AGB星
AGB星的相关文献在1990年到2014年内共计79篇,主要集中在天文学、系统科学、金属学与金属工艺
等领域,其中期刊论文79篇、专利文献16013篇;相关期刊26种,包括石家庄学院学报、河北科技大学学报、中国科学院上海天文台年刊等;
AGB星的相关文献由97位作者贡献,包括张波、刘俊红、张凤华等。
AGB星—发文量
专利文献>
论文:16013篇
占比:99.51%
总计:16092篇
AGB星
-研究学者
- 张波
- 刘俊红
- 张凤华
- 张彩霞
- 蒋苏云
- 孙锦
- 崔文元
- 彭秋和
- 刘永利
- 刘清华
- 周贵德
- 姜碧沩
- 牛萍
- 舒能川
- 陈永寿
- 黄润乾
- 东艳晖
- 刘建成
- 刘鑫
- 吴开谡
- 张承岳
- 张江
- 曾晟
- 李二涛
- 李云居
- 李志宏
- 李志常
- 柳卫平
- 梁艳春
- 樊启文
- 汪志云
- 熊关柱
- 王友宝
- 王宝祥
- 白希祥
- 等
- 胡景耀
- 苏俊
- 连钢
- 郭冰
- 金孙均
- 陈培杰
- 韩占文
- 颜胜权
- 马坤
- A. I. Karakas
- CHEN YongShou
- CUI WenYuan
- Chapm.J
- GUO JianYou
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郭冰;
白希祥;
陈永寿;
杜先超;
樊启文;
甘林;
金孙均;
A. I. Karakas;
李二涛;
李志常;
连钢;
李志宏;
刘建成;
刘鑫;
施建荣;
舒能川;
王宝祥;
王友宝;
曾晟;
柳卫平;
M. Lugaro;
J. Buntain;
庞丹阳;
李云居;
苏俊;
颜胜权;
吴志丹
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摘要:
13 C(α,n)16 O is the main neutron source reaction of slow neutron capture (s) process in asymptotic giant branch (AGB) stars .The 6.356 MeV 1/2+ subthreshold resonancein17O plays an important role in the 13C(α,n)16O reaction .The 13C(11B , 7 Li)17 O angular distributions were measured using HI-13 tandem accelerator and Q3D magnetic spectrograph , and then used to determine the α-width of the subthreshold resonant state w hich is currently the most uncertain parameter for determining the 13 C (α,n)16 O reaction rate .By using the present α-width ,the astrophysical S-factor and the stellar rate of the 13C(α,n)16 O reaction were derived .This shed some light on the existing discrepancies up to a factor of 25 in S-factors derived from different authors . The simulation of s-process in AGB stars shows that the new reaction rate produces 25% more Pb than the CF88 compilation .%13C(α,n)16O是渐进巨星支(AGB)星中慢速中子俘获(s)过程的主中子源反应,而17O 6.356 MeV 1/2+阈下共振对13 C(α,n)16 O反应影响很大。本文使用 HI-13串列加速器和Q3D磁谱仪,首次测量了13C (11B ,7Li)17O转移反应角分布,确定了影响13C(α,n)16O反应最关键、最不确定的17O(Ex =6.356 MeV)阈下共振态的α宽度,从而得出天体物理能区13 C (α,n)16 O反应的天体物理 S因子和反应率,澄清了国际上已有S因子数据间高达25倍的巨大分歧。AGB星s过程核合成网络计算表明:新反应率数据导致恒星中铅的丰度增加了25%。
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周贵德
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摘要:
介绍了重元素核合成理论,利用对流模型计算了AGB星核合成产量随金属丰度的变化.发现在低金属丰度条件下的不同质量AGB星中存在的较大的内禀性质的中子辐照量弥散,可以自然地解释观测到的重元素丰度比[1s/Fe]和[hs/Fe]随着金属丰度的降低而出现的离散现象.根据AGB星的重叠因子与其初始质量的变化关系,我们可以推测:较大的[1s/Fe]和[hs/Fe]数值对应着初始质量较小的AGB星,而小的[1s/Fe]和[hs/Fe]数值则对应着具有较大初始质量的AGB星.
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马坤
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摘要:
对富碳贫金属星CS 22964-161元素丰度的研究发现,该星碳和重元素丰度都高,这对于s-过程核合成研究是很有意义的.利用参数化模型研究了CS 22964-161的重元素丰度,重叠因子取值较高,r=0.57,这意味着原AGB星的初始质量应小于3M⊙.中子辐照量的取值为0.49mb-1,平均中子辐照量τ0≈0.87(T9/0.348)1/2,大于太阳系的平均中子辐照量,这是对s-过程元素,尤其是Pb元素超丰的有利解释.S-过程和r-过程分量系数都较小,这就意味着双星系统的轨道距离较远.
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马坤;
吴海滨
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摘要:
利用参数化模型研究了s-过程与r-过程元素均超丰的贫金属星(s+r星)CS 31062-050的观测丰度.计算得到,原AGB星的重叠因子取值为0.35,其初始质量应小于3~4 M⊙.s-过程分量系数Cs为0.002 7,r-过程分量系数Cr为70.5,Cs与Cr取值较高,这是对CS 31062-050形成于AIC机制的一个有力支持.%In this paper,the authors use the parametric model to fit the elemental abundances observed in the s-and r-rich,very metal-poor star(s+r star) CS 31062-050.The value of overlap factor in the AGB star is 0.35;this value could possibly be explained by the binary system with low-mass AGB star(M3~4 M⊙).The component coefficient of the s-process is 0.002 7.The component coefficient of the r-process is 70.5.The high value of Cs and Cr provides strong support for the scenario that the r-process material in CS 31062-050 comes from an AIC.
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洪雅芳;
蒋苏云
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摘要:
通过对3~ 10M☉恒星在赫罗图上演化轨迹的研究,分析恒星内部氦壳层燃烧峰值处能量、密度、温度、氦壳层表面光度与恒星表面光度比及恒星半径的变化,给出了中等质量恒星由早期AGB星演化至热脉冲AGB星阶段在赫罗图上的分界点,与119颗碳星的观测结果吻合得相当好.同时提出:在恒星演化至该分界点之后,其星风物质损失公式可能需要引入一个与表面光度无关的量以主导超星风的形成.在此基础上,通过对考虑湍流压效应下5M☉恒星的结构和演化及星风物质损失率的分析,发现湍流压在热脉冲AGB星阶段对星风物质损失影响较大,从而使得热脉冲AGB星的湍流压不可忽略,进而提出了影响热脉冲AGB星星风物质损失的可能的物理因素.%Stars with the initial masses in the range of 3 < M/Mq < 10 have evolved from the main-sequence phase to the end of the asymptotic giant branch (AGB). The evolutionary tracks in the Hertzsprung-Russel diagram (HR diagram) are investigated. The temporal variations of the energy productive rate, density and temperature at the maximum of helium burning in the helium-shell, stellar radius, and the ratio of the luminosity at the upper border of helium-shell to that of the stellar surface are analyzed. The demarcation point from E-AGB to TP-AGB in HR diagram for the intermediate-mass stars are proposed. They are in excellent agreement with the millimetric observations of 119 carbonrich giants. In order to form continuous superwind, a mass-loss function, which is unaffected by the luminosity of stellar surface after the demarcation point, is possibly necessary.Based on the above ideas, turbulent pressure has been taken into account for the mass-loss, structure and evolution of stars with masses of 5 MQ. The effect of turbulent pressure cannot be overlooked in the TP-AGB phase, particularly for stellar mass-loss. Also, the possible physical factors influencing on the superwind during the TP-AGB phase are discussed.
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刘清华
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摘要:
ACB星是渐近巨星分支,具有H-He双燃烧壳层,其内部会发生热脉冲过程和第三次挖掘,由于中子辐照发生核合成,是S-过程核素的主要产地.本文对AGB星的结构及演化进行了分析.
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