The SunCh 26.1

Spring 2011

Discovery Science

The sun is the source of light and warmth in our solar system, so it is a natural object of human curiosity. It is also the one star that is most clearly visible from Earth. The interaction of light and matter, which you studied in Chapter 18, can reveal the secrets of the sun and introduce you to the stars.

In this section (26.1), you will discover how the analysis of the solar spectrum can paint a detailed picture of the sun’s atmosphere and how basis physics has solved the mystery of the sun’s core.

Guidepost

Here you will answer four essential questions:

• What do you see when you look at the sun?

• How does the sun make its energy?

• What are the dark sunspots?

• Why does the sun go through a cycle of activity?

Although this chapter is confined to the center of the solar system, it introduces you to a star and leads your thoughts onward among the stars and galaxies that fill the universe.

Guidepost (continued)

I. The Solar AtmosphereA. The PhotosphereB. The ChromosphereC. The Solar CoronaD. Below the Photosphere

Outline

II. Nuclear Fusion in the SunA. Nuclear Binding EnergyB. Hydrogen FusionC. Energy Transport in the SunD. Counting Solar Neutrinos

Outline (continued)

III. Solar ActivityA. Observing the SunB. SunspotsC. The Sun's Magnetic CycleD. Spots and Magnetic Cycles on Other StarsE. Chromospheric and Coronal ActivityF. The Solar Constant

General Properties

• Average star

• Absolute visual magnitude = 4.83 (magnitude if it were at a distance of 32.6 light years)

• Central temperature = 15 million K

• 333,000 times Earth’s mass

• 109 times Earth’s diameter

• Consists entirely of gas (av. density = 1.4 g/cm3)

• Only appears so bright because it is so close.

• Spectral type G2

• Surface temperature = 5800 K

The Solar Atmosphere

Hea

t F

low

Solar interior

Temp. incr. inward

Only visible during solar eclipses

Apparent surface of the sun

• Apparent surface layer of the sun

The Photosphere

The solar corona

• Depth ≈ 500 km• Temperature ≈ 5800 K• Highly opaque (H- ions)• Absorbs and re-emits radiation produced in the sun

Energy Transport near the PhotosphereEnergy generated in the sun’s center must be transported outward.

Near the photosphere, this happens through

Convection:

Bubbles of hot gas rising up

Cool gas sinking down

≈ 1000 km

Bubbles last for ≈ 10 – 20 min

Granulation

… is the visible consequence of convection.

The Chromosphere• Region of sun’s atmosphere just above the photosphere

• Visible, UV, and X-ray lines from highly ionized gases

• Temperature increases gradually from ≈ 4500 K to ≈ 10,000 K, then jumps to ≈ 1 million K

Transition region

The Layers of the Solar Atmosphere

Visible

Photosphere

Ultraviolet

Chromosphere

Coronal activity, seen in visible

light

Corona

Sun Spot Regions

The Magnetic Carpet of the Corona

• Corona contains very low-density, very hot (1 million K) gas

• Coronal gas is heated through motions of magnetic fields anchored in the photosphere below (“magnetic

carpet”)

Computer model of the magnetic carpet

The Solar Wind

Constant flow of particles from the sun

Velocity ≈ 300 – 800 km/s

The sun is constantly losing mass:

107 tons/year

(≈ 10-14 of its mass per year)

Energy ProductionEnergy generation in the sun

(and all other stars):

Nuclear Fusion

= fusing together 2 or more lighter nuclei to produce heavier ones.

Nuclear fusion can produce energy up to the production of iron;

For elements heavier than iron, energy is gained by nuclear fission.

Binding energy due to strong force = on short range, strongest of the 4 known forces: electromagnetic, weak, strong, gravitational

Energy Generation in the Sun: The Proton-Proton Chain

Basic reaction:

4 1H 4He + energy

4 protons have 0.048*10-27 kg (= 0.7 %) more mass than 4He.

Energy gain = m*c2

= 0.43*10-11 J

per reaction

Need large proton speed ( high temperature) to overcome

Coulomb barrier (electrostatic repulsion between protons)

Sun needs 1038 reactions, transforming 5 million tons of mass into energy every second, to resist its own gravity.

T ≥ 107 0K = 10 million 0K

Energy Transport in the Sun

Radiative energy

transport

-rays

Counting Solar NeutrinosThe solar interior can not be observed directly because it is highly opaque to radiation.

But, neutrinos can penetrate huge amounts of material without being absorbed.

Davis solar neutrino experiment

Neutrino Detection confirms fusion in the Sun

Very Important Warning:

Never look directly at the sun through

a telescope or binoculars!!!

This can cause permanent eye damage – even blindness.

Use a projection technique or a special sun viewing filter.

Observing the Sun

Sun SpotsCooler regions of the

photosphere (T ≈ 4240 K)

They only appear dark against the bright sun; they would still be brighter than the full moon when placed on the night sky!

Sun Spots (2)

Active Regions

Visible

Ultraviolet

Sunspot regions show up as bright (active) regions in ultraviolet and X-ray images.

Magnetic Field Lines

Magnetic North Pole

Magnetic South Pole

Magnetic Field Lines

Magnetic Field Lines

Hot gas ejected from the sun often

follows magnetic field lines and

traces out the loop structure of the magnetic field.

Video Clip

The Solar Cycle

11-year cycle

Reversal of magnetic polarity

After 11 years, North/South order of

leading/trailing sun spots is reversed

=> Total solar cycle = 22 years

The Sun’s Magnetic Dynamo

This differential rotation might be responsible for magnetic activity of the sun.

The sun rotates faster at the equator than near the poles.

Magnetic Loops Video Clip

Magnetic field lines

Prominences

Looped Prominences: gas ejected from the sun’s photosphere, flowing along magnetic loops

Relatively cool gas (60,000 – 80,000 oK)

May be seen as dark filaments against the bright background of

the photosphere

Eruptive Prominences

(Ultraviolet images)

Extreme events (solar flares) can significantly influence Earth’s magnetic field structure and

cause northern lights (aurora borealis).

Solar Magnetic Phenomena

Aurora Borealis

Sound waves

produced by a

solar flare

~ 5

min

utes

The Solar Constant

The energy we receive from the sun is essential for all life on Earth.

The amount of energy we receive from the sun can be expressed as the Solar Constant:

F = 1360 J/m2/s

F = Energy Flux =

= Energy received in the form of radiation, per unit time and per unit surface area [J/s/m2]

HEA Video

Energy Flux