The Complex Behaviour of s-Process Element Abundances at Young Ages

被引:8
|
作者
D'Orazi, Valentina [1 ,2 ]
Baratella, Martina [3 ]
Lugaro, Maria [2 ,4 ,5 ]
Magrini, Laura [6 ]
Pignatari, Marco [4 ,7 ,8 ]
机构
[1] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy
[2] Monash Univ, Sch Phys & Astron, Melbourne, Vic 3800, Australia
[3] Leibniz Inst AstroPhys, Sternwarte 16, D-14482 Potsdam, Germany
[4] Eotvos Lorand Res Network ELKH, Konkoly Observ, Res Ctr Astron & Earth Sci CSFK, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary
[5] Eotvos Lorand Univ, Inst Phys, Pazmany Peter Setany 1-A, H-1117 Budapest, Hungary
[6] Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy
[7] Univ Hull, Dept Math & Phys, EA Milne Ctr Astrophys, Kingston Upon Hull HU6 7RX, N Humberside, England
[8] Michigan State Univ, Joint Inst Nucl Astrophys, Ctr Evolut Elements, 640 South Shaw Lane, E Lansing, MI 48824 USA
关键词
stars; abundances; AGB and post-AGB; pre-main sequence; individual; RZ Psc; Galaxy; open clusters and associations; general; solar neighbourhood; OPEN CLUSTERS; CHEMICAL-COMPOSITION; EVOLUTION MODELS; NEUTRON-CAPTURE; STELLAR MODELS; STARS; DWARFS; ASSOCIATIONS; BARIUM;
D O I
10.3390/universe8020110
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Open clusters appear as simple objects in many respects, with a high degree of homogeneity in their (initial) chemical composition, and the typical solar-scaled abundance pattern that they exhibit for the majority of the chemical species. The striking singularity is represented by heavy elements produced from the slow process of the neutron-capture reactions. In particular, young open clusters (ages less than a few hundred Myr) give rise to the so-called barium puzzle: that is an extreme enhancement in their [Be/Fe] ratios, up to a factor of four of the solar value, which is not followed by other nearby s-process elements (e.g., lanthanum and cerium). The definite explanation for such a peculiar trend is still wanting, as many different solutions have been envisaged. We review the status of this field and present our new results on young open clusters and the pre-main sequence star RZ Piscium.
引用
收藏
页数:11
相关论文
共 50 条
  • [41] α-, r-, and s-process element trends in the Galactic thin and thick disks
    Bensby, T
    Feltzing, S
    Lundström, I
    Ilyin, I
    ASTRONOMY & ASTROPHYSICS, 2005, 433 (01) : 185 - 203
  • [42] STELLAR NUCLEOSYNTHESIS AND S-PROCESS
    不详
    NATURE, 1973, 242 (5398) : 438 - 438
  • [43] The s-process at low metallicity
    Stancliffe, Richard J.
    Lugaro, Maria A.
    Karakas, Amanda I.
    Rijs, Carlos
    FIRST STARS IV - FROM HAYASHI TO THE FUTURE, 2012, 1480 : 156 - 159
  • [44] The rise of the s-process in the galaxy
    Simmerer, J
    Sneden, C
    Cowan, JJ
    Collier, J
    Woolf, VM
    ASTROPHYSICAL JOURNAL, 2004, 617 (02): : 1091 - 1114
  • [45] s-process element abundance results for 47 Tuc stairs using SALT
    Worley, C. C.
    Cottrell, P. L.
    de Boer, E. C. Wylie
    NINTH TORINO WORKSHOP ON EVOLUTION AND NUCLEOSYNTHESIS IN AGB STARS AND THE SECOND PERUGIA WORKSHOP ON NUCLEAR ASTROPHYSICS, 2008, : 220 - +
  • [46] Nucleosynthesis and mixing on the asymptotic giant branch.: III.: Predicted and observed s-process abundances
    Busso, M
    Gallino, R
    Lambert, DL
    Travaglio, C
    Smith, VV
    ASTROPHYSICAL JOURNAL, 2001, 557 (02): : 802 - 821
  • [47] Advances in s-process models
    Lugaro, M
    Herwig, F
    NUCLEAR PHYSICS A, 2001, 688 (1-2) : 201C - 208C
  • [48] The s-process in stellar sites
    Cristallo, Sergio
    9TH EUROPEAN SUMMER SCHOOL ON EXPERIMENTAL NUCLEAR ASTROPHYSICS, 2018, 184
  • [49] WEAK S-PROCESS IRRADIATIONS
    PETERS, JG
    CLAYTON, DD
    FOWLER, WA
    ASTROPHYSICAL JOURNAL, 1972, 173 (03): : 637 - &
  • [50] REMARKS CONCERNING S-PROCESS
    ZEH, HD
    ASTRONOMY & ASTROPHYSICS, 1973, 28 (03) : 427 - 428