By Willem A. Baan, Huib Jan van Langevelde
Those complaints summarize our current wisdom on astronomical molecules, spotlight significant difficulties to be addressed, and eventually suggest destiny paintings. Their theoretical realizing comprises physics, numerical simulations and chemistry.
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Extra resources for Dense Molecular Gas around Protostars and in Galactic Nuclei: European Workshop on Astronomical Molecules 2004
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2002) also use the mean velocity separation as function of pair separation, Dα (δ log r ) = ( |δVLSR |α )/N , where in each logarithmically spaced interval of angular separation δ log r , there are N pairs, each with velocity separation δVLSR . In the case of Kolmogorov turbulence, for α = 1, 2, 3, d log Dα /d log r = q = 1/3, 2/3, 1, respectively. 16. 2. 5. Conclusions The position and velocity of the newly detected maser region C suggests that the CO cloud collision is occurring at an oblique angle to the line of site.
2001). It is suggested that the polarization properties are age related, with younger sources being more highly organized, having stronger polarization and greater alignment with the outﬂow direction. 0 GHz have Zeeman splitting comparable to their linewidths, so that Zeeman pairs are common. 0-GHz OH masers and found many cases of matching Zeeman pairs at 6035 and 6030 MHz, from which reliable B values can be deduced even without interferometry. Blending of maser lines (including hyperﬁne components) is difﬁcult to deal with.
Dense Molecular Gas around Protostars and in Galactic Nuclei: European Workshop on Astronomical Molecules 2004 by Willem A. Baan, Huib Jan van Langevelde