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Exact Solutions and Scalar Fields in Gravity - Instituto Avanzado de ...

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232 EXACT SOLUTIONS AND SCALAR FIELDS IN GRAVITY<br />

where the isothermal collapse yields a th<strong>in</strong> filament. Thus, fragmentation<br />

of the Gaussian cloud mo<strong>de</strong>l appears to <strong>de</strong>pend sensitively on both<br />

the numerical resolution <strong>and</strong> the <strong>de</strong>tailed thermodynamical treatment.<br />

4. CONCLUSIONS<br />

Here we have presented a further <strong>in</strong>terco<strong>de</strong> comparison with high spatial<br />

resolution for the same Gaussian cloud mo<strong>de</strong>l of Refs. [10] <strong>and</strong> [17].<br />

The calculation was ma<strong>de</strong> us<strong>in</strong>g a variant of the spherical co<strong>de</strong> <strong>de</strong>scribed<br />

<strong>in</strong> Ref. [18], which employs zoom<strong>in</strong>g coord<strong>in</strong>ates to achieve sufficiently<br />

high spatial resolution. With the zoom<strong>in</strong>g coord<strong>in</strong>ates, the computational<br />

cells shr<strong>in</strong>k adaptively <strong>in</strong> accordance with the cloud collapse so<br />

that the resolution <strong>in</strong>creases <strong>in</strong> proportion to the Jeans length as the<br />

<strong>de</strong>nsity enhances. In this framework, we are able to follow the collapse<br />

of the Gaussian cloud mo<strong>de</strong>l through 7 or<strong>de</strong>rs of magnitu<strong>de</strong> <strong>in</strong>crease <strong>in</strong><br />

central <strong>de</strong>nsity without violat<strong>in</strong>g the Jeans condition <strong>and</strong> reproduce the<br />

filamentary solution obta<strong>in</strong>ed <strong>in</strong> Refs. [10] <strong>and</strong> [17] us<strong>in</strong>g a completely<br />

<strong>in</strong><strong>de</strong>pen<strong>de</strong>nt numerical method. The present approach can compete with<br />

the AMR methodology <strong>and</strong> other grid ref<strong>in</strong>ement techniques to provi<strong>de</strong><br />

unprece<strong>de</strong>ntedly high resolution <strong>in</strong> collapse calculations.<br />

The isothermal collapse of the Gaussian cloud mo<strong>de</strong>l is an excellent<br />

test case for any gravitational hydrodynamics co<strong>de</strong> <strong>and</strong> should then be<br />

used to check the reliability of the results for the isothermal phase of collapse<br />

calculations. This paper represents a further step <strong>in</strong> this direction<br />

<strong>and</strong> provi<strong>de</strong>s extra evi<strong>de</strong>nce that the outcome of the isothermal collapse<br />

of the Gaussian cloud is the formation of a s<strong>in</strong>gular filament rather than<br />

the fragmentation <strong>in</strong>to two or more clumps as found <strong>in</strong> previous lowresolution<br />

calculations.<br />

Acknowledgments<br />

The calculation of this paper was performed on the Orig<strong>in</strong> 2000 supercomputer<br />

of the <strong>Instituto</strong> Mexicano <strong>de</strong>l Petroleo (IMP). This work was<br />

partially supported by the Consejo Nacional <strong>de</strong> Investigaciones Científicas<br />

y Tecnológicas (CONICIT) of Venezuela <strong>and</strong> by the Consejo Nacional<br />

<strong>de</strong> Ciencia y Tecnología (CONACyT) of México.<br />

References<br />

[1]<br />

[2]<br />

[3]<br />

R. Mathieu, ARA&A 32 (1994) 465.<br />

A. Duquennoy <strong>and</strong> M. Mayor, A&A 248 (1991) 485.<br />

O.P. Lay, J.E. Carlstrom <strong>and</strong> R.E. Hills, Astrophys. J. 452 (1995) L73.<br />

[4] L.W. Looney, L.G. Mundy <strong>and</strong> W.J. Welch, Astrophys. J. 484 (1997) L157.

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