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Properties of the accretion ring in an X-ray binary, and accretion and excretion two-layer flows from it
Publications of the Astronomical Society of Japan ( IF 2.3 ) Pub Date : 2021-05-03 , DOI: 10.1093/pasj/psab043 Hajime Inoue 1
Publications of the Astronomical Society of Japan ( IF 2.3 ) Pub Date : 2021-05-03 , DOI: 10.1093/pasj/psab043 Hajime Inoue 1
Affiliation
We study properties of an accretion ring in a steady mass flow from a companion star to a compact object in an X-ray binary. The accretion ring is a place where matter inflowing from a companion star sojourns for a while to bifurcate to accretion and excretion flows due to angular momentum transfer. The matter in the accretion ring rotates along the Keplerian circular orbit determined by the intrinsic specific angular momentum of the inflowing matter and forms a thick ring-envelope. Two internal flows are expected to appear in the thick envelope. One is a mass-spreading flow bifurcating to a thick accretion flow and a thick excretion flow, as a result of the angular momentum transfer within the ring-envelope. The other is a cooling flow toward the envelope center governed by radiative cooling under the effect of X-ray irradiation. This cooling flow eventually forms a core in the torus, from which a thin accretion disk and a thin excretion disk spread out, again as a result of the angular momentum transfer there. Evaluating and comparing the timescales for the two internal flows, the accretion ring is shown to generally originate a two-layer accretion flow in which a thin accretion disk is sandwiched by a thick accretion flow, unless the accretion rate is very low. Properties of the thin excretion disk and the thick excretion flow are also investigated. The thin excretion disk is expected to terminate at a distance of four times the accretion ring radius and to form another ring there, unless tidal effects from the companion star exist. The thick excretion flow is, on the other hand, likely to turn into a supersonic wind flow reaching infinity.
中文翻译:
X射线双星吸积环的性质,吸积和排泄两层从它流出
我们研究了从伴星到 X 射线双星中致密物体的稳定质量流中吸积环的特性。吸积环是从伴星流入的物质停留一段时间的地方,由于角动量传递而分叉为吸积和排泄流动。吸积环中的物质沿着由流入物质的固有比角动量决定的开普勒圆形轨道旋转,并形成一个厚的环包络。预计厚信封中会出现两个内部流动。一种是质量扩散流,由于环包络内的角动量转移,分叉为厚吸积流和厚排泄流。另一种是在X射线照射作用下由辐射冷却支配的向包络中心的冷却流。这种冷却流最终在圆环中形成一个核心,一个薄的吸积盘和一个薄的排泄盘从该核心展开,这也是角动量转移的结果。评估和比较两个内部流动的时间尺度,表明吸积环通常起源于两层吸积流,其中薄吸积盘被厚吸积流夹在中间,除非吸积率非常低。还研究了薄排泄盘和厚排泄流的性质。除非伴星的潮汐效应存在,否则薄的排泄盘预计将在吸积环半径四倍的距离处终止,并在那里形成另一个环。另一方面,浓稠的排泄流很可能会变成超音速风流,达到无穷大。
更新日期:2021-05-03
中文翻译:
X射线双星吸积环的性质,吸积和排泄两层从它流出
我们研究了从伴星到 X 射线双星中致密物体的稳定质量流中吸积环的特性。吸积环是从伴星流入的物质停留一段时间的地方,由于角动量传递而分叉为吸积和排泄流动。吸积环中的物质沿着由流入物质的固有比角动量决定的开普勒圆形轨道旋转,并形成一个厚的环包络。预计厚信封中会出现两个内部流动。一种是质量扩散流,由于环包络内的角动量转移,分叉为厚吸积流和厚排泄流。另一种是在X射线照射作用下由辐射冷却支配的向包络中心的冷却流。这种冷却流最终在圆环中形成一个核心,一个薄的吸积盘和一个薄的排泄盘从该核心展开,这也是角动量转移的结果。评估和比较两个内部流动的时间尺度,表明吸积环通常起源于两层吸积流,其中薄吸积盘被厚吸积流夹在中间,除非吸积率非常低。还研究了薄排泄盘和厚排泄流的性质。除非伴星的潮汐效应存在,否则薄的排泄盘预计将在吸积环半径四倍的距离处终止,并在那里形成另一个环。另一方面,浓稠的排泄流很可能会变成超音速风流,达到无穷大。