Skip this Video
Download Presentation
Click the mouse to advance

Loading in 2 Seconds...

play fullscreen
1 / 55

Click the mouse to advance - PowerPoint PPT Presentation

  • Uploaded on

Click the mouse to advance. with new images and information from NASA/ESA’s SOHO spacecraft. The Solar and Heliospheric Observatory. created by Steele Hill at Goddard Space Flight Center Greenbelt, MD. The Sun as photographed by the SOHO spacecraft in 1997.

I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
Download Presentation

PowerPoint Slideshow about 'Click the mouse to advance' - rocco

An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.

- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
the solar and heliospheric observatory
with new images and information from NASA/ESA’s SOHO spacecraft

The Solar andHeliosphericObservatory

created by Steele Hill

at Goddard Space Flight Center

Greenbelt, MD

the sun as photographed by the soho spacecraft in 1997

The Sun as photographed by the SOHO spacecraft in 1997

The Sun as revealed in extreme ultraviolet light. Differences in the Sun’s densities cause the uneven appearance on its surface.

the sun viewed in different ultraviolet wavelengths
The Sun viewed in different ultraviolet wavelengths
  • The Sun is revealed in three different wavelengths, each one showing cooler material than the one before it. These images were taken at nearly the same time on the same day.

• Note how certain features are revealed or hidden in different wavelengths.

Click on the image to view the clip

the sun s rotation
The Sun’s Rotation
  • Video of the Sun covering 12 days shows its rotation and some regions of activity. The Sun rotates about every 27 days.
  • The green color is added so that scientists can easily know which filter was used here.

Click on the image to view the clip

earth s size in relation to sun
Earth’s size in relation to Sun

The black dot represents the approximate size of the Earth.

  • Question:
  • About how many Earth’s do you think could fit inside the Sun?

The Sun is 865,000 miles in diameter or 110 Earths across.

real facts about the sun
Real facts about the Sun
  • is 93 million miles from the Earth
  • 1 second of its energy = U.S. energy needs for 90,000 years
  • light from the Sun gets to the Earth in 8 minutes
  • consists of 92% Hydrogen, 7% Helium, and 1% other gases
  • has an 11-year cycle of solar activity
  • is 5 billion years old, another 5 billion to go
  • is a medium-size star, one of about 2 billion in our galaxy

Click the mouse to add each bullet

fun facts about the sun
Fun facts about the Sun
  • The ancient Mayan, Egyptian, and other cultures worshipped the Sun.
  • We measure time by and base our calendar on the Sun. How long does it take for the Earth to go around the Sun?
  • Answer: 365 days or 1 year
  • If you drove a car at 100 miles per hour to the Sun, how many years would it take to get there? 5, 50 or 100.
  • Answer: About 100 years. Now that’s a long drive!

Most of us know that radiant energy from the Sun heats and lights the Earth, but did you know that:

Click the mouse to add each bullet

solar eclipses
Solar Eclipses
  • Eclipses occur when the moon blocks our view of the Sun from specific areas of the Earth. Here you see a relatively rare total eclipse, which lasted only about five minutes or less but reveals a detailed view of the corona.
stonehenge and the sun
Stonehenge and the Sun
  • Stonehenge in England, built about 3,000 years ago, is composed of 30 upright stones, each over ten feet tall, aligned in a circle, with horizontal stones perched upon them. There is also an

inner circle composed of similar stones. A mysterious site, many believe it served as a prehistoric astronomical observatory, especially for charting the Sun’s movements.

the sun is the source of all our energy
The Sun is the source of all our energy
  • Every second, millions of protons in the Sun's corecollide with other protons due to powerful pressures to produce helium nuclei in a fusionreaction that releases energy.

Neutrons + protons Helium nucleus + light and energy



Without the Sun’s heat and light,

life on Earth would not be possible.

what about solar energy
What about solar energy?
  • Solar energy is the least polluting and most inexhaustable of all energy sources, with great potential but still somewhat costly. The two most common systems heat buildings and create electricity. Most spacecraft use solar power for their instrumentation and communication.

The concept

The reality: solar panels

radiation in the sun s interior
Radiation in the Sun’s interior
  • This animation illustrates how the energy created by the extremely powerful fusion process in the Sun’s core radiates out through the radiation zone (bright yellow) to the convection zone (gold).

Click on the image to view the clip again

convection in the sun
Convection in the Sun

In the Sun’s outer layers, matter rises up and transports its energy from a hotter, lower level to a cooler, higher one. Thus, there is a constant circular rising and falling of gases in its convection zone.

Illustration of solar convection

the solar corona
The Solar Corona
  • The corona is the area just above the surface. While the surface is about 5,000o Celsius, the temperature in the corona reaches about 2 million degrees Celsius. What causes this rapid increase in temperature is not well understood.

5,000o C

2,000,000 o C

The black circle divides two images.

granulation on the sun s surface
Granulation on the Sun’s surface
  • The Sun’s surface pattern looks like rice grains. Large convection cells cause this granulation, since each cell has a column of hot gas rising and cool gas descending. Granules the size of Earth and larger constantly evolve and change in a churning kind of motion. This clip represents about four hours of activity.

Click on the image to view the clip

sounds of the sun
Sounds of the Sun
  • Waves of motion pushing out from within the Sun have actually been recorded as sound and converted to audible levels. Since we could not hear them as they are (too low a sound), they have been greatly raised in pitch. Listen closely . . .

The Sun hums along!

Click there to play the sound.

(The volume on your computer must be turned up.)

what is the solar wind
What is the solar wind?
  • A constant stream of particles flows from the Sun’s corona, with a temperature of about a million degrees and with a velocity of about 450 kilometers per second. The solar wind reaches out beyond Pluto's orbit (about 5900 million kilometers). The drawing showshow it pushes onand shapes the Earth’s magnetosphere(the dotted line).
the sun s magnetic field
The Sun’s magnetic field
  • The Sun is strongly affected by magnetic forces. The redarrows show open magnetic field lines emerging from the poles. The grayarrowsrepresent solar wind particles which carry field lines with it. The bright active regions have closed magnetic field lines (orange).
the sun s extended magnetic lines
The Sun’s extended magnetic lines
  • Some of the Sun’s magnetic field lines are closed (yellow, but others from the poles are open (red. Most are carried out into space by the solar wind (light dotted lines.
sun spots
Sun Spots
  • Darker and cooler areas are caused by a concentration of the Sun's magnetic field lines, which last from several hours to several months. Their frequency varies with the solar cycle (11 years), in 1997 near its minimum.

Light and dark in this magnetic scan of the Sun indicate concentrated areas of intense magnetic field lines.

Close-up of sunspots

polar coronal holes
Polar coronal holes
  • Shown with special filters in extreme ultraviolet light (the green tint is a false color). Hot gas flows out from the coronal holes (where magnetic field lines are open to space) into the solar wind.
multiple solar prominences
Multiple solar prominences
  • A fairly common occurrence, these eruptions are caused by magnetic forces. Cooler gases above the photosphere can often be seen flowing along magnetic field lines.

This is an active


prominences and magnetic loops
Prominences and magnetic loops
  • This image is tinted blue to identify to scientists which filter was used to create it.
large solar prominence
Large Solar Prominence
  • This is the largest prominence observed by SOHO. Twisting magnetic fields forced this huge eruptive prominence 100,000 kilometers above the Sun. The plasma is heated to about 150,000 degrees C.

28 Earths high

August 27, 1997

video clip showing solar activity
Video clip showing solar activity
  • The Sun is surprisingly active. The motion captured here occurred over a 12-hour period. The sliding movement of gases follows the lines of magnetic forces. You can also see the boiling type of motion on the surface.

Click on the image to play the video

comet hale bopp and aurora borealis
Comet Hale-Bopp and Aurora Borealis
  • Both these dramatic events, rarely seen together, are directly influenced by the Sun. Keep on going to find out how!
comets and the solar wind
Comets and the solar wind
  • By studying the tails of comets, scientists determined there must be a solar wind pushing out from the Sun because the tails always head away from the Sun. (Note the comet’s blue ion tail as well.)



sun grazing comet as it approaches the sun
Sun grazing comet as it approaches the Sun
  • A comet is seen entering from the lower left streaks towards the Sun on Dec. 23, 1996, and is presumably consumed by the heat soon after this image was taken. Solar particles can also be seen blowing out into space on the right side.

Click on the image to play the video

The clip spans about 3 days.

Note: the Sun is blocked by a disk but represented by the white circle.

auroral lights
Auroral Lights
  • They are also Northern or Southern lights. These often brilliant and colorful phenomena, seen in the night sky usually closer to the poles, are caused by the impact of solar wind particles and magnetic forces on the Earth’s magnetosphere.

Click on this image to play the video

aurora as seen from space
Aurora as seen from space

Aurora taken from the space shuttle

large coronal mass ejection cme sequence
Large coronal mass ejection (CME) sequence
  • CMEs are clouds of million degree Celsius gases ejected from the Sun at hundreds of miles per second. This one clearly heads off to the right. CMEs are caused by the breaking apart of magnetic forces. This sequence occurred over an 8-hour period in 1996.
another cme sequence
Another CME sequence

1 2

  • CMEs release a billion tons of matter at millions miles/hr.
  • CMEs occur almost every day but few are Earth-directed
  • a CME wave, moving through space, is preceded by a shock wave of matter pushed ahead of it
  • the bright spot (lower left in each) is Venus

3 4

cme shown in soft x rays
CME shown in soft X-rays
  • This dramatic footage taken by the Yohkoh spacecraft shows a very strong storm blasting particles out from the Sun over a 36-hour period.

Click on the image to view the clip again

solar flare and cme event
Solar flare and CME event
  • This video of an April 7, 1997 event captures the dynamics of a solar storm building up then flaring out over a 4-day period.
  • Solar flares are "explosions" on the Sun where tensions in the magnetic field are released. These generate a lot of energy that heats up material and shoots it into outer space. Solar flares are usually associated with active regions.

Click on the image to play the video

another view of april 7 cme event
Another view of April 7 CME event
  • This is a “running difference” video sequence where the imaging highlights the difference between each successive image so that the changes are easier to visualize. The Sun is blocked by a disk but represented by the white circle.

Click on the image to play the video

animation of a cme approaching earth
Animation of a CME approaching Earth
  • It takes 2 to 4 days for a CME blast to reach Earth, as it expands up to 30 million miles wide. The white lines represent the shape of Earth’s magnetosphere (magnetic field).

Click on the image to view the clip again

cme initial blast and later impact
CME: initial blast and later impact
  • This illustrates a CMEs progress from a blast on the Sun’s surface (lower left) to its impact on the Earth’s magnetosphere days later (drawing not to scale)
earth s magnetosphere and a cme
Earth’s Magnetosphere and a CME
  • Normal shape

Changed by CME

Electrically charged particles from a CME both compress and lengthen Earth’s magnetosphere. The particles are guided by Earth’s magnetic field lines into the polar regions.

cme impact on earth s magnetosphere
CME impact on Earth’s magnetosphere
  • Seen on Earth as aurora, the impact of a CME on Earth’s magnetic field is captured in an ultraviolet video from the perspective of a spacecraft. The red areas indicate the most intense magnetic activity.

Click on the image to play the video

some effects of cmes on earth
Some effects of CMEs on Earth
  • When CME’s interact with our magneto-sphere, strong magnetic changes occur, impacting a wide range of things. A CME knocked out power in Quebec in 1989 and interfered with communications.
how do some of these effects occur
How do some of these effects occur?

As a result of major magnetic storm activity:

  • When charged particles and radiation from a CME strike satellites, they can disrupt electronic equipment and even cause total failure. The atmosphere also heats and expands, increasing the drag on satellites in orbit around the Earth and changing their orbits.

Intense electric currents flow in the Earth’s atmosphere induces currents in pipelines (which act like electric conductors), causing increased corrosion of the pipeline.

Irregularities in the ionosphere (about 40-400 km above Earth) occur, disrupting radio signals passing through it to satellites and back, as well as Earth-to-Earth communications.

how can we prepare for cmes
How can we prepare for CMEs?

With greater reliance on technology for travel, communications, transportation, and power generation, we need to find ways to avoid damage and disruptions from CMEs.

  • Further improve space weather predictions
  • Build stronger satellites and more protected systems
  • Take operational precautions in response to warnings
  • NOTE: there is no human health risk from CMEs.

Click the mouse to add each bullet

the soho spacecraft
The SOHO spacecraft
  • Is a joint mission of NASA and the European Space Agency (ESA) to study the Sun for over 3 years
  • Has 12 instruments to study the Sun’s interior, atmosphere,and solar wind
  • Provided most of the images and video in this presentation

Click the mouse to add each bullet

soho s orbit
SOHO’s orbit
  • positioned about 1 million miles towards the Sunfrom the Earth
  • keeps that position as Earth orbits around the Sun
  • studies the Sun 24 hours a day without interference from the Earth’s atmosphere
x ray images of sun reveal changes
X-ray images of Sun reveal changes
  • The 12 x-ray images of the Sun's atmosphere, 1991-95 at 90 day increments, show how the corona changes during the solar cycle. Only very hot gases can emit x rays; the Sun's atmosphere, at millions of degrees, is hot enough to emit x rays;

the sun’s surface is not. As the solar activity cycle declines, the Sun's magnetic field changes from a complex structure to a simpler configuration.

This represents another way to study the Sun over time.

Taken by Yohkoh, an orbiting Japanese sun-study spacecraft.

the sun transformed through 3 wavelengths
The Sun transformed through 3 wavelengths
  • This video shows three different views of the Sun in different wavelengths of light captured by another spacecraft’s instrument. Layers are built out from the Sun’s photosphere (surface), to the chromosphere (lower atmosphere), and finally the corona (outer atmosphere).

Click on the image to view the clip

ground based observatories
Ground-based Observatories
  • Numerous observatories around the world continue to study and capture different images of the Sun.

National Solar Observatory (Sacramento Peak, NM)

Helium white light

image (Kitt Peak Observatory, NM)


image (Mauna Loa Solar Observatory,Hawaii)

H-Alpha white light image

(Learmonth, Australia)

soho s web site
SOHO’s Web site
  • Updated daily, the SOHO Web pages offer images, movies, information, exercises, links, and even a place to ask questions about the Sun.
  • Click on Teachers, and try out oureducational section!

Click the mouse to add each bullet

many related web sites can be explored
Many related Web sites can be explored
  • Windows to the Universe
  • • engaging Web-site that spans the Earth and Space sciences. Offers classroom activities and resources.
  • NASA’sEducation Program
  • • introduces educators to NASA’s extensive resources available
  • NASA’s Space Image Libraries
  • • a variety of sources for NASA’s space-related images
  • Views of the Solar System
  • • an educational tour of the solar system, with images and information about the Sun, planets, moons, asteroids, comets and meteoroids
new views of the sun poster
New Views of the Sun poster
  • Available for educators from NASA for free (lots of information and images on the back, too).
  • (See the accompanying handout for details)
stay tuned for more sun developments
Stay tuned for more SUN developments

Remember, it is dangerous to look right at the Sun, so DO NOT.