1Stellar EvolutionBefore…..During……and After….The Main SequenceIt’s all about gravity……Stellar Evolution on the Main Sequence2The Main-Sequence Lifetime of a Star• The length of time a star spends fusing hydrogen into helium is called itsmain sequence lifetime– Stars spend most of their lives on the main sequence– Lifetime depends on the star’s mass and luminosity– More luminous stars burn their energy more rapidly than less luminous stars.– High-mass stars are more luminous than low-mass stars– High mass stars are therefore shorter-lived!• Cooler, smaller red stars have been around for a long time• Hot, blue stars are relatively young.High-mass stars 10 mpg Low-mass stars 60 mpgWhat determines when a star becomes a main-sequence star?a) When nuclear fusion generates the energy required to balancegravityb) When convection begins in the core.c) When optical radiation leaves the stard) When the temperature in the core reaches a highertemperature than the corona.3Main Sequence Turn-offWhat are we looking at?a) Stars of the samemass?b) Stars of the samecolor?c) Stars of the samemagnitude?d) Stars of the sameage?Main sequenceStellar Evolution on the Main SequenceHigh mass stars4The CNO cycle• Low-mass stars rely on the proton-protoncycle for their internal energy• Higher mass stars have much higherinternal temperatures (20 million K!), soanother fusion process dominates– An interaction involving Carbon, Nitrogenand Oxygen absorbs protons and releaseshelium nuclei– Roughly the same energy released perinteraction as in the proton-proton cycle. Butit runs much faster!– The C-N-O cycle!The solar corona has temperatures roughly the same levelas temperatures in the Sun's core, where nuclear fusiontakes place.Why doesn't fusion occur in the corona? a) The density in the corona is too low. b) The corona has too many free electrons. c) Atoms in the corona are mostly ionized. d) The corona has more heavy atoms than the core. e) Two of the above.5Internal Structure of Stars - Convection• Convection occurs in theinteriors of stars wheneverenergy transport away fromthe core becomes too slow– Radiation carries awayenergy in regions wherethe photons are not readilyabsorbed by stellar gas– Close to the cores ofmassive stars, there isenough material to impedethe flow of energy throughradiation– In less massive stars like the Sun, coolerupper layers of the Sun’s interior absorbradiation, so convection kicks in there– The lowest-mass stars are fullyconvective, and are well mixed in theinterior.Solar thermostatNuclear reaction rateGravitational contraction•Greater pressure is required to balance higher gravitational force due to higher mass.•Greater pressure produces higher temperature (and reaches this faster).•Higher temperature produces greater luminosity.•Higher luminosity leads to faster fuel consumption.•Faster fuel usage means high-mass stars burn out sooner than low-mass stars.Solar thermostat6In a Main Sequence star Hydrostatic Equilibrium balances 2 forces,pressure and gravity, to keep the star from imploding orexploding. If the mass of the outer portion of the star wassuddenly decreased slightly what would happen?a) Pressure in the center would decrease, the core would contractand the star would shrink slightly.b) Pressure in the center would increase, core expand and the starwould contract slightlyc) Pressure in the center would decrease, core would contract thestar would expand slightly.d) Pressure in the center would decrease, core would expand and thestar would expand slightly.Evolution to red giant phase• The star is expanding and cooling, so its luminosityincreases while its temperature decreases• Position on the HR diagram shifts up and to the right…Fuel runs outCore pressure dropsGravity compressescoreCore temperature risesShell burningPressure puffs outer layers Core heats up moreShell burning grows strongerAtmosphere expands and cools further7Evolutionary tracks of giant starsHelium Fusion• Normally, the core of a star is not hotenough to fuse helium– Electrostatic repulsion of the twocharged nuclei keeps them apart• The core of a red giant star is verydense, and can get to very hightemperatures– If the temperature is high enough,helium fuses into Beryllium, andthen fuses with another heliumnuclei to form carbon.8A (temporary) new lease on life• The triple-alphaprocess provides anew energy sourcefor giant stars• Their temperaturesincrease temporarily,until the helium runsout• The stars cool, andexpand once again• The end is near…Light Curves• To characterize the variabilityof a star, scientists measurethe brightness, and plot it as afunction of time.– Light Curves• Different kinds of variability– Irregular Variable• Novae (death)• T Tauri stars (birth)– Pulsating Variable• Periodic changes inbrightness9Yellow Giants and Pulsating Stars• If you plot the positions of variable stars on the HRdiagram, many of them fall in the “instability strip”– Most have surface temperatures of ~5000K, so appear yellow– Most are giants (Yellow Giants)– Instability comes from partial absorption of radiation in theinterior of the star• Helium absorbs radiation, and the outer layers of the star get pushedaway from core• As the star expands, the density decreases, letting photons escape• Outer layers head back inward toward core• Repeat– RR Lyrae and Cepheid variables are useful for finding distancesto the stars, as the star’s period is proportional to its luminosity.Cepheid and RR Lyrae VariablesThe Period-Luminosity Relation10Periods of Variable