PCINS aft/7e Sun
Corona — Chromosphe Photosphere
Forms the sun’s re _ thin region — the part of the
outer atmosphere below the corona sun we can see
from the Earth
Convection Radiative Core — center
Zone — region Zone — very Of the Sun Where
where the gases dense region the sun’s energy
eireulate is produced.
k E nergiii* p1'0c1’uCii0n in the S1117
t it ,
° Energy from gravity is not
enough to power the sun,
because if all of the sun’s
gravitational energy were
released, the sun would last for
only 45 million years.
% N llC]€cIIt' F zzsion in the S 2m
° Is Where 2 or more low mass
nuclei join together.
° Normally Hydrogen nuclei
would repel each other b/ c they
have the same charge (+)
F 2151' on
° Due to high heat and high
pressure, hydrogen nuclei have
enough energy to over come the
repulsion and fuse together into
helium. (see pic. Pg 289, or
5 Ci enfis IS
Einstein showed matter and
energy are interchangeable.
° The Formula used to show the
relationship b/ t matter and
energy is. . .
Everything should be as simole as
" uossiblre. but not simnler
E = MC squared. ..
° Energy = mass X square the
speed of light.
How it all works. ..
° Energy is made in the core of
° Energy then passes through a
dense region called the
° Hot gases are carried to the sun’s
visible surface from a region called
the convective zone.
° Energy leaves the sun as light from
a region called the photosphere.
° Some areas of the photosphere
become cooler than surrounding
areas b/ c the sun’s magnetic ﬁeld
tends to slow down activity in the
convective zone. When this
happens, parts of the photosphere
become cooler than the rest of it.
“St()rI72.s' on the S1117
° The constant ﬂow of magnetic
ﬁelds from the sun is called solar
' Cooler, darker areas of the
photosphere of the sun are called
sunspots. A sunspot cycle lasts
about 11 years.