Results 71 to 80 of about 52,754 (240)

Explosive Nucleosynthesis: What we learned and what we still do not understand

, 2018
This review touches on historical aspects, going back to the early days of nuclear astrophysics, initiated by B$^2$FH and Cameron, discusses (i) the required nuclear input from reaction rates and decay properties up to the nuclear equation of state ...
A Arcones, A Burrows, A Burrows, A Heger, A Khokhlov, A Perego, A Sobiczewski, AB McDonald, AGW Cameron, AGW Cameron, AL Sallaska, B Côté, B Paxton, B Wehmeyer, BS Meyer, C Angulo, C Georgy, C Iliadis, C Kobayashi, C Li, C Sneden, C Winteler, D Argast, D Bodansky, D Eichler, D Maoz, DA Goldstein, E Müller, EM Burbidge, F Hoyle, F Käppeler, F Matteucci, F Voort van de, F-K Thielemann, F-K Thielemann, F-K Thielemann, F-K Thielemann, FX Timmes, FX Timmes, G Cescutti, G Halevi, G Martínez-Pinedo, G Michaud, G Michaud, GM Fuller, GR Caughlan, H-T Janka, H-T Janka, HA Bethe, I Dillmann, I Iben Jr, I Iben Jr, I Petermann, IU Roederer, IV Panov, J Lippuner, J Pruet, JA Holmes, JA Morgan, JC Wheeler, JJ Cowan, JM Lattimer, JW Truran, JW Truran, JW Truran, JW Truran, JW Truran, K Farouqi, K Langanke, K Nakamura, K Nomoto, K Nomoto, K Nomoto, K Nomoto, K Nomoto, K Takahashi, K-C Pan, K-L Kratz, LF Roberts, M Arnould, M Arnould, M Arnould, M Arnould, M Eichler, M Limongi, M Oertel, M Ruffert, M Ugliano, M Zingale, MB Davies, N Nishimura, N Nishimura, P Hoeflich, P Möller, P Mösta, P Mösta, R Longland, RF Webbink, RH Cyburt, RJ deBoer, RM Cabezón, S Goriely, S Goriely, S Nishimura, S Rosswog, S Shen, S Wanajo, S-C Leung, S-I Fujimoto, SE Woosley, SE Woosley, SE Woosley, SE Woosley, SE Woosley, T Ertl, T Foglizzo, T Kuroda, T Marketin, T Mishenina, T Rauscher, T Rauscher, T Rauscher, T Sukhbold, T Tsujimoto, T Yoshida, TA Weaver, TT Hansen, UM Noebauer, WA Fowler, WA Fowler, WA Fowler, WD Arnett, WD Arnett, WD Arnett, WD Arnett, WD Arnett, WM Howard, WR Hix, Y Hirai, Y Xu, ZY Bao, ZY Bao   +141 more
core   +1 more source

Mass‐Loss, Composition and Observational Signatures of Stellar Winds From X‐Ray Bursts

Astronomische Nachrichten, Volume 346, Issue 1, January 2025.
ABSTRACT X‐Ray bursts (XRBs) are powerful thermonuclear events on the surface of accreting neutron stars (NSs), which can synthesize intermediate‐mass elements. Although the high surface gravity prevents an explosive ejection, a small fraction of the envelope may be ejected by radiation‐driven winds.
Yago Herrera, Daniel Muñoz Vela, Gloria Sala, Jordi José, Yuri Cavecchi   +4 more
wiley   +1 more source

Nucleosynthesis in Thermonuclear Supernovae [PDF]

, 2017
The explosion energy of thermonuclear (Type Ia) supernovae is derived from the difference in nuclear binding energy liberated in the explosive fusion of light 'fuel' nuclei, predominantly carbon and oxygen, into more tightly bound nuclear 'ash' dominated by iron and silicon group elements.
Dean M. Townsley, Ivo R. Seitenzahl
openaire   +3 more sources

Extremely Metal-Poor Asymptotic Giant Branch Stars

Universe, 2022
Little is known about the first stars, but hints on this stellar population can be derived from the peculiar chemical composition of the most metal-poor objects in the Milky Way and in resolved stellar populations of nearby galaxies.
Mario Cirillo, Luciano Piersanti, Oscar Straniero   +2 more
doaj   +1 more source

The s-process Nucleosynthesis [PDF]

Proceedings of the International Astronomical Union, 2005
Theoretical as well as observational aspects of the s-process nucleosynthesis are reviewed. The classical site-independent s-process model as well as the s-process in massive stars are shortly described. A special attention is paid to the nucleosynthesis taking place in AGB stars and the extra-mixing invoked to explain the production of neutrons in the
Lionel Siess, Stéphane Goriely
openaire   +2 more sources

An Analytical Method for Quantification of Sn Isotope Variations in Geological Materials Using MC‐ICP‐MS

Geostandards and Geoanalytical Research, Volume 48, Issue 4, Page 863-885, December 2024.
Key Points A method is described to obtain high precision Sn isotope ratios using the double spike technique in geological reference materials containing 0.03 to 7 μg g−1 of Sn. δ122/118Sn values are reported for sixteen geological RMs. Improved precision was achieved compared with previous studies by using low concentration Sn analyte.
Dipankar Pathak, Klaus Mezger
wiley   +1 more source

Mixing and Magnetic Fields in Asymptotic Giant Branch Stars in the Framework of FRUITY Models

Universe, 2021
In the last few years, the modeling of asymptotic giant branch (AGB) stars has been much investigated, both focusing on nucleosynthesis and stellar evolution aspects. Recent advances in the input physics required for stellar computations made it possible
Diego Vescovi
doaj   +1 more source

SNR-calibrated Type Ia supernova models [PDF]

, 2019
Current Type Ia supernova (SN Ia) models can reproduce most visible+IR + UV observations. In the X-ray band, the determination of elemental abundance ratios in supernova remnants (SNRs) through their spectra has reached enough precision to constrain SN ...
Badenes Montoliu, Carles, Bravo Guil, Eduardo, Martinez Rodriguez, Hector   +2 more
core   +2 more sources

Detection of Inconsistencies in Isotope Ratios Certified in the Isotopic Primary Standards for Copper, Zinc and Nickel

Geostandards and Geoanalytical Research, Volume 48, Issue 4, Page 795-805, December 2024.
Key Points Isotopic reference materials are rarely cross‐examined. An optimised regression model and MC‐ICP‐MS offer a cost‐effective way to assess the reliability of values assigned to multi‐isotope reference materials. A significant lack of consistency has been observed in the long‐standing isotopic reference materials for nickel and zinc. Calibrated
Juris Meija, Juan He, Brad Methven, Zoltán Mester, Lu Yang   +4 more
wiley   +1 more source

Big Bang Nucleosynthesis

, 2022
As the early universe expands and cools the rates of the weak interactions that keep neutrinos in thermal equilibrium with the matter and the related rates of the reactions that inter-convert neutrons and protons decrease. Eventually, these rates fall below the expansion rate -- they freeze out.
Grohs, Evan, Fuller, George M.
openaire   +2 more sources