Get Dense Molecular Gas around Protostars and in Galactic PDF

By Willem A. Baan, Huib Jan van Langevelde

ISBN-10: 140203038X

ISBN-13: 9781402030383

ISBN-10: 1402038313

ISBN-13: 9781402038310

Those lawsuits summarize our current wisdom on astronomical molecules, spotlight significant difficulties to be addressed, and eventually suggest destiny paintings. Their theoretical figuring out consists of physics, numerical simulations and chemistry.

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Additional resources for Dense Molecular Gas around Protostars and in Galactic Nuclei: European Workshop on Astronomical Molecules 2004

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Field, D. : 1992, A&A 262, 555. S. : 2000, A&A 362, 1093. J. : 2004, MNRAS 350, 1409. M. : 2004, MNRAS 347, 1164. J. : 2000, MNRAS 312, 211. , Curiel, S. : 1997, ApJ 489, 744. J. : 1998, ApJ 509, 262. MAGNETIC FIELDS IN STAR-FORMING REGIONS: THEORETICAL ASPECTS DANIELE GALLI INAF-Osservatorio Astrofisico di Arcetri, Largo E. it (Received 16 April 2004; accepted 15 June 2004) Abstract. We review the basic theoretical elements leading to our current understanding of the role of magnetic fields in the process of star formation.

08. All components were projected at the S–W edge of the H II region labelled as 3b by Hughes and Wouterloot (1984) (Figure 1). We also searched for the 4660- and 4750-MHz lines but we did not find any of them above a level of 20 mJy. Searching for the OH ground-state masers in Cep A we detected the 1665-, 1667- and 1720-MHz emission. 3 km s−1 (Figure 1). These components coincided within 23 mas in the sky and are a Zeeman pair. It is striking that the 1720-MHz spots coincided with group EVIDENCE FOR CO-PROPAGATION OF OH MASERS 39 Figure 1.

It (Received 16 April 2004; accepted 15 June 2004) Abstract. We review the basic theoretical elements leading to our current understanding of the role of magnetic fields in the process of star formation. In particular, we concentrate on: (i) the relevance of the mass-to-flux ratio for the stability of molecular clouds; (ii) the consequences of magnetic flux leakage for the evolution of cloud cores; (iii) the phase of anisotropic dynamical collapse following the formation of strongly peaked density distributions; (iv) the mechanism of magnetic braking as a possible solution to the angular momentum problem in star formation.

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Dense Molecular Gas around Protostars and in Galactic Nuclei: European Workshop on Astronomical Molecules 2004 by Willem A. Baan, Huib Jan van Langevelde


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