We think you have liked this presentation. If you wish to download it, please recommend it to your friends in any social system. Share buttons are a little bit lower. Thank you!
Presentation is loading. Please wait.
Published byAlyssa West
Modified over 2 years ago
Alessandro Chieffi (Istituto di Astrofisica Spaziale e Fisica Cosmica & INAF)
25 M O 1 M O 5 M O
REMEMBER that: The interplay between the evolution of a star and the nuclear processes occurs through the RATES and NOT the cross sections: R lk => X l x X k x screening x lk
25 M O 5 M O 1 M O PP chain CNO cycle 14 N(p, ) 15 O p(p,e + )d t(H-burn)= - 0.3% t(H-burn)= - 4% M(He) => 0.91 to 0.97 M O M(He) => 8.3 to 8.6 M O 3 x 10 is NOT appreciable x 10 t(H-burn)= - 3%
MS TO RGB HB
10 Gyr Z=10 -4 Y=0.23 Dashed => ( 14 N(p, ) 15 O) / 2 13 Gyr Solid => reference
M=0.8 M O Y=0.23 Z=10 -4 M He = 1% M bol (tip) = Mag Red – reference Blue – 14 N(p, ) 15 O / Mag => Gyr
CO core H-rich mantle He burning shell He (+C) intershell H burning shell AGB phase R(H shell ) ~10 -5 R star 0.7 < M / M O < 7 Neutron production s process nucleosynthesis
Convective envelope He shell H shell t(yr) M(M O )
Convective envelope He shell H shell t(yr) M(M O ) He conv. shell
Base conv. env. H burn. shell He burn. shell Log(Surf. C abund.) Log(Tmax He shell) Log(T base conv. Env.)
M=3 M O Z=0.02 Y=0.284 Neutron captures on: Fe Kr84 – Rb – Sr – Y – Zr92 Xe132 – Cs – Ba – La – Ce – Pr – Nd144 Hg202 – Tl – Pb – Bi209 Network: H to Si (full) + 92 nuclei
Log 10 (PF) Element
Log 10 (PF) Stable Isotopes
Reference 3 / 2 3 x 2 M=3 M O - Z= Np
Reference 3 / 2 3 x 2 14 Np SURFACE CARBON ABUNDANCE
The mother of all rates: 12 C(, ) 16 O
Roadmap... 1) WR stars: evolution & explosive nucleosynthesis ) Intermediate Mass Stars: elemental yields
INAF The advanced evolutionary phases of the massive stars and their explosive yields Alessandro Chieffi Istituto Nazionale di AstroFisica (Istituto di.
The massive zero metal stars: their evolutionary properties and their explosive yields. Alessandro Chieffi Istituto Nazionale di AstroFisica (Istituto.
More Nucleosynthesis –final products are altered by the core collapse supernova shock before dispersal to the ISM hydrogen, helium, and carbon burning.
Stellar Fuel, Nuclear Energy and Elements How do stars shine? E = mc 2 How did matter come into being? Big bang stellar nucleosynthesis How did different.
Selected Topics in Astrophysics. Solar Model (statstar) Density Mass Luminosity Temperature Nuclear Reaction Rate Pressure.
On the Nature of the Thermal Pulses on the Asymptotic Giant Branch Alessandro Chieffi Istituto Nazionale di AstroFisica (Istituto di Astrofisica Spaziale.
Presolar grains and AGB stars Maria Lugaro Sterrenkundig Instituut University of Utrecht.
52° CONGRESSO SAIT TERAMO, MAGGIO 2008 The s-nucleosynthesis process in massive AGB and Super-AGB stars M.L. Pumo CSFNSM - Università di Catania.
Lecture 2: Formation of the chemical elements Bengt Gustafsson: Current problems in Astrophysics Ångström Laboratory, Spring 2010.
The origin of heavy elements in the solar system each process contribution is a mix of many events ! (Pagel, Fig 6.8) Location of peaks indicates n-capture.
Prelim Review. <1.2 M <1.2 M 1.Hayashi track - fully convective cooler surface temp. requires super- sonic convection. Ends.
Asymptotic Giant Branch. Learning outcomes Evolution and internal structure of low mass stars from the core He burning phase to the tip of the AGB Nucleosynthesis.
Study of the s-process in low mass stars of Galactic disc metallicity Laura Husti Roberto Gallino Sara Bisterzo.
Selected Topics in Astrophysics. Evolution of high mass stars ⊙ The evolution we covered in last class is for low mass stars (M < 4 M ⊙ ) temperature.
Stellar Structure Section 6: Introduction to Stellar Evolution Lecture 16 – Evolution of core after S-C instability Formation of red giant Evolution up.
Core Collapse SNe Inma Domínguez Marco Limongi. Evolution of Massive Stars Hydrostatic Nucleosynthesis Explosion Mechanism Explosive Nucleosynthesis.
The synthesis of 26 Al, 60 Fe and 44 Ti in massive stars and their current inventory in our Galaxy Alessandro Chieffi Istituto Nazionale di AstroFisica.
25 seconds left….. 24 seconds left….. 23 seconds left…..
1/34 PRESUPERNOVA EVOLUTION AND EXPLOSION OF MASSIVE STARS: CHALLENGES OF THE NEXT CENTURY Marco Limongi INAF – Osservatorio Astronomico di Roma, ITALY.
CSI661/ASTR530 Spring, 2011 Chap. 2 An Overview of Stellar Evolution Feb. 23, 2011 Jie Zhang Copyright ©
Susan CartwrightOur Evolving Universe1 The Lives of Stars n From studying nearby stars and stellar clusters l most stars are on the main sequence l stars.
Massive Star Evolution overview Michael Palmer. Intro - Massive Stars Massive stars M > 8M o Many differences compared to low mass stars, ex: Lifetime.
O. Straniero, L. Piersanti (Osservatorio di Teramo, INAF) R. Gallino (Universita’ di Torino) I. Dominguez (Univerdad de Granada) Light and heavy elements.
The Red Giant Branch. L shell drives expansion L shell driven by M core - as | |, | T| increase outside contracting core shell narrows, also L core.
The Sun in the Red Giant Phase (view from the Earth!)
The stick diagram for molybdenum looks lilke this: MS for Mo 1.How many isotopes does Mo have? 2.Write symbol for each isotope. 3.Which isotope is most.
Lesson 13 Nuclear Astrophysics. Elemental and Isotopic Abundances.
Jeopardy Topic 1Topic Q 1Q 6Q 11Q 16Q 21 Q 2Q 7Q 12Q 17Q 22 Q 3Q 8Q 13Q 18Q 23 Q 4Q 9Q 14Q 19Q 24 Q 5Q 10Q 15Q 20Q 25 Final Jeopardy.
Stellar Evolution Beyond the Main Sequence. On the Main Sequence Hydrostatic Equilibrium Hydrogen to Helium in Core All sizes of stars do this After this,
Nuclear Fission 235 U + n 93 Rb Cs + 2 n Not unique. Low-energy fission processes. 1Nuclear Reactor Theory, JU, Second Semester, (Saed.
Chapter 5: Cosmic foundations for origins of life - stars.
Nuclear Reactions. Binding Energies The mass law below represents the masses of thousands of nuclei with a few parameters B=(Z(m p +m e )+(A-Z)m n - M(A,Z))c.
Isotopes & Average Atomic Mass. What are isotopes? Atoms of the same element that have different numbers of neutrons and different atomic masses.
The origin of the (lighter) elements The Late Stages of Stellar Evolution Supernova of 1604 (Kepler’s)
ASTR730 / CSI661 Fall 2012 CH2. An Overview of Stellar Evolution September 04, 2012 Jie Zhang Copyright ©
Why Galaxies care about Asymptotic Giant Branch stars S. Cristallo (INAF - Osservatorio Astronomico di Teramo) Collaborators: O. Straniero, R. Gallino,
H205 Cosmic Origins Our last class! Origin of the Elements Hand in EP7 APOD Tom Lehrer's "The Elements". A Flash animation by Mike Stanfill, Private.
Addition 1’s to
Nuclear and Radiation Physics, BAU, First Semester, (Saed Dababneh). 1 Nuclear Binding Energy B tot (A,Z) = [ Zm H + Nm n - m(A,Z) ] c 2 B m.
18-19 Settembre 2006 Dottorato in Astronomia Università di Bologna.
We will resume in: 25 Minutes We will resume in: 24 Minutes.
M up Oscar Straniero & Luciano Piersanti INAF - Osservatorio di Teramo.
Eugenio Carretta INAF- Osservatorio Astronomico di Padova L’anticorrelazione Na-O: sonda per la formazione e la prima evoluzione degli ammassi globulari?
The Reactions The Main Sequence – The P – P Chain 1 H + 1 H 2 H + proton + neutrino 2 H + 1 H 3 He + energy 3 He + 3 He 4 H + 1 H + 1 H + energy.
Center for Stellar and Planetary Astrophysics Monash University Summary prepared by John Lattanzio, Dec 2003 Abundances in NGC6752.
NUCLEOSYNTHESIS IN STELLAR EVOLUTION AND EXPLOSIONS: ABUNDANCE YIELDS FOR CHEMICAL EVOLUTION. MASSIVE STARS Marco Limongi INAF – Osservatorio Astronomico.
Descriptive Inorganic Chemistry Chem M, W, F Bill Vining 61 Bacon Hall
Test B, 100 Subtraction Facts
© 2017 SlidePlayer.com Inc. All rights reserved.