"The sun, with all those planets revolving around it and dependent on it, can still ripen a bunch of
grapes as if it had nothing else in the universe to do."
The Structure of the Sun
The sun is essentially a giant ball of gas and plasma that gets hotter and denser as you travel from the outer rim to the centre.
Temperatures run from a mere 5780K on the outer visible layer (the photosphere) to about 15 MILLION Kelvin in the middle!
(0K = - 273°C)
The core of the sun is the the real powerhouse. With temperatures at 15 million K and a density of 160,000 Kg/m3, this is the place
where the nuclear fusion that generates massive amounts of energy takes place.
The Radiative Zone
Between the core and the convective zone, the radiative zone extends to about 70% of the sun's radius. The energy flowing from the core
through the radiative zone, traveling in a very haphazard path, losing energy in the process.
The Convection Zone
The convection zone is a turbulent mass of material through which the radiation cannot pass as the temperature is too low (about 2 million K
at the bottom of the convection zone). The energy pouring from the radiative zone gets trapped and cannot escape, so giant convection currents
are set up with hot matter rising and the cooler matter sinking. This results in large bubbles of ionised gas rising through the convection zone,
reaching the surface in about 10 days. It help to imagine a boiling pot of water with hot rising bubbles and cooler sinking material. The
hot bubbles rise quickly to higher levels, cooling and expanding, just like hot air rising in the atmosphere of the earth. When it becomes
cooler that its surroundings, the gas sinks to become reheated and rise again. In this way rolling currents of hot and cold gas create a
churning motion that carries heat from the bottom to the top. It seems that largest currents of gas and heat generate myriad smaller ones and these
manifest themselves as the granulation we can see in white light and H-Alpha.
Sunlight as we know it - the visible white light, is emitted from the photosphere.
The photosphere is one of the coolest regions of the Sun (about 6000 K), and it is here that we can see the granulation caused by the
bubbling gas in the convection layer and the sunspots caused by strong magnetic fields.
The chromosphere is 2000-3000 km thick and the temperature rises from around 6000k to 20,000K.
These high temperatures result in hydrogen
emitting a reddish light (H-alpha emission
) and can be seen in the exciting prominences that project from the sun and in the thin reddish line that
can sometimes be seen as a 'rim' round the dark disk of the moon inside the corona. It is this colour that gives the chromosphere
its name (color-sphere). The image to the left of a total solar eclipse demonstrates the colouring of the chromosphere.
The chromosphere contains spikes of gas called spicules that rise through it. Spicules are short-lived
phenomena, corresponding to rising jets of gas that move upward at about 30km/sec and last only about 10 minutes.
This is the outer layer of the sun and is the whitish halo seen around the disc in a total solar eclipse. This can be seen in the picture
of the solar eclipse above. Temperatures range from 2 to 3 million °.
The corona can exhibit coronal holes which can be seen in the
spectacular x-ray image of the sun (right). It is from these 'holes' that a high velocity solar wind emanates. The wind consists of high speed
particles streaming from the sun and can be viewed as an extension of the the corona into interplanetary space.
Coronal Mass Ejections
Coronal mass ejections occur when the confined solar atmosphere can suddenly and violently release bubbles or
tongues of gas and magnetic fields. These result from a change in the magnetic field. If one of these coronal mass ejections
erupts towards the earth it can effect electromagnetic equipment. Satellites are particularly vulnerable. However, the really
exciting effect of a coronal mass ejection coming our way is the auroras that we see usually nearer the poles. In April 2000 a spectacularly
big CME brought the aurora down as far as the south of England.
Pictures take at Hampshire Astronomy Group Observatory in April 2000 by Ninian Boyle
A Brilliant Book
In September of 1859, the entire Earth was engulfed in a gigantic cloud of seething gas, and a blood-red aurora
erupted across the planet from the poles to the tropics.
Around the world, telegraph systems crashed, machines burst into flames, and electric shocks
rendered operators unconscious. Compasses and other sensitive instruments reeled as if struck
by a massive magnetic fist. For the first time, people began to suspect that the Earth was not
isolated from the rest of the universe. However, nobody knew what could have released such strange
forces upon the Earth--nobody, that is, except the amateur English astronomer Richard Carrington.
In this riveting account, Stuart Clark tells for the first time the full story behind Carrington's observations of a mysterious explosion on the surface of the Sun and how his brilliant insight--that the Sun's magnetism directly influences the Earth--helped to usher in the modern era of astronomy. Clark vividly brings to life the scientists who roundly rejected the significance of Carrington's discovery of solar flares, as well as those who took up his struggle to prove the notion that the Earth could be touched by influences from space. Clark also reveals new details about the sordid scandal that destroyed Carrington's reputation and led him from the highest echelons of science to the very lowest reaches of love, villainy, and revenge.
The Sun Kings transports us back to Victorian England, into the very heart of the great nineteenth-century scientific controversy about the Sun's hidden influence over our planet.
Visible Features of the Sun
You can view the sun as a projection, through a white light filter, or through a Hydrogen Alpha telescope or filter.
* * * * *
NEVER NEVER look directly at the sun with your eyes or through any magnifying equipment (telescope, binoculars) that has not been
It could be the last thing you see!
* * * * *
A full disc image of the sun taken by Jack Newton on a Solarview 50 Telescope, showing
the main features that are visible in hydrogen alpha
. Sunspots are the only
features readily visible in white light, but you can occasionally see faculae and flares.
Sunspots are the dark spots you can see when you look at the sun in white light (through an
appropriate filter) or when you project an image of the sun on to a screen. The picture shows
sunspots on the surface of the sun as viewed in hydrogen alpha.
These spots are dark because they are cooler than their surroundings (a mere 4000K or so, compared
to the 5780K of the surrounding photosphere - K is degrees Kelvin. IK = 1°C and 0K = 273°C,
so to convert K to °C just add 273.)
The sun generates very strong magnetic fields, and it is a localised concentration of these
magnetic fields that causes the cooling that we see as sunspots. Sunspots usually occur in
pairs or groups of opposite magnetic polarity that move in unison across the face of the sun
as it rotates. They can last anything from a few hours to a few weeks, or even months for the
very biggest. Interestingly sunspot activity exhibits an 11 year cycle in terms of the position
and number of spots.
The glowing region around the sunspot (seen in the picture above) is called Plage (from the French
for beach). They always appear with a sunspot but can outlive them. They are bright dense
regions of the chromosphere.
You can find out more about actually observing the sun and how to do it SAFELY in one of the FREE bonuses
you can get with Ninian's online Astronomy Course
Basic Astronomy with a Telescope
Faculae are bright areas in the photosphere that are visible near the limb, or edge, of the
solar disk. They appear a few hours before a sunspot that arises in the same place
and can remain for months after the sunspots have gone. They are also the result of the
magnetic fields produced by the sun, being areas where the magnetic field is concentrated in
much smaller bundles than in sunspots. While the sunspots tend to make the Sun look darker,
the faculae make it look brighter. The word facula comes from the Latin for 'Little Torch'.
A Prominence is an elongated structure full of material hundreds of times cooler and denser
than the surrounding corona. They are held up and insulated by huge magnetic structures and
are seen as prominences at the edge of the sun against the black background of space. They can
stay suspended above the photosphere for weeks and even months, but eventually become unstable.
Surprisingly, rather then collapse at that point, they actually erupt!
Filaments are prominences that are within the disc of the sun as we view it, and so are seen
as dark lines of cool matter and against the hotter bright chromosphere behind.
Solar flares are huge explosions on the surface of the sun, throwing out massive amount of material
as matter is heated to millions of degrees in a few minutes. It can last from minutes to hours.
A collection of granules - a bright region or cell ( about 1000 km across), which cover the
entire Sun except for those areas covered by sunspots. They are formed by hot gases rising
to the photosphere, spreading and cooling and falling back again - hence the bright centre and
darker edges. Individual granules last for only about 20 minutes so the pattern of granulation
is continually changing as old granules are pushed aside by newly emerging ones.
The flow within the granules can reach supersonic speeds of more than 7 km/s
(15,000 mph) and produce sonic "booms" and other noise. Shown on the right in H-Alpha, granulation
can be seen in white light as well.
Coronal Mass Ejection
Often associated with flares and prominences, a coronal mass ejection (CME) is the release
of a huge amount of coronal material - measured in billions of tons and traveling at