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Signatures of Peculiar Supernova Nucleosynthesis in Extremely α-enhanced Stars We have performed a spectroscopic study on several extremely alpha-enhanced stars having FeH…
Early Galactic Nucleosynthesis: The Impact of HST/STIS Spectra of Metal-Poor Stars Chris Sneden University of Texas A Very Collaborative Effort Definitions: [A/B] = log10(NA/NB)star…
Astron. Astrophys. 335, 1009–1017 (1998) ASTRONOMY AND ASTROPHYSICS Abundance analysis of the λ Bootis stars HD 192640, HD 183324 and HD 84123? U. Heiter, F. Kupka, E.…
Stellar evolution and nucleosynthesis in helium- enriched stars Amanda Karakas With Anna F. Marino & David M. Nataf, Luke Shingles, Carolyn Doherty, & John Lattanzio…
lecture15Explosive Nucleosynthesis and the r-Process As the shock wave passes through the star, matter is briefly heated to temperatures far above what it would have experienced
Early Galactic Nucleosynthesis: The Impact of HST/STIS Spectra of Metal-Poor Stars Chris Sneden University of Texas A Very Collaborative Effort Definitions: [A/B] = log10(NA/NB)star…
Nucleosynthesis Big Bang Nucleosynthesis light elements deuterium bottleneck Nuclear Reactions in Stars hydrogen burning triple-α process BBN板書 Nuclear binding energy…
P o S ( N I C X I ) 0 0 3 Study of the Big Bang Nucleosynthesis reaction D(α,γ)6Li deep underground at LUNA M. Erhard∗ for the LUNA-Collaboration (http://luna.lngs.infn.it/)
MNRAS 456, 1886–1900 2016 doi:10.1093mnrasstv2648 2MTF – V. Cosmography, β, and the residual bulk flow Christopher M. Springob,1,2‹ Tao Hong,1,2,3 Lister Staveley-Smith,1,2…
ΕΤΗΣΙΑ ΕΚΔΟΣΗ • ΔΙΑΝΕΜΕΤΑΙ ΔΩΡΕΑΝ • FREE COPY • ΚΑΛΟΚΑΙΡΙ 2011 • SUMMER 2011 1GOLDENSTARS 2 GOLDENSTARS Ετήσια Έκδοση…
Bland-Hawthorn First stars Bland-Hawthorn Bland-Hawthorn When did the first star form? Maybe as early as z~65? But certainly by z~20-30 5σ 1σ 4σ ???? Bland-Hawthorn Bland-Hawthorn…
Lecture 9 Hydrogen Burning Nucleosynthesis, Classical Novae, and X-Ray Bursts red = slow , , , ( ) ( )I I j jk L k kj j k k j L L k I j dY Y Y I Y Y L dt ρ λ ρ λ ∍…
σσσσ(E) = S(E) e–2πηπηπηπη E-1 2πη = 31.29 Ζπη = 31.29 Ζπη = 31.29 Ζπη = 31.29 Ζ1111ΖΖΖΖ2222 √√√√µ/Εµ/Εµ/Εµ/Ε µ = µ = µ =…
10 Nucleosynthesis Roland Diehl 101 Introduction Radioactive decay of unstable nuclei is one of the main γ-ray source pro- cesses The radioactive nuclei are a by-product…
Components of Galaxies – Stars What Properties of Stars are Important for Understanding Galaxies? • Temperature – Determines the λ range over which the radiation is…
FLUORINE of the University of Notre Dame in Partial Fulfillment of the Requirements for the Degree of FLUORINE Abstract by Claudio Ugalde The 19F (α, p)22Ne reaction
Stars Part One: Brightness and Distance Concept -1 – Temperature λmax (metres) = 2.90 x 10-3 m k T (Kelvin) λmax = Peak black body wavelength T = The star’s surface…
ΕΤΗΣΙΑ ΕΚΔΟΣΗ • ΔΙΑΝΕΜΕΤΑΙ ΔΩΡΕΑΝ • FREE COPY • ΚΑΛΟΚΑΙΡΙ 2011 • SUMMER 2011 1GOLDENSTARS 2 GOLDENSTARS Ετήσια Έκδοση…
ΕΤΗΣΙΑ ΕΚΔΟΣΗ • ΔΙΑΝΕΜΕΤΑΙ ΔΩΡΕΑΝ • FREE COPY • ΚΑΛΟΚΑΙΡΙ 2012 • SUMMER 2012 ΑΝΔΡΟΣ / ANDROS 1GOLDENSTARS ΑΝΔΡΟΣ…
PowerPoint Presentation Nano Encapsulated Transforming Growth Factor-β (TGF-β) Possibly Attenuates NF-κB Activation Pathway in Pulmonary Hypertension Leandro Fernandez,…