Life of a Star. Pillars of Creation

Life of a Star

Life of a Star Pillars of Creation

Life of a Star Pillars of Creation Stars form from massive clouds of gas that primarily consist of hydrogen.

Life of a Star Gravity causes gas to contract and increase in temperature. (Gravitational contraction)

Life of a Star This is known as a protostar. A protostar has not started nuclear fusion yet.

Life of a Star Eventually nuclear fusion begins in the core.

Life of a Star

Life of a Star Stars can be born with masses from.08m to 150M.

Life of a Star Stars that are only converting hydrogen to helium are called main sequence stars.

Life of a Star Hertzsprung-Russell diagram plots luminosity of a star versus its surface temperature. (HR diagram)

Life of a Star

Life of a Low Mass Star Our Sun is a low mass star.

Life of a Low Mass Star

Life of a Low Mass Star A low mass star will stay on the main sequence for about 10 billion years until it stops burning hydrogen in its core.

Life of a Low Mass Star The star will fill up its core with helium and stop nuclear fusion.

Life of a Low Mass Star Gravity will contract the star and cause the hydrogen around the helium core to start nuclear fusion.

Life of a Low Mass Star The nuclear fusion in the shell around the core will force the star to expand. (Red Giant)

Life of a Low Mass Star The star will stay like this for a few hundred million years.

Life of a Low Mass Star More helium is created and forced into the core, heating it up. Eventually helium will start nuclear fusion (helium flash).

Life of a Low Mass Star Helium to Carbon nuclear fusion. 3 helium nuclei are fused into 1 carbon which releases energy.

Life of a Low Mass Star The star stabilizes, shrinks back down, and becomes more yellow.

Life of a Low Mass Star The star will stay like this for 100 million years.

Life of a Low Mass Star Eventually the star will fill its core up with carbon and nuclear fusion in the core will stop.

Life of a Low Mass Star Gravity will contract the star and cause the helium around the carbon core to start nuclear fusion.

Life of a Low Mass Star The nuclear fusion in both shells around the core will force the star to expand even more than before. (Red Giant)

Life of a Low Mass Star The star will stay like this for 1 million years.

Life of a Low Mass Star Eventually nuclear fusion will stop all together and the outer layers of the star will be carried away by the solar wind.

Life of a Low Mass Star The outer layers float away and are called planetary nebula.

Life of a Low Mass Star planetary nebula the glowing cloud of gas ejected from a low-mass star at the end of its life.

Life of a Low Mass Star Only the small core of the star is left which shines from the left over heat. (White dwarf)

Life of a Low Mass Star White dwarf -- The hot, compact corpses of low-mass stars, typically with a mass similar to the Sun compressed to a volume the size of the Earth.

Life of a Low Mass Star

Life of a Low Mass Star Low mass star life cycle.

Life of a High Mass Star

Life of a High Mass Star A massive star will have a hotter core which will increase the nuclear fusion rate, thus a shorter life span.

Life of a High Mass Star A high mass star may live for only 10 to 100 million years.

Life of a High Mass Star High mass stars enter the main sequence in this area. While on the main sequence, stars fuse hydrogen to helium.

Life of a High Mass Star CNO Nuclear Fusion Cycle

Proton-proton Nuclear Fusion (Low mass stars) Life of a High Mass Star CNO Nuclear Fusion Cycle CNO Nuclear Fusion (High mass stars)

Proton-proton Nuclear Fusion (Low mass stars) Life of a High Mass Star CNO Nuclear Fusion Cycle CNO Nuclear Fusion (High mass stars) Produces more energy

Life of a High Mass Star A high mass star will exhaust its hydrogen fuel and begin nuclear fusion in a shell around the core expanding into a Supergiant.

Life of a High Mass Star Eventually nuclear fusion will begin in the core, fusing helium to carbon, and the star will stabilize.

Life of a High Mass Star This process happens many times as the star begins nuclear fusion with heavier elements.

Life of a High Mass Star The star continues the fusion process until it reaches iron (Fe), which the star cannot fuse into heavier elements.

Life of a High Mass Star Fusion in the core stops, but the outer shells continue fusion, depositing more iron in the core.

Life of a High Mass Star The extreme pressure on the iron core pushes the core electrons into the protons, creating neutrons, shrinking the core.

Life of a High Mass Star Empty space is created around the tiny core. The outside layers rush towards the center of the star and collide. Theoretically, the collision in the core causes a massive explosion called a supernova.

Life of a High Mass Star Theoretically, the collision in the core causes a massive explosion called a supernova.

Life of a High Mass Star Supernova can be as bright as 10 billion Suns.

Life of a High Mass Star Either a neutron star or a black hole will be left behind.

Life of a High Mass Star Neutron star -- The compact corpse of a high-mass star left over after a supernova; typically 1M with a radius of a few kilometers.

Life of a High Mass Star Neutron star -- The compact corpse of a high-mass star left over after a supernova; typically 1M with a radius of a few kilometers. Earth White dwarf

Life of a High Mass Star Neutron star -- The compact corpse of a high-mass star left over after a supernova; typically 1M with a radius of a few kilometers.

Life of a High Mass Star If the star has enough mass, it will leave a black hole instead of a neutron star.

Life of a High Mass Star Black hole a region of spacetime from which gravity prevents anything, including light, from escaping.

Life of a High Mass Star How can we see black holes if no light can escape?

Life of a High Mass Star

Life of a Low Mass Star High-mass star life cycle.

Life of a Low Mass Star

http://boojum.as.arizona.edu/~jill/ns102_2006/lectures/lecture20/hrdiagram/16-10.jpg http://www.proprofs.com/flashcards/upload/a6412310.jpg http://www.messagetoeagle.com/images/supernovadestrplanet.jpg http://imgsrc.hubblesite.org/hu/db/images/hs-1995-44-a-full_jpg.jpg http://upload.wikimedia.org/wikipedia/commons/1/16/ngc2392.jpg http://scitechdaily.com/images/image-of-the-planetary-nebula-ngc-5189.jpg http://upload.wikimedia.org/wikipedia/commons/f/f3/sirius_a_and_b_hubble_photo.jpg http://lnns.webs.com/lnns/star_main_seq.jpg http://cse.ssl.berkeley.edu/bmendez/ay10/2000/cycle/redgiant.gif http://www.ast.smith.edu/james/a111f06/lectures/figs/bt2lf1609_a.jpg http://astronomyonline.org/stars/images/massivestarlifecycle.gif http://www.astrobio.net/images/galleryimages_images/gallery_image_6538.jpg https://lh5.googleusercontent.com/-yat7uzggtvu/um3o2fkmhhi/aaaaaaaaalu/fth6mg5vnb0/w500/tumblr_mf2rfhuzd31qa77t4o1_500.jpg http://www.seasky.org/celestial-objects/assets/images/starlife.jpg http://intouniverse.weebly.com/uploads/5/5/9/8/5598621/star_evolution.jpg http://web.utah.edu/astro/astroinfo/casa_broadband.jpg http://www.daviddarling.info/images/shell_burning.jpg http://abyss.uoregon.edu/~js/images/core_exhaustion.gif http://cse.ssl.berkeley.edu/bmendez/ay10/2002/notes/pics/bt2lf16un1_a.jpg http://apod.nasa.gov/apod/image/0702/ngc2440_hst_full.jpg http://upload.wikimedia.org/wikipedia/commons/5/5a/ngc6543.jpg http://nssdc.gsfc.nasa.gov/image/astro/hst_hourglass_nebula.jpg http://www.physics.unlv.edu/~jeffery/astro/starevol/planetary/planetary_catseye.jpg http://www.dailygalaxy.com/.a/6a00d8341bf7f753ef017ee8bb15b8970d-pi http://www.astronomy.ohio-state.edu/~pogge/ast162/unit3/images/whitedwarf.gif http://www.bbc.co.uk/schools/gcsebitesize/science/images/star_dwarf_5.jpg http://www.oswego.edu/~kanbur/a100/images/cnocycle.jpg http://www.physast.uga.edu/~rls/1020/ch17/17-17.jpg http://woodahl.physics.iupui.edu/astro105/17_12figure.jpg http://astronomy.nmsu.edu/tharriso/ast110/1322_1616.jpg http://sciencequestionswithchris.files.wordpress.com/2013/01/momentumtransfer.gif http://thunderf00tdotorg.files.wordpress.com/2011/08/first-supernova-animated-gif.gif http://www.backyardastronomer.com/sn/m51_sn_2011_1.gif http://img.gawkerassets.com/img/194x89g3upe61gif/k-bigpic.gif http://www.davelane.ca/aro/sn/sn.gif http://media.skyandtelescope.com/images/m101_supernova.gif http://newswatch.nationalgeographic.com/files/2011/06/sn_m51_lamotte.gif http://ttt.astro.su.se/~mstri/sn09bb_rgbblink.gif http://www.pitt.edu/news2010/supernova_explode.gif http://okc.albanova.se/blog/wp-content/uploads/2013/05/sn2011dh-bvr-pre-post-comb-4.gif http://img.gawkerassets.com/img/194x89g3upe61gif/ku-xlarge.gif http://upload.wikimedia.org/wikipedia/commons/thumb/3/37/evolved_star_fusion_shells.svg/280px-evolved_star_fusion_shells.svg.png http://pensivetoaster.com/wp-content/uploads/2013/09/geminga.jpg https://heasarc.gsfc.nasa.gov/images/xte/earthwd.gif http://api.ning.com/files/qg3gjv95bu-axtithy2wxgnlzjnkkr3jisrcfvr-lpwzsa9kc*sba88bhbqhw*ofszaeseur5aktocfgxzr2iyq11k2c91oo/neutronstar_vancouver600.jpg http://www.askamathematician.com/wp-content/uploads/2012/02/black-hole-star-accretion.jpg http://walkwithjesusonline.com/wp-content/uploads/2013/10/black_hole_weaponry_wallpaper-normal.jpg http://www.nasa.gov/sites/default/files/images/729665main_a-blackholeart-pia16695_full.jpg http://ircamera.as.arizona.edu/natsci102/natsci102/movies/gclarge.gif http://www.mpe.mpg.de/410729/orbits3d_small_gif.gif http://www.phas.ubc.ca/~heyl/astr304_2003w/orbits_pause.gif