The Initial Mass–Final Luminosity Relation of Type II Supernova Progenitors: Hints of New Physics?
The Initial Mass–Final Luminosity Relation of Type II Supernova Progenitors: Hints of New Physics?
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II 型超新星前身的初始质量-最终光度关系：新物理学的提示？
DOI：
10.3847/1538-4357/ab3222
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发表时间：
2019
期刊：
影响因子：
--
通讯作者：
A. Mirizzi
中科院分区：
文献类型：
--
作者：
O. Straniero;I. Domínguez;L. Piersanti;M. Giannotti;A. Mirizzi
本文修正了IIP型和IIL型超新星前身星的理论初始质量-最终光度关系。主要的不确定性的影响，如由于处理对流，对流，旋转，质量损失，核反应速率和中微子的产生率，进行了详细的讨论。也被认为是密切的二元系统的组件之间的质量传递的影响。通过比较的理论预测的样本的II型超新星的初始质量的祖先和爆炸前的光度是可用的，我们得出结论，恒星旋转可以解释一些祖先出现比预期的情况下，非旋转模型更亮。在最极端的情况下，SN 2012 ec需要高达300 km s−1的初始旋转速度。或者，这些物体可能是密近双星的质量损失组件。然而，大多数观察到的祖细胞似乎比预期的要暗淡。这种情况似乎表明，康普顿和对中微子的能量损失率，如标准电弱理论所预测的，是不够有效的，需要一个额外的负面贡献的恒星能量平衡。我们表明，轴子加上参数访问目前计划的实验，如IAO，可能，BabyIAO和轴子样粒子，可能占失踪的贡献恒星能量损失。
We revise the theoretical initial mass–final luminosity relation for progenitors of Type IIP and IIL supernovae. The effects of the major uncertainties, such as those due to the treatment of convection, semiconvection, rotation, mass loss, nuclear reaction rates, and neutrinos production rates, are discussed in some detail. The effects of mass transfer between components of close-binary systems are also considered. By comparing the theoretical predictions to a sample of Type II supernovae for which the initial mass of the progenitors and the pre-explosive luminosity are available, we conclude that stellar rotation may explain a few progenitors that appear brighter than expected in the case of nonrotating models. In the most extreme case, SN 2012ec, an initial rotational velocity up to 300 km s−1 is required. Alternatively, these objects could be mass-losing components of close binaries. However, most of the observed progenitors appear fainter than expected. This occurrence seems to indicate that the Compton and pair neutrino energy-loss rates, as predicted by the standard electro-weak theory, are not efficient enough and that an additional negative contribution to the stellar energy balance is required. We show that axions coupled with parameters accessible to currently planned experiments, such as IAXO and, possibly, BabyIAXO and axion-like particles, may account for the missing contribution to the stellar energy loss.
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影响因子：
56.9
作者：
H. Sana;S. D. Mink;A. D. Koter;N. Langer;C. Evans;M. Gieles;E. Gosset;R. Izzard;J. L. Bouquin-J.
通讯作者：
H. Sana;S. D. Mink;A. D. Koter;N. Langer;C. Evans;M. Gieles;E. Gosset;R. Izzard;J. L. Bouquin-J.
影响因子：
19.6
作者：
Anastassopoulos, V.;Aune, S.;Zioutas, K.
通讯作者：
Zioutas, K.
影响因子：
4.8
作者：
C. Barbarino;M. Dall’ora;M. Botticella;M. Valle;L. Zampieri;J. Maund;M. L. Pumo;A. Jerkstrand;S. Benetti;N. Elias-Rosa;M. Fraser;A. Gal-yam;M. Hamuy;M. Hamuy;C. Inserra;C. Knapic;A. Lacluyze;M. Molinaro;P. Ochner;A. Pastorello;G. Pignata;D. Reichart;C. Ries;A. Riffeser;B. Schmidt;M. Schmidt;R. Smareglia;S. Smartt;K. Smith;J. Sollerman;M. Sullivan;L. Tomasella;M. Turatto;S. Valenti;O. Yaron;D. Young
通讯作者：
C. Barbarino;M. Dall’ora;M. Botticella;M. Valle;L. Zampieri;J. Maund;M. L. Pumo;A. Jerkstrand;S. Benetti;N. Elias-Rosa;M. Fraser;A. Gal-yam;M. Hamuy;M. Hamuy;C. Inserra;C. Knapic;A. Lacluyze;M. Molinaro;P. Ochner;A. Pastorello;G. Pignata;D. Reichart;C. Ries;A. Riffeser;B. Schmidt;M. Schmidt;R. Smareglia;S. Smartt;K. Smith;J. Sollerman;M. Sullivan;L. Tomasella;M. Turatto;S. Valenti;O. Yaron;D. Young
DOI：
10.1088/1475-7516/2016/11/017
发表时间：
2016-11-01
影响因子：
6.4
作者：
Aalbers, J.;Agostini, F.;Zuber, K.
通讯作者：
Zuber, K.