1. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere1 THE SUN & EARTH’S UPPER ATMOSPHERE 9.IONOSPHERIC AND OPERATIONAL EFFECTS OF SOLAR FLARES a) radio noise including effects on GPSb) PCA events c) HF absorption d) sudden ionospheric disturbances 1.GENERAL CHARACTERISTICS OF THE SUN Descriptive Data Electromagnetic Radiation Particle Radiation 2.ENERGY GENERATION AND TRANSFER Core  Radiation Zone  Convection Zone  Solar Atmosphere 3.REGIONS OF THE SOLAR ATMOSPHERE Photosphere, Chromosphere, Corona 4.FEATURES OF THE SOLAR ATMOSPHERE Coronal Holes, Flares, Sunspots, Plages, Filaments & Prominences 5.THE SOLAR CYCLE 6.SOLAR FLARES AND CORONAL MASS EJECTIONS Description and Physical Processes Classifications 7.SOLAR RADIATION AND EARTH’S NEUTRAL UPPER ATMOSPHERE Temperature and Composition Structure Hydrostatic equilibrium 8. SOLAR RADIATION AND EARTH’S IONOSPHERE

2. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere2 Our Sun Our Sun is a massive ball of gas held together and compressed under its own gravitational attraction. Our Sun is located in a spiral arm of our Galaxy, in the so-called Orions arm, some 30,000 light-years from the center. Our Sun orbits the center of the Milky Way in about 225 million years. Thus, the solar system has a velocity of 220 km/s Our galaxy consists of about 2 billion other stars and there are about 100 billion other galaxies Our Sun is 333,000 times more massive than the Earth. It consists of 90% Hydrogen, 9% Helium and 1% of other elements Total energy radiated: equivalent to 100 billion tons of TNT per second, or the U.S. energy needs for 90,000 years Is 5 billions years old; another 5 billion to go Takes 8 minutes for light to travel to Earth The Sun has inspired mythology in many cultures including the ancient Egyptians, the Aztecs, the Native Americans, and the Chinese.

3. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere3 OTHER SUN FACTS radius 6.96 x 10 5 Km 109 R E mean distance from earth (1 AU) = 1.49 x 10 8 Km 215 R S mass 1.99 x 10 30 Kg 330,000 M E mean density 1.4 x 10 3 Kg m -3 1/4  E surface pressure200 mb1/5 p sE mass loss rate10 9 Kg s -1 surface gravity 274 ms -2 28 g E equatorial rotation period 26 days near poles 36 days inclination of sun's equator to ecliptic 7.5°23.5° for Earth total luminosity 3.86 x 10 26 W 1366.1 Wm -2 @ Earth escape velocity at surface618 km s -1 effective blackbody temperature5778 K

4. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere4 STRUCTURE OF THE SUN

5. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere5 REGIONS OF THE SUN’S INTERIOR AND ATMOSPHERE p-modes g-modes

6. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere6 ENERGY GENERATION AND TRANSFER The core of the Sun is a very efficient fusion reactor burning hydrogen fuel at temperatures ~1.5 x 10 7 K and producing He nuclei: 4 H 1  He 4 + 26.73 MeV This 26.73 MeV is the equivalent of the mass difference between four hydrogen nuclei and a helium nucleus. It is this energy that fuels the Sun, sustains life, and drives most physical processes in the solar system. D = Deuteron  = gamma ray = neutrino e + = positron e - = electron alpha particle Beryllium 6 (unstable)

7. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere7 Between the radiation zone and the surface, temperature decreases sufficiently that electrons can be trapped into some atomic band states, increasing opacity; convection then assumes main role as energy transfer mechanism. ( If radiation came straight out, it would take 2 seconds; due to all the scatterings, it takes 10 million years !)

8. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere8 The photosphere is the Sun’s visible “surface”, a few hundred km thick, characterized by sunspots and granules REGIONS OF THE SOLAR ATMOSPHERE: THE PHOTOSPHERE The photosphere is the lowest region of the solar atmosphere extending from the surface to the temperature minimum at around 500 km. 99% of the Sun’s light and heat comes out of this narrow layer. The solar surface is defined as the location where the optical depth of a = 5,000 Å photon is 1 (the probability of escaping from the surface is 1/e)

9. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere9 THE CHROMOSPHERE The chromosphere is the ~ 2000 km layer above the photosphere where the temperature rises from 6000 K to about 20,000 K. At these higher temperatures hydrogen emits light that gives off a reddish color (H-alpha emission) that can be seen in eruptions (prominences) that project above the limb of the sun during total solar eclipses. When viewed through an H-alpha filter, the sun appears red. This is what gives the chromosphere its name (color-sphere). In H- , a number of chromospheric features can be seen, such as bright plages around sunspots, dark filaments, and prominences above the limb. 6563 Å

10. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere10 The corona is the outermost, most tenuous region of the solar atmosphere extending to large distance and eventually becoming the solar wind. THE CORONA The most common coronal structure seen on eclipse photographs is the coronal streamer, bright elongated structures, which are fairly wide near the solar surface, but taper off to a long, narrow spike.

11. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere11 The corona is characterized by very high temperature (a few million degrees) and by the presence of a low density, fully ionized plasma. Here closed field lines trap plasma and keep densities high, and open field lines allow plasma to escape, allowing much lower density regions to exist called coronal holes. At the top of the chromosphere the temperature rapidly increases from about 10 4 K to over 10 6 K. This sharp increase takes place within a narrow region, called the transition region. The heating mechanism is not understood and remains one of the outstanding questions of solar physics TRANSITION REGION The corona is the main source of emissions at wavelengths < 100 nm

12. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere12 The Sun emits radiation over a range of wavelengths Emissions shown in this video come from progressively hotter regions of the Sun, and reveal different features. ELECTROMAGNETIC RADIATION

13. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere13 The Sun radiates at a blackbody temperature of 5770 K A blackbody is a “perfect radiator” in that the radiated energy depends only on temperature of the body, resulting in a characteristic emission spectrum. radiated energy insulation In the laboratory In a star The radiation reacts thoroughly with the body and is characteristic of the body T1T1 T2T2 T 1 >T 2 max  1/T radiated energy wavelength area  T 4 heating element

14. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere14 Total Solar Irradiance (TSI) Composite Database compiled from many satellite TSI data 1978-present, by Claus Frohlich and Judith Lean

15. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere15 T1T1 T2T2 T 1 >T 2 max  1/T radiated energy wavelength The wavelengths most significant for the space environment are X-rays, EUV and radio waves. Although these wavelengths contribute only about 1% of the total energy radiated, energy at these wavelengths is most variable.

16. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere16 A representative view of how the EUV portion of the solar spectrum affects the upper atmosphere. The strongest line is the He II (30.4nm), appearing near the left portion of the figure. As solar irradiance at EUV wavelengths varies on the order of 30%, the effect on thermosphere heating - and subsequent density increases - is significant. One effect is increased satellite drag; another is the significant ionization that results from increased X-ray and EUV fluxes, sometimes causing disrupted radio communications. Upper Atmosphere Solar heating Rates What is causing the heating ?

17. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere17 Density at 200 km

18. ASEN 5335 Aerospace Environments -- The Sun & Intro to Earth’s Upper Atmosphere18 Density at 200 km