SOLAR WIND & INTERACTION
WITH THE SOLAR SYSTEM &
INTERSTELLAR SPACE
Astronomy Power Point Presentation
WeEXCEL
By Wayne King
Miamisburg High School
May 12, 2008
LESSON PLAN - SOLAR WIND & EFFECTS UPON THE SOLAR
SYSTEM & INTERSTELLAR MEDIUM
OBJECTIVE:
Students will understand the concept Solar Wind, its composition, it origin, how it
interacts with the Earth and interstellar medium. This will be evidenced by at
least a standard deviation increase in the post test grade over the pretest using
the pretest standard deviation.
•Students will be given challenging information that will enhance their
understanding of traditional concepts and see applications to previously learned
material.
• The Solar Wing Project will be given to freshmen and upper class students to
see if there is a significant difference between the three groups
•Physical World students – 9th graders
•Astronomy students – 11th and 12th graders but not strong students
•Honors Physics students - 11th and 12th graders who are strong
students
STANDARDS:
• Physical World – 9th grade Physical Science Standards
Standards A, D, E, F, G, H
• Honors Physics and Astronomy – 11th & 12th grade Physical Science Standards
Standards A, C, D, E
RUBRIC - SOLAR WIND & EFFECTS UPON THE SOLAR SYSTEM
& INTERSTELLAR SPACE
OBJECTIVE: Students will do the following tasks in this project and will receive two
test grade.
•
Take a pretest quiz – Counts as 10% of test grade
•
Watch a 120+ slide power point presentation
•
Write a 1000 word report (750 word for freshmen) – counts as one test grade
•
Actually half the report is due after sections 1&2 and the other
half after section 3
•
Do a group discussion on a set of questions given the group / one written paper
will be submitted for the entire group – counts as a homework grade
•
Physics class will do a calculation assignment over the many physics aspects of
this topic
•
Take a post test – counts as 90% of test grade
Include all (51) words in report
Alpha particle
Auraora
Bow Shock
Chromosphere
Convection Zone
Coriolis Effect
Corona
Coronal Hole
Coronal Mass Ejection
Cosmic Rays
Dark Dust Cloud
Doppler Effect
Dynamo Process
Electrojets
Electromagnetic Spectrum
Emission Spectrum
Flux
Heliopause
Heliosheath
Heliosphere
Heliospheric Current Sheet
Interplanetary Medium (dust & gas)
Interstellar Medium (dust & gas)
Ion
Magnetic Mirror
Magnetic Reconnection
Magnetic Tail
Magnetohydrodynamic
Magnetopause
Magnetosphere
Maxwell-Boltzmann Distribution
Molecular Cloud Complex
Ohm’s Law
Parsec
Photon
Photosphere
Physics Equations applied to
presentation
Plasma
Polar wind
Polarization
Primordial Nucleosynthesis
Prominence
Radiation Zone
Red Shift & Blue Shift
Ring Current
Solar Wind
Spicules
Sun Spots
Termination Shock
Tesla
Van Allen Radiation Belts
Pretest – Post test
[SCANTRON]
Solar Wind Project
1. How long does it take the Solar Wind to reach Earth?
a. 8 minutes
b. 8 hours
c. 8 days
d. 8 years
2. Coronal Mass Ejections is another name for the Solar Wind. [T/F]
3. Which are not a part of the solar wind?
a. protons
b. alpha particles c. photons
d. neutrons
e. Both c & d
4. In the radiation zone of the sun what condition exists?
a. there are no electrons attached to the nuclei
b. Most electrons are attached to nuclei
c. photons are attached to nuclei
d. none of these
5. What zone of the sun has the photons being absorbed and re-emitted 1025 times
before they leave the sun’s surface?
a. Chromosphere b. Corona
c. Convection
d. Radiation
e. Photosphere
6. The Granules seen as satellites look down upon the sun are actually located in
which zone of the sun?
a. Chromosphere b. Corona
c. Convection
d. Radiation
e. Photosphere
SOLAR WIND & INTERACTION
WITH THE SOLAR SYSTEM &
INTERSTELLAR SPACE
Astronomy Power Point Presentation
WeEXCEL
By Wayne King
Miamisburg High School
May 12, 2008
Table of Contents
1. The Solar Wind and its origin
2. Comparison of the Interplanetary Medium with
the Interstellar Medium and its interactions at
the fringe of our Solar System
3. Earth’s magnetism, Magnetosphere and
interaction with the Solar Wind
1. The Solar Wind and its Origin
At the base of the Convections Zone the gas cells
are about 30,000 km across and at the top 1,000 km
 It is from the convection cells that the solar wind
begins its journey, first to the Corona and then
through the solar system to interstellar space.
 This diagram shows
the temperature increase
in the three zones above
the Photosphere.
 The temperature at
the Photosphere is 5800
K and it drops to 4500 K
in the Choromosphere.
 The temperature soars to over a million K at
10,000 K and readings of 100 million K have been
obtained by SOHO and other solar satellites.
 Astronomers believe that magnetic effects like
those that cause spicules plus prominences and
solar flares are responsible for these temperatures.
The Physics of the Solar Wind

Kinetic Energy = Thermal Energy
 For a gas molecule or particle
½ mv2 = 3/2 kTK
where:
m = mass of particle
v = velocity squared
k = Boltzmann’s Constant
k = 1.3806 x 10-23 J/K
TK = Temperature in Kelvin’s
 Notice that temperature (TK) is proportional to the velocity
(v)
 The higher the temperature the greater the velocity and it
escapes the gravitational and magnetic pull of the sun
2. The Solar Wind’s effects Upon The
Solar System and Interstellar Medium
 Bow Shock: The point where the interstellar medium, travelling in the
opposite direction, becomes subsonic as it collides with the Heliosphere and
the interstellar medium particles are no longer as energetic.
 Outside the Heliopause, is the turbulent region caused by the pressure
of the advancing interstellar medium against the Heliopause.
 The picture to the right should be reversed to be consistent with the
directional orientation of the first picture.
 This picture shows the make-up of
interstellar space and the difficulty in analyzing
radiant energy received in our telescopes and
spectroscopes.
 The various mediums that the EM radiation
goes through effects the results received as it
goes through the two clouds.
 This contour map shows Formaldehyde molecules,
especially abundant in the darkest interstellar regions and
decreasing as we move in toward the center.
 The green and red lines show the Formaldehyde (H2CO)
at two different frequencies of rotation.
 Other kinds of molecules are found to be similarly
distributed. (cyanide HCN, ammonia NH3, water H2O, etc.)
 As the molecular Formaldehyde changes from the
rapid rotation on the left to the slower rotation on the
right, a photon is emitted that can be detected by a
radio telescope on Earth.
Interstellar Medium - (Continued)
 As a result of primordial nucleosynthesis, the gas is roughly
90% hydrogen and 10% helium by number of nuclei, with
additional heavier elements present in trace amounts.
 There is no contradiction when it was stated that by mass
hydrogen is 75% and helium is about 25% of the interstellar gas
with minor amounts of heavier atoms.
 Primordial Nucleosynthesis refers to the production of elements
heavier than hydrogen by nuclear fusion, but NOT inside of stars,
right after the Big Bang.
 About 2 minutes after the Big Bang was it cool enough for
deuterium (H-2) to stabilize and begin synthesis into heavier
elements such as alpha particles by the fusion process. There was
still great pressure and KE while no stars were present.
The Maxwell–Boltzmann
distribution is a probability
distribution with applications in
physics and astronomy.
The temperature of any
physical system is the result of
the motions of the molecules
which make up the system.

These particles have a range of different velocities, and the
velocity of any single particle constantly changes due to collisions
with other particles.
Shown above is the range of velocities for four Noble Gases at
the temperature of 25 C. Notice that the more massive particles
(Xe) has the slowest velocity and the speeds are grouped close
together as compared with He which is faster and spread out.
3. THE MAGNETOSPHERE OF THE
EARTH AND ITS INTERACTIONS
WITH THE SOLAR WIND
 The top picture shows the differential rotation of
the inner core and that of the outer core where the
inner core takes 2/3 of a second less per day to
complete one daily rotation than the rest of the
Earth.
This means it gains a quarter of a turn each
century.
 There is a rapidly moving jet stream of partially
molten matter, “a mushy zone”, between the two
cores helping the inner core to “super-rotate” as
shown in the “red” in the bottom picture.
 The P-waves (longitudinal pressure waves) can
pass through the core region and these waves,
resulting from earthquake activity, are gradually
shifting eastward in the direction of the core rotation.
This implies that the inner core has a faster
rotation than the rest of the planet.
Notice the quarter of a rotation increase since
1900 which is a shift of 1o per year relative to
the crust above.
The arrows of the
magnetosphere
are correct.
To be correct the
poles of the
magnet must be
reversed.
 The first rigorous study of the Earth’s magnetism was done by W. Gilbert's "De
Magnete," written in the reign of Elizabeth I at the end of the 16th century. He realized
that the Earth was a giant magnet with a dipolar magnetic field.
It was realized not long afterward that the internal magnetic field varied with time as
the table shows.
While at present the principal variation is a eastward drift of 45o in 440 years.
 The magnitude has diminished by 18.8% in the same period of time.
The tilt angle from the axis of rotation has increased by 8.4o to 11.5o and is
decreasing again to 10.8o and if the pattern is continues it is probably at 10.6o
today.
 Both pictures to the left show the solar
wind being diverted and the Earth
protected by its magnetosphere.
 The picture to the upper right shows the
two Van Allen Radiation Belts surrounding
the Earth. These are a torus of energetic
charge particles (plasma) around Earth,
held in place by Earth's magnetic field.
 The inner belt 1.1 - 3.3 Earth radii,
contains primarily protons
 Outer belt 3 - 9 Re contains electrons
MAGNETIC RECONNECTION
 This picture presents a new finding where Magnetic Reconnection occurs at
about 100 Earth diameters from the Earth.
The typical end to the Magnetosphere is about 60 Earth radii.
 A Reconnection Zone has
been discovered where
electrons are energized and
excited to almost the speed of
light (2.41 E8 m/s which is
80% the speed of light).
 It is the Magnetic
Reconnection model that is
believed to occur on the sun
with solar flares explaining
how they obtain such high
energy (T=100 million K) as
compared to the surface of
the sun (T=5800 K).
 To the left are the Aurora Ovals
 Below are various auroras
GROUP DISCUSSION QUESTIONS
Names_________________________
Period ____
Directions: Students will get into their groups and discuss the following questions. The
“Recorder” will write down all the answers given by the members of the group on
this paper. All group members will receive the same class-work grade. Only one
paper is to be turned in per group. The teacher will discuss these answers at the
end of the period as a check on your work.
1) Discuss what is the Solar Wind? Identify all the components that make up the
Solar Wind.
2) Discuss the various ways that the Solar Wind is released from the sun.
3) Discuss the role of Magnetism with the Solar Wind.
4) Discuss as many facts as possible about the Interplanetary Medium.
(14 Total Questions)
Honors Physics – Solar Wind Worksheet
Name _________________________
Solve each problem showing all your work with at least 3 digit accuracy.
7) Given the Coriolis Equations:
a. [ac = -2ω x v where x is a cross product meaning to multiply by sinθ]
b. [Fc = -2mω x v]
c. [Coriolis Parameter f = 2ωsinθ]
d. [Rossby Number Ro = v/fL]
__________________Determine the acceleration of a 250 kg missile, with a
velocity of 160 m/s being shot from Miamisburg (latitude 40o and longitude
84o) to a point on the equator west of Miamisburg with a latitude 0o and
longitude of 200o. [ Note: Be careful of the angle determination - Assume the
Earth is perfectly round with a radius of 6.38 E6 m and ω is determined by what
you know about a day on the Earth]
__________________What distance would you miss the target by if you did not
take the proper corrective action? (How many meters East or West of the target
on the equator?) State the direction you would miss by along with the distance
in meters.
__________________Determine the Coriolis Force acting upon the missile.
__________________Determine the Rossby Number and interpret this number as
to what it implies and give the reason for your statement.
FRESHMEN – PHYSICAL WORLD RESULTS
Pretest
Post
test
Percent
20905
23
29
6
16925
14
29
15
21651
13
28
14
Percent
Percent
Difference
15491
9
28
19
15103
32
64
31
113019
11
26
15
15292
17
51
34
15131
18
26
8
13699
25
51
26
123166
9
26
17
103290
21
44
23
15083
24
25
1
15355
35
44
9
15802
18
25
7
22146
15
44
28
16307
12
24
12
15224
11
44
33
15216
7
24
17
15300
22
43
20
16794
13
23
9
17985
12
41
29
114905
12
23
11
21337
15
40
25
21514
16
21
5
20385
18
39
21
15600
11
21
10
20009
15
39
24
14948
11
21
10
21197
34
38
4
123189
12
20
8
15233
19
38
18
14083
13
19
6
19843
10
38
28
15369
14
19
5
15287
22
36
14
15311
18
15
-3
15080
14
36
22
15262
15
33
18
15293
0
31
31
15537
10
31
21
15817
15
30
15
Average
16.17
32.20
16.03
50747
25
29
4
7.03
10.48
9.48
STD
Astronomy
ID #
Pretest
Percent
Post
test
Percent
Pretest
Post
test
Percent
Percent
Percent
Increase
12574
53
46
-7
22204
50
83
33
23686
49
45
-4
21604
48
28
-20
18793
47
44
-3
13247
42
56
14
13067
40
65
25
ID #
Percent
Increase
Honors Physics
15409
15
29
14
17435
34
40
6
19898
36
61
25
11968
18
29
11
24716
35
58
23
23699
15
39
24
11669
34
65
31
18299
32
46
14
21603
32
49
17
16660
38
54
16
11398
32
70
38
17617
21
20
-1
19906
30
55
25
24834
38
51
14
16590
29
46
18
12178
0
25
25
15739
28
45
17
11837
40
50
10
14505
26
60
34
11856
16
0
-16
21613
21
50
29
1032
15
23
8
11444
13
64
51
Average
23.35
33.75
10.40
Average
35.74
54.93
19.19
STD
12.49
15.87
11.03
STD
10.94
12.44
17.88
Comparisons
Average
35.74
54.93
19.19
STD
10.94
12.44
17.88
Astronomy
Average
23.35
33.75
10.40
STD
12.49
15.87
11.03
Physical World
Average
16.17
32.20
16.03
7.03
10.48
9.48
Honors Physics
STD
CONCLUSIONS ????