Lecture Notes for Astronomy 321, W 2004 1 Stellar Energy ...

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Figure 6: The main branch CNO chain. Ostlie.) (Equation 10.51 of Carroll and However, as hydrogen is depleted the PP pressure is reduced, allowing further gravitational contraction, in turn requiring larger pressure to maintain mechanical equilibrium with a correspondingly larger T . The larger T rapidly increases the rate of the higher-A processes. So as the lighter nuclei are consumed, the burning of these elements will continue at layers ar larger radius, while the inner core will involve the processes with heavier nuclei. These larger rates will consume the fuels relatively quickly. At some point in this evolution, electron degeneracy becomes important. This will be discussed in subsequent lectures. Figure 7: Another high-temperature fusion process. (Equation 10.59 of Carroll and Ostlie.) 14
Figure 8: Yet another high-temperature fusion process. (Equation 10.60 of Carroll and Ostlie.) 15
Page 1 and 2: Lecture Notes for Astronomy 321, W
Page 3 and 4: 1.3 Four forces of nature The elect
Page 5 and 6: Figure 1: Binding energy per nucleo
Page 7 and 8: 2 Stellar Energy Generation - PP-ch
Page 9 and 10: 2.2 The pp interaction: Coulomb bar
Page 11 and 12: compared to the quantum barrier pen
Page 13: 0.01 0.009 0.008 0.007 0.006 I (MeV
Page 17 and 18: part due to the solar neutrinos dis
Page 19 and 20: came up with a viable detector cons
Page 21 and 22: neutrino species have small, but fi
Page 23 and 24: urning in the next sub-shell outwar
Page 25 and 26: solar luminosity, which is comparab
Page 27 and 28: As it turns out, the neutral curren
Page 29 and 30: 4.6 Further collapse and black hole
Page 31 and 32: approaches zero. This distance R s
Page 33 and 34: 5.3 The Friedmann equation and a us
Page 35 and 36: Figure 12: Time evolution of the sc
Page 37 and 38: Table 1: Properties of cosmic fluid
Page 39 and 40: 7 Vacuum energy and Inflation In Se
Page 41 and 42: 7.2 Inflationary scenario We saw ab
Page 43 and 44: 8 Fluids and 2nd Friedmann equation
Page 45 and 46: Figure 15: Energy (kT ) per particl
Page 47 and 48: decay modes, and hence N ν . The c
Page 49 and 50: Figure 18 gives this critical densi

Lecture Notes for Astronomy 321, W 2004 1 Stellar Energy ...

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