Answer:
Resistance is a measure of the opposition to current flow in an electrical circuit.
Explanation:
Answer:
.a = 849.05 m / s²
Explanation
The centripetal acceleration is
a = v² / r
Linear and angular velocity are related
v = w r
Angular velocity and frequency are related by
w = 2π f
Let's replace
a = w² r
a = 4π² f² r
Let's reduce to the SI system
f = 2.30 rev / s (2π rad / 1 rev) = 14.45 rad / s
.r = 10.3 cm = 0.103 m
Let's calculate
a = 4π² 14.45² 0.103
.a = 849.05 m / s²
1. it is difficult to search for it . Because infrared rays will never penetrate through earth atmosphere.
2. we are unaware of how it looks like and we only know it is red and will glow . A damaged star also looks like this.
3. Dust also makes is hard to detect Dyson spheres . So we will get confused between Dyson sphere and a star surrounded by dust.
The solution for this problem is:
For 1st minimum, let m be equal to 1.
d = slit width
D = screen distance.
Θ = arcsin (m * lambda/ (d))
= 0.13934 rad, 7.9836 deg
y = D*tan (Θ)
y = 6.50 * tan (7.9836)
= 0.91161 m is the distance from the central maximum to the first-order minimum
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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