The collapse of a fast rotating interstellar gas cloud

Narita, Shinji; McNally, D.; Pearce, G. L.; Sorensen, Søren-Aksel

doi:10.1093/mnras/203.2.491

Cited by 3 publications

(7 citation statements)

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“…Case (C) (2)(3)(4)(5)(6)(7)(8)(9)(10)(11)(12)(13) where Po, Wo and (50 are all constants and ao was set equal to RI 2. As for the outer boundary condition, we adopted dRldt=O.…”

Section: Thin Disk Approximation and One-dimensional Simulationmentioning

confidence: 99%

“…Initial mass-angular momentum relation is the same for all cases (A) to (D) and it is rewritten as (2)(3)(4)(5)(6)(7)(8)(9)(10)(11)(12)(13)(14) where M is the total mass of the cloud, 47[PoR 3 13. **> Originally, we adopted Eq.…”

Section: J(?i1)-m(?i1) Relation and Initial Parametersmentioning

confidence: 99%

“…(2 -14). Now, in each of cases (A) to (0), the initial condition is specified by the two parameters, (2)(3)(4)(5)(6)(7)(8)(9)(10)(11)(12)(13)(14)(15) which represent the ratios of thermal and rotational energies to gravitational energy of a corresponding homogeneous sphere with the same equatorial radius, respectively. In all cases, time is measured in units of a free-fall time of a corresponding homogeneous sphere, Le., t ff ( =';37[/ 32Gpo).…”

Section: J(?i1)-m(?i1) Relation and Initial Parametersmentioning

confidence: 99%

“…The flatness of an equi-density contour defined in §3 is given by the ratio of TJJ at Pe=P in Eq_ (4)(5)(6)(7)(8)(9)(10)(11)(12)(13)(14)(15)(16)(17)(18) to z at ((JZ/(JPe)p=O in Eq. (4)(5)(6)(7)(8)(9)(10)(11)(12)(13)(14)(15)(16)(17)(18)(19).…”

Section: J(?i1)-m(?i1) Relation and Initial Parametersmentioning

confidence: 99%

“…(4)(5)(6)(7)(8)(9)(10)(11)(12)(13)(14)(15)(16)(17)(18)(19). Thus, we find /~{r , 1.51 r- (4)(5)(6)(7)(8)(9)(10)(11)(12)(13)(14)(15)(16)(17)(18)(19)(20) In advanced stages of collapse, r is about 4 as mentioned above and, hence, the inner envelope has a flatness of about 6. It is to be noticed that this result has been obtained almost independently of the initial condition of the cloud and is, in fact, in agreement with the results of the two-dimensional simulations described in §3.…”

Section: J(?i1)-m(?i1) Relation and Initial Parametersmentioning

confidence: 99%

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Characteristics of Collapse of Rotating Isothermal Clouds

Narita

Hayashi²,

Miyama

1984

Progress of Theoretical Physics

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In order to solve the long-standing "centrifugal bounce or runaway" problem and also the problem of subsequent dynamical evolution, the collapse of rotating isothermal clouds has· been investigated by axisymmetric two-dimensional simulations and also by one-dimensional analysis as well as simulations in a thin disk approximation. For the initial condition, we have considered flattened configurations besides a uniform sphere.The results show that the collapse of the inner region follows a series of similar disk-like configurations nearly independent of initial and boundary conditions: The angular velocity and the column density of the disk are both proportional to (ac 2

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“…Case (C) (2)(3)(4)(5)(6)(7)(8)(9)(10)(11)(12)(13) where Po, Wo and (50 are all constants and ao was set equal to RI 2. As for the outer boundary condition, we adopted dRldt=O.…”

Section: Thin Disk Approximation and One-dimensional Simulationmentioning

confidence: 99%