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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Gravitational Instability of Shocked Interstellar Gas Layers
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Gravitational Instability of Shocked Interstellar Gas Layers

机译：冲击星际气层的重力失稳

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Inthispaperweinvestigategravitationalinstabilityofshockedgaslayersusinglinearanalysis.Anunperturbedstateisaself-gravitatingisothermallayerwhichgrowswithtimebytheaccretionofgasthroughshockfrontsduetoacloud-cloudcollision.Sincetheunperturbedstateisnotstatic,andcannotbedescribedbyaself-similarsolution,wenumericallysolvedtheperturbationequationsanddirectlyintegratedthemovertime.Wetookaccountofthedistributionofphysicalquantitiesacrossthethickness.LinearizedRankine-Hugoniotrelationswereimposedatshockfrontsasboundaryconditions.Thefollowingresultsarefoundfromourunsteadylinearanalysis:theperturbationinitiallyevolvesinoscillatorymode,andbeginstogrowatacertainepoch.Thewavenumberofthefastestgrowingmodeisgivenby$$k=2sqrt{2piG ho_mathrm{E}{calMmit}}/c_mathrm{s}$$,where$$ ho_mathrm{E},;c_mathrm{s}$$and$$calMmit$$arethedensityoftheparentclouds,thesoundvelocityandtheMachnumberofthecollisionvelocity,respectively.Forthismode,thetransitionepochfromoscillatorytogrowingmodeisgivenby$$t_g=1.2/sqrt{2piG ho_mathrm{E}{calMmit}}$$.Theepochatwhichthefastestgrowingmodebecomesnon-linearisgivenby$$2.4delta_0^{-0.1}/sqrt{2piG ho_mathrm{E}{calMmit}}$$,where$$delta_0$$istheinitialamplitudeoftheperturbationofthecolumndensity.Asanapplicationofourlinearanalysis,weinvestigatedcriteriaforcollision-inducedfragmentation.Collision-inducedfragmentationwilloccuronlywhenparentcloudsarecold,or$$alpha_0=$$5$$c_mathrm{s}^2R/2GM1$$,where$$R$$and$$M$$aretheradiusandthemassofparentclouds,respectively.
机译：Inthispaperweinvestigategravitationalinstabilityofshockedgaslayersusinglinearanalysis.Anunperturbedstateisaself-gravitatingisothermallayerwhichgrowswithtimebytheaccretionofgasthroughshockfrontsduetoacloud-cloudcollision.Sincetheunperturbedstateisnotstatic，andcannotbedescribedbyaself-similarsolution，wenumericallysolvedtheperturbationequationsanddirectlyintegratedthemovertime.Wetookaccountofthedistributionofphysicalquantitiesacrossthethickness.LinearizedRankine-Hugoniotrelationswereimposedatshockfrontsasboundaryconditions.Thefollowingresultsarefoundfromourunsteadylinearanalysis：theperturbationinitiallyevolvesinoscillatorymode，andbeginstogrowatacertainepoch.Thewavenumberofthefastestgrowingmodeisgivenby $$ K = 2sqrt {2piG ho_mathrm {E} {calMmit}} / c_mathrm {S} $ $，其中$$ ho_mathrm {E} ,; c_mathrm {s} $和$$ calMmit $$分别是父云的密度，声速和碰撞速度的马赫数。对于该模式，给出了从摆动到生长模式的过渡时期，由$$ t_g = 1.2 / thrm {E} {calMmit}} $$。通过$ 2.4delta_0 ^ {-0.1} / sqrt {2piG ho_mathrm {E} {calMmit}} $$给出最快增长模式的时期，其中$$ delta_0 $$是对应用程序的扰动的初始强度，对解决方案的兴趣在于它对解决方法的兴趣。碰撞诱发的碎片只会在父云残酷时出现，或者$$ alpha_0 = $ 5 $$ c_mathrm {s} ^ 2R / 2GM 1 $$，其中$$ R $$和$$ M $$分别是父云的半径和质量。

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