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TEACHER RESOURCE PLANETARIUM STARDOME OBSERVATORY & TIES ON... TIVI FACTS, RESOURCES AND AC STARS HOLES, NEUTRON PART 2 - BLACKIT ARFS STARS AND WH E DW ond part of isiting the stars in the sec In this resource, we’re rev You can find r. sta a of cle ut the life-cy our star series to learn abo part one here. of hydrogen into verts 700 million tonnes Every second the Sun con c2, we can E=m n atio ium. Using the equ 695 million tonnes of hel tonnes of energy st expel about 5 million calculate that the Sun mu the energy to Sun ing the size of the every second! By compar ut halfway abo y onl is it ted ula have calc it emits, astrophysicists Sun starts the en wh rs, another 5 billion yea through its lifecycle. In nt. As the helium gia red a into w gro will l, it running out of nuclear fue ses where the outer will undergo thermal pul core burns out, the Sun and the core of the ing a planetary nebula, layers will spread out, form size of Earth). the out (ab white dwarf star Sun will become a dense rs, but the yea of disperse over thousands universe. The planetary nebula will the in of w kno we ger than anything white dwarf will last lon can continue times larger than the Sun Stars that are about ten y reach iron. the il unt way the elements all nuclear fusion, creating the pressure e anc bal the star can no longer the star This is the point where and d, war out ng iati rad of energy of gravity with the force ire ent the in – the largest explosion explodes in a supernova nts heavier rks the creation of eleme spa on losi exp universe. The supernovae are rs outer layers of these sta than iron. The expelled neutron stars into n dow se lap col stars can remnants. The core of the or black holes. stars but contain smaller than white dwarf Neutron stars are even massive star. re mo a e they form from much more mass becaus ual ivid ind e forc rs sta se the of The pressure in the core ns to ctro ele e fus themselves and atoms to collapse in on ns to ctro ele no h wit and ns, tro protons. This creates neu into trons squeeze together force atoms apart, the neu m ntu me mo r ula ang s, ink shr a dense ball. As the star to ses rea inc r ation of the sta is conserved, and the rot . ond sec per hundreds of revolutions mic gets to a point where ato r sta the of sity If the den gravity er, eth tog ser clo any structures cannot get rity with es. This creates a singula overwhelms all other forc Gravity e. hol ck core becomes a bla infinite density, and the than er fast e hol ck bla a of core is pulling objects into the led pul s get re, anything that the speed of light. Therefo what is called the event from ble visi be to se in will cea escape, not even light. can g hin not horizon. From there e is no stronger than hol a black However, the gravity of the same l star. A black hole with the gravity of the origina rble, but ma of size the ut be abo mass as the Earth would Earth. ire ent tional pull as the still have the same gravita SCIEN CONTE CE NT/ CURRIC ULUM L ASTRON INK O MIC PHYSIC AL SYSTEMS, AND PH AL INQUIRY YSICS C THE STR ONCEPTS, UCT OF MAT URE TER. Sagittarius A* is the black hole at the centre of the Milky Way galaxy. Credits: NASA/UMass/ D.Wang et al., IR: NASA/STScI Black holes are invisible because nothing, not even light can escape. Credit: NASA and the Night Sky Network Check out these other resources... Wikipedia – Stellar Evolution: https://en.wikipedia.org/wiki/Stellar_evolution HubbleSite Black Holes: http://hubblesite.org/explore_astronomy/black_holes/encyc_mod3_q3.html DISCUSSION POINT What types of telescopes have observed black holes, and what behaviour of matter has been observed to conclude a black hole may be nearby? STARDOME.ORG.NZ 09 624 1246 ACTIVITY PLANETARIUM STARDOME OBSERVATORY & F O S E G A T S THE FINALEVOLUTION STELLAR You’ll need... Objective... on and some life with a ballo ’s ar st a of d en discover for To simulate the ity students will tiv ac is th t effect In il. work, and wha aluminium fo transformations e es star. th t w an ho illi s br themselve the once itational pull of av gr e th on ve they ha aluminium foil balloons pump scales tape measures Instructions... BLACK HOLE MASSIVE STAR it star) and cover lloon fully (the ar). st e th of • Blow up a ba s er lay il (the outer fo m iu in m alu with e scale al mass using th ecord the initi •R using the ” ar st he “t nce of and circumfere tape measure. e ar by having th llapse of the st . ps imulate the co po •S it til e the balloon un students squeez ts of foil to ee sh re e of the squa m eze so r fo w llo A • ”, but then sque the “supernova til un on llo ba “explode” off in ed ound the popp ar il fo g in ain m the re here. it is a dense sp rence. s and circumfe ecord the mas and •R ar ” from before 3 st nsity of “the de e r, th e )π at /3 ul (4 alc •C , volume= e (density=m/v after the collaps rence/2π). r radius=circumfe nt that no matte ould be appare sh it e, re tim is he th sp y •B to their sure they add on ill how much pres itational pull, w av gr e or ef and ther that the mass, ly the density. not increase, on rizon using e of the event ho t alculate the siz •C 2 ius of the even 2GM/c (R=rad al rs ive un the equation: R= G= , le s of the black ho -2 d -8 cm3 g-1 s , c=spee horizon, M=mas nstant 6.67x10 co l na tio ita av gr 10 /sec). e of light 3x10 cm it would becom ams, the radius-27 gr 30 is s e as th m d (If the x 10 cm, an uld be about 479 3 a black hole wo g/cm ). 10 x be about 9 density would eum of Nature the Denver Mus Adapted from ator Guide. ack Holes Educ and Science Bl 1 2 3 send it to us. d an ity tiv ac ur yo of o ot ph a ke Ta ardome.org.nz We’d love to see it! education@st STARDOME.ORG.NZ 09 624 1246