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Co-operative Study of Compact and Diffuse Remnants in Supernova 1987A

1987A 超新星致密和弥散遗迹的合作研究

基本信息

批准号：
02302024
负责人：
NOMOTO Ken'ichi
金额：
$ 5.63万
依托单位：
University of Tokyo
依托单位国家：
日本
项目类别：
Grant-in-Aid for Co-operative Research (A)
财政年份：
1990
资助国家：
日本
起止时间：
1990 至 1991
项目状态：
已结题

来源：
https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-02302024/
关键词：
Supernova Neutrino X-ray gamma-ray Cosmic Ray Dust Pulsar Neutron Star ニュ-トリノパルサ-

项目摘要

SN 1987A provides us with an excellent material to test the theory of massive star evolution, nucleosynthesis, and supernova explosion. Presupernova evolution of the progenitor, hydrodynamics of explosion, explosive nucleosynthesis, optical, X-ray and gamma-ray light curves due to ^<56>Co decay are calculated and compared with the observations of SN 1987A.1. The unique evolution of the progenitor in the HR diagram can be understood in terms of mass loss and mixing. The mass loss drives the star to move from a blue to red supergiant. The excursion from the red back to the blue occurs if the hydrogen-rich envelope is metal deficient and becomes sufficiently helium-rich due to mixing.2. The light curves in all wave bands indicate the explosion energy of E/M<@D2env@>D2=1.5(]SY.+-。[)0.5*10<@D150@>D1 erg/M<@D2(]SY.sun.[)@>D2, production of <@D156@>D1Ni with M<@D2Ni@>D2-0.07M<@D2(]SY.sun.[)@>D2. The plateau-like peak is found to be formed by the hydrogen recombination front and lasts longer if the hydrogen layr is deeper. This indicates the mixing of hydrogen into the deep interior.3. The distribution of heavy elements in the ejecta is inferred also from the X-ray and gamma-ray light curves. The early emergence of X-ray and gamma-ray indicate the mixing of ^<56>Ni into the hydrogen-rich envelope. Flat X-ray light curve observed by Ginga would be due to the clumpy structure of the core.4. Such a mixing is well modeled by the Rayleigh-Taylor instabilities during explosion. Two-dimensional hydrodynamical simulations have shown that the instability grows at the hydrogen/helium interface and mixes the supernova meterials.5. The recent slowdown of the decline of the optical light curve is due to the contribution from another energy source, which would be either radioactive ^<56>Co or the buried neutron star. Recent balloon experiments have provided the upper limit to ^<57>Co and suggested that the pulsar activity is more likely the source.

SN 1987 A为我们检验大质量星星演化、核合成和超新星爆炸理论提供了极好的材料。计算了前身星的前超新星演化、爆炸流体动力学、爆炸核合成、^ Co衰变引起的光学、X射线和γ射线光变曲线<56>，并与SN 1987A.1的观测结果进行了比较。在HR图中，祖先的独特演化可以从质量损失和混合的角度来理解。质量的损失驱使这颗星星从蓝超巨星变成红超巨星。如果富氢包层缺乏金属，并且由于混合而变得足够富氦，则会发生从红色到蓝色的偏移。所有波段的光变曲线表明E/M<@D2env@>D2=1.5（± SY）的爆炸能量。[)0.5*10<@D150@>D1 erg/M<@D2（]SY.sun. [D_2]、用M<@D_2Ni @> D_2 -0.07M<@D_2（] SY. sun生产<@D_156 @> D_1Ni。[）@>D2.平台状峰是由氢复合前沿形成的，氢层越深，平台状峰持续时间越长。这表明氢混合进入了深层走廊。3.喷出物中重元素的分布也推断从X射线和伽马射线光变曲线。X射线和γ射线的早期出现表明^ Ni<56>混入富氢包层。Ginga观察到的平坦X射线光变曲线可能是由于地核的团簇结构.这样的混合很好地模拟了爆炸过程中的瑞利-泰勒不稳定性。二维流体动力学模拟表明，不稳定性在氢/氦界面增长，并混合超新星物质。最近光学光变曲线下降的减缓是由于另一种能源的贡献，这可能是放射性的^<56>Co或掩埋的中子星星。最近的气球实验提供了^ Co的上限<57>，并表明脉冲星活动更可能是来源。