Quark-novae in neutron star - white dwarf binaries: a model for luminous (spin-down powered) sub-Chandrasekhar-mass Type Ia supernovae?
Quark-novae in neutron star - white dwarf binaries: a model for luminous (spin-down powered) sub-Chandrasekhar-mass Type Ia supernovae?
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DOI：
10.1088/1674-4527/13/4/006
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发表时间：
2011-11
影响因子：
1.8
通讯作者：
R. Ouyed;J. Staff
中科院分区：
文献类型：
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作者：
R. Ouyed;J. Staff
我们证明，在包含一颗大质量中子星和一颗CO白矮星(WD)的紧密双星系统中，通过求助于夸克-新星(QN)，可以发生Ia型爆炸。QN喷射物与WD相撞，驱动激波，在简并条件下触发碳燃烧(QN-Ia)。在我们的模型中，压缩的低质量WD(MWD<；0.9M⊙)中的条件类似于Chandrasekhar质量WD的条件。QN致密残骸(夸克星)的自旋向下光度提供了额外的能量，使QN-Ia的光曲线比具有类似56Ni产额的标准SN-Ia更亮、更宽。在QNe-Ia中，光度学和光谱学不一定是联系在一起的，因为抛射物的动能来自自旋下降功率和核衰变。尽管QNe-Ia可能不遵守菲利普斯关系，但它们的亮度和相对“看起来正常”的光曲线意味着它们可能会被包括在宇宙学样本中。光曲线拟合法会被峰值光谱学和光度学之间的差异所迷惑，并将通过有效地使QNe-Ia表观星等变亮或变暗来纠正这一点，从而高估或低估了这些自旋减弱动力的SNE-Ia的真实星等。用于宇宙学分析的SNE-Ia样品中的QNe-Ia的污染可能会系统地影响宇宙学参数的测量，如果QNe-Ia在高红移时足够多的话。在QNe-Ia中，由于自旋下降风引起的强混合和低的56Ni产额意味着，尽管它们是发光的，但它们在I波段没有第二个极大值。我们讨论了可能的QNe-Ia前身。
We show that, by appealing to a Quark-Nova (QN) in a tight binary system containing a massive neutron star and a CO white dwarf (WD), a Type Ia explosion could occur. The QN ejecta collides with the WD, driving a shock that triggers carbon burning under degenerate conditions (the QN-Ia). The conditions in the compressed low-mass WD (MWD < 0.9 M⊙) in our model mimic those of a Chandrasekhar mass WD. The spin-down luminosity from the QN compact remnant (the quark star) provides additional power that makes the QN-Ia light-curve brighter and broader than a standard SN-Ia with similar 56Ni yield. In QNe-Ia, photometry and spectroscopy are not necessarily linked since the kinetic energy of the ejecta has a contribution from spin-down power and nuclear decay. Although QNe-Ia may not obey the Phillips relationship, their brightness and their relatively “normal looking" light-curves mean they could be included in the cosmological sample. Light-curve fitters would be confused by the discrepancy between spectroscopy at peak and photometry and would correct for it by effectively brightening or dimming the QNe-Ia apparent magnitudes, thus over- or under-estimating the true magnitude of these spin-down powered SNe-Ia. Contamination of QNe-Ia in samples of SNe-Ia used for cosmological analyses could systematically bias measurements of cosmological parameters if QNe-Ia are numerous enough at high-redshift. The strong mixing induced by spin-down wind combined with the low 56Ni yields in QNe-Ia means that these would lack a secondary maximum in the i-band despite their luminous nature. We discuss possible QNe-Ia progenitors.