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首页> 外文期刊>Physical review, C >Precise measurement of the thermal and stellar Fe-54(n,gamma) Fe-55 cross sections via accelerator mass spectrometry
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Precise measurement of the thermal and stellar Fe-54(n,gamma) Fe-55 cross sections via accelerator mass spectrometry

机译：通过加速器质谱法精确测量热和恒星Fe-54（N，γ）Fe-55横截面的横截面

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摘要

Accelerator mass spectrometry (AMS) represents a complementary approach for precise measurements of neutron capture cross sections, e.g., for nuclear astrophysics. This technique, completely independent of previous experimental methods, was applied for the measurement of the Fe-54(n,gamma) Fe-55 reaction. Following a series of irradiations with neutrons from cold and thermal to keV energies, the produced long-lived Fe-55 nuclei (t(1/2) = 2.744+-0.009) yr) were analyzed at the Vienna Environmental Research Accelerator. A reproducibility of about 1% could be achieved for the detection of Fe-55, yielding cross-section uncertainties of less than 3%. Thus, this method produces new and precise data that can serve as anchor points for time-of-flight experiments. We report significantly improved neutron capture cross sections at thermal energy (sigma(th) = 2.30 +/- 0.07 b) as well as for a quasi-Maxwellian spectrum of kT = 25 keV (sigma = 30.3 +/- 1.2 mb) and for E-n = 481 +/- 53 keV (sigma = 6.01 +/- 0.23 mb). The new experimental cross sections have been used to deduce improved Maxwellian-averaged cross sections in the temperature regime of the common s-process scenarios. The astrophysical impact is discussed by using stellar models for low-mass asymptotic giant branch stars.
机译：加速器质谱（AMS）表示用于核天体物理学的中子捕获横截面精确测量的互补方法。该技术完全独立于先前的实验方法，用于测量Fe-54（N，γ）Fe-55反应。在维也纳环境研究促进剂中分析了一系列与寒冷和热量从寒冷和热量的中子与中子的照射，产生的长寿命的Fe-55核（T（1/2）= 2.744 + -0.009 + -0.009）。对于检测Fe-55，可以实现约1％的再现性，从而产生小于3％的横截面不确定性。因此，该方法产生新的和精确的数据，可以用作飞行时间实验的锚点。我们报告了热能（Sigma（Th）= 2.30 +/- 0.07b）的显着改善的中子捕获横截面以及Kt = 25kev（Sigma = 30.3 +/- 1.2 MB）的准麦克斯韦频谱和en = 481 +/- 53 kev（Sigma = 6.01 +/- 0.23 MB）。新的实验横截面已被用于在共同的S-Process场景的温度制度中推断出改进的Maxwellian平均横截面。通过使用低质量渐近巨星星星的恒星模型讨论了天体物理影响。

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  • 来源
    《Physical review, C》 |2017年第2期|共13页
  • 作者

    Wallner A.; Buczak K.; Belgya T.; Bichler M.; Coquard L.; Dillmann I.; Golser R.; Kaeppeler F.; Karakas A.; Kutschera W.; Lederer C.; Mengoni A.; Pignatari M.; Priller A.; Reifarth R.; Steier P.; Szentmiklosi L.;

  • 作者单位

    Australian Natl Univ Res Sch Phys &

    Engn Dept Nucl Phys Canberra ACT 2601 Australia;

    Univ Vienna Fac Phys VERA Lab Vienna Austria;

    Hungarian Acad Sci Ctr Energy Res Inst Energy Secur &

    Environm Safety Nucl Anal &

    Radiog Dept Budapest Hungary;

    Vienna Univ Technol Atominst Vienna Austria;

    Karlsruhe Inst Technol Inst Nucl Phys Campus North POB 3640 Karlsruhe Germany;

    Karlsruhe Inst Technol Inst Nucl Phys Campus North POB 3640 Karlsruhe Germany;

    Univ Vienna Fac Phys VERA Lab Vienna Austria;

    Karlsruhe Inst Technol Inst Nucl Phys Campus North POB 3640 Karlsruhe Germany;

    Monash Univ Sch Phys &

    Astron Monash Ctr Astrophys Clayton Vic 3800 Australia;

    Univ Vienna Fac Phys VERA Lab Vienna Austria;

    Univ Vienna Fac Phys VERA Lab Vienna Austria;

    CERN CH-1211 Geneva 23 Switzerland;

    Univ Hull Dept Phys &

    Math EA Milne Ctr Astrophys Kingston Upon Hull N Humberside England;

    Univ Vienna Fac Phys VERA Lab Vienna Austria;

    Goethe Univ Frankfurt Inst Appl Phys Frankfurt Germany;

    Univ Vienna Fac Phys VERA Lab Vienna Austria;

    Hungarian Acad Sci Ctr Energy Res Inst Energy Secur &

    Environm Safety Nucl Anal &

    Radiog Dept Budapest Hungary;

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  • 正文语种 eng
  • 中图分类 原子核物理学、高能物理学;
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