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| (1kW/m2). Power (flux) from the sun that hits the earths surface. [energy/second/area at the radius of the earth Lsun/4piR^2] |
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| another term for the solar constant |
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| Equal pressure in every direction [pressure from heat matches the gravitational pull] |
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| Uniform temperature throughout and not changing |
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| Rotation Period: equator = 25days, pole = 30 days |
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| Fusion -> radiation-convection-radiation (gamma -> thermal) |
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| Particle not known to have a substructure (not made up of smaller particles)... Hadrons (Baryons, Mesons) Leptons (electrons, muons, tau) |
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| inverse x^2 graph centered at Fe57. Toward middle is exothermic, toward outside endothermic. Fusion left side, Fission right side. [know graph] |
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| Two or more atomic nuclei join to become one. Matter not conserved given off as energy [e=mc2] |
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| One atomic nucleus splits in to multiple nuclei. Ofter releasing neutrons or protons and gamma rays. Lots of energy release [e=mc2] |
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| 4H(1) -> He(4) + 2e(+) + gamma + neutrino [sun cycle]. the rate is proportional to time to the 4th. [10^7K req.] |
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| 4H(1) -> He(4) + 2e(+) + gamma + neutrino [pop 1 star]. the rate is proportional to time to the 17th. same net reaction but requires carbon and 20million K. |
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| high frequency [high energy] e-mag radiation. released in fusion/fission |
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| electrically neutral super-tiny subatomic particle. given off by fusion. |
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T = 15million K, density = 150 g/cm3 [HT via gamma radiation due to proton-proton fusion] ionized gas
- radius of 200,000km |
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-no electrons on atoms to capture photons
-thus, transparent to light
-density too high for convection
- width of 300,000km |
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-density and T lower -> some atoms become non-ionized and capture photons
-becomes opaque to light making radiation hard
- hot gas rises and cool gas sinks at about 1km/s
-width of 200,000km |
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Region of the sun where externally visible light originates.
- low density makes it transparent to light again -> radiation takes over again
-500km wide |
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-1500km wide
- about 6000K
- low density -> emits very little light
- emits spicules (warm jets at 100km/s) - last minutes
- reddish hue (3->2 H emission) |
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Temp about 10^6 k (rises from the chromosphere) due to magnetic activity
- trasition from gas pressure/fluid mech dominance to magnetic dominance
- ultraviolet emission |
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- Fe13+ emission ---> HOT (1million K)
- means "crown"
- Gas Hot enough to escape -> solar wind
- F corona - reflecting interplanetary dust
- K corona - free electron scattering |
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| Diminishing of the intensity of light as you move towards the outside of the star (due to optical depth and a lower temperature further from the core) |
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| Emission spectrum of the photosphere moments before of after a total solar eclipse. |
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| an instrument that captures an image of the sun at a single wavelength of light. [monochromatic image] |
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| Telescopic attachment that blocks the visible light from the sun to view the corona |
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Chromosphere -> warm jets of matter at 100km/s (minutes)
- due to magnetic disturbance |
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| a sudden brightening of the sun (large release of energy) |
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| bright feature extending outward form the suns circular surface (cooler than the chromosphere) following magnetic lines between a sunspot |
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| bright extended regions in the chromosphere |
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| prominences viewed directly overhead |
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areas where the corona is darker -> lower temperature and lower density plasma
- source of solar wind |
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| convection cells in the photosphere (hot gas rises then cools by radiation and falls back down - diameter around 1000km, time about 10 minutes) |
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- about 10000km across
- may be hundreds or none (come in pairs, cycle)
- same latitude
- same hemisphere = same magnetic configuration
- dark because cooler than photospheric gas (4500K)
- magnetic field prevents hot gasses from rising (1000x)
- days -> months
- used to determine differential rotation (Galileo)
- because of the differential rotation -> mag fields twist |
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| very dark region in the middle of a sunspot |
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| outer region of the sunspot, not as dark as umbra, grey areas |
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solar maximum every 11 years. [know graph of cycles]
- maunder minimum, dalton minimum, modern maximum |
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| 0 to hundreds. depending on the point in the cycle |
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| sharp spectral lines are split into close lines in the presence of a magnetic field |
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| solar-terrestrial relationships |
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-Aurorae
-solar wind
-magnetic storms
-radio fadeouts
-cosmic rays
-weather |
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| very low number of sunspots around the 1600s (almost disappeared) |
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| depends on temp only. gamma ray hits nucleus which releases multiple gamma rays (energy conserved so each ray has lower energy than original) |
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hot coronal gas ejected from the sun
- v=500km/s
- reaches earth in 3 days
- emits mostly in x-rays
- 1 million K |
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| system of a pair (or multiple pairs) of stars that are close enough they orbit their common center of mass |
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the two stars can be independently resolved by telescope:
- large separation, large period |
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differentiation due to the doppler effect
single line - 1 moving spect, 1 full spect (white dwarf)
double line - 2 moving spects
tend to have small orbits, short periods |
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unresolved stars but periodical flux change due to edge-on orbit
- small separation, short periods |
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| fake binary... naked eye sees two stars together but they might be at different distances |
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| unresolved but can tell due to the proper motion of the 1st object |
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1-orbit is an elipse around a foci.
2-sweeps equal area in equal time
3-semi major axis cubed proportional to period squared |
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| measure of the difference of the orbital plane to the ecliptic plane |
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| measure of the transparency of an object |
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