Episodic mass ejections from common-envelope objects
Episodic mass ejections from common-envelope objects
复制标题
共同包层物体的间歇性物质抛射
DOI：
10.1093/mnras/stx1290
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发表时间：
2017-05
影响因子：
4.8
通讯作者：
Justham Stephen
中科院分区：
文献类型：
--
作者：
Clayton Matthew;Podsiadlowski Philipp;Ivanova Natasha;Justham Stephen
在经历了公共包络双星最初的快速螺旋进入阶段后，系统可能进入一个缓慢的自我调节阶段，可能持续数百年，在这个阶段，轨道衰变释放的所有能量都可以有效地传输到表面，在那里它被辐射出去。如果在这个阶段要移除剩余的包络，这种移除必须通过某种尚不确定的机制发生。我们利用恒星演化程序MESA对低质量红巨星在这样一个缓慢的螺旋同相中经历了一个合成的共同包络事件进行了一维流体动力学模拟。我们模拟了不同构型的双星轨道摩擦耗散对包层的加热作用，并研究了包层的响应。我们发现，我们的模型包络变得动态不稳定，并发展出大幅度的脉动，周期在3-20年之间，增长时间尺度很短，相似数量级。在某些情况下，随着这些脉动的增长而产生的冲击和相关的反弹足够强，足以从高于逃逸速度的恒星表面动态弹出高达0.1M⊙的物质壳，约占包层质量的10%。这些抛射被认为在几十年内重复，导致时间平均质量损失率约为10-3M⊙yr-1，这足以代表一种候选机制，在缓慢的螺旋相持续时间内消除整个包层。
After the initial fast spiral-in phase experienced by a common-envelope binary, the system mayenter a slow, self-regulated phase, possibly lasting hundreds of years, in which all the energy released by orbital decay can be efficiently transported to the surface, where it is radiated away.If the remaining envelope is to be removed during this phase, this removal must occur throughsome as-yet-undetermined mechanism. We carried out 1D hydrodynamic simulations of alow-mass red giant undergoing a synthetic common-envelope event in such a slow spiral-inphase, using the stellar evolutionary code MESA. We simulated the heating of the envelopedue to frictional dissipation from a binary companion's orbit in multiple configurations and investigated the response of the giant's envelope. We find that our model envelopes become dynamically unstable and develop large-amplitude pulsations, with periods in the range 3-20yr and very short growth time-scales of similar order. The shocks and associated rebounds that emerge as these pulsations grow are in some cases strong enough to dynamically eject shellsof matter of up to 0.1 M⊙, ~10 percent of the mass of the envelope, from the stellar surfaceat above escape velocity. These ejections are seen to repeat within a few decades, leading toa time-averaged mass-loss rate of the order of 10 -3 M⊙ yr -1 , which is sufficiently high torepresent a candidate mechanism for removing the entire envelope over the duration of theslow spiral-in phase.
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DOI：
10.1046/j.1365-8711.2002.05752.x
发表时间：
2002-06
影响因子：
4.8
作者：
Zhanwen Han;P. Podsiadlowski;P. Maxted;T. Marsh;N. Ivanova
通讯作者：
Zhanwen Han;P. Podsiadlowski;P. Maxted;T. Marsh;N. Ivanova
影响因子：
--
作者：
G. Darwin
通讯作者：
G. Darwin
DOI：
10.1046/j.1365-8711.2002.05038.x
发表时间：
2002-01
影响因子：
4.8
作者：
J. Hurley;C. Tout;O. Pols
通讯作者：
J. Hurley;C. Tout;O. Pols
DOI：
10.1086/155767
发表时间：
1978
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Y. Tuchman;N. Sack;Z. Barkat
通讯作者：
Y. Tuchman;N. Sack;Z. Barkat
影响因子：
4.8
作者：
M. M. Kiminki-M.;M. Reiter;N. Smith
通讯作者：
M. M. Kiminki-M.;M. Reiter;N. Smith