Stellar Nucleosynthesis

Transcription

1 Stellar Nucleosynthesis What makes the sun shine? Gravita7onal contrac7on Chemical reac7ons Nucleosynthesis Stellar Nucleosynthesis The PP chain The CNO cycle The Triple alpha process and on to Fe Stellar Spectra Blackbody spectrum Con7nuum Emission and absorp7on lines The Harvard classifica7on sequence

2 What makes the Sun Shine Luminosity of Sun measured to be: 3.8x10 26 W (from measured flux W m - 2 and distance) Gravita7onal contrac7on (Kelvin- Helmholtz): Grav. Energy is u=m.gm/r = 4 x10 41 J (if all mass placed at surface) Sufficient to fuel sun for 33 million years Oldest rocks dated to be ~4billion years Chemical reac7ons: Burning Coal releases: J per atom Luminosity implies a mass loss of 2x10 26 kg per year Sufficient for sun to last 10 thousand years Nuclear Fusion (Einstein): E=mc 2 implies E=1.8x10 47 J Sufficient to fuel sun for 15,010 billion years

3 Stellar Nucleosynthesis Base fuel is hydrogen (and some helium with traces of CNO) Three key reac7on chains: Proton- proton chain Carbon- Nitrogen- Oxygen cycle Triple- Alpha process But fusion requires high temperatures

4 Core Temperature of Sun Assuming the Sun is in hydrosta7c equilibrium the thermal pressure is sufficient to resist gravita7onal contrac7on Crudely, consider the mass (m) pressing on the core: m =!AR F = GmM R 2 P c = F A =!GM R = G!AM R = (N /V)kT c P c = nkt c =!GM R T c = nm pgm nkr = m pgm kr T c = 23 million K Assumes constant density so not quite right but true answer based on more precise equa7ons which incorporate the density varia7on is close: 15 million K Enough to overcome the Coulomb Force to allow Fusion to occur

5 Nucleon Binding Energies

6 Valley of Stability

7 The p- p chain

8 CNO cycle Another way to progress Hydrogen to Helium Requires Carbon to be present which acts as a catalyst

9 To pp or to CNO? Efficiency depends on temperature of the core, which govern the reac7on rates. For M O. < 1.3 pp dominates. For M O. > 1.3 CNO will dominate.

10 Beyond Helium Numerous paths exist to progress up the valley of stability if other elements are already present but generally require even more temperature/pressure to occur This will only happen in very massive stars or during SN explosion (see later lecture). CNO cycle

11 Beyond Helium: Triple alpha Major bojle neck due to instability (low binding energy) of elements with atomic numbers 5-8 Progression depends on reversible reac7on. High density and abundant energy required For triple- alpha to occur = High mass stars only

12 Triple- α only occurs in massive stars

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14 Black body spectrum Hojer star spectra peak at bluer wavelengths = BLUE Colder star spectra peak at red or near- IR wavelengths= RED Overall a hojer objects gives off more energy (integral under curve)

15 Solar spectrum v Black Body General con7nuum shape OK but lots of lines on top, why?

16 Stellar spectra Stars are hot gas balls and behave like any hot gas: Black body spectrum Intensity Energy density I(!,T ) = 2h! 3 c 2 (e h! kt!1) u(!,t ) = 4" c I(v,T ) in Wm - 2 Hz - 1 ster - 1 in Wm - 3 Hz - 1 Wien s displacement Law! MAX = 2.9!10"3 T Stephan- Boltzmann Law From integra7ng the energy density or for spherically symmetrical systems:! " 0! = " AT 4 = u(v,t )dv L = 4# R 2 "T 4

17 Surface Temp of Sun The Sun s black body spectrum peaks at 500nm use Wein s Law to get temperature? T Surface = 2.9!10"3 = 5800K "9 500!10 Surface temperature is 5800K Core temperature is 15 million K Nuclo- synthesis only occurs in the solar core Core radius ~20-25% of the Solar Radius, enclosing ~10% of the Sun s mass

18 Implied solar radius Can use Stefan- Boltzmann Law to measure implied solar radius, using known Luminosity and Temp. R = L 4!"T 4 = 3.8! ! (5.67!10 "8 ) R = 7.0!10 8 m Note have used slightly more accurate value of Temp

19 Kirchhoff s laws Spectral analysis shows us: 1) A hot opaque body, such as a hot dense gas, emits light at all wavelengths - i.e. it produces a con7nuous 'blackbody' spectrum 2) A hot transparent gas emits an emission- line spectrum - a series of bright spectral lines, plus a faint superimposed con7nuous spectrum. 3) A cool transparent gas in front of a con7nuous- spectrum source produces an absorp7on- line spectrum - a series of dark spectral lines superimposed upon the con7nuous spectrum.

20 Kirchhoff s laws of spectral analysis blackbody 3. Continuous + absorption-line spectrum Cloud of gas prism prism prism 2. Emission-line spectrum + weak continuum 1. Continuous spectrum

21 Absorp7on and Emission Lines

22 Hydrogen oren seen in both emission and absorp7on.

23 Hydrogen series UV OPTICAL NIR FIR mm/radio

24 Rydberg Formulae for Hydrogen 1 " = R % #' & 1 n 1 2 $ 1 n 2 2 ( * )

25 Each element has a characteris7c spectral pajern

26 Cold, low- mass, red Examples of stellar spectra Hot, high- mass, Blue

27 Harvard Spectral Sequence No longer used Oh, Be A Fine Girl/Guy Kiss Me (Right Now Swee7e)

28 Stellar sequence in 2D format