Answer:
top speed = 17.25
Total height = 281.19 m
Explanation:
given data
mass = 75 kg
thrust = 160 N
coefficient of kinetic friction = 0.1
solution
we get here frictional force acting that is
frictional force = 
.............1
frictional force = 0.1 × 75 × 9.8
frictional force = 73.5 N
and
Net force acting will be F = 160 - 73.5 N
F = 86.5 N
so
Acceleration in the First 15 second will be
F = ma .........2
86.5 = 75 × a
a = 1.15 m/s²
and
now After 15 second the velocity will be as
v = u + at ..........3
here u is 0
so v will be
V = 1.15 × 15
v = 17.25
and
now we get travels distance S in 15 s
s = u × t + 0.5 × a × t²
here u is 0
so distance s will be
s = 0.5 × a × t²
s = 0.5 × 1.15 × 15²
s = 129.37 m
and
now acceleration acting is
F =
m a =
a = 
a = - 0.98
here it is negative it mean downward nature of acceleration
and
now we get distance s by this formula
V² - u² = 2 a s
here v velocity is 0 and
u initial velocity is 17.25 m/s
put here value
0 - 17.25² = 2 × (-0.98) × s
solve it we get
s = 151.82 m
so
Total height is
Total height = 129.37 m + 151.82 m
Total height = 281.19 m
F=ma
Therefore the net force = 1000kg × 2 metres per second per second
So F=2000 N
Transverse waves are always characterized by particle motion being perpendicular to wave motion. A longitudinal wave is a wave in which particles of the medium move in a direction parallel to the direction that the wave moves.
Answer:
TAJUK
Explanation:
Sebab saya suka makan ayam goreng, esok saya nak pesan daripada kedai pak abu, terima kasih bosku
My answer -
the corona,
the sun's outer layer, reaches temperatures of up to 2 million degrees
Fahrenheit (1.1 million Celsius). At this level, the sun's gravity can't
hold on to the rapidly moving particles, and it streams away from the
star.
The sun's activity shifts over the course of its 11-year cycle, with
sun spot numbers, radiation levels, and ejected material changing over
time. These alterations affect the properties of the solar wind,
including its magnetic field properties, velocity, temperature and
density. The wind also differs based on where on the sun it comes from
and how quickly that portion is rotating.
The velocity of the solar wind
is higher over coronal holes, reaching speeds of up to 500 miles (800
kilometers) per second. The temperature and density over coronal holes
are low, and the magnetic field is weak, so the field lines are open to
space. These holes occur at the poles and low latitudes, and reach their
largest when activity on the sun is at its minimum. Temperatures in the
fast wind can reach up to 1 million degrees F (800,000 C).
At the coronal streamer belt around the equator, the solar wind travels
more slowly, at around 200 miles (300 km) per second. Temperatures in
the slow wind reach up to 2.9 million F (1.6 million C).
p.s
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