| radius: |
6.96 x10*8 meters (100 times Earth's radius) |
| mass: |
1.99 x10*30 kg (330,000 times Earth's mass) |
| average density: |
1410 kg/m*3 (about the density of water) |
| surface temperature: |
5780K (about 10,000 degrees F) |
| luminosity: |
3.86 x 10*26 W (4-trillion-trillion 100W light bulbs) |
| angular size: |
0.5' (about the size of the tip of the little finger held at arm's length) |
| average distance from Earth: |
8.3 light minutes (the distance light travels in 8.3 minutes)
or 1 Astronomical Unit
or 93 million miles
or 150 million kilometers |
The
Sun is the star closest to us. It is the center of our solar system; all the planets orbit the Sun in elliptical
paths. The Sun is the powerhouse of energy that keeps the solar system running, and it produces the source for
order according to the laws of physics.
As with all stars, the Sun is, in general, a big,
burning ball of gas. The gas our Sun burns is
hydrogen. It is a G-type star on the Hertzsprung-Russell scale of spectra versus luminosity. The Sun's luminosity
is about the same as 4-trillion-trillion 100 Watt light bulbs buming each second. That figures to be an apparent
magnitude of -26.8 and an absolute magnitude of 4.8.
Since the Sun is the star we know best, it is the star we use as a standard for study of other
stars. We can directly observe what is going on with the Sun and can apply what we see to other stars, giving us
ideas of stellar processes and evolution.
How do we know what we know about the Sun? We cannot go to the Sun. Even if we could, its temperature
is about 6000 Kelvin (about 10,000 degrees Fahrenheit) and it has no solid surface. We would not survive. Instead,
we have to determine what is going on in the Sun using indirect means.
The Standard Solar Model
We have the Standard Solar Model. Examining the Sun layer by layer, we develop theories as to
what is happening, We observe what is going on on the outside of the top layer, and using those observations, the
laws of physics, and a bit of common sense, we can determine what conditions must be on the bottom.
Once we determine what the conditions must be on the bottom of the first layer, we go to the
next layer, since the bottom of the first layer is the top of the second layer. Then we go to the next layer, and
on and on, until we get to the core.
The Solar Core
The core of the Sun consists of fusing hydrogen. The fusion process is what gives the Sun its
energy. It fuses 600 million tons of hydrogen into 595 million tons of helium per second. That's a lot of energy!
The energy starts its million-year trek from the core to the surface through a series of processes.
First it is radiated. The energy transfer through the radiation zone is fast, so fast that it begins to build up
to the point where it becomes opaque to radiation. The electrons created from the fusion process become so dense
they have to use another means to be transported to the "surface" from that point.
The next energy transport is that of convection. Convection is the transfer of energy through
the movement of mass. The mass in this case is the dense amounts of electrons. It is hotter on the side toward
the core, and cooler toward the "surface." Heat tends to rise to a cooler region, where it becomes cooled
and sinks. Watch water boil; it has the same effect. The convection zone gathers the hot energy from the radiation
zone and "boils" it to the cooler outside layers of the Sun.
The Photosphere
Once the hot energy is taken to the top of the convection zone, the energy is given off to the
photosphere. This is the layer which represents the "surface" from our vantage point of Earth. Energy
is released in many forms from this point: heat, light at various wavelengths, and particles. The photosphere is
the layer of the Sun which contains visible markings such as sunspots and granulation. The photosphere is cooler
than the convection zone, but not as cool as the next layer.
Sun photo shot with 100 ASA Focal Color film at 1/125s, C-8,
aluminized mylar solar filter, Mayetta, Kans. 05/18/99.
The Chromosphere
The chromosphere is the next layer of the Sun. This is the layer close to the solar "surface"
that we see during an eclipse. We consider the chromosphere part of the solar atmosphere. It, too, has many features
we like to look at, such as spicules.
Next is the transition zone. We do not fully understand what is happening in this layer of the
solar atmosphere, but temperatures rise drastically in this zone. High amounts of energy are released from this
zone into the next layer.
The Corona
The corona is the next layer of the solar atmosphere. During solar eclipses, the corona illuminates
the area around the Sun as an eerie glow. The corona can restrict the energy flow from the Sun, or allow free-flowing
particles to escape through coronal holes at one million tons per second.
The ftee-flowing particles coming from the coronal holes go into the solar wind, which sends
the energy and particles out into the solar system, During high solar activity, many coronal holes are detected.
Particles the Sun emits interact with the geomagnetic fields of planets. The interaction sometimes causes aurora.
The Solar Wind
The solar wind is the last part of the solar atmosphere. It extends past the farthest reaches
of the solar system and is the result of the high temperature of the corona.
Escaping electromagnetic radiation (light) travels at the speed of about 500 km/s. At this speed they reach Earth
in just a few days.
The Sun is the powerhouse of our solar system. Without it, we would not exist.
Brenda Culbertson
Mayetta, KS 66509
stargazr@mail.holton.kl2.ks.us
