Self-similar collapse of isothermal spheres and star formation

Shu, Frank H.

doi:10.1086/155274

Cited by 1,532 publications

(2,107 citation statements)

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“…The method is illustrated on the left-hand side of Figure 13 projected baseline length for SMM 1 (right hand side of Figure 13) indicates a power-law density distribution; different prescriptions like, e.g., a Gaussian distribution, are excluded by the data. A power-law index of −2.0±0.5 gives a good fit to the observations, which agrees well with models for protostellar collapse (e.g., Shu 1977). The fluxes on long baselines suggest the presence of extra, unresolved emission, probably associated with the inner few hundred AU of the envelope where the temperature is likely to exceed the adopted T dust ∝ r −0.4 distribution.…”

Section: An Intermediate-mass Class 0 Yso In Serpenssupporting

confidence: 85%

“…The only exceptions are H 2 , He, H + 3 and perhaps N 2 . Models appropriate for the cold outer envelopes have been made by Rawlings et al (1992), Willacy et al (1994), and Shalabiea & Greenberg (1995), using parametrized fits to the density profiles in simple collapse models such as that of Shu (1977) or Basu & Mouschovias (1994). They differ strongly in the adopted mechanisms that return molecules to the gas, ranging from none in Rawlings et al's to efficient desorption in Shalabiea & Greenberg's.…”

Section: Modelsmentioning

confidence: 99%

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Models and Observations of the Chemistry Near Young Stellar Objects

Dishoeck

Hogerheijde

1999

The Origin of Stars and Planetary Systems

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Section: An Intermediate-mass Class 0 Yso In Serpenssupporting

confidence: 85%

Section: Modelsmentioning

confidence: 99%

Models and Observations of the Chemistry Near Young Stellar Objects

Dishoeck

Hogerheijde

1999

The Origin of Stars and Planetary Systems

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“…They rule out some theoretical models (e.g. so-called "logatropic" one) but are consistent with the "standard" theory of star formation (Shu 1977).…”

Section: Radial Density Profilessupporting

confidence: 62%

Physical and chemical structure of dense cores in regions of high mass star formation

Зинченко

Pirogov

Caselli³

et al. 2005

Proc. IAU

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Abstract. We found that in regions of high mass star formation the CS emission correlates well with the dust continuum emission and is therefore a good tracer of the total mass while the N2H + distribution is frequently very different. This is opposite to their typical behavior in low-mass cores. The behavior of other high density tracers varies from source to source but most of them are closer to CS. Radial density profiles in massive cores are fitted by power laws with indices about −1.6, as derived from the dust continuum emission. The radial temperature dependence on intermediate scales is close to the theoretically expected one for a centrally heated optically thin cloud. The velocity dispersion either remains constant or decreases from the core center to the edge. Several cores including those without known embedded IR sources show signs of infall motions. They can represent the earliest phases of massive protostars. There are implicit arguments in favor of small-scale clumpiness in the cores.

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“…The critical nature of the core is consistent with (1) the starless characteristic of the core (Forbrich et al 2009), (2) a lack of detection of supersonic infalling gas motion (Aguti et al 2007), and (3) the detection of possible oscillating gas motion in the outer layer of the core (Aguti et al 2007). Further magnetic diffusion and/or turbulent dissipation can eventually trigger the collapse of the core (e.g., Shu 1977;Nakano 1998). Note that external compression of the core (e.g., Frau et al 2015 for the possibility of the cloud-cloud collision in the Pipe Nebula) may also initiate or disrupt the star formation in the core.…”

Section: Magnetic Properties Of the Corementioning

confidence: 99%

Distortion of Magnetic Fields in a Starless Core II: 3D Magnetic Field Structure of FeSt 1-457

Kandori

Tamura

Tomisaka

et al. 2017

ApJ

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Three-dimensional (3D) magnetic field information on molecular clouds and cores is important for revealing their kinematical stability (magnetic support) against gravity, which is fundamental for studying the initial conditions of star formation. In the present study, the 3D magnetic field structure of the dense starless core FeSt 1-457 is determined based on the near-infrared polarimetric observations of the dichroic polarization of background stars and simple 3D modeling. With an obtained angle of line-of-sight magnetic inclination axis inc q of 45 10    and previously determined plane-of-sky magnetic field strength B pol of 23.8±12.1 G m , the total magnetic field strength for FeSt 1-457 is derived to be 33.7±18.0 G m . The critical mass of FeSt 1-457, evaluated using both magnetic and thermal/turbulent support is M 3.70 0.92 cr =  M  , which is identical to the observed core mass, M 3.55 0.75 core =  M  . We thus conclude that the stability of FeSt 1-457 is in a condition close to the critical state. Without infalling gas motion and no associated young stars, the core is regarded to be in the earliest stage of star formation, i.e., the stage just before the onset of dynamical collapse following the attainment of a supercritical condition. These properties could make FeSt 1-457 one of the best starless cores for future studies of the initial conditions of star formation.

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Self-similar collapse of isothermal spheres and star formation

Cited by 1,532 publications

References 0 publications

Models and Observations of the Chemistry Near Young Stellar Objects

Models and Observations of the Chemistry Near Young Stellar Objects

Physical and chemical structure of dense cores in regions of high mass star formation

Distortion of Magnetic Fields in a Starless Core II: 3D Magnetic Field Structure of FeSt 1-457

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