star formation
DESCRIPTION
Star Formation. The surface temperature of a star T is compared to a black body. Luminosity L Radius R The absolute magnitude calculates the brightness as if the stars were 10 pc away. Related to luminosity. Type Temperature O35,000 K B20,000 K A10,000 K F 7,000 K - PowerPoint PPT PresentationTRANSCRIPT
![Page 1: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/1.jpg)
Star Formation
![Page 2: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/2.jpg)
Classifying Stars
• The surface temperature of a star T is compared to a black body.– Luminosity L– Radius R
• The absolute magnitude calculates the brightness as if the stars were 10 pc away.– Related to luminosity
• • Type Temperature
O 35,000 K B
20,000 K A 10,000 K F
7,000 K G 6,000 K K 4,000 K M 3,000 K
424 TRL
72.4)/log(5.2 sunLLM
![Page 3: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/3.jpg)
Stellar Relations
• Some bright stars (class) (absolute magnitude)– Sun G2 4.8– Sirius A1 1.4– Alpha Centauri G2 4.1– Capella G8 0.4– Rigel B8 -7.1– Betelgeuse M1 -5.6– Aldebaran K5 -0.3
![Page 4: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/4.jpg)
Luminosity vs. Temperature
• Most stars show a relationship between temperature and luminosity.– Absolute magnitude can
replace luminosity.– Spectral type/class can
replace temperature.
-20
-15
-10
-5
0
5
10
15
20
Abs
. Mag
nitu
de
O B A F G K MSpectral Type
Sun
![Page 5: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/5.jpg)
Hertzsprung-Russell Diagram
• The chart of the stars’ luminosity vs. temperature is called the Hertzsprung-Russell diagram.
• This is the H-R diagram for hundreds of nearby stars.– Temperature decreases to
the right
![Page 6: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/6.jpg)
Main Sequence
• Most stars are on a line called the main sequence.
• The size is related to temperature and luminosity:– hot = large radius– medium = medium radius– cool = small radius
-20
-15
-10
-5
0
5
10
15
20
Abs
. Mag
nitu
de
O B A F G K MSpectral Type
1 solar radius
Sirius
![Page 7: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/7.jpg)
-20
-15
-10
-5
0
5
10
15
20
Abs
. Mag
nitu
de
O B A F G K MSpectral Type
Giants
• Stars that are brighter than expected are large and are called giants or supergiants.
• Betelgeuse is a red supergiant with a radius hundreds of times larger than the sun.
AldebaranCapella
RigelBetelgeusesupergiants
giants
![Page 8: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/8.jpg)
Dwarves
• Stars on the main sequence that dim and cool are red dwarves.
• Small, hot stars that are dim are not on the main sequence and are called white dwarves.
-20
-15
-10
-5
0
5
10
15
20
Abs
. Mag
nitu
de
O B A F G K MSpectral Type
white dwarves
![Page 9: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/9.jpg)
Interstellar Medium
• Interstellar space is filled with gas (99%) and dust (1%).• Interstellar gas, like the sun, is 74% hydrogen and 25%
helium.• Interstellar dust, like clouds in the gas giants, are molecular
carbon monoxide, ammonia, and water.• Traces of all other elements are present.
• Atoms are widely spaced, about 1 atom per cm3, a nearly perfect vacuum.
• The temperature is cold, less than 100 K.
![Page 10: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/10.jpg)
Molecular Clouds
• The small mass of atoms creates very weak gravity.• Gravity can pull atoms and molecules together.• Concentrations equal to 1 million solar masses can form
giant molecular clouds over 100 ly across.
![Page 11: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/11.jpg)
Catalysts for Star Formation
• A cool (10 K) nebula can be compressed by shock waves.• These shock waves are from new stars and exploding
supernovae.
exploding star shock waves nebula with areas of higher density
![Page 12: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/12.jpg)
Gravitational Contraction
• Density fluctuations cause mass centers to appear.
• Mass at a distance will be accelerated by gravity.
• If there is no outward pressure there will be free fall.– Mass m0 within radius r– Conservation of energy– Calculate free fall time
2
)()(r
rGmrg
r
rdrrrm0
24)()(
0
002
21
rGm
rGm
dtdr
021
0
000
00
22rr
drr
Gmr
Gmdrdrdt
0323
G
![Page 13: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/13.jpg)
Protostars
• Local concentrations in a nebula can be compressed by gravity. With low temperature they don’t fly apart again.– Contracting material forms one or more centers– The contracting material begins to radiate– These are protostars, called T Tauri stars (G, K, M).
![Page 14: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/14.jpg)
Hydrostatic Equilibrium
• Gravity is balanced by pressure.– Equilibrium condition– True at all radii
• The left side is related to average pressure.– Integrated by parts
• The right side is the gravitational potential energy.
2
)()(r
rrGmdrdP
RR
dmr
rGmdrdPr
0 20
3 )(4
gravEVP 3
VPdrdPr
R34
0
3
VE
P grav
3
![Page 15: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/15.jpg)
Adiabatic Index
• Adiabatic compression is not linear in pressure and volume.– Parameter is adiabatic
index – Relate to internal energy
• The gravitational energy was also related to the pressure.– Energy condition for
equilibrium
)(1
1 PVdPdVdEint
0P
dPVdV
VEP int)1(
VE
VE intgrav )1(3
0)1(3 intgrav EE
![Page 16: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/16.jpg)
Formation Conditions
• Contraction requires gravitational energy to exceed internal energy.– Thermal kinetic energy
3kT/2
• The conditions for cloud collapse follow from mass or density.– Jeans mass, density MJ, J
RmG
kTM23
min
intgrav EE
3
2 23
43
mGkT
MJ
RGMfEgrav
2
![Page 17: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/17.jpg)
Fusion Begins
• Initial energy is absorbed by hydrogen ionization.– D = 4.5 eV
– I = 13.6 eV• Apply this to hydrostatic
equilibrium.
• Continued contraction results in quantum electron gas.– When degenerate it resists
compression– Sets temperature at core
IH
DH
I mM
mME
2
eV6.22121
IDkT
3
23)(hkTmm e
342
382
Mh
mmGkT e
![Page 18: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/18.jpg)
Birth of the Sun
• Gravity continues to pull the gas together.– Temperature and density
increases
• If the temperature at the center becomes 5 million degrees then hydrogen fusion begins.
• At this point the star has reached the main sequence.
-20
-15
-10
-5
0
5
10
15
20
Abs
. Mag
nitu
de
O B A F G K MSpectral Type
1 M
![Page 19: Star Formation](https://reader036.vdocuments.us/reader036/viewer/2022062520/56815be8550346895dc9dc5f/html5/thumbnails/19.jpg)
Birth of Other Stars
• Large masses become brighter, hotter stars.
• Gravity causes fusion to start sooner, about 100,000 years.
• Small masses become dimmer, cooler stars.
• Gravity takes longer to start fusion, up to 100 million years.
-20
-15
-10
-5
0
5
10
15
20
Abs
. Mag
nitu
de
O B A F G K MSpectral Type
10 M
3 M
0.02 M
0.5 M