[PDF] Top 20 Outflow forces in intermediate-mass star formation

... evolved intermediate-mass protostellar cluster was included. Outflow forces are factors of 10 to 300 higher than low-mass protostars (Bontemps et ...the outflow forces ... See full document

... hyperfine components together often exceeds 1 toward the main core peak positions (e.g., Fig. 5), the moment maps are done with the isolated hyperfine component 8 km s −1 apart from the main component at a relative ... See full document

... the outflow direc- tions for the different sources using ...filament formation and the following star ...the outflow direction of the first ...core formation in two steps, could provide ... See full document

... The multiple-planet systems give us deep insight into the formation and evolution of planetary systems (e.g., Ford 2006). For example, evidence of planet–planet scattering events could be preserved in the current ... See full document

... The internal random motions observed in molecular clouds, known as turbulence, pro- vide another means to support them against collapse. These both sub- and supersonic mo- tions are observed down to the scales of the ... See full document

... molecular outflow and perpendicular to the previously inferred disk ...the outflow rather suggests that it stems from the inner jet and outflow ... See full document

... molecular outflow and perpendicular to the previously inferred disk ...the outflow rather suggests that it stems from the inner jet and outflow ... See full document

... the mass completeness limit, both in cluster and field ...given mass, tend to have lower star formation rates and smoother structure as compared to the galaxies in ... See full document

... hole formation, some core features are outlined here. In low mass main sequence stars (core Hydrogen burning) the internal gas pressure remains approximately constant through the lifetime of the main ... See full document

... the star, as a result of which the internal temperature of the protostar ...its mass from a surrounding infalling envelope and accretion disk, even as it continues to get ...a star, if it were the ... See full document

... ≥200 K) with a clear velocity gradient approximately perpendic- ular to the (main) outflow orientation, interpreted as evidence for rotational motion of the core. The rotating envelope has a pro- jected diameter ... See full document

... Other IM protostars studied to date include IRAS 22198 + 6336 (S´anchez-Monge et al. 2010; Palau et al. 2011), AFGL 5142 (Palau et al. 2011), IC 1396 N (Neri et al. 2007; Fuente et al. 2009), 13 S in R CrA (Saul 2015), ... See full document

... galactic outflow, so that the latter can grow strong enough to escape from the galactic ...low mass systems with comparatively small ram pressure, whereas larger ones will typically exhibit galactic ... See full document

... the mass outflow rates and kinetic en- ergy in the wind from the composite stack, we first investi- gate the dependence of broad-line Hα properties with galaxy ...the mass out- flow rates, kinetic ... See full document

... galaxy formation, as originally proposed by White & Rees (1978), gas condenses at the center of hierarchically merging dark matter ...The mass function of dark matter halos, which grow hierarchically by ... See full document

... of star-forming galaxies are independent of environ- ...that star-forming galaxies have slightly higher metallicities in high density envi- ronments when compared to lower density/more typical envi- ... See full document

... critical mass of star-forming MC core (see Figures 2-8 and Table ...critical mass for MCc to collapse and form ...critical mass of star-forming molecular cloud core in different cases ... See full document

... stellar mass, and morphological type to the Milky ...stellar mass diagram of galaxies, which indicate they both lost most of their cold gas and hence have a low star formation ... See full document

... In general, determining the stellar content of galaxies is difficult due to the non- linear nature of the masses, luminosities, and timescales of evolutionary phases of stars, as they range over many orders of magnitude. ... See full document

... the star formation rate and stellar mass surface densities, ...resolved star-forming main sequence (rSFMS), and between the gas metallicity and the stellar mass surface density, ... See full document