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40 Cards in this Set
- Front
- Back
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Main Sequence Life of Sun, Age of Sun, Age of Universe
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11 Billion, 4.5 Billion, 13.7 Billio
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Keppler's 3rd and Newton's
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P^2=a^3/M
P- years, a- AU, M- Solar Masses |
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Find from Radial Velocity Curve?
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Mass: Relative to star's mass
(Lower Limit Mass, incline) Period: Time between peaks Eccentricity: Sine = circular |
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Find From Transit Light Curve?
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Mass of planet
Radius of Planet/Star Period Temp (Infrared) |
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Stefan Boltzman Laws
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L=T^4xR^2
F=T^4 (yardsticks) |
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Inverse Square Law
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B=L/d^2
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Units of Flux and Luminosity
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Flux= Joules per second per m^2 Or Watts/m^2
Luminosity = Joules/s or Watts |
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classification of stars:
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O, B, A, F, G, K, M
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Diff. between temp and heat:
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temp = average kinetic energy
heat = total energy |
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HR Diagram x and y's
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Y's: luminosity and magnitue
X's: Temp and Classification Temp inc from left to right |
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Categories on HR Diagram
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Main Sequence, Blue Super Giants, Red Super Giants, Giants, White Dwarfs
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sun produces energy?
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H -> He
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Wien's Law
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Max Wave length = 3x10^-3/T
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Balance Between pressure force and Gravity?
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Hydrostatic Balance
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Proton-Proton chain outcomes?
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4H -> ^4 He + neutrinos + gamma rays
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Why does fusion require high level of temp and density?
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To create strong nuclear force and be close enough to fuse
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Strong Nuclear Force vs. Electrostatic Force
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Force between nuclei, very strong, short range; Force between proton and electron, also very strong
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Sun structure and temps
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Core (hottest), Envelope (cooler), Photosphere (5800K), Chromosphere (25,000K), Corona(2,000,000K)
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Sun After Main Sequence
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Red Giant Phase, Helium Flash, Horizontal Branch, Second Giant Phase, Planetary Nebula, White Dwarf
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Red Giant Phase
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Envelope expands, core contracts, degeneracy pressure, T rises until fusion of helium
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Helium Flash
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Temp rises to point of point of huge energy, core becomes normal again
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Horizontal branch
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fusion of He -> C,O in core
fusion of H in shell |
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Red giant two
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Core contracts, degeneracy pressure, fusion of He in shell, fusion of H in bigger shell, 20,000,000 years
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Planetary Nebula
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Envelope driven into space, exhaustion of energy, 100,000 years
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White Dwarf
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no energy source, degenerate core slowly cooling
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Chandrasekhar Limit
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limit of mass for white dwarf, 1.4 solar masses
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Type 1a supernova
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Material added to white dwarf, passes Chan. limit, collapses, explodes
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Type II supernova
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high mass star reaches Fe in core, collapses, explodes. Leaves behind neutron star (if 8-20 solar masses) or black hole
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Neutron Stars
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Small, 19m across, super dense, neutron degeneracy pressure, pulsars
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pulsars
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beams of light from neutron stars' magnetic fields
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the singularity
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point in black hole with infinite mass
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support against grav in white dwarf?
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degenracy pressure
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How were heavy elements delivered to universe?
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type II super novas
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Two most abundant elements?
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H, He, big bang
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Schwarzchild radius
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distance from singularity point at which object can escape.
Rsch=2MG/c^2 |
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stellar-mass black holes?
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binary systems
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super massive black holes?
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center of galaxies
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observing black holes?
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Light shifts redder the closer it originates to black hole. shifts bluer as it approaches black hole
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Doppler effect
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light shifts red as it moves away, shifts blue as object of emission moves towards us.
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Electromagnetic Spectrum
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visible light: 400 (blue) through 700 ( red)
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