lab eleven - aidann gia bacolodan
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School
Pace University *
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Course
150
Subject
Astronomy
Date
Jan 9, 2024
Type
Pages
8
Uploaded by AgentFang12036
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Introduction
Spectrocopy
is the study
of
light.
Stars
emit
light
energy
in the
form of
wavelengths
called
the
electromagnetic spectrum. By
analyzing
the
light that
comes
from distant
starb,
astronomers
can
determine
what
elements
they
are made
of
and
better
understand the chem-
istry
of all stars.
Background
Early
astronomers like Eijnar Hertzsprung (Danish)
and
Henry
Russell
(American) studied
the
thousands of stars visible
to
the
eye
from Earth. They found
that
stars
could
be
classified
according
to their
color (which
indicates
the
stars relative temperature) and
their
luminosity.
Luminosity
is
the relative brightness
of
a
star
compared
to the brightness
of
Sol
(our
Sun).
This
is
a
concept
that
can be confusing
because
if
we
look at
all
other
stars
in the night
sky
com-
pared
to
Sol
in
the
daytime
sky,
all
other
stars appear
dimmer. However,
that
is
because
of
the
distances
they
are
from
Earth.
One reason
why
Sol
appears
so
bright is
because
it
is only
(on
average)
93,000,000
miles
flom
Earth. Luminosity
takes
distances
into
account
and categorizes
stars
as
brighter
than
Sol,
or dimmer than
Sol
by orders
of magnitude.
Hertzsprung and
Russell recognized
early on
that by
comparing
stellar
temperatures,
luminosities
and
the
actual
output
of
energy
(magnitude)
of stars
that
they could
determine
stellar
distances. The diagram
they
came
to
develop was called
the
Herztsprung-Russell
Diagram, and
it
is most commonly
used
for plotting
the
evolution
of stars.
Since
Herztsprung-Russell,
astronomers
have used
satellite technology
to
collect
data
on various stars
in our
gala:iy. We
now understand
that
stars
fuse
lighter
elements
first
in
their
cores. These
runaway fusion chain reactions
yield
heavier
elements
that
take
up
less
space
in the
stars. If
the star
has
enough
mass,
it
will
begin
to
fuse
the
heavier element once
most of
the original
elements have been fused.
This
change
in
fuel
creates
a
change
in
the
star's
size
and color. The
star
moves
off
the
"Main
Sequence"
as
it
is rib
longer stable
but
changing
in
characteristics. The
star is
much closer
to
its
death
stage,
usually
seen
as
enlarged
in
size,
and
red
in
color. The more
massive
the
star,
the shorter the life
span-it
burns
through
its fuel
very
quickly. The
less massive
the
star,
the longer
the
life
span.
Activity
Overview
This
activity
will
show
you how
astronomers determine
the chemistry
of
stars by
using
spectra, and how
to
recreate
the
Hertzsprung-Ruqsell Diagram
that
astronomers use
to
determine
the
distances
to
and
evolution
of
stars.
Materials
Pencil
Highlighter
Colored
pencils
(red,
orange,
yellow
and
blue)
Astronomy Actiuity
Lab
Manual
19
Activity
1
The
Electromagnetic Spectrum
and
"Spectra"
Astronomers
use
instruments
called spectrometers
to
determine
the
elements
that
stars
are made
of.
Since each element has
a different "signature"
or
pattern when
it
absorbs
and
radiates heat and
light,
astronomers
can use
these
special
patterns
to
determine
just
what
elements
are
present in
the light
coming
from distant
stars.
Using
the spectral
patterns
below
of
the
elements, determine
what
elements
are
present in Spectrum
Q.
(Spectral Lines)
Most of
the
universe
is
composed of Hydrogen
atoms-it
is
the first
gas
that
is fused in the core
of
stars like
So1.
Silicon
Silicon
and
oxygen
are the
two
most
abundant elements
in
the
rocks of
Earth's crust.
Oxygen
Helium
Lithium
Carbon
All
life known to
humans is based
on molecules
using carbon.
Hydrogen
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HrnrzsPRUNG-RussELL
DTAGRAM
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What elements
are
represented
in
Spectrum
Q
below?
Astronomy Actiaity
Lab
Manual
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Activity
2
Procedure
Creating the Hertzsprung-Russell Diagram
1.
Plotting
Stellar
Temperatures. Temperature
is plotted
along
the
x-axis. Tempera-
tures
increase
from
RIGHT
to
LEFT.
The x-axis
is
not
divided
equal
in
temperatures
differences
Start
with
2,000 "C
at
the right corner
of the
x-axis. Place
the following
temperatures
on
the
x-axis
from
right
to
left:
3,000
'C;
4,000
'C;
5,000 "C; 6,000
'C;
7,500
'C;
10,000
'C;
25,000
"C;
35,000'C; 45,000'C;
and
50,000'C.
Stellar
color
is related
to
the
surface
temperature
of
the
star. Using
colored
pencils,
lightly
shade
in
the
x-axis
(where
the
surface
temperature is
represented)
with
the
following colors.
Temperatures
from
2,000
"C
to
3,500
'C
will
be red
stars.
Temperatures between
3,500
'C
and
5,000
"C
will
be orange
stars. Temperatures
from
5,000
'C
to
6,500'"C
will
be
yellow
stars.
From
6,500
"C
to
7,500
"C
are
bluewhite
stars.
Blue
stars
will
be
from
7,500
'C
to
11,000 "C. Use
a
very
dark, indigo.blue
color
for the
stars
with
temperatures greater
than
11,000'C.
2.
Luminosity. Luminosity
is
plotted
along
the
y.aris
and values increase
from
bottom
to
top
on
the
diagram.
Luminosity
represents
the
relative brightness of
a
star compared
to the
brightness of
Sol
(that
has
a
luminosity of
1).
Values
on
this
scale increase and
decrease
by factors
of ten.
At
the
top
of
the chart
write
the words "Bright, high energy
output."
and
down toward the bottom,
write
"Dim,
low
energy
output."
For
each
mark
made
on the
y-axis,
complete
the
appropriate
scale
for
luminosity
with
the
luminosity
values. Note
that
the value of
Sol
has
already
been
placed on
the
chart
as "1."
3.
Drawing Stellar
Size.
Use
the
Stellar
Luminosities
and Temperature Table
to
deter-
mine
the position for
each
star.
Place a
dot at
each
location.
Determine
which
of
the
three
sizes
the star should
be and
draw
this
sized
circle
around
your dot
to.represent
its
relative
size compared
to
the other
stars on
the
chart.
You
do nof
need
to
Iabel
your
stars.
Supergiants
Giants
O
Dwarf
Stars
The stellar groups are outlined on
the
Hertzsprung-Russell
Diagram
by
name. The
"Supergiants"
are
the
largest
stars
that
extend
across
the
top
of
the
diagram, "Giants"
are
smaller and "Dwarf" stars are'the smallest. Though
in
space
actual stellar
sizes
vary, draw
each
group
as
a
specific
size.
The
sizes
of stars
in the
Main
Sequence
will
vary
from dwarf
to
supergiant
size.
Delermine the most
appropriate
size
for
each
star
based
upon its
position
in the
diagram.
.
Connect
the
"X's" on the
stars.
Label
this
line.
Astronomy
Actioity Lab
Manual
diagram
to
show
the location
of the
Main
Sequence
2l
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r
Give Sol
a
special symbol
and
provide
a
legend on
the
right border
of
the
diagram.
.
When stars overlap
due
to
sizes,
draw them
as
if
one
were behind
the
other.
That
way
the
center
point
of
each
circle
will still
represent
the most
accurate
position
of the
star.
4.
Coloring
Stars
Using
their
placement upon
the
Hertzsprung-Russell
Diagram and
their
representative surface temperatures,
Iightly color in
each
star
using
the
appro-
priate
colors previously
mapped
on
the
diagram.
5.
Mapping Stellar
Evolution
High Massed
Stars
Using a
highlighter, draw
an
arrow from the
Blue Supergiants across
the
diagram
to
the
Red Supergiants. These
most
massive
stars live
the
shortest
periods-on
the
scale
of
only millions
of
years.
Intermediate
Massed
Sfars
Using
your
highlighter, draw
an
arrow from the
Giant
stars
on
the
Main
Sequence
to
the
Red
Giants.
Inu
Massed Stars
(though
Sol
is
technically
an
intermediate
massed
star,
it
is like.
ly that
it
will
follow this
death
sequence.) Using a
highlighter, draw
an
arrow
along
the
Main
Sequence
from
Orange
to
Yellow.
Continue
this arrow
off the main
sequence
to
the
Red
Giant
Stars. Now,
change
the direction
of the
arrow by
drawing
it
to
the
White
Dwarfs.
These
least
massive
stars live
the
longest
periods of
time-on
the
scale
of
billions
of years.
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Stellar Luminosities
and Temperatures Table
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Name
Luminosity
Temperature
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Cygnus
B
.04
3,600
AA
star
.36
3.900
Alpha
Centauri
C
.00006
2,500
Alpha Crucis
2,700
20,700
4,400
4,600
Arcturus
Bernard's
Star
.004
2,600
Beta
Crucis
3,000
2r.700
Fomalhaut
J5T
Star
8,500
6,600
K900
Star
900,000
14,000
Luyten 7894A
.00006
2,400
Mimosa
30,000
26,20Q.
P78
Star
P98C
Star
6,000
Polaris
8,000
6,000
Sirius
B
.008
r0,400
V89
Star
.08
6,400
Wolf
2,400
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Star
.3
8,500
Canopus
,
1,500
7,700
Deneb
40,000
9,600
Procyon
B
.0005
7,100
R34
Star
250,000
5,400
250
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5344
Star
250,000
8,000
24
211
Star
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Astronomy Actiuity
Lab
Manual
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HEnTzsPRUNG-RussErr
DncRAM
Questions
to
Master
1.
a.
On
the
H-R
Diagram,
the
larger stars
are
found
toward the
(top/bottom/left/right/
center).
Large
stars
can be
part
of
which two
groups:
The
brightest
stars
are
found
toward the
(top/bottom/left/right/center).
The
hottest
(temp.) stars
are
found
toward the
(top/bottom/left/right/center).
Stars
with
the
highest temperatures
are
the
color
The
smallest stars
are
found
toward the
(top/bottom/left/right/center).
The
smallest stars
are
part
of
a
group called
the
The dimmest stars
are
found
toward the
(top/bottom/left/right/center).
The
coolest (temp.) stars
are
found
toward the
(top/bottom/left/right/center).
Stars
with
the coolest temperatures
are
the color
Sol
is
found at
the (top/bottom/Qeft/right/center).
What
color
is
Sol?
Sol,
like most stars, is found in
a
region of stable stars called
k.
Stars
in The Main
Sequence are
considered relatively
_,
or
unchanging.
What
does
"H-R"
Diagram
stand
for
(include
first
and last names)?
3.
What
two
major
uses does
this
diagram
have
for
astronomers?
a.
b.
4.
Why
are
there no
Nova's
or
Black
Holes
shown on
this evolutionary
diagram?
5.
Briefly
describe
the
death
sequence
of a high
massed
star
once
it
leaves
the
H-R
Diagram.
e.
f.
o
D'
h.
i.
j.
a
1
1
a
a
a
a
a
7s
a
2
a
a
a
a
a
a
a
a
a
a
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-
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Astronomy
Actiaity Lab
Manual
25
6.
Briefly
describe
the
death
sequence
of
an intermediate
massed
star
once
it
leaves
the H-R
Diagram.
7.
Briefly
describe
the
death
sequence
of
a low
massed
star
once
it
leaves
the
H-R
Diagram.
8. Describe
two
changes
a
star undergoes once
it
leaves
the
Main
Sequence.
9.
Once
a
star
changes
color,
what
does
that tell
astronomers
about the
fusion process
d
occurring
in
the stellar
core?
10.
What
one
variable
will
determine
the
death-sequence
a
star
will
take
at
the
end of
its
life?
!
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HEnTzsPRUNG-RussErr
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Astronomy
Actiaity Lab
Manual