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pro vyhledávání: '"s-process"'
Akademický článek
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Publikováno v:
The Astrophysical Journal Letters, Vol 973, Iss 2, p L56 (2024)
A large population of intermediate-separation binaries, consisting of a main-sequence (MS) star and a white dwarf (WD), recently emerged from Gaia’s third data release (DR3), posing challenges to current models of binary evolution. Here we examine
Externí odkaz:
https://doaj.org/article/212a6f01a8954ba5995f09e924b61893
Publikováno v:
The Astrophysical Journal Letters, Vol 970, Iss 2, p L39 (2024)
We report the discovery of a barium blue straggler star (BSS) in M67, exhibiting enhancements in slow neutron-capture ( s -)process elements. Spectroscopic analysis of two BSSs (WOCS 9005 & WOCS 1020) and four stars located near the main-sequence tur
Externí odkaz:
https://doaj.org/article/b37259bd4fea4b299632628870eaa93a
Autor:
Zhenyu He, Toshitaka Kajino, Motohiko Kusakabe, Shan-Gui Zhou, Hiroyuki Koura, Satoshi Chiba, Haining Li, Yangming Lin
Publikováno v:
The Astrophysical Journal Letters, Vol 966, Iss 2, p L37 (2024)
The slow and intermediate neutron-capture processes, s - and i -processes, are believed to occur in asymptotic giant branch stars to provide half of the heavy atomic nuclei with A ≥ 90. We suggest a possibility that certain types of outflows found
Externí odkaz:
https://doaj.org/article/36500d780d134d1a9b907bb291d92c4f
Autor:
HUANG Tianxing;WU Xinhui
Publikováno v:
Yuanzineng kexue jishu, Vol 57, Iss 4, Pp 743-750 (2023)
The origin of elements in the universe is a basic scientific problem. The slow neutron capture process (s-process) is believed to be responsible for the nucleosynthesis of about half of the elements heavier than iron. The neutron capture reaction rat
Externí odkaz:
https://doaj.org/article/7711efdbe41b41b1befff6f89ef1670a
Autor:
G. L. Guardo, L. Lamia, J. P. Fernández-García, S. Piskor, M. La Cognata, G. D’Agata, S. Palmerini, D. Vescovi, V. Burjan, R. J. deBoer, V. Kroha, D. Lattuada, J. Mrazek, A. A. Oliva, R. G. Pizzone, G. G. Rapisarda, S. Romano, M. L. Sergi, R. Spartá, A. Tumino
Publikováno v:
The Astrophysical Journal, Vol 975, Iss 1, p 32 (2024)
Indirect methods have proven to be a complementary approach for extending our knowledge of nuclear structure and low-energy cross sections. Among these, the neutron-induced reaction cross sections appear to be of particular interest since their role
Externí odkaz:
https://doaj.org/article/d4bc6305f7224b5898d1e195b0c7c0b8
Publikováno v:
The Astrophysical Journal, Vol 974, Iss 1, p 78 (2024)
Barium stars are peculiar stars with enhanced slow neutron capture process ( s -process) elements. Abundance analysis of them aids in better understanding the chemical evolution of the Milky Way. In this paper, we introduce a data-driven method named
Externí odkaz:
https://doaj.org/article/dc08c5b1f43140a3ab401d16062b499e
Autor:
B. F. Rauch, W. V. Zober, Q. Abarr, Y. Akaike, W. R. Binns, R. F. Borda, R. G. Bose, T. J. Brandt, D. L. Braun, J. H. Buckley, N. W. Cannady, S. Coutu, R. M. Crabill, P. F. Dowkontt, M. H. Israel, M. Kandula, J. F. Krizmanic, A. W. Labrador, W. Labrador, L. Lisalda, J. V. Martins, M. P. McPherson, R. A. Mewaldt, J. G. Mitchell, J. W. Mitchell, S. A. I. Mognet, R. P. Murphy, G. A. de Nolfo, S. Nutter, M. A. Olevitch, N. E. Osborn, I. M. Pastrana, K. Sakai, M. Sasaki, S. Smith, H. A. Tolentino, N. E. Walsh, J. E. Ward, D. Washington, A. T. West, L. P. Williams
Publikováno v:
Instruments, Vol 8, Iss 1, p 4 (2024)
The Trans-Iron Galactic Element Recorder (TIGER) family of instruments is optimized to measure the relative abundances of the rare, ultra-heavy galactic cosmic rays (UHGCRs) with atomic number (Z) Z ≥ 30. Observing the UHGCRs places a premium on ex
Externí odkaz:
https://doaj.org/article/129b9cd1040945a0a8379866d2ebf234
Publikováno v:
The Astrophysical Journal Supplement Series, Vol 270, Iss 2, p 28 (2024)
We present the evolution and the explosion of two massive stars, 15 and 25 M _⊙ , spanning a wide range of initial rotation velocities (from 0 to 800 km s ^−1 ) and three initial metallicities: Z = 0 ([Fe/H] = −∞), 3.236 × 10 ^−7 ([Fe/H] =
Externí odkaz:
https://doaj.org/article/349243b4d91944838551a78aea81d4de
Akademický článek
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