Answer:
f1/f2 =W1/W2 = 1/3
.0 f2 = 3f1
As ,
1/F= 1/f1 +1/f2
...1/40 = 1/f1 - 1/3f1
f1=> 80/3 cm
... f2 = 2f1 = 3 x 80/3 = 80 cm
The formula used to find potential energy is <em>P.E. = M * G * H</em> (P.E. is potential energy, M is mass, G is gravitational pull, and H is height). So the answer to your question is <em>5 * 9.8 * 2</em>, which equals 98.
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
Glad to help you and if you need anything else on brainly let me know so I can elp you again have an AWESOME!!! :^)
Answer:
1.275 m
Explanation:
Let the maximum height reached be h.
Here initial velocity, u = 5 m/s
Final velocity, V = 0
Use third equation of motion
V^2 = u^2 + 2 g h
0 = 25 - 2 × 9.8 × h
h = 25/19.6 = 1.275 m
