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Chapter 8 The Sun

Guidepost The preceding chapter described how we can get information from a spectrum. In this chapter, we apply these techniques to the sun, to learn about its complexities. This chapter gives us our first close look at how scientists work, how they use evidence and hypothesis to understand nature. Here we will follow carefully developed logical arguments to understand our sun. Most important, this chapter gives us our first detailed look at a star. The chapters that follow will discuss the many kinds of stars that fill the heavens, but this chapter shows us that each of them is both complex and beautiful; each is a sun.

Outline I. The Solar Atmosphere A. Heat Flow in the Sun I. The Solar Atmosphere A. Heat Flow in the Sun B. The Photosphere C. The Chromosphere D. The Solar Corona E. Helioseismology II. Nuclear Fusion in the Sun A. Nuclear Binding Energy B. Hydrogen Fusion C. Energy Transport in the Sun D. The Solar Neutrino Problem

Outline (continued) III. Solar Activity A. Observing the Sun III. Solar Activity A. Observing the Sun B. Sunspots and Active Regions C. The Sunspot Cycle D. The Sun's Magnetic Cycle E. Spots and Magnetic Cycles on Other Stars E. Chromospheric and Coronal Activity F. The Solar Constant

General Properties Stars (like our sun) are great balls of gas held together by their own gravity. Why does their gravity not make them collapse into small dense bodies? Because of their high internal pressure, why do they not explode? Simple structures balanced between opposing forces that individually would destroy them! How does our sun affect life on Earth? Average star Spectral type G2 Only appears so bright because it is so close. Absolute visual magnitude = 4.83 (magnitude if it were at a distance of 32.6 light years) 109 times Earth’s diameter 333,000 times Earth’s mass Consists entirely of gas (av. density = 1.4 g/cm3) Central temperature = 15 million 0K Surface temperature = 5800 0K

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.

General Properties Average star Spectral type G2 Average star Spectral type G2 Only appears so bright because it is so close. Absolute visual magnitude = 4.83 (magnitude if it were at a distance of 32.6 light years) 109 times Earth’s diameter 333,000 times Earth’s mass Consists entirely of gas (av. density = 1.4 g/cm3) Central temperature = 15 million 0K (almost 27 million F) Surface temperature = 5800 0K

The Solar Atmosphere Only visible during solar eclipses Only visible during solar eclipses Apparent surface of the sun Heat Flow Temp. incr. inward Solar interior

The Photosphere Apparent surface layer of the sun Apparent surface layer of the sun Depth ≈ 500 km (310.686 miles) Temperature ≈ 5800 oK (9980.330 F) Highly opaque (H- ions absorb photons)) Absorbs and re-emits radiation produced in the solar interior The solar corona

The Photosphere gas marked by sunspots gas marked by sunspots Thin layer of gases (tissue covering a bowling ball) Gas from outer layers to core Emits the visible portion of light Less dense than the air you breathe

Layers of the sun

Energy Transport in the Photosphere Energy generated in the sun’s center must be transported outward. Near the photosphere, this happens through (energy is flowing upward through the photosphere) Convection: Cool gas sinking down Bubbles of hot gas rising up ≈ 1000 km Bubbles last for ≈ 10 – 20 min.

Granulation … is the visible consequence of convection … is the visible consequence of convection Each one is about the size of Texas! Last for 10-20 minutes

Chromospheric structures visible in Ha emission (filtergram) 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 oK to ≈ 10,000 oK (17,540.33°F), then jumps to 1 million oK (1,799,540.33 F) Filaments Transition region Chromospheric structures visible in Ha emission (filtergram)

The Chromosphere Lies just above the visible surface of the sun and blends with the corona 1000X more faint than the photosphere Thin line of pink during a solar eclipse Low density ionized gas Transition region----temperature rises fast form 45000 K to 1,000,000 K Using H alpha filter grams (pictures using a certain dark absorption line of light) shows filaments and spicules lasting from 5 to 15 minutes (flame like jets of cooler gas)

Each one lasting about 5 – 15 min. The Chromosphere (2) Spicules: Filaments of cooler gas from the photosphere, rising up into the chromosphere. Visible in Ha emission. Each one lasting about 5 – 15 min.

The Layers of the Solar Atmosphere Ultraviolet Visible Sun Spot Regions Photosphere Corona Chromosphere Coronal activity, seen in visible light

Corona Outermost part of the sun’s atmosphere (Greek for crown) Outermost part of the sun’s atmosphere (Greek for crown) Dim, not visible, can be seen during a solar eclipse Coronagraphs- specialized telescopes Magnetic field links the sunspots with features in the chromosphere and corona Light is reflected off of dust particles SOHO satellite has mapped a magnetic carpet, accounting for the increase in heat Solar wind—gases flow away from the sun due to the magnetic fields pointing outward the sun is losing mass----but will last for billions of years

The Magnetic Carpet of the Corona Corona contains very low-density, very hot (1 million oK) 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 gas particles from the sun. Constant flow of gas particles from the sun. Velocity ≈ 300 – 800 km/s (671,000 m/hr- 1,789,500 m/hr) Sun is constantly losing mass: 107 tons/year (≈ 10-14 of its mass per year)

Approx. 10 million wave patterns! Helioseismology The solar interior is opaque (i.e. it absorbs light) out to the photosphere. Only way to investigate solar interior is through Helioseismology = analysis of vibration patterns visible on the solar surface: Approx. 10 million wave patterns!

Helioseismology Detect rumblings in the sun using Doppler shifts in the solar surface Information comes from SOHO and GONG (Global Oscillation Network Group) a network of telescopes around the world Similar to a geologists studying the interior of the Earth using vibrations Using wavelengths of the vibrations, astronomers can determine: temperature, density, pressure, composition, and motion at different depths Reveals the rotation of the sun, and sunspots before they reach the surface

How does it work? How does the sun work? What is it’s Fuel? How does the sun work? What is it’s Fuel? How does it burn fuel? How does the heat travel? Light? Temperature? Solar winds? Solar flares? Will it ever burn out?

Energy generation in the sun (and all other stars): Energy Production Energy generation in the sun (and all other stars): Binding energy due to strong force = on short range, strongest of the 4 known forces: electromagnetic, weak, strong, gravitational 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.

Energy Generation in the Sun: The Proton-Proton Chain Basic reaction: 4 1H  4He + energy Need large proton speed ( high temperature) to overcome Coulomb barrier (electrostatic repulsion between protons). 4 protons have 0.048*10-27 kg (= 0.7 %) more mass than 4He. T ≥ 107 0K = 10 million 0K Energy gain = Dm*c2 = 0.43*10-11 J per reaction. Sun needs 1038 reactions, transforming 5 million tons of mass into energy every second, to resist its own gravity.

The Solar Neutrino Problem The 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. Early solar neutrino experiments detected a much lower flux of neutrinos than expected ( the “solar neutrino problem”). Recent results have proven that neutrinos change (“oscillate”) between different types (“flavors”), thus solving the solar neutrino problem. Sudbury neutrino observatory

Sun Spots; weather on the sun is magnetic Sun Spots; weather on the sun is magnetic Cooler regions of the photosphere (T ≈ 4240 K). Only appear dark against the bright sun. Would still be brighter than the full moon when placed on the night sky!

Sun Spots (2) Active Regions Visible Ultraviolet

The Active Sun Solar Activity, seen in soft X-rays

Magnetic Fields in Sun Spots Magnetic fields on the photosphere can be measured through the Zeeman effect on a spectrograph  Sun Spots are related to magnetic activity on the photosphere

Sun Spots (3) Magnetic field in sun spots is about 1000 times stronger than Earth’s. Magnetic North Poles Magnetic South Poles In sun spots, magnetic field lines emerge out of the photosphere.

Magnetic Field Lines Magnetic North Pole Magnetic South Pole Magnetic North Pole Magnetic South Pole Magnetic Field Lines

Reversal of magnetic polarity The Solar Cycle After 11 years, North/South order of leading/trailing sun spots is reversed 11-year cycle Reversal of magnetic polarity => Total solar magnetic cycle = 22 years

Maunder Butterfly Diagram The Solar Cycle (2) Maunder Butterfly Diagram Sun spot cycle starts out with spots at higher latitudes on the sun Evolve to lower latitudes (towards the equator) throughout the cycle.

The sun spot number also fluctuates on much longer time scales: The Maunder Minimum The sun spot number also fluctuates on much longer time scales: Historical data indicate a very quiet phase of the sun, ~ 1650 – 1700: The Maunder Minimum

Rotation Differential rotation: our gaseous sun is divided into different zones and layers, with each of our host star's regions moving at varying speeds. On average, the sun rotates on its axis once every 27 days. However, its equator spins the fastest and takes about 24 days to rotate, while the poles take more than 30 days. The inner parts of the sun also spin faster than the outer layers, according to NASA.

The Sun’s Magnetic Dynamo The sun rotates faster at the equator than near the poles. This differential rotation might be responsible for magnetic activity of the sun.

Magnetic Loops Magnetic field lines

The Sun’s Magnetic Cycle After 11 years, the magnetic field pattern becomes so complex that the field structure is re-arranged.  New magnetic field structure is similar to the original one, but reversed!  New 11-year cycle starts with reversed magnetic-field orientation

Image constructed from changing Doppler shift measurements Star Spots? Other stars might also have sun spot activity: Image constructed from changing Doppler shift measurements

Magnetic Cycles on Other Stars H and K line emission of ionized Calcium indicate magnetic activity also on other stars.

Relatively cool gas (60,000 – 80,000 oK) Prominences Relatively cool gas (60,000 – 80,000 oK) May be seen as dark filaments against the bright background of the photosphere Looped Prominences: gas ejected from the sun’s photosphere, flowing along magnetic loops

Eruptive Prominences (Ultraviolet images) (Ultraviolet images) Extreme events (solar flares) can significantly influence Earth’s magnetic field structure and cause northern lights (aurora borealis).

Coronal mass ejections Space Weather ~ 5 minutes Solar Aurora Sound waves produced by a solar flare Coronal mass ejections

Coronal Holes X-ray images of the sun reveal coronal holes. X-ray images of the sun reveal coronal holes. These arise at the foot points of open field lines and are the origin of the solar wind.

The energy we receive from the sun is essential for all life on Earth. 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: Energy Flux 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];