Dense Molecular Gas around Protostars and in Galactic by Willem A. Baan, Huib Jan van Langevelde

By Willem A. Baan, Huib Jan van Langevelde

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

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By Willem A. Baan, Huib Jan van Langevelde

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

Show description

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2 . P O L A R I Z A T I O N FROM ALIGNED DUST GRAINS At shorter wavelengths, from mm-wave through submm and infrared to optical, aligned dust grains are thought to be responsible for the polarization we observe. There are three possible scenarios: – thermal emission, where the electric field vector E is perpendicular to B, – scattering, where E is perpendicular to B, or – extinction, the residual radiation that is not scattered, where E is parallel to B. Polarization of starlight by extinction dominates at optical wavelengths.

2000, ApJ 537, L135. : 2002, ApJ 567, 962. M. TORRELLES1 , N. F. GOMEZ , G. ANGLADA4 and L. es 2 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA, USA 3 Laboratorio de Astrof´ısica Espacial y F´ısica Fundamental (INTA), Apartado de Correos 50727, Madrid, Spain 4 Instituto de Astrof´ısica de Andaluc´ıa (CSIC), Apartado de Correos 3004, Granada, Spain 5 Instituto de Astronom´ıa (UNAM), Apdo Postal 70-264, Cd. Universitaria, Mexico DF, Mexico (Received 16 April 2004; accepted 15 June 2004) Abstract.

2000) but their positions are a few arcsec far away from 1720-/4765-MHz regions. Concluding, in both sources we found the association of EVIDENCE FOR CO-PROPAGATION OF OH MASERS 41 Figure 2. , 2002) and 4765-MHz OH masers (this paper) in W75N marked as diamonds, open circles and dots, respectively. The crosses and labels indicate the centres of H II regions taken from Torrelles et al. (1997). Relative positions of OH 4765-MHz masers is presented on the enlarged region. The central velocity VLSR (km s−1 ) of each group and relative position errors of components are given.

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