6. Composición del Universo

7. Las Pléyades

15. Gran explosión
Tras una pequeña
fracción de segundo
Tras 380.000 años
Tras 13.700 millones de años

18. 10-4 s

19. 100 s
10-4 s

20. 400.000 años
3 min

21. Hoy
Temperatura Tiempo

22. Fondo Cósmico de microondas (1964)
hoy
400.000 años

23. Arno Penzias Robert Wilson

25. RADIACIÓN NO HOMOGÉNEA
Mapa Fondo Cósmico de Microondas: COBE

26. 3 min

27. Hace 13.000 millones de años
Grumos de materia = gérmenes de galaxias

28. Stars start from clouds

29. Clouds provide the gas and dust from which stars form.

30. But what kind of dust ?

31. Stars begin with slow accumulation of gas and dust.

32. • Contraction causes Temperature and
Pressure to slowly increase.

34. Rather: Irregular Grains of Carbon or Silicon

35. • Gravitational attraction of Clumps attracts
more material.

37. G m1 m 2
F 2
r

39. The Life Cycles of Stars

40. Collapse to Protostar

41. Nuclear Fusion !

42. All Types of Stars
E = mc2

43. Where does the energy come from ?
At 15 million degrees Celsius in the center
of the star, fusion ignites !

44. Mass of four 1H > Mass of one 4He

45. 4 (1H) --> 4He + 2 e+ + 2 neutrinos + energy
At 100 million degrees Celsius, Helium fuses:

46. Energy released = 25 MeV= 4 x 10 -12 Joules=
1 x 10 -15 Calories
But the sun does this 1038 times a second !
Sun has 1056 H atoms to burn !

47. Edad 50001 de años
5.800º en la superficie
151 º en el núcleo

50. Solar Heliospheric Observatory

58. New Stars are not quiet !

60. Throughout its life, these two forces determine
the stages of a star’s life.

61. Expulsion of gas from a young binary star system
Energy released from nuclear fusion
counter-acts inward force of gravity.

63. After Helium exhausted, outer layers of star expelled

67. The end for solar type stars

70. LA COMPOSICIÓN DE LOS ASTROS MÁS ANTIGUOS
75 % hidrógeno
25 % helio
<0.01 % litio

77. The Beginning of the End: Red Giants

81. The End of the Line for Massive Stars

83. 4He + 16O 20Ne + energy
4 (1H) 4He + energy
3(4He) 12C + energy
12C + 12C 24Mg + energy
28Si + 7(4He) 56Ni + energy 56Fe
4He + 12C 16O + energy
16O + 16O 32S + energy

85. Supernova !
a b SN1987A
a): optical
b): radio
c d c): X Ray
d): X Ray

89. http://imagine.gsfc.nasa.gov/docs/teachers/lifecycles/stars.html

90. Annie J Cannon
(1863-1941)

91. Oh! Be a Fine Girl - Kiss Me Right Now Sweetheart !
Out Beyond Andromeda, Fiery Gases Kindle Many Red New Stars

105. Vía Láctea

106. What is a Galaxy ?
Distance from Earth to Sun = 8 light-minutes
Solar System
Size of Solar System = 5.5 light-hours

107. What is a Galaxy?
Stellar Region
Sun
(solar system 30
too small to be light-years
seen on this scale)

108. What is a Galaxy?
Galaxy
Sun’s Stellar Region
a massive collection of stars, gas, and dust kept together by gravity
200,000 light-years

109. What is a Galaxy?
If our solar system was the size of a cell in the human body, our galaxy
would still measure over one mile across.
Using this same analogy, the Andromeda Galaxy would be 22 miles away.

111. Types of Galaxies

114. M 33

115. Cúmulos de Galaxias

116. M 100

118. NGC 1365

119. M 31

120. M 51

122. M 51

123. M 109

124. M 91

125. M 33

126. NGC 5128

127. NGC 7742

128. NGC 4319

129. M 100

142. La Vía Láctea
Grupo Local
La Tierra El Sistema Solar

144. Brazos de la Vía Láctea

145. Brazo de Sagitario
Brazo de Perseo
Brazo de Orión
Núcleo
Brazo a 3 Kpc
Cúmulos globulares
Sistema
Solar

163. Edwin Hubble
1889-1953

172. M 82´s Middle Mass Black hole

209. Agujeros negros

211. Hace 4.600 millones de años
Nace el sistema Solar

213. Increasing Temperature and Pressure ...

214. More Fusion !

223. Masa del Sol (M)=1

233. Hace 4.000 millones de años

240. Hace 200 millones de años

241. Hace 3.5 millones de años

242. Hace 5.000 años