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The Sun

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Title: The Sun


1
The Sun
2
Sun Fact Sheet
The Sun is a normal G2 star, one of more than 100
billion stars in our galaxy. Diameter
1,390,000 km (Earth 12,742 km or nearly 100 times
smaller) Mass 1.1989 x 1030 kg (333,000 times
Earths mass) Temperature 5800 K (surface)
15,600,000 K (core) The Sun contains more than
99.8 of the total mass of the Solar System
(Jupiter contains most of the rest). Chemical
composition Hydrogen 92.1 Helium 7.8 Rest
of the other 90 naturally occurring elements
0.1
3
General Properties
4
The Sun and its Planets to Scale
5
Energy is created in the core when hydrogen is
fused to helium. This energy flows out from the
core by radiation through the radiative layer, by
convection through the convective layer, and by
radiation from the surface of the photosphere,
which is the portion of the Sun we see.
6
Chapter 10The Sun, Our Star
  • The Sun support life on Earth
  • The Sun provides energy for photosynthesis, which
    releases oxygen into the atmosphere.
  • The greenhouse effect trap some of the solar
    energy on Earth, keeping it warm (at the right
    temperature for us).
  • The Sun ultimately determines the fate of the
    life on Earth.
  • The Sun is the only star that we can study in
    details.
  • The Sun is the test bed for our theory of the
    stars.

7
Activities of the Sun
  • General Properties
  • Luminosity
  • Solar Energy
  • Internal Structure
  • Solar Atmosphere
  • Surface Features
  • Magnetic Fields
  • Solar Activities
  • Solar Cycle

8
Luminosity, Watts, Joules, and Calories
  • Luminosity
  • The energy an object radiates per unit time. So,
    it is a measure of power.
  • Watt
  • Unit of power. One watt is one Joule per second.
  • Joule
  • Unit of energy.
  • Lifting a 1 kg (2.2 lb) mass up by 10 cm (4
    inches) on the surface of Earth would requires 1
    joule of energy.
  • Accelerating a 2 kilograms (4.4 Pounds) mass from
    rest to a speed of 1 m/sec (2.25 miles/hour)
    requires 1 joule of energy.
  • 1 Calories 4.2 Joules. ( a calorie is the
    amount of energy required to raise the
    temperature of one kilogram of water by one
    degree Celcius.
  • The Sun generates 9 ? 1025 calories of energy
    every second, or
  • 90,000,000,000,000,000,000,000,000 calories per
    second.

9
The Energy Source of the Sun
  • Before Einsteins special theory of relativity,
    the most plausible theory for the generation of
    the energy in the Sun was gravitational
    contraction
  • as the solar nebula collapses due to the
    gravitational pull of the denser core region,
    gravitational potential energy is converted into
    thermal energy. However, according to
    calculation, the Sun can sustain its energy
    output for only about 25 million years if
    gravitational potential energy is the source of
    the solar energy.
  • Today, we understand that the energy source of
    the Sun is the nuclear fusion process which
    combines hydrogen nuclei to form helium, and at
    the same time releasing a very large amount of
    energy per reaction. The increase of temperature
    at the center of the Sun due to gravitational
    contraction eventually trigger nuclear fusion,
    which converts some of the mass into energy,
    according to Einsteins mass-energy equation, E
    mc2.

This is a simplified picture thats not exactly
correct. Electric charge is not conserved!
10
The Internal Structure of the Sun
  • Core
  • The region where nuclear fusion takes place to
    generate the solar energy.
  • T 15 million degrees K.
  • Radiation Zone
  • Energy is transported outward primarily by
    photons traveling through this region.
  • T 10 million degrees K and decreases outward.
  • No nuclear fusion.
  • Convection Zone
  • Energy is transported through convection hot gas
    rises, irradiates their energy, and becomes cold.
    Cold gas sink to the bottom.
  • Example at home boiling water.
  • Example at play glider and hang-glider.

11
The Equilibrium Between Gravity and Pressure
The temperature and density inside the Sun
increase due to gravitational contraction.
Without a force to counter gravitation force, the
Sun will continue to contract. However, as the
Sun contracts, the density and temperature of the
interior also increase. This increases the
thermal pressure of the interior, pushing outward
against the gravitational force.
  • Gravitational force pulls the gas inward
  • Thermal pressure push the gas outward
  • When inward gravitational force is equal to the
    outward push of thermal pressure, the size of the
    Sun remains constant
  • If the mass of the Sun is high enough, the
    internal pressure and temperature can be high
    enough for nuclear fusion to begin

12
Why Does Nuclear Fusion Occurs Only at the Center
of the Sun?
  • Temperature Density
  • Temperature is a measurement of the average
    kinetic energy of the particles.
  • A volume of gas at very high temperature means
    that the particles of the gas move at very high
    speed.
  • The very high speed is needed to overcome the
    repulsive electromagnetic force between the
    protons to get them very close to each other.
  • High density is necessary so that the probability
    of fusion is high.
  • Once the protons are close to each other, the
    strong nuclear force can bind them together to
    make a new and heavier element.

Click on image to start animation
13
Nuclear Fission and Fusion
  • Nuclear Fission
  • The process of splitting an atomic nucleus is
    called nuclear fission.
  • Our nuclear power plants generate power by
    splitting large nuclei such as uranium or
    plutonium into smaller ones.
  • Nuclear Fusion
  • The process of combining (or fusing) two small
    atoms into a larger one

14
Proton-Proton Chain
  • There are many different fusions that can take
    placefor example,
  • The predominant fusion process in the core of the
    Sun is the proton-proton chain
  • Proton-Proton chain fuses four protons into one
    helium,

Click on picture to start animation
15
How does the energy generated at the center get
to the surface and to us?
  • The energy generated by the nuclear fusion
    process is released in the form of photons
    (radiative energy). The photons interact with the
    solar plasma (mostly with the electrons). Each
    time a photon encounters an electron, it changes
    its direction. Thus, the photons go through a
    zigzag path to the surface. It takes about 1
    million years for a photon to travel from the
    center of the Sun to its surface.
  • Because of all the interactions along the way,
    the photons lost memory about the core where they
    originate
  • At the upper portion of the solar interior,
    convection is the more efficient energy transport
    mechanism to get the energy to the surface.

The random walk of photon to the surface.
16
The Solar Thermostat
  • Nuclear fusion is the source of all the energy
    the Sun releases into space. The Sun fuses
    hydrogen at a steady rate, because of a natural
    feedback process that acts as a thermostat for
    the Suns interior.
  • Because the nuclear fusion rate is very sensitive
    to temperature, if the temperature of the core
    increases by some amount, the fusion rate would
    go up very rapidly, generating a large amount of
    energy.
  • Because the energy is transported slowly to the
    surface, this extra energy will pile up in the
    interior, causing the temperature and the
    pressure to increase.
  • The increased pressure pushes the envelop to
    expand and cool, reducing the fusion rate.
  • If the temperature is decreased below its steady
    state value, the reverse would happenthe
    decrease core temperature would reduce the fusion
    rate, causing the core to contract. The
    contraction in turn increases the temperature and
    pressure, restoring the fusion rate

17
Energy from the Sun passes through an imaginary
disc that has a diameter equal to the Earth's
diameter. The flux of energy through the disc is
1370 watts per square meter. The amount of energy
that hits a square meter on the Earth's surface
is maximum at the point where the incoming
radiation is perpendicular to the Earth's surface.
18
The seasons occur because the tilt of the Earth's
axis keeps a constant orientation as the Earth
revolves around the Sun. A. Summer in northern
hemisphere. B. Winter in southern hemisphere
19
Sun does not rotate as a rigid sphere. The
equator of the Sun rotates faster than the poles
of the Sun. This is called the differential
rotation. Sunspots and many other solar
activities are due to this differential rotation.
20
Internal Rotation
False color image showing a theoretical model of
relatively hotter (red) and colder (blue) regions
in the solar interior. The red layer may be a
shear region between the radiative and
convective zones, powering a dynamo that gives
rise to the Suns magnetic field.
21
Suns Magnetic Field
The Sun's corona is threaded with a complex
network of magnetic fields. Solar storms and
flares result from changes in the structure and
connections of these fields.
When some of the Sun's magnetic field lines are
filled with hot gas, we see a magnetic loop.
22
X-ray images of the Sun taken by the Yohkoh
spacecraft, showing changes in the corona in
1991 (left) at a solar maximum to 1995, a solar
minimum (right).
The most rapid changes to the Sun's magnetic
field occur locally, in restricted regions of the
magnetic field. However, the entire structure of
the Sun's global magnetic field changes on an 11
year cycle. Every 11 years, the Sun moves through
a period of fewer, smaller sunspots, prominences,
and flares - called a "solar minimum" - and a
period of more, larger sunspots, prominences and
flares - called a "solar maximum. After 11
years, when the next cycle starts, the magnetic
field poles are reversed. The last solar minimum
was in 2006
23
Sunspots
Sunspots appear as dark spots on the surface of
the Sun. Temperatures in the dark centers of
sunspots drop to about 3700 K (compared to 5700 K
for the surrounding photosphere). They typically
last for several days, although very large ones
may live for several weeks.
24
Spectrum analysis shows that sunspots have strong
magnetic field, about 1000 times stronger than
the Sun's average. Sunspots usually appear in
pairs. The two sunspots of a pair have different
polarities, one would be a magnetic north and the
other is a magnetic south, and can be joined by
magnetic field lines. The strong magnetic field
locks the gas of the photosphere in places and
inhibits the hotter gas below to rise at the
sunspots. As a result, the sunspots are cooler.
Sunspots appear to coincide with changes in the
climate of the Earth. Studies show that during
the last ice age, there were very few sunspots
25
The sunspot cycle over the past 400 years. Note
the period before 1700, when, for reasons that
are not understood, very few sunspots were
observed. Sunspots have reached a maximum about
every 11 years since 1700, and there is also a
suggestion of some sort of cycle on a 55- to
57-year time scale. Because the pre-1700 period
of low sunspot activity coincides with a
prolonged cool period that is sometimes called
the Little Ice Age, some scientists have
speculated that sunspot activity and climate are
connected somehow.
26
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27
Granules
Convection from inside the sun causes the
photosphere to be subdivided into 1000-2000km
cells.
Energy rises to the surface as gas wells up in
the cores of the granules, and cool gas sinks
around their edges.
28
Solar Prominences
Prominences are dense clouds of material
suspended above the surface of the Sun by loops
of magnetic field. Prominences can remain in a
quiet or quiescent state for days or weeks.
However, as the magnetic loops that support them
slowly change, prominences can erupt and rise off
of the Sun over the course of a few minutes or
hours
29
Solar Flares
Solar flares are tremendous explosions on the
surface of the Sun. In a matter of just a few
minutes they heat material to many millions of
degrees and release as much energy as a billion
megatons of TNT. They occur near sunspots,
usually along the dividing line (neutral line)
between areas of oppositely directed magnetic
fields.
Images from SOHO
NASA/ESA Solar and Heliospheric Observatory
spacecraft
30
Coronal Mass Ejections (CMEs)
Coronal mass ejections (CMEs) are huge bubbles of
gas threaded with magnetic field lines that are
ejected from the Sun over the course of several
hours.
CMEs disrupt the flow of the solar wind and
produce disturbances that strike the Earth with
sometimes catastrophic results.
31
Corona and Solar Wind
The Suns Corona is forever expanding into
interplanetary space filling the solar system
with a constant flow of solar wind.
Solar wind is the continuous flow of charged
particles (ions, electrons, and neutrons) that
comes from the Sun in every direction. Solar
wind consists of slow and fast components. Slow
solar wind is a consequence of the coronas high
temperature. The speed of the solar wind varies
from less than 300 km/s (about half a million
miles per hour) to over 800 km/s.
32
Solar wind shapes the Earth's magnetosphere and
magnetic storms are illustrated here as
approaching Earth. These storms, which occur
frequently, can disrupt communications and
navigational equipment, damage satellites, and
even cause blackouts. The white lines represent
the solar wind the purple line is the bow shock
line and the blue lines surrounding the Earth
represent its protective magnetosphere.
33
Wednesday, 24 September 2008 1419 UK
Solar wind blows at 50-year low
The solar wind - the stream of charged particles
billowing away from the Sun - is at its weakest
for 50 years. Scientists made the assessment
after studying 18 years of data from the Ulysses
satellite which has sampled the space environment
all around our star. They expect the reduced
output to have effects right across the Solar
System. Indeed, one impact is to diminish
slightly the influence the Sun has over its local
environment which extends billions of kilometres
into space. The charged wind particles also
carry with them the Sun's magnetic field, and
this has a protective role in limiting the number
of high-energy cosmic rays that can enter the
Solar System. More of them will probably now make
their way through.
34
Hertzsprung-Russell diagram of star luminosity
versus surface temperatures. The vertical axis is
a comparative one based on the Sun having a
luminosity of 1. The horizontal axis is reversed
from the normal order, with values of surface
temperature increasing to the left. Note that the
Sun is a middle-range, main-sequence star.
35
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36
Anticipated Future of the Sun
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