Structure of a massive common envelope in the common-envelope wind model for Type Ia supernovae
Structure of a massive common envelope in the common-envelope wind model for Type Ia supernovae
复制标题
Ia 型超新星共包络风模型中大质量共包络的结构
DOI：
10.1051/0004-6361/201936526
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发表时间：
2020-01
影响因子：
6.5
通讯作者：
Cui Yingzhen
中科院分区：
文献类型：
--
作者：
Song Ren;Meng Xiangcun;Podsiadlowski Philipp;Cui Yingzhen
上下文虽然Ia型超新星（SNe Ia）在许多天体物理学领域都很重要，但它们的祖先的性质仍然不清楚。最近发展了一种新的单简并模型，即共包络风（CEW）模型，在该模型中，双星在主吸积阶段被包裹在一个共包络（CE）中。该模型仍在开发中，并且有许多未决问题，例如，在CE阶段，这样的系统的确切外观是什么？目标。在本文中，我们研究这个问题的系统与大量CE。方法.我们用一颗热脉冲渐近巨星分支（TPAGB）星星来代表这个双星系统，它的CO核为0.976 M圆点，包层为0.6 M圆点。通过修改引力常数来模拟伴星引力和CE自转的影响。从二元和CE之间的摩擦输入的能量被考虑由一个额外的加热源。结果对于厚的包层，修改后的TPAGB星星看起来与典型的TPAGB星星相似，但具有更小的半径，更高的有效温度和更高的表面光度。这主要是由于伴星的重力作用，这是改变包层结构的主要因素。在伴星位置的混合长度可能大于当地半径，这意味着混合长度理论的崩溃，并建议在这个区域需要更多的湍流。修正后的TPAGB星星比标准TPAGB星星更稳定，伴星周围的CE密度明显高于原CEW模型中的假设。结论.今后的工作将需要模拟具有较低包层质量的系统，并在CE阶段纳入流体动力学效应。
Context. Although Type Ia supernovae (SNe Ia) are important in many astrophysical fields, the nature of their progenitors is still unclear. A new version of the single-degenerate model has been developed recently, the common-envelope wind (CEW) model, in which the binary is enshrouded in a common envelope (CE) during the main accretion phase. This model is still in development and has a number of open issues, for example what is the exact appearance of such a system during the CE phase? Aims. In this paper we investigate this question for a system with a massive CE. Methods. We use a thermally pulsing asymptotic giant branch (TPAGB) star with a CO core of 0.976 M-circle dot and an envelope of 0.6 M-circle dot to represent the binary system. The effects of the companion's gravity and the rotation of the CE are mimicked by modifying the gravitational constant. The energy input from the friction between the binary and the CE is taken into account by an extra heating source. Results. For a thick envelope, the modified TPAGB star looks similar to a canonical TPAGB star but with a smaller radius, a higher effective temperature, and a higher surface luminosity. This is primarily caused by the effect of the companion's gravity, which is the dominant factor in changing the envelope structure. The mixing length at the position of the companion can be larger than the local radius, implying a breakdown of mixing-length theory and suggesting the need for more turbulence in this region. The modified TPAGB star is more stable than the canonical TPAGB star and the CE density around the companion is significantly higher than that assumed in the original CEW model. Conclusions. Future work will require the modelling of systems with lower envelope masses and the inclusion of hydrodynamical effects during the CE phase.
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影响因子：
6.5
作者：
W. Hamann;M. Peña;G. Gräfener;M. Ruiz
通讯作者：
W. Hamann;M. Peña;G. Gräfener;M. Ruiz
共同包层物体的间歇性物质抛射
影响因子：
4.8
作者：
Clayton Matthew;Podsiadlowski Philipp;Ivanova Natasha;Justham Stephen
通讯作者：
Justham Stephen
影响因子：
7.5
作者：
W. Hillebrandt;M. Kromer;F. Röpke;A. Ruiter
通讯作者：
W. Hillebrandt;M. Kromer;F. Röpke;A. Ruiter
DOI：
10.3847/0004-6256/151/2/47
发表时间：
2015-08
期刊：
The Astronomical Journal
影响因子：
--
作者：
S. Rodney;A. Riess;D. Scolnic;David O. Jones;S. Hemmati;A. Molino;C. McCully;B. Mobasher;
通讯作者：
S. Rodney;A. Riess;D. Scolnic;David O. Jones;S. Hemmati;A. Molino;C. McCully;B. Mobasher;
DOI：
10.1088/0067-0049/220/1/15
发表时间：
2015-06
期刊：
The Astrophysical Journal Supplement Series
影响因子：
--
作者：
B. Paxton;P. Marchant;J. Schwab;E. Bauer;L. Bildsten;L. Bildsten;M. Cantiello;L. Dessart;
通讯作者：
B. Paxton;P. Marchant;J. Schwab;E. Bauer;L. Bildsten;L. Bildsten;M. Cantiello;L. Dessart;