

  • is there some mysterious “repulsive” force on large scales?

  • how did galaxies form?

Some of these questions all depend upon the values of certain parameters in the model, which we may derive from observations. Others have nothing to do with the Big Bang itself.

Our understanding of the laws of nature permit us to track the physical state of the universe back to a certain point, when the density and temperature were REALLY high.

Beyond that point, we don’t know exactly how matter and radiation behave. Let’s call that moment the starting point. It doesn’t mean that the universe “began” at that time, it just means that we don’t know what happened before that point.


Big Bang Nucleosynthesis

One of the primary successes of the Big Bang theory is its explanation for the chemical composition of the universe. Recall that the universe is mostly hydrogen and helium, with very small amounts of heavier elements. How does this relate to the Big Bang?

Well, a long time ago, the universe was hot and dense. When the temperature is high enough (a few thousand degrees), atoms lose all their electrons; we call this state of matter, a mix of nuclei and electrons, a fully-ionized plasma. If the temperature is even higher (millions of degrees), then the nuclei break up into fundamental particles, and one is left with a “soup” of fundamental particles:

  • protons

  • neutrons

  • electrons

Now, if the “soup” is very dense, then these particles will collide with each other frequently. Occasionally, groups of protons and neutrons will stick together to form nuclei of light elements … but under extremely high pressure and temperature, the nuclei are broken up by subsequent collisions. The Big Bang theory postulates that the entire universe was so hot at one time that it was filled with this proton-neutron-electron “soup.”

But the Big Bang theory then states that, as the universe expanded, both the density and temperature dropped. As the temperature and density fell, collisions between particles became less violent, and less frequent. There was a brief “window of opportunity” when protons and neutrons could collide hard enough to stick together and form light nuclei, yet not suffer so many subsequent collisions that the nuclei would be destroyed. This “window” appeared about three minutes after the starting point, and lasted for a bit less than a minute.

Which nuclei would form under these conditions? Experiments with particle colliders have shown us that most of the possible nuclei are unstable, meaning they break up all by themselves, or fragile, meaning they are easily broken by collisions.

Helium (the ordinary sort, with 2 protons and 2 neutrons) is by far the most stable and robust compound nucleus. Deuterium (one proton and one neutron) is easily destroyed, and so is helium-3 (2 protons, one neutron).

So, it seems that this period of hot, dense plasma would create a lot of helium. Could it create other, heavier elements, too?

 

It turns out that none of the heavier nuclei which are easily made by collisions of single particles with helium nuclei, or helium nuclei with each other, are stable or robust. Almost all nuclei heavier than helium are likely to be destroyed by subsequent collisions. The only heavier nucleus which might possibly survive is lithium-7 (3 protons and 4 neutrons), but it requires the collision of a helium nucleus plus 2 or 3 other particles simultaneously, which isn’t very likely.

Detailed models of Big Bang nucleosynthesis predict that the brief “window of opportunity” lasted only a minute or two. After that, about three and a half minutes after the starting point, the temperature and density dropped so much that collisions between particles were rare, and of such low energy that the electric forces of repulsion between positively-charged nuclei prevented fusion. The result is

  • lots of hydrogen

  • some helium (ordinary helium-4)

  • tiny bits of deuterium

  • tiny bits of lithium

  • not much else

The relative amounts of hydrogen, helium, deuterium and lithium depend very sensitively on the exact density of matter in the universe during this window of opportunity. We’ll discuss this later.


The Cosmic Microwave Background

So, during the first few minutes after the starting point, the universe was hot enough to fuse particles into helium nuclei. The result was a ratio of about 12 hydrogen nuclei to 1 helium nucleus; that’s equivalent to saying that three quarters of the mass of the universe was hydrogen nuclei, and one quarter of the mass was helium nuclei.

But these nuclei were totally ionized: they lacked the normal collection of electrons surrounding them. The electrons were free to fly around space on their own. Free electrons are very efficient at scattering photons. Any light rays or radio waves or X-rays in this ionized plasma were scattered before they could travel far. The universe was opaque.

After a few thousand years, as the universe continued to expand and cool, the temperature reached a critical point. About 100,000 years after the starting point, the temperature dropped to about 3,000 degrees Kelvin. At this point, hydrogen nuclei (protons) were able to capture electrons, and hold them against collisions. We call this process of capturing electrons recombination (even though it was really the first “combination”, not a re-“combination”).

The universe became largely neutral, with electrons bound into hydrogen and helium atoms. Neutral atoms are nearly transparent to light rays and radio waves. Suddenly, the universe became transparent.

What this meant was that light rays which were produced by the hot, 3,000-degree gas were free to fly throughout the universe without being scattered or absorbed.

What kind of photons were they? Since they were produced by a hot gas, they had a blackbody spectrum appropriate for a temperature of about 3,000 Kelvin:

As the universe continued to expand, the wavelength of these photons increased: each time the universe doubled in size, the wavelength of the photons doubled. However, since the wavelength of each photon increased by the same factor, the relative wavelengths of the photons remained fixed.

It turns out that when one increases all the wavelengths of a blackbody spectrum by the same amount, one gets another blackbody spectrum — but one which corresponds to a lower temperature than the original.

The universe has expanded by a factor of about 1,000 since the time of recombination, which means that the wavelengths of these blackbody photons have increased by a factor of about 1,000 as they have flown through the cosmos. The Big Bang theory predicts that we should be able to detect these stretched-out photons, if we look in the right part of the electromagnetic spectrum:

blackbody-3-kelvin

The peak of the shifted blackbody spectrum now falls in the microwave range, with a wavelength of about one millimeter. This corresponds to a blackbody temperature of about 3 Kelvin: a factor of 1,000 times lower than the original 3,000 Kelvin when the gas became neutral.

It is reasonable to say that as the universe expands, its “temperature” drops in sync: expansion by a factor of 2 means the temperature drops by a factor of 2, expansion by a factor of 10 means the temperature drops by a factor of 10, and so on.

And when we look at the universe with radio telescopes in the microwave range, we see a spectrum which is exactly like a blackbody …

blackbody-from-cobe

with a peak at a wavelength of 1.869 millimeters, corresponding to a temperature 2.726 Kelvin.

Does the temperature of the microwave background change with time?

The Big Bang model predicts that this temperature drops as the universe expands. If we could somehow measure the temperature of the CMB at some time long ago, we ought to find a temperature higher than 2.7 Kelvin. And … we can!

  • some clouds of gas contain atoms which can be excited by absorbing a photon from the CMB; the atoms then decay into their ground states by emitting several secondary photons

  • by detecting these secondary photons, and measuring atomic properties of these atoms very carefully in a lab on Earth, we can deduce properties of the photons from the CMB which excited the atoms

  • if we look at such clouds of gas in our own Milky Way, we can calculate that the radiation absorbed by the atoms has a spectrum corresponding to a blackbody at a temperature of about 2.7 Kelvin

  • if we look at such clouds in very distant galaxies, the we can determine properties of the CMB spectrum long ago in time

The measurements are very difficult: they involve taking high-resolution spectra of very distant quasars, and looking at absorption by intervening material in galaxies that just happen to lie between us and the quasar. One recent attempt used the ratio of several lines of neutral carbon:

Astronomers have tried to use such measurements to calculate the temperature of the CMB as a function of redshift (and, in turn, as a function of time).

Most of the attempts have yielded only upper limits to the CMB temperature in the past, but in December, 2000, a team of astronomers using one of the 8.2-meter Very Large Telescopes in Chile succeeded in making an honest-to-goodness determination:

on the plot below, their value is the solid line denoting a temperature 6K < T < 14K at a redshift z=2.34.

Why is the CMB lumpy?

Now, if the universe was perfectly uniform at the time of recombination — same density everywhere, same temperature everywhere — then we should see a perfectly uniform microwave background. But, if the gas in the early universe had gathered into clumps by the time of recombination, even very fluffy clumps, the radiation it produced would be slightly more intense in the clumpy areas, and less intense in between them. The amplitude and size of fluctuations in the microwave background can tell us a lot about the conditions of the hot gas just 100,000 years after the starting point. We’ll discuss this later…


The distance/velocity connection

The Big Bang theory states that the universe is expanding, though it does not explain why the universe should behave in this way. As a result, objects which are subject to no forces should move away from each other. In a uniformly-expanding universe, the rate at which objects move away from each other depends linearly on their distance from each other.

And that linear relationship between distance and radial velocity is just what we see when we look at distant galaxies:

relationship-distance-and-radial-velocity-hubble

But … wait a minute. Does this expansion occur on all scales? What about

  • the distance between two people on opposite sides of the room?

  • the distance between the Earth and the Sun?

  • the distance between the Sun and the center of the Milky Way?

  • the distance between the Milky Way and the Andromeda Galaxy?

If there are “significant” attractive forces between objects, they do not move away from each other as time goes by.

These attractive forces may be

  "chemical" forces between              important on microscopic,
   neighboring molecules or atoms         human, and planet-sized
   (these are really due to               scales
   electric forces)

  gravitational forces between           important on solar-system,
   large bodies of matter                 galaxy, and galaxy-cluster
                                          scales

So the distance between the Earth and Sun has not increased over the past 4 billion years.

Nor does the length of a meterstick grow due to the expansion of the universe.

Only on the very largest scales, distances between isolated galaxies or clusters of galaxies, are the attractive forces so weak that the expansion of the universe is able to move objects apart.

The rate of expansion depends sensitively on the exact amount of matter in the universe. I

f the density of matter is high, long-range gravitational forces can slow down the expansion, or even stop it.

If the density of matter is very low, the expansion will go on forever. We will discuss this in greater detail later.


Summary

The Big Bang theory explains

  • the relative amount of light elements (depends on conditions a few minutes after the starting point)

  • the cosmic microwave background (depends on conditions 100,000 years after the starting point)

  • the expansion of distant galaxies away from each other (depends on the density of matter in the universe, and on the cosmological constant, if it is not zero)

It doesn’t provide answers to all our questions, but it does a better job than any alternative which has yet been proposed. All but a handful of astronomers have adopted the Big Bang as the standard theory for the evolution of the universe.

 

Related article There Was No Big Bang Singularity


For more information,

Creative Commons License Copyright © Michael Richmond. This work is licensed under a Creative Commons Li

I Was a Big Bang Skeptic

Also see: Evidence for the Big Bang FAQs

This essay is by Richard Carrier.

For years I argued that there might not have been a Big Bang, since the evidence for it was rather poor. I encountered as a result a sea of snobbery and condescension from physicists. I encountered bias and closed-mindedness, and this was all the more reason to go on record against it. I found my experience was not unique: even some professional astronomers had been pressured to advocate the Big Bang in order to get telescope time, which makes or breaks every astronomer’s career.[1]. This kind of arrogance was appalling.

…. I always kept an open mind and continued my investigations. And over the past two years enough evidence has arisen, and two physicists (Victor Stenger and Bjoern Feuerbacher) took enough trouble to patiently persuade me with genuine facts and argument, that I have “seen the light” so to speak, and changed my mind. Equally important was my careful reading of the  works of Barry Parker and Joseph Silk. I now conclude that the Big Bang Theory, in some formulation, is probably true. The odds are well in its favor. Why and how this is so I explain in this essay.

My Position Now

The current Big Bang Theory should be thought of as having two distinct elements.

The first part is a theory about the origin (or at least the early evolution) of the observed universe.

The second part is a theory about how that came about.

By confusing these two aspects of the theory I and others were easily led astray in our assessments of the evidence. The first element of the Big Bang theory now has about as firm an evidential foundation as anyone could reasonably expect of it. There is no good reason to doubt that the observable universe had its origin in a small, superheated state about 14 billion years ago, from which it expanded and cooled, condensing into the cosmos we now see.

The second element of the Big Bang Theory is another story. Hardly anyone can agree on the details, and evidence for or against any particular position is scarce and indecisive. But even if we had no clue at all as to why the universe began in a small, superheated state, this would not detract from the evidence that it did. And as it happens, we have more than a clue about the why.

The basic outlines of Inflation theory account for the Big Bang and other observations fairly well. They do not have enough specifics to fit or explain all the facts that we observe, and both are largely undetailed and untested as far as theories go. So this element remains highly contentious and speculative, and much in need of more fact-finding. But it is the best game in town, and it makes a lot of sense.

Evidence

(1) General Relativity and Vacuum Energy Imply a Big Bang Inflation Event

When Einstein applied the equations of General Relativity to the entire universe, rather than just the solar system, he found they predicted either that the universe must expand from or collapse to a singularity. Einstein eliminated this result by arbitrarily adding a “cosmological constant” that balanced everything out.

As Parker notes, “Einstein was reluctant to add the term. It destroyed the simplicity and beauty of his equations” (p. 51).

As Einstein himself said, “If Hubble’s expansion had been discovered at the time of the creation of the general theory of relativity, the cosmological member would never have been introduced. It seems now so much less justified to introduce such a member into the field equations” (Letter of 1932, quoted by Parker, p. 59).

When later scientists worked out all the possible solutions to this problem, it was found that the entire universe would inevitably have one of several particular shapes. Some of those shapes included a singularity at the beginning of time followed by an expansion: a Big Bang.

As it happens, the known properties of the universe as presently observed entail that only one of those descriptions can be correct. So the universe had to have begun as a singularity. The only way this could not be correct is if General Relativity is false (and that is unlikely: it is very well corroborated) or if some as-yet unknown force or factor prevented it.

As it happens, Stephen Hawking proved quantum mechanics is such a factor, since quantum uncertainty makes a singularity impossible (see “The Truth about Singularities“).

So contemporary Big Bang theory no longer involves a singularity at all. Instead, scientists do not yet know what the shape and content of the universe was prior to the Planck time, a tiny fraction of a second. But on present theory the observable universe still begins very, very small.

Much later it was noticed that such a Big Bang event would experience a very brief period of “supercooling” which would cause a rapid but brief period of “inflation,” at least if we are right about currently-accepted physics. This in turn predicts many peculiar observations, like the near-perfect density, smootheness and flatness of the universe.

Though Inflation Theory does not explain everything or fit all the facts, it has two things going for it: it appears to be independently predicted by other physical laws, and it explains a lot that otherwise would remain a mystery. Still, many physicists remain skeptical of Inflation Theory, even as they agree that the Big Bang theory is probably true.

(2) Expansion is Confirmed by Multiple Lines of Evidence.

There are five independent lines of evidence that all converge on a common conclusion: the universe began between 14 and 15 billion years ago in a superheated state where even atoms could not form, and has rapidly expanded and cooled ever since.[5]

The first and most important piece of evidence is the observation of redshifts, which can only be explained by assuming that every galaxy cluster in the universe is moving away from every other: the more distant, the greater the speed.

Though many scientists have shown or argued that some redshift has other causes, these explanations do not account for even a significant fraction of the observed objects, or of the observed redshift overall, which is simply too enormous to be accounted for by any other known means.

The most obvious contrary explanation is that something to do with the space the light passes through causes the frequency to decay, but this has been soundly refuted by two observations. First, the expansion rate is accelerating, which only a change in velocity can explain (since the rate of a space-caused decay could not change but would have to be constant).[6] Second, many observations of redshifted objects have been made whose light is split by a gravitational lens. These studies show that even when light coming from the same object traverses different distances, the redshift remains the same.[7]

So light is not decaying as it passes through space. The redshift must originate with the object, and only velocity can explain that.

The five independent lines of evidence for the universe’s age are as follows:

  • First, taking into account all known factors, including the recently-confirmed acceleration of the cosmic expansion rate, scientists have shown that if you rewind the observed behavior of the known universe, it all comes together in a tiny, superheated state about 14.5 billion years ago.

  • Second, we have confirmed that the oldest stars in our own galaxy are between 12 and 13 billion years old. Though Pickrell (cf. n. 5) notes that these “were probably not among the universe’s very first stars,” they would have formed no more than a billion years after the cosmos itself began to form. Though this only proves an age for our galaxy, not necessarily the universe, the result of 14 billion years perfectly matches the most recent calculation of the projected start-point for the universe’s observed expansion.

  • Third, the most distant galaxy yet observed, based on the most precise and accurate observations to date, lies between 12 and 13 billion lightyears away, and thus is just as old as ours.

  • Fourth, the observed interstellar abundance of certain radioactive elements, calculating backwards from their known rate of decay, entails that they must have been produced at least 12 to 13 billion years ago, about the time we would expect them to have formed if the universe began about 15 billion years ago.

  • Fifth, the current calculated age of various globular clusters beyond our galaxy is no more than 15 billion years. This corroborates an age of the universe of about 15 billion years.

These five facts, especially in combination with all the other “evidences” enumerated in this essay, would be a remarkable coincidence if the universe didn’t in fact originate between 14 and 15 billion years ago. So it probably did.

It must be noted that Lerner discusses experimental evidence that the pressure-action of light itself, upon galactic or stellar magnetic fields, would inevitably accelerate all objects away from each other: in other words, there is a possible explanation of expansion other than a Big Bang, indeed, an explanation of accelerating expansion.

And despite critics who originally attacked this suggestion, intergalactic magnetic fields have recently been demonstrated to exist on a vast scale.[8] Many other theories could perhaps account for it, too. However, all the other evidence concurs with a Big Bang event, not any of these other theories.

Likewise, M-Theory has recently provided an alternative that is just as successful as Inflation Theory without any Big Bang as ordinarily conceived. Called the ekpyriotic or “brane” theory, developed by Dr. Paul Steinhardt and others, this theorizes a “Big Collision” instead of a Big Bang.[9] Or, as Boslough puts it, “Maybe the big bang was just a big bang, an explosion in our little neighborhood of the universe that was neither the beginning of time nor the creation of the cosmos. Nobody knows.”[10]

This fact should be kept in mind throughout this paper: Big Bang theory is consistent with many different interpretations of the originating event. It is no longer tied to Singularity Theory nor does it logically require Inflation Theory, nor does it entail that nothing else exists apart from what we observe: there may be other universes, and even this universe is probably much larger than we will ever see.

(3) The Microwave Background Radiation is Consistent with a Big Bang Event

Not only did Big Bang Theory predict a microwave background glow, it exactly predicted its temperature. Though there are problems with the exact pattern of that radiation, and though there may yet be other causes for it,[11] no one has demonstrated any better explanation to be correct.

In contrast, analysis of the microwave background as observed by numerous independent instruments confirms certain features that suggest the universe was indeed in a superheated state (indeed, the very state that “Inflation” would have ended with) about 14 billion years ago.

The evidence is of sound waves that passed through the early superheated universe, in such a way that predicts the current existence of roughly 4.5% “baryonic matter,” based on experimentally proven ratios in particle accelerators, which is almost exactly what we observe.[12] This is not a slam dunk proof, but it is very strong evidence that the universe was once in a superheated state 14 billion years ago, again corroborating the basic elements of the Big Bang Theory.

No other theory can explain this acoustic peak, except theories already resembling the Big Bang, like Brane Theory.

(4) There are Too Many Light Elements to be Explained Any Other Way

I originally saw this as a failed evidence because we know too little to get anything like a precise ratio of light to heavy elements and thus could not base any argument on what that ratio was. However, on closer examination I found that this ambiguity does not matter so much.

Even though a lot of matter remains unobserved, and the time and rate of star formation is not securely known so the actual ratio today is not securely known,[13] the vast quantity of key light elements that we do observe is far too great to be accounted for in any other way than by something like a Big Bang. Alternative theories are at present entirely speculative, while Big Bang theory has experimental basis in particle physics.

This is most clear in the case of the verified presence of natural deuterium. Its quantity is not even important: its mere existence is inexplicable–except, so far, by the Big Bang theory. There is no other natural process known that can create stable deuterium. In fact, stars destroy this element.

But the evidence doesn’t end there: beginning at a superheated state entails a vast abundance of light elements over heavy, with more light elements in older epochs. Both observations are confirmed. The exact ratios are unknown, but everywhere (even in our own galaxy) older stars are comprised of more light elements than newer stars, and the vast scale of light elements is undeniable. There is simply way too much helium, for example, to explain by any other means.

And no other theory can account for the precise kinds of light elements we observe in superabundance: not just any helium, for example, but only helium-3 and helium-4; not just any lithium, but lithium-7; and so on. Other light elements exist in only trace amounts. This is exactly what would be predicted if the universe began as a superheated mass of superhot protons and neutrons which then cooled, according to the experimental results of atomic physics.

Evidence Against

Those are the four lines of evidence for the Big Bang that carry convincing weight. Other evidence might be uncertain (such as that for epochal change on a galactic scale, cf. n. 13), or equally predicted by other theories (such as that the universe is very nearly flat, a finding now well confirmed [15]).

But when we examine the evidence above, there really is no better theory than the Big Bang: all lines of evidence point there. Inflation Theory could be false, yet even then some form of the original Big Bang theory might still be true (i.e. Lamaître’s theory that the cosmos began as a spherical superheated mass a few lightyears across).

However, Inflation explains, even predicts, so much of the evidence we do have, and is predicted by well-tested theories like the Standard Model of Particle Physics, Quantum Mechanics, and General Relativity, that it is probably approximately true, at least in some fashion. But even if that is false, the Big Bang theory in some form is still probably true.

This remains so even despite problems. Indeed, some problems have been removed: for instance, more accurate measurements with higher resolution have resolved any doubts about the existence of observable objects more distant than 13 or 14 billion lightyears. None have been observed. Though some still might, current observation remains consistent with the Big Bang.

Note that it is only the observable objects that matter–the universe may easily be larger than 14 billion lightyears on any Big Bang theory, we just shouldn’t yet be able to see farther than that if the theory is true, and so far it seems we can’t. Likewise, though a value for the Hubble Constant had been confirmed that caused problems with earlier theories, the discovery of accelerating expansion has resolved that issue.[16]

Likewise, while there has been trepidation over inconsistencies in observed vs. required mass, gravity observations have confirmed the existence of 30% of this missing mass (in some form as yet unobservable to current instruments),[17] and much has been accounted for by the expected volume of neutrinos in the universe, according to the recently-confirmed neutrino mass.[18]

The number of observed kinds of neutrinos is also partly predicted by the Big Bang theory, so neutrinos are starting to provide an additional line of evidence for the Big Bang. Though this proof is less secure than the others, it is impressive that it happens to match and corroborate the same result as the stronger proofs (cf. Parker, pp. 105-111).

But some problems remain. Primarily, no version of the Big Bang theory yet explains supercosmic structure. As Peter Coles puts it, some scientists “argue, controversially, that the Universe is not uniform at all, but has a never-ending hierarchical structure in which galaxies group together in clusters which, in turn, group together in superclusters, and so on. These claims are completely at odds with the Cosmological Principle and therefore with the Friedmann models and the entire Big Bang theory.”[19]

Certainly, the observation of very large-scale structure going very far back in time is as yet not entirely explained. Yet Wane Hu notes that evidence of supercosmic structure in the most accurate microwave background data so far (retrieved by BOOMERANG) shows such structure “on the largest scales at the earliest times.”[20] But the incorporation of heavy neutrinos into cosmological models may be changing that.[21]

Conclusion

Still, this is simply a mystery that remains to be solved. The evidence for the Big Bang theory is simply too strong to dismiss on this account. All we can be sure of is that we don’t know exactly how or why the universe existed in a superheated state about 14 billion years ago, though it seems to have had something to do with singularities and inflation. But the basic fact, that the universe existed in a superheated state about 14 billion years ago, now seems hard to dispute. I, for one, believe it.

Related resources

https://kaiserscience.wordpress.com/earth-science/astronomy/the-big-bang-theory/

https://kaiserscience.wordpress.com/2017/02/22/big-bang-nucleosynthesis/

 

Copyright 2002 by Richard Carrier. Copying of this material is permitted provided credit is given to the author and no material herein is sold for profit.


[1] “Heaven’s Gatekeepers: the Galactic Battle for Telescope Time,”Lingua Franca, September, 1999, pp. 56-61.

[2] Barry Parker, The Vindication of the Big Bang: Breakthroughs and Barriers, 1993. This is out of print, but I found it an excellent lay summary of the evidence by a bona fide expert and well worth acquiring. Though some of his facts (particularly concerning chronology) are out of date, recent advancements have made his case stronger, not weaker. He also summarizes quite fairly many problems with the Big Bang theory (pp. 159-208, 231-2, 281-300; but compare pp. 233-57 and 305-12), and several alternatives to it that were proposed before 1993 (pp. 302-04, 313-36). All the same is true of the very up-to-date work of Joseph Silk, The Big Bang, 3rd ed., 2000. Far less useful but still in the same genre lies the relevant chapter in Robert Ehrlich’s Nine Crazy Ideas in Science (2001) and of course Fox, op. cit. n. 9.

[5] The first three “proofs” are reported by J. Pickrell, “Faded Stars Get New Role: Hubble Takes a Long Look” and R. Cowen, “Sharper Images: New Hubble Camera Goes the Distance,” Science News 161 (May 4, 2002), pp. 277-78. The other facts are described by Parker, op. cit., n. 2, pp. 96-101.

[6] e.g. J. Glanz, in Science, vol. 282, 1998, pp. 2156-7; Idit Zehavi and Avishai Dekel, in Nature, no. 6750, 1999, pp. 252-4.

[7] e.g. G. Goldhaber, et al. Timescale Stretch Parameterization of Type Ia Supernova B-band Light Curves (2001).

[8] cf. Science News, May 6, 2000, p. 294.

[9] See Karen Fox, The Big Bang Theory: What It Is, Where It Came From, and Why it Works, 2002, pp. 152-7. Brane theory fits superstring theory better than Inflation, and makes all the same predictions but one: different features in the gravity wave background, which we will probably not be able to measure for decades. See: J.R. Minkel & George Musser, “A Recycled Universe: Crashing branes and cosmic acceleration may power an infinite cycle in which our universe is but a phase,” Scientific American (March 2002), pp. 25-26. See also: “When Branes Collide: Stringing together a new theory for the origin of the universe,” Science News 160:12 (Sept. 22, 2001), pp. 184-5.

[10] John Boslough, Masters of Time, 1992, p. 223.

[11] e.g. Hoyle and Burbidge, “A Different Approach to Cosmology,” Physics Today, April 1999, pp. 38, 41. Their theory predicts a blackbody metallic dust as the source of the microwave background, and unexpected metallic dust has indeed been found in intergalactic voids (J. Michael Shull, “Intergalactic Pollution,” Nature, 2 July, 1998, p.17-19; Lennox Cowie and Antoinette Songaila, “Heavy-element enrichment in low-density regions of the intergalactic medium,” ibid., pp. 44-6). Another theory is Hannes Alfvén’s “plasma theory,” which is given at least a nod of respect by the science community: cf. Boslough, op. cit., n. 10, and Anthony Peratt, “Not with a Bang,” The Sciences, January/February, 1990. Fox also agrees that this makes all the same predictions as Big Bang theory with fewer difficulties, and has yet to be falsified by experiment or observation (op. cit., n. 9, pp. 133-4). Her one objection (“we must be at the very center of a matter…region of the universe”) operates on the mistaken assumption that such a region would be exactly as small as the visible universe: if these regions are trillions of lightyears across, we need be nowhere near the center of ours. It is also a known fact that such a glow would be created by, as Boslough puts it, “the continuous emission and absorption of electrons by the strong magnetic fields” of galaxies and their intergalactic filaments–fields and filaments recently proved to exist. However, as intriguing as these theories are, all the evidence taken together still more strongly supports the Big Bang interpretation.

[12] cf. Fox, op. cit., n. 9, pp. 150-2.

[13] Science News, July 25, 1998, p. 55 (cf. also January 10, 1998, p. 20): “maps of the far-infrared background glow had already demonstrated that visible-light images drastically underestimate the amount of star formation,” and based on submillimeter photography, “at early times in the universe, stars were born at a rate five times higher than visible-light studies have indicated,” etc. Also: J.K Webb, et al., “A High Deuterium Abundance at Redshift z=0.7,” Nature, 17 July, 1997, pp. 250-2: finds far more hydrogen isotopes than there should be; and J. Michael Shull, Lennox Cowie and Antoinette Songaila show there are far more heavy elements strewn throughout the intergalactic voids than anyone thought (Shull, op. cit. n. 11); and Ron Cowen, “All Aglow in the Early Universe,” Science News, May 27, 2000, pp. 348-50: “most of the light emitted by the very first galaxies in the cosmos is much too dim to be seen today. Objects that were bright long ago appear faint now, and less brilliant objects are entirely invisible,” p. 349.

[15] P.  de Bernardis, et al., “A Flat Universe from High-Resolution Maps of the Cosmic Microwave Background Radiation,” Nature, 27 April, 2000, pp.  955-9.  These results (from BOOMERANG) have been confirmed by a second balloon probe (MAXIMA), cf. Science News, June 3, 2000, p. 363.

[16] Riccardo Giovanelli, “Less Expansion, More Agreement,” Nature, 8 July, 1999, pp. 111-2. The “constant” lies in the range of 66-70 km/sMpc, which was not good news, for “values…above 60 have the embarrassing feature of yielding an age for the Universe since the Big Bang that is exceeded by the oldest stars in our Galaxy” unless the expansion is accelerating, and as it happens, it is. Further research has made both observations indisputable: cf. “Age of the Universe: A New Determination” Science News 160:17 (October 27, 2001), p. 261. It is 95% certain that the universe cannot be more than 14.5 billion years old (and that is the uppermost limit–its probable age is only 14 billion). This research also demonstrated that the hubble constant cannot be less than 55 and is probably around 72. See L. Knox, N. Christensen, & C. Skordis, “The Age of the Universe and the Cosmological Constant Determined from Cosmic Microwave Background Anisotropy Measurements,” updated Feb. 2002.

[17] This is the firm result of the Two Degree Field Galaxy Redshift Survey, cf. Science News, June 10, 2000, p. 374.

[18] “Physics Bedrock Cracks, Sun Shines In,” Science News 159:25 (23 June 2001). See also n. 21 and: “Laboratory measurements and limits for neutrino properties“; Super-Kamiokande at UC Irvine and New Results from Neutrino Oscillations Experiment.

[19] Peter Coles, “Cosmology–An unprincipled Universe?” Nature 391: 120-121 (8 Jan. 1998).

[20] Wane Hu, Nature, 17 April, 2000, pp. 939-40. Cf. also, Ron Cowen, “A Cosmic Crisis? Dark Doings in the Universe,” Science News 160:15 (Oct. 13, 2001), pp. 234-6). Cf. also Science News, June 7, 1997, pp. 354-5.

[21] Peter Weiss, “Double or Nothing: Physicists bet the neutrino’s its own eerie twin,” Science News 162:1 (6 July 2002), pp. 10-12.

originally found at https://infidels.org/library/modern/richard_carrier/bigbangredux.html

Blue sky

This is the outline for a future lesson on Rayleigh Scattering: Why the sky is blue

– Rayleigh scattering occurs when light is scattered off many very small particles.

– Mie scattering occurs when light is scattered off of many larger particles.

text

Addressing misconceptions

Question: Particles in the air cause shorter wavelengths (blue-ish0 to scatter more than the longer wavelengths (reddish.) This causes us to see the sky as being blue. So why does the sunrise (or sunset) and sun look red/orange?

Answer: “When you look at the sky and see blue you’re seeing blue light being scattered towards your eye.”

“When you look at the sun and it looks red or orange that’s because the blue light is being scattered away from your eye – leaving the remaining light to enter your eye.”

“The blue light is being scattered in all directions by Raleigh scattering. The colors you see depend on what direction you’re looking.”

Reference Physicsforums.com How-does-rayleigh-scattering-work

 

External resources

Why the sky is blue, by Chuck Weidman, Atmo 170A1 Sect. 3 Fall 2013

http://math.ucr.edu/home/baez/physics/General/BlueSky/blue_sky.html

https://www.itp.uni-hannover.de/~zawischa/ITP/scattering.html

http://hyperphysics.phy-astr.gsu.edu/hbase/atmos/blusky.html

http://www.thephysicsmill.com/2014/03/23/sky-blue-lord-rayleigh-sir-raman-scattering/

Brownian motion app  galileoandeinstein Brownian motion app

Lesson EarthRef.org Digital Archive ematm.lesson3.scattering.pptx

EM in the Atmosphere: Reflection, Absorption, and Scattering Lesson Plan

Powerpoint for the lesson plan

Learning standards

SAT subject test in Physics: Waves and optics

• General wave properties, such as wave speed, frequency, wavelength, superposition, standing wave diffraction, and Doppler effect
• Reflection and refraction, such as Snell’s law and changes in wavelength and speed
• Ray optics, such as image formation using pinholes, mirrors, and lenses
• Physical optics, such as single-slit diffraction, double-slit interference, polarization, and color

AP Learning Objectives

IV.A.2.b: Students should understand the inverse-square law, so they can calculate the intensity of waves at a given distance from a source of specified power and compare the intensities at different distances from the source.

IV.B.2.b: Know the names associated with electromagnetic radiation and be able to arrange in order of increasing wavelength the following: visible light of various colors, ultraviolet light, infrared light, radio waves, x-rays, and gamma rays.

L.2: Observe and measure real phenomena: Students should be able to make relevant observations, and be able to take measurements with a variety of instruments (cannot be assessed via paper-and-pencil examinations).

L.3: Analyze data: Students should understand how to analyze data, so they can:
– a) Display data in graphical or tabular form.
– b) Fit lines and curves to data points in graphs.

L.5: Communicate results: Students should understand how to summarize and communicate results, so they can:
– a) Draw inferences and conclusions from experimental data.
– b) Suggest ways to improve experiment.
– c) Propose questions for further study