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HUV 5NPF5HUV lMM H$ 5O5 H$ P UUe "  H$ 5PN5H$ lOO HH5QD HHAR UTUT ` #  Evolution off the Main Sequence 5` $  R` % #Mass of star   Mass of SUN 6o` &  ` ' % Main Sequence: Star in equilibrium ` ( UUHydrogen burning in core ` *  ` +  Hydrogen depleted in core ` , &Core shrinks and T c  increases ` ) *Radius increases and T e  decreases I` 2 Then... The Helium Flash Ht` 3 5) Helium Main Sequence  (Red Giant) ` 4 Helium burns in core ` 5 Hydrogen burns in shell ` 6  ` 7  Helium depleted in core ` 8 UU*Core shrinks and Radius increases (again) "` -  ?` . # Nuclear reactions come to a stop H\` 9 5-Atmosphere blows off:  Planetary Nebula Ay` /   White Dwarf  remains HH5RD inHHlUQQ s od5S &UU HH5TS HHjni` * U ` 0 teLimits of Stellar Mass ` ,;` 1 a TX` : s 'How big can a star be? How small? d Tu` ; s  ` = T%Maximum mass limited by mass loss: ` > M9 The Sun loses 1 0 -14   M SUN /year m` A $ < 0.01%  lost on Main Sequence he` ? 66 O-stars lose 1 0 -6   M SUN /year ` B UU,  few  %  lost on Main Sequence #` C > M 100 M SUN    ~50%  lost during life @` @ At!  Exposed core, violent life N]` M Wolf Rayet Stars Dwz` D  ` E *Minimum mass limited by hydrogen burning: ` F Small mass ` G %  Low central temperature T c ` H   PP Chain cant start T ` I  (` J ni1Find:  M >0.1 M SUN  is necessary E` K 0 eb` L r )Note: M JUPITER =0.001 M SUN HH5USml?HHlRXTT e !d5VM XX14HH5WV HH>in` ? 6Xse ` < SInterpreting the C ` \  HR Diagrams of Clusters inf` N  ` O 10)Color-Magnitude HR Diagrams tell you the g` P , Distance   (Last Weeks Studio) ` Q W/and  Age    (This Weeks Studio) ` R muof star clusters. ` S  ` ^ l  s1` T GMeasuring the Age: al N` U  k W /Assumption: All stars in the cluster formed at  @ W nithe same time. >0.` Y is c V 1What is the highest mass (or most luminous) star R@ V Son the Main Sequence? ` Z /  This star is just about to leave the MS. ` [ !*  The cluster age is the (calculated) 6` X lifetime of this kind of star! HH5XVHHlU[WW d6 Y[[luerHH6 ZY O10HH0ia[D ` ] kSynthesis of the Elements ;` _   X` ` s*The Big Bang created Hydrogen and Helium. u` a  S` b /Carbon, oxygen, nitrogen, silicon, iron, ... ? ge:` c U ` d W"These were manufactured in stars!  f 0Nuclear reactions (other than hydrogen burning) @ f 8are possible  if the temperature is high enough . st#` g V S@` h en Examples: ]` m  sz` i t M4 He  + 4 He  + 4 He   12 C  +  energy t` j X<12 C  + 4 He   16 O  +  energy 5` k =16 O  + 4 He   20 Ne  +  energy ` p  ` l ;...  until you reach   A =56   (iron). 6  ` n O 0(` o *Then, core collapses   Supernova! 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