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General Properties Internal Structure Solar Atmosphere Photosphere, chromosphere, and corona Surface Features and Magnet

General Properties Internal Structure Solar Atmosphere Photosphere, chromosphere, and corona Surface Features and Magnetic Fields Solar Activities Solar Cycle Sun-Earth Connection. The Surface of the Sun….

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General Properties Internal Structure Solar Atmosphere Photosphere, chromosphere, and corona Surface Features and Magnet

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  1. General Properties • Internal Structure • Solar Atmosphere • Photosphere, chromosphere, and corona • Surface Features and Magnetic Fields • Solar Activities • Solar Cycle • Sun-Earth Connection

  2. The Surface of the Sun… In images of the Sun, we see a sharp edge, which we perceive as the surface of the Sun. However, like the surfaces of the Jovian planets (the Gas Giants), it is not a firm, solid, thick surface that we can stand on like on the Earth… • Density of the atmosphere on the surface of the Earth is • 1.3 kg/m3, or about • 1  1025 N2 molecules per cubic meter, and • Density of the atmosphere on the surface of the Sun is • 1  1023 particles per cubic meter, or about only 1% the density of the Earth’s atmosphere. • Density of the solar atmosphere just a few thousand kilometer above the ‘surface’, or in the solar corona • 1  1014 particles per cubic meter • The rapid decrease of the density within a • short distance is the reason that we see a • sharp edge… • The surface layer is where sunlight are • generated. It is referred to as the Photosphere.

  3. Chromosphere The Chromosphere is a thin, irregular layer above the photosphere in which the temperature rises up from 5,800 K to about 20,000 K. This layer is usually observed in the red wavelength of the Hydrogen absorption line. It is therefore termed Chromosphere, meaning color-sphere, The Sun in Calcium absorption line in blue (393 nm) wavelength. The Sun in Hydrogen absorption line in red (656 nm) wavelength. Bright patches (the Plages) and dark spots (sunspots) are related to higher magnetic field regions.

  4. The Sun in UV and X-Ray – Corona The Sun in X-ray shows the structure of the very hot (1,000,000 K) corona • Recall that high temperature blackbody produces radiation with shorter wavelength. X-ray are produced by blackbody with million degree temperature. • We don’t know why the coronal temperature is so high… • The Sun in one of the emission spectra of Helium in the UV (30.4 nm) shows the structure of a cool regions of the corona. X-ray image of the Sun. UV image of the Sun in He II 30.4

  5. The Solar Corona in ‘White Light’ This is an image of total solar eclipse. • The radiation are reflection of sunlight by the electrons in the corona. • A radial gradient has been removed from the image to enhance the coronal features. • The streamers are where slow solar wind leave the Sun. • The coronal holes are where fast solar wind leave the Sun.

  6. MDI MAGNETOGRAM 01-May-2005 20:48 UT MDI WHITE LIGHT 01-May-2005 20:48 UT BBSO GHN H 01-May-2005 20:48 UT EIT FeX 195 A 01-May-2005 20:48 UT EIT FeXV 284 A 01-May-2005 20:48 UT GOES SOFT X-RAY 01-May-2005 20:48 UT The Many Faces of the Sun By observing the Sun simultaneously at many different wavelengths (or colors), we can see different layer of the solar atmosphere, and get a better understanding of what’s going on…

  7. The Coronal Heating Problems • The temperature of the Sun is the highest in its core, about 15 million degrees. • The temperature decreases as we move outward toward the surface, dropping to 6,000 K at the photosphere. • The temperature then rises to about 20,000 K in the chromosphere, just a few thousand km above the photosphere. • The temperature than rises rapidly to 1to 2 million degrees in the corona. • We do not understand how the corona is heated, and this is one of the important unresolved questions of solar physics.

  8. General Properties • Internal Structure • Solar Atmosphere • Surface Features and Magnetic Fields • Sunspots, Granulation, Filaments and Prominences, Coronal Loops… • Solar Activities • Solar Cycle • Sun-Earth Connection

  9. High-Resolution View of the Solar Surface This is what the surface of the Sun looks like with high resolution…we see • Sunspot • Umbra • Penumbra • Solar Granulation

  10. Solar Granulation On the surface of the Sun, we can see the action of convection… • Image of solar granulation. The bright center of the cells are where hot gas rise to the surface. The narrow dark lanes are where cold gas sink to the ‘bottom’. • Each cell is about 1,000 km in size

  11. Sunspots Sunspots are dark features on the surface of the Sun. Sunspots are strongly magnetized region on the surface of the Sun. They appear dark because the presence of very strong magnetic fields helps the plasma inside the sunspot to balance the pressure of the plasma outside of the sunspot. Therefore, the thermal pressure (related to the temperature of the plasma) of the plasma inside the sunspot is lower, leading to lower temperature, and lower intensity (darker compared with the surrounding area). We still don’t know why there is an umbra and a penumbra in sunspots. Neither do we know why there are such sharp boundary between different regions…

  12. Early Clues of Sunspot Magnetic Field Sunspot group seen in H (Hydrogen absorption line) Sunspots are strongly magnetized region on the surface of the Sun. The brightness structure of a sunspot seen in the absorption line of hydrogen resemble the magnetic field lines surrounding a bar magnet. Bar Magnet The pattern formed by the small magnetized iron bars shows the magnetic field lines.

  13. Evidence of Magnetic Field in Sunspot Spectra of magnetic field sensitive absorption lines from a slice (the dark vertical line at the center of the image on the left) of a sunspot. The presence of a magnetic field in the solar atmosphere can be seen in the Zeeman Effect of the spectral line on the right. Some spectral lines have three components…and magnetic field can change the energy level of two of them. Thus, the spectral line will be split into three lines when there is a strong magnetic field. The separation between the lines measures the strength of the magnetic fields

  14. The Sun as a Magnetic Star • Today, we know that almost all the solar surface and coronal features (except for solar granulation, which is generated by convection) we talked about so fare are related to magnetic fields… • Sunspots • Filaments and Prominences • Coronal loops • Without the magnetic fields, the Sun • would be a very boring star to look at…

  15. Magnetic Field of the Whole Sun • A magnetogram shows the magnetic field on the surface (the photosphere) of the Sun. The black and white patches show where the magnetic fields are strong. • White indicates magnetic field pointing toward us. • Black indicates magnetic fields pointed away from us. • The large patches of black and white are due to sunspot and active regions with strong magnetic fields. • The pepper-and-salt patterns outside of the active regions indicates that there are magnetic fields everywhere on the surface of the Sun.

  16. Filaments and Prominences Filaments and prominences are cool and dense gas suspended high in the solar atmosphere, and embedded in the very hot solar corona. • When they are observed on the solar surface, they appear as dark absorption features…filaments! • When the are observed outside of the solar limb, they appears as bright features because they reflect sunlight toward us…prominences! • How they can survive in the million-degree temperature corona, and stay high up against gravity is still a mystery. We know magnetic field plays an important role, but the details is not well understood. The Grand Daddy Prominence A huge solar prominence observed in 1946

  17. Coronal Loops We believe that the loops we see in the solar corona trace the magnetic field lines. However, the magnetic fields are everywhere in the corona. we are not quite sure why only some of the field lines are bright… High resolution image of the coronal obtained in the UV wavelength obtained by TRACE satellite.

  18. General Properties • Internal Structure • Solar Atmosphere • Surface Features and Magnetic Fields • Solar Activities • Flares, CMEs, and Filament Eruptions • Solar Cycle • Sun-Earth Connection

  19. Solar Activities---Flares A flare is defined as a sudden, rapid, and intense variation in brightness. A solar flare occurs when magnetic energy that has built up in the solar atmosphere is suddenly released. Radiation is emitted across virtually the entire electromagnetic spectrum, from radio waves at the long wavelength end, through optical emission to x-rays and gamma rays at the short wavelength end. The amount of energy released is the equivalent of millions of 100-megaton hydrogen bombs exploding at the same time! Or, about a few percent of the total energy released by the Sun every second.

  20. Filament Eruptions Filament eruptions are usually associated with flares and coronal mass ejection. Exactly how they work is still under investigation...

  21. General Properties • Internal Structure • Solar Atmosphere • Surface Features • Magnetic Fields • Solar Activities • Solar Cycle • Sun-Earth Connection

  22. Solar Cycle---Sunspot Numbers and the Butterfly Diagram Solar Cycle The number of sunspots on the surface of the Sun follows a 11-year cycle. Butterfly diagram Sunspots appear at higher latitude at the beginning of the solar cycle, and migrate toward the equator as the cycle evolve. So, when we plot the latitude of the sunspots as a function of time, the patterns looks like a series of butterfly…therefore it is referred to as the butterfly diagram’

  23. Magnetic Field and X-Ray Variation Through one Solar Cycle • The temperature of the solar corona a few million degrees (no explanation yet). • The high temperature causes it to emit photons mostly in the UV and X-ray wavelengths (high energy photons). • The activities in the solar corona also follow the solar cycle. • In fact, the level of almost every aspect of solar activities (flares, coronal mass ejections, etc.) follows the solar cycle. The black-and-white patterns show the surface magnetic field variation through one sunspot cycle (11 years). Notice the reversal of the ordering at the beginning and the end of the cycle.

  24. How Does Solar Cycle Work? • The magnetic field of the Sun is postulated to be generated at the bottom of the convection zone. This magnetic field then rises up to the surface and expand into the corona, to produce the magnetic features we see. • Since the magnetic field of the Sun reverse its orientation every 11 years, the solar cycle is really a 22-year magnetic cycle. In comparison, the Earth’s magnetic field direction is stable. • The number of sunspot only depends on the strength of the solar magnetic activities, but not the orientation of the magnetic fields. Therefore, sunspot number cycle is half that of the magnetic field cycle. • How does the Sun changes its magnetic field orientation every 22 years? • We don’t have a complete theory yet. However, there are a few clues. For example, we believe that the differential rotation of the Sun must play a role in changing the magnetic field configuration from that of a dipole (like a bar magnet) to that of a torus (shaped like a doughnut). • The exact mechanism of the solar cycle is still unknown!

  25. Differential Rotation of the Sun The Sun does not rotate like a solid body. It rotates every 25 days at the equator and takes progressively longer to rotate one revolution at higher latitudes, up to 35 days at the poles. This is known as differential rotation. • You can pick a few sunspots located at different latitude from the movie on the right, and trace them as they rotate across the solar disk. Using the time information at the lower-left-hand corner of the images, you can calculate the rate of rotation of the Sun at different latitudes. • You should find that sunspots near the equator rotate faster than those at higher latitude.

  26. Effects of Differential Rotation At the surface of the Sun, and deeper in the interior, when we move the solar plasma, the magnetic fields embedded in the plasma will move with the plasma. This is referred to as the frozen-in magnetic fields. • So, the effect of differential rotation is the stretching of the magnetic fields that was originally in the north-south direction to make them runs along the east-west direction… • Sometimes a small section of the magnetic field would pop up through the surface. This will make a sunspot, and it happens more frequently during solar maximum… Solid (dashed) lines represents magnetic field lines above (under) the surface.

  27. ~5 years later… S 22 years later… N Evolution of Solar Magnetic Field During the Solar Cycle • Solar Minimum • Dipole Magnetic Field • No Sunspot • Solar Maximum • ToroidalMagnetic Field • Many Sunspots But, this is only half of the story! The magnetic field configuration of the Sun evolves with a 22 year cycle. 11 years later…

  28. The Solar Cycle Problem and the Sunspot Phenomenon • At this point, we don’t have a satisfactory theory for the solar cycle. Neither do we have a complete understanding of the sunspot phenomenon. These are two more important problems of solar physics that needs to be solved.

  29. General Properties • Internal Structure • Solar Atmosphere • Surface Features • Magnetic Fields • Solar Activities • Solar Cycle • Sun-Earth Connection

  30. Sun-Earth Connection • How do Solar Activities Affect Earth? • In short time scale (compared with the lifetime of the Sun) • Space Weather and Geomagnetic Storm • Flares and Coronal Mass Ejections (CME) bombard the Earth with high energy charged particles, causing interruption to communications, and power grids • Solar Irradiance Variations and Possible climate change • The solar energy input determines the temperature on the surface of the Earth. If the Sun is to increase its luminosity by 1%, it will have significant effect on Earth’s temperature. It will increase by about 0.75 K. • In long time scale • The Sun will eventually evolve into a red giant star, increases its energy output and its physical size. Earth may eventually be engulfed by this enlarged Sun, and life will be extinguished on Earth  Next chapter…

  31. Space Weather Space Weather (from NASA SoHO Space Weather Website) Space weather happens with a solar storm from the Sun travels through space and impacts the Earth’s magnetosphere. Studying space weather is important to our national economy because solar storms can affect the advanced technology we have become so dependent upon in our everyday lives. Energy and radiation from solar flares and coronal mass ejections can • Harm astronauts in space • Damage sensitive electronics on orbiting spacecraft? • Cause colorful auroras, often seen in the higher latitudes? • Create blackouts on Earth when they cause surges in power grids. http://sohowww.nascom.nasa.gov/spaceweather/lenticular/

  32. From Coronal Mass Ejections… Space weather starts with Coronal Mass Ejection on the Sun… Coronal mass ejections and flares are due to the changes in the magnetic field structures in the solar corona. However, details mechanism is still not clear, and we cannot predict when flares and CME are going to occur yet!

  33. To Geomagnetic Storm… • Flares and coronal mass ejection send high energy charged particles (electrons, protons) into space. If the direction and speed of these particles are just right, they can reach the Earth. These high energy particles are harmful to life on Earth. They can also cause damages to satellites operating in space, as well as power grids. • Charged particles travel along the magnetic field lines • We are protected by Earth’s magnetic field, which directs the majority of the high energy charged particles toward the north and south poles to produce the aurora borealis and aurora Australis. Charged particles spiral around the magnetic field lines.

  34. Effects of Geomagnetic Storm • In October 31, 2003, a series of strong geomagnetic storms damaged two satellites, caused the power grid in Sweden to shutdown, cutting power to 20,000 customers, disrupted radio communication and broadcast systems, and forced the airlines to change flight plans. • The large variation of the Earth’s magnetic fields can induce strong, uncontrolled electric current in the power lines, causing the power grid to overload and shutdown… • The high energy charged particles from the Sun are a health risk to astronauts in space orbit and passengers in jets flying at high altitudes over the north and south polar regions . • Aurora were reported as far south as New Mexico, Texas, and Florida. http://www.space.com/scienceastronomy/power_outage_031031.html

  35. Solar Irradiance Variations Modern measurements showed that the solar constant is really not a constant. The energy output of the Sun is modulated by the magnetic activity. But details of how this happens is still under study…Nevertheless, we know that • Solar irradiance is higher when the surface magnetic field is stronger (when ther are more sunspots)… • The amplitude of the solar irradiance variation is about 2 W/m2, or about 0.1%. • This variation is too weak to cause climate change. • But, if solar magnetic activities was significantly reduced or enhanced for a long period of time, it can change the climate of the Earth…for example, did the Sun caused the Little Ice Age? Solar constant measurements from several satellite experiments Sunspot Maximum

  36. Little Ice Age (1650-1700) • During a period that lasted approximately 50 years from the mid 1650s to the early 1700, the temperatures in northern Europe had their lowest values for the past millennium, with winter temperatures being on average 1 to 2 degrees colder than in later periods. • This period has been called the Little Ice Age. During this period, access to Greenland was largely cut off by ice from 1410 to the 1720s. At the same time, canals in Holland routinely froze solid, glaciers advanced in the Alps, and sea-ice increased so much that no open water was present in any direction around Iceland in 1695. Aert van der Neer, Dutch, 1603-1688 Winter Scene with Frozen Canal

  37. Was The Sun Responsible for the Little Ice Age? • Maunder Minimum, the period with reduced sunspot number around 1,650 AD, was coincident with the little ice age of western Europe. • Does the reduced sunspot number imply reduced solar energy output, causing the temperature on Earth to drop? • Given the small amplitude of the total solar irradiance variation (0.1%), it is unlikely that the total solar irradiance variation is responsible for the global warming trend we have seen in the last 100 years. But the amplitude of the UV irradiance variation is much larger… • Solar UV radiation interact with Earth’s upper atmosphere. What’s the effect of solar UV variations on Earth’s climate?

  38. Solar UV Variation and Global Warming? From Haberreiter et al., Advances in Space Research 35 (2005) 365-369… 1. Introduction It is known that the variability of the solar UV irradiance has a considerable effect on the terrestrial atmosphere. Recently, Egorova et al. (2004) have shown that the introduction of solar UV flux into a spectral Global Circulation Model (GCM) with a chemistry transport model leads to an intensification of the polar vortex and a statistically significant warming of up to 1.2 K over North America and Siberia. Due to a missing longterm record of the solar UV irradiance with a sufficient temporal resolution,

  39. Like the effect of the increasing CO2 content in Earth’s atmosphere is still not clear, we do not understand the mechanisms that are causing the variations of the solar irradiance, nor do we understanding the details of how solar input affect the global climate.

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