Module 2 Lab #4 Our Sun
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School
Red Rocks Community College *
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Course
1032
Subject
Astronomy
Date
Dec 6, 2023
Type
docx
Pages
5
Uploaded by AgentHeatKangaroo212
Morgan Peschong no partner
10/23/26
Sun and Sunspot Groups
Date of Solar
Image
Distance (in millimeters) from the left edge of
Sun
Group 1728
Morgan Peschong
10/23/26
Group
1730
Group 1731
1
April 25
14mm
20mm
0mm
2
April 26
22mm
28mm
8mm
3
April 27
31mm
41mm
17mm
4
April 28
42mm
50mm
23mm
5
April 29
50mm
59mm
36mm
6
April 30
60mm
71mm
45mm
1.
The distance traveled by each group of sunspots is calculated as the difference between
the distance first recorded in the table and the distance last recorded in the table
2.
1728: 46 millimeters
1730: 51 millimeters
1731: 45 millimeters
3.
1.3927 million km radius
in kilometers: ____696,340 km
4.
90 mm
5.
15,474 km/mm
6.
1728: 711,804 km
Morgan Peschong no partner
10/23/26
1730: 789,174 km
1731: 696,330 km
7.
732,436 km
8.
5 days
9.
146,487km/day
10. = 2(3.14) x 696,340= _4,373,015.2 km
11. 30 days
12. 24.47days
13. 0.22599%
14. The Sun exhibits differential rotation, meaning that the rotation speeds of its north and
south poles differ from the equator. The motion of sunspots varies in terms of speed and
direction, depending on their location on the Sun's surface. Sunspots located closer to the
poles move and rotate more slowly, whereas those positioned near the equator have a
higher rate of movement and rotation
.
15. I have over 50% error in my calculations and seem to have overestimated the rotational
speed. I think the data sources I used to do my calculations may have measurement
imprecision. It’s possible that my calculations are inaccurate, and it’s possible that human
error could occur in the process
.
Morgan Peschong
10/23/26
Universal
Time
Time
Interval
(t2-t1)
(sec)
Position
(s page(cm)
Position
(s actual)
(km)
Average
Velocity
(km/s)
Average
Acceleratio
n (km/
S2)
08:05
29,100
sec
8,610 cm
0.5111
0.5111
0.5 km x
3600 s/h
08:36
30,960
sec
91,772,337,448,000c
m
0.84km
0.84km
0.84km
09:27
34,020
sec
104,388,373,824,000
96.67km
96.67km
96.67km
10:25
37,500
sec
1.1244681935 ×
10^15cm
1,041.67k
m
1,041.67k
m
1,041.67km
11:23
40,980
sec
409,800cm
11.4 km
11.4 km
11.4 km
Morgan Peschong no partner
10/23/26
1=37,500t2−t1=37,500 seconds
S page=104,388,373,824,000 cm
37,500 sec1,041.67 km−104,388,373,824,000 cm=0.84 km/
1=40,980t2−t1=40,980 seconds
S page=409,800 cm
S actual=11.4 km
9. 548,245.62 days
10. It appears to be moving faster
11.
Coronal mass ejection (CME) shapes can change over time as they propagate through space.
A CME is a massive burst of solar wind and magnetic field that rises above the solar corona or is
released into space
.
12. The combination of these forces and correlations can explain the observed behavior and
properties of CMEs, affected by their shape changing over time as the CME moves away from
the Sun and can propagate under solar wind pressure around. Magnetic forces can affect the
shape and alignment of CMEs with respect to the magnetic field of the solar wind. These
correlations are important for understanding how CMEs propagate through space and how they
can affect the Earth and other planets.
13. Your average speed for the CME was 11.4 km/s. This speed is much slower than the range
you described for CMEs, which can travel from slower than 250 km/s to about 3000 km/s In
contrast the CME you examined is much slower. Based on the slow velocity of 11.4 km/s, this
CME would have taken much longer to reach Earth, compared to the fastest Earth-guided CMEs
that can occur within hours CME slower varieties, such as 11.4 with an average speed of km/s,
may take several days or even longer to reach our planet. The exact time at which this CME will
reach the Earth will depend on its initial state and the distance between the Sun and the Earth at
the time of the CME eruption.
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