Life Cycle of a Star Introduction to Stellar
- Slides: 50
Life Cycle of a Star Introduction to Stellar Stages & Blackbody Spectrum
Table Talk w/Chalk 1. 2. 3. 4. 5. How does the sun produce energy? How is fusion different from bonding? Do small stars or large stars burn faster? Do small stars or large stars burn hotter? When does fusion stop in a red supergiant? Why? 6. What determines the life cycle of a star? 7. Where do stars begin to form?
The Big Bang and Soon After The “Cosmic Microwave Background Radiation” (CMB), Present Day "Ilc 9 yr moll 4096" by NASA / WMAP Science Team - http: //map. gsfc. nasa. gov/media/121238/ilc_9 yr_moll 4096. png. Licensed under Public Domain via Wikimedia Commons http: //commons. wikimedia. org/wiki/File: Ilc_9 yr_moll 4096. png#mediaviewer/File: Ilc_9 yr_moll 4096. png
The Big Bang and Soon After (ctd. ) Temp Cools from 10 Billion K to 1 Billion K "Scheme of nuclear reaction chains for Big Bang nucleosynthesis" by Pamputt - Own work ; vectorisation de The main nuclear reaction chains for Big Bang nucleosynthesis. jpg. Licensed under CC BY-SA 4. 0 via Wikimedia Commons http: //commons. wikimedia. org/wiki/File: Scheme_of_nuclear_reaction_chains_for_Big_Bang_nucleosynthesis. svg#mediaviewer/File: Scheme_of_nuclear_reaction_chains_for_Big_Bang_nucleosynthesis. svg
Life and Death of Stars Recapitulation of How Elements are Formed
Life Cycle of a Star
Life of a Small Star Around the mass of 1 Sun up to ~5 Solar Masses
“Before she became a star…” Nebula – Cloud of Gas (mostly H) "Eagle nebula pillars" by Credit: NASA, Jeff Hester, and Paul Scowen (Arizona State University) - http: //hubblesite. org/newscenter/newsdesk/archive/releases/2003/34/image/a. Licensed under Public Domain via Wikimedia Commons - http: //commons. wikimedia. org/wiki/File: Eagle_nebula_pillars. jpg#mediaviewer/File: Eagle_nebula_pillars. jpg
“On her way to the audition…” Protostar (NOT A STAR YET) "Witness the Birth of a Star" by NASA/JPL-Caltech/R. Hurt (SSC) - Image of the day gallery. Licensed under Public Domain via Wikimedia Commons http: //commons. wikimedia. org/wiki/File: Witness_the_Birth_of_a_Star. jpg#mediaviewer/File: Witness_the_Birth_of_a_Star. jpg
Once it’s hot enough… NUCLEAR FUSION "Fusioninthe. Sun" by Borb. Licensed under CC BY-SA 3. 0 via Wikimedia Commons - http: //commons. wikimedia. org/wiki/File: Fusioninthe. Sun. svg#mediaviewer/File: Fusioninthe. Sun. svg
How Fusion Works (Yes, you can actually know this. ) • Need very high temperatures, ~10 -15 million K • Protons overcome repulsion – Stick due to “Strong Nuclear Force” • Mass of 4 p+ > Mass of 1 He – Where did the missing mass go?
How Fusion Works (ctd. ) • E = mc 2 • Lost mass is converted to energy! • Basis for all fusion processes that release (or absorb) energy
“A star is born!” Main Sequence – Doing H Fusion "The Sun in extreme ultraviolet" by NASA - [1]. Licensed under Public Domain via Wikimedia Commons http: //commons. wikimedia. org/wiki/File: The_Sun_in_extreme_ultraviolet. jpg#mediaviewer/File: Th e_Sun_in_extreme_ultraviolet. jpg "Sirius A and B Hubble photo" by NASA, ESA, H. Bond (STSc. I), and M. Barstow (University of Leicester) - http: //www. spacetelescope. org/images/html/heic 0516 a. html. Licensed under CC BY 3. 0 via Wikimedia Commons http: //commons. wikimedia. org/wiki/File: Sirius_A_and_B_Hubble_photo. jpg#mediaviewer/File: Siri us_A_and_B_Hubble_photo. jpg
After billions of years… • H fuel runs out in the middle, He accumulates • Not hot enough to fuse together He atoms • Gravity starts to take over!
“She suffered a partial collapse…” A Small Star Evolves • Outside comes in, REHEATING DUE TO GRAVITATIONAL POTENTIAL • It’s Red Giant time! • Hot enough to fuse He into C, N • (See next slide for size comparison)
Red Giant Stage – An Old “Small” Star "The life cycle of a Sun-like star (annotated)" by ESO/M. Kornmesser - http: //www. eso. org/public/images/eso 1337 a/. Licensed under CC BY 4. 0 via Wikimedia Commons http: //commons. wikimedia. org/wiki/File: The_life_cycle_of_a_Sun-like_star_(annotated). jpg#mediaviewer/File: The_life_cycle_of_a_Sun-like_star_(annotated). jpg
“So explosive!” Losing the Shell – Planetary Nebula • Fusion of He to C, N releases much more energy • Gravity can’t hold it together • Loses the outer gases – Planetary Nebula – NOTHING TO DO WITH PLANETS "Seeing into the Heart of Mira A and its Partner" by ESO/S. Ramstedt (Uppsala University, Sweden) & W. Vlemmings (Chalmers University of Technology, Sweden) http: //www. eso. org/public/images/potw 1447 a/. Licensed under CC BY 4. 0 via Wikimedia Commons http: //commons. wikimedia. org/wiki/File: Seeing_into_the_Heart_of_Mira_A_and_its_Partner. jpg# mediaviewer/File: Seeing_into_the_Heart_of_Mira_A_and_its_Partner. jpg
Another Planetary Nebula Colors = different elements • helium (blue) • oxygen (green) • nitrogen (red) "M 57 The Ring Nebula" by The Hubble Heritage Team (AURA/STSc. I/NASA) - http: //hubblesite. org/newscenter/archive/releases/1999/01/image/a/ (direct link). Licensed under Public Domain via Wikimedia Commons - http: //commons. wikimedia. org/wiki/File: M 57_The_Ring_Nebula. JPG#mediaviewer/File: M 57_The_Ring_Nebula. JPG
“How do you feel inside? ” The Leftover Core – White Dwarf • Core is white hot, but NOT hot enough to fuse C with C • Most white dwarfs simply fade out over a LONG time – Theoretical “black dwarf” is typical fate • But there may be another way to go out! "Sirius A and B Hubble photo. editted" by Bokus http: //upload. wikimedia. org/wikipedia/commons/f/f 3/Sirius_A_and_B_Hubble_photo. jpg. Licensed under Public Domain via Wikimedia Commons http: //commons. wikimedia. org/wiki/File: Sirius_A_and_B_Hubble_photo. editted. PNG#mediaviewe r/File: Sirius_A_and_B_Hubble_photo. editted. PNG
Type Ia Supernova “She got help from a friend…” Enough energy is released to fuse C into elements heavier than C. "Progenitor IA supernova" by NASA, ESA and A. Feild (STSc. I); vectorisation by chris 論 - http: //hubblesite. org/newscenter/archive/releases/star/supernova/2004/34/image/d/. Licensed under CC BY 3. 0 via Wikimedia Commons - http: //commons. wikimedia. org/wiki/File: Progenitor_IA_supernova. svg#mediaviewer/File: Progenitor_IA_supernova. svg
Type Ia Supernova – Example High-Z Supernova Search Team/HST/NASA
Life of a Large Star Around the mass of 8 Suns and up
Life Cycle of a Star
Large Stars on the Main Sequence More mass → More gravitational energy → Higher core temperature → Faster fusion rate → Shorter time on the main sequence "Hot and brilliant O stars in star-forming regions" by ESO - http: //www. eso. org/public/images/eso 1230 b/. Licensed under CC BY 3. 0 via Wikimedia Commons http: //commons. wikimedia. org/wiki/File: Hot_and_brilliant_O_stars_in_star-forming_regions. jpg#mediaviewer/File: Hot_and_brilliant_O_stars_in_star-forming_regions. jpg
A Large Star Evolves – Red Supergiant Stage(s) • Akin to small mass star, fuel runs out, core reheats, fusing He to C • Enough mass to repeat the process, fusing heavier and heavier elements – Ne, Mg, Al, for example – All the way up to Fe • Resembles an onion Betelgeuse at upper left is a red supergiant "Orion Head to Toe" by Rogelio Bernal Andreo - http: //deepskycolors. com/astro/JPEG/RBA_Orion_Head. Toes. jpg. Licensed under CC BY-SA 3. 0 via Wikimedia Commons http: //commons. wikimedia. org/wiki/File: Orion_Head_to_Toe. jpg#mediaviewer/File: Orion_Head_to_Toe. jpg
“A total collapse!” End of a Large Star • Fe builds up in the core • Not enough outward pressure – Gravity takes over • Outer layers rush in, and BOUNCE off the core – Enough energy released to fuse ANY naturally occurring element – Surplus of energy can form Au, Pb, I, etc. "HST SN 1987 A 20 th anniversary" by NASA, ESA, P. Challis, and R. Kirshner (Harvard. Smithsonian Center for Astrophysics) http: //hubblesite. org/newscenter/archive/releases/2007/10/image/a/ (direct link). Licensed under Public Domain via Wikimedia Commons http: //commons. wikimedia. org/wiki/File: HST_SN_1987 A_20 th_anniversary. jpg#mediaviewer/File: HST_SN_1987 A_20 th_anniversary. jpg
The Aftermath – Neutron Stars and Black Holes "Isolated. Neutron. Star" by Original uploader was Northgrove at en. wikipedia - Transferred from en. wikipedia. Licensed under Public Domain via Wikimedia Commons http: //commons. wikimedia. org/wiki/File: Isolated. Neutron. Star. jpg#mediaviewer/File: Isolated. Neutro n. Star. jpg "BH LMC" by User: Alain r - Own work. Licensed under CC BY-SA 2. 5 via Wikimedia Commons http: //commons. wikimedia. org/wiki/File: BH_LMC. png#mediaviewer/File: BH_LMC. png
Other Element Formation – Cosmic Rays • High-energy particles either left over from the Big Bang or ejected from stars/supernovae • Slam into heavier elements occasionally and split them into smaller nuclei – E. g. , Li, Be, B Earth’s Moon blocks muon cosmic rays "Moon's shadow in muons" by http: //hepweb. rl. ac. uk/pp. UKpics/POW/pr_990602. html. Licensed under Fair use via Wikipedia http: //en. wikipedia. org/wiki/File: Moon%27 s_shadow_in_muons. gif#mediaviewer/File: Moon%27 s_ shadow_in_muons. gif
Life Cycle of a Star
Summary – Different Processes Make Elements • Big Bang – H, He, Li (a little) • Small Mass Stars – He (main sequence) – C, N (red giant) – Heavier than C (only type Ia supernova) • Large Mass Stars – He (main sequence) – C, N, etc. , all the way up to Fe (red supergiant) – All natural elements (only type II supernova) • Cosmic Rays – Li, Be, B (split off from larger atoms)
Stellar Nursery Eagle Nebula Pillars from Hubble, opposite. stsci. edu Columns: H gas What do you notice at the top? Pillars are slowly eroded away by UV light = Evaporating Gas Globules (Eggs) denser gas uncovered
Can the color of a glowing object tell us the temperature of the object? Hot……. . . Hotter…. . . Hottest!
The electromagnetic spectrum Google images
Blackbody Simulation
How do we sample the universe? Betelgeuse Red Giant making Ca and beyond. Future supernova. p 3 steadily making He. Future C, N Orion Nebula New stars getting heavy elements. Future Earths? Rigel - Blue Supergiant making, He, C, N. Future heavy elements.
What is light?
What do you see? By The copyright holder of this image, Christopher Down, allows anyone to use it, Attribution, https: //commons. wikimedia. org/w/index. php? curid=3642142
What accounts for sunlight? By The copyright holder of this image, Christopher Down, allows anyone to use it, Attribution, https: //commons. wikimedia. org/w/index. php? curid=3642142
Recapitulate the Bohr Model : Shown above – Red line is 656 nm transition By A_hidrogen_szinkepei. jpg: User: Szdoriderivative work: Orange. Dog (talk • contribs) A_hidrogen_szinkepei. jpg, CC BY 2. 5, https: //commons. wikimedia. org/w/index. php? curid=6273602 By Jan Homann - Own work, CC BY-SA 3. 0, https: //commons. wikimedia. org/w/index. php? curid=6504291
Sample Emissions (Plasma Light Version) • You need… – Diffraction tools (rough spectrometers) – Reference sheet of emission/absorption spectra • Your teacher will energize a few gaseous elements with an electric current • Observe the distinct wavelengths – Sample A is _______ and overall appears _______ – Sample B is _______ and overall appears _______ – Sample C is _______ and overall appears _______
Sunlight Through a Spectroscope By Fraunhofer_lines. jpg: nl: Gebruiker: Maureen. VSpectrum-s. RGB. svg: Phrood. Fraunhofer_lines_DE. svg: *Fraunhofer_lines. jpg: Saperaud 19: 26, 5. Jul. 2005 derivative work: Cepheiden (talk) - Fraunhofer_lines. jpg. Spectrum-s. RGB. svg. Fraunhofer_lines_DE. svg, Public Domain, https: //commons. wikimedia. org/w/index. php? curid=7003857 Discuss: What do you think determines this pattern of light?
How do these compare to what we just saw? Richmond, Michael. http: //spiff. rit. edu/classes/phys 301/lectures/class. html
Putting the Moves Together (Pictorially) http: //www. uni. edu/morgans/astro/course/Notes/section 1/new 4. html
Putting the Moves Together (Verbally) • Stars release many energies of light – The spread based on temperature • Elements can absorb light on its way out – The colors based on electron transitions • Between the kinds of light released and absorbed, we can draw conclusions about the star’s temperature, composition, and other features
Challenge: 1. Order these like a human 2. Identify some present elements 3. Infer some other star features Richmond, Michael. http: //spiff. rit. edu/classes/phys 301/lectures/class. html
Ordering Created by Annie Jump Cannon (a Human) Note: Not the exact spectra you used. Richmond, Michael. http: //spiff. rit. edu/classes/phys 301/lectures/class. html
Further mysteries await…
What is happening in the lower spectra? NOAO/AURA/NSF
Univ. Chicago Press (1943) http: //ned. ipac. caltech. edu/level 5/ASS_Atlas/Plate 23. html
Stellar Spectra – Summary • A mystery star is far away and hard to access directly • Star emits a continuum (spectrum) of light – Based on temperature, particles release many wavelengths • Only particular elements are present in the star • Elements absorb only particular wavelengths as the light is leaving – Energy absorbed to cause electron jumps (same as emission lines) • Based on the blanks (absorption lines), we can deduce what elements are present in greater abundance
- Flowchart of the life cycle of a star
- Bearing gifts we traverse afar
- Stellar evolution diagram
- Which island is the oldest
- What is charted on an hr diagram
- Life cycle of a low to medium mass star
- What is the life cycle of a star
- Life cycle of a star
- Star life cycle
- Rad model in software engineering
- High mass star life cycle
- Star lifecycle model
- Star life cycle model
- What are the stages of a stars life cycle
- Life cycle of an average star
- Star life cycle from birth to death
- The life cycle of a star nebular hypothesis
- Our sun life cycle
- Star life cycle from birth to death
- Life cycle of a star video
- Subgiant star life cycle
- Life cycle of a star
- Hci in software process
- Life cycle of a star
- Star life cycle diagram
- Concurrent development model advantages and disadvantages
- Medium mass star life cycle
- Conclusion butterfly life cycle
- Section 26.3 life cycles of stars
- Hananel hazan
- What do star events stand for
- Atmospheric heaven
- Mizar luminosity
- Stellar evolution diagram
- Stellar motion matlab
- Virgo stellar
- Masses in the stellar graveyard
- Iptv hosting
- Stellar assessment
- Stellar saga
- What is stellar parallax?
- Stellar evolution
- Stellar
- Stellar formation
- Stellar asset management
- Stellar evolution
- Becquerel
- Stellar evolution
- Hr diagram
- Stellar wifi
- Stellar alchemy