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Supersonic turbulence in the cold massive core jcmt 18354���0649s���
No full textAn example of a cold massive core, JCMT 18354-0649S which is a possible high-mass analogue to a low-mass star-forming core, is studied. Line and continuum observations from James Clerk Maxwell Telescope, Mopra Telescope and Spitzer are presented and modelled in detail using a 3D molecular line radiative transfer code. In almost every way, JCMT 18354-0649S is a scaled-up version of a typical low-mass core with similar temperatures, chemical abundances and densities. The difference is that both the infall velocity and the turbulent width of the line profiles are an order of magnitude larger. While the higher infall velocity is expected due to the large mass of JCMT 18354-0649S, we suggest that the dissipation of this highly supersonic turbulence may lead to the creation of dense clumps of gas that surround the high-mass core.peer-reviewe
Decreto 18354-MOPT-H
No full textDocumento en PDF, 1 páginas.Modifica, en lo conducente, los Decretos Ejecutivos números 1958-H, de 10 de setiembre de 1971; 7974-H de 27 de enero de 1978, y 12568-T-S-H, de 30 de abril de 1981, a fin de que se entienda que la competencia en materia de regulación y control de transporte marítimo internacional, de cabotaje y por vías de navegación interior, que dichos decretos atribuyen el Ministerio de Hacienda y a la Dirección General de Hacienda, corresponden en realidad al Ministerio de Obras Públicas y Transportes y a la Dirección General de Transporte por Agua respectivamente.Universidad Estatal a Distancia de Costa Ric
Supersonic turbulence in the cold massive core JCMT 18354-0649S
No full textAn example of a cold massive core, JCMT 18354-0649S, a possible high mass analogue to a low mass star forming core is studied. Line and continuum observations from JCMT, Mopra Telescope and Spitzer are presented and modelled in detail using a 3D molecular line radiative transfer code. In almost every way JCMT 18354-0649S is a scaled-up version of a typical low mass core with similar temperatures, chemical abundances and densities. The difference is that both the infall velocity and the turbulent width of the line profiles are an order of magnitude larger. While the higher infall velocity is expected due to the large mass of JCMT 18354-0649S, we suggest that the dissipation of this highly supersonic turbulence may lead to the creation of dense clumps of gas that surround the high mass core.peer-reviewe
Supersonic turbulence in the cold massive core JCMT 18354-0649S
No full textAn example of a cold massive core, JCMT 18354-0649S, a possible high mass analogue to a low mass star forming core is studied. Line and continuum observations from JCMT, Mopra Telescope and Spitzer are presented and modelled in detail using a 3D molecular line radiative transfer code. In almost every way JCMT 18354-0649S is a scaled-up version of a typical low mass core with similar temperatures, chemical abundances and densities. The difference is that both the infall velocity and the turbulent width of the line profiles are an order of magnitude larger. While the higher infall velocity is expected due to the large mass of JCMT 18354-0649S, we suggest that the dissipation of this highly supersonic turbulence may lead to the creation of dense clumps of gas that surround the high mass core
Supersonic turbulence in the cold massive core jcmt 18354���0649s���
No full textAn example of a cold massive core, JCMT 18354-0649S which is a possible high-mass analogue to a low-mass star-forming core, is studied. Line and continuum observations from James Clerk Maxwell Telescope, Mopra Telescope and Spitzer are presented and modelled in detail using a 3D molecular line radiative transfer code. In almost every way, JCMT 18354-0649S is a scaled-up version of a typical low-mass core with similar temperatures, chemical abundances and densities. The difference is that both the infall velocity and the turbulent width of the line profiles are an order of magnitude larger. While the higher infall velocity is expected due to the large mass of JCMT 18354-0649S, we suggest that the dissipation of this highly supersonic turbulence may lead to the creation of dense clumps of gas that surround the high-mass core
Inverstigations on neurosecretion in central and peripheral nervous system of pulmonate snail lymnaea-stagnalis
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Supersonic turbulence in the cold massive core JCMT 18354-0649S star
Get PDFAn example of a cold massive core, JCMT 18354−0649S which is a possible high-mass analogue to a low-mass star-forming core, is studied. Line and continuum observations from James Clerk Maxwell Telescope, Mopra Telescope and Spitzer are presented and modelled in detail using a 3D molecular line radiative transfer code. In almost every way, JCMT 18354−0649S is a scaled-up version of a typical low-mass core with similar temperatures, chemical abundances and densities. The difference is that both the infall velocity and the turbulent width of the line profiles are an order of magnitude larger. While the higher infall velocity is expected due to the large mass of JCMT 18354−0649S, we suggest that the dissipation of this highly supersonic turbulence may lead to the creation of dense clumps of gas that surround the high-mass core
A MASSIVE PROTOSTAR EMBEDDED IN THE SCUBA CORE JCMT 18354-0649S
Get PDFWe report the discovery of an extremely red object embedded in the massive SCUBA core JCMT 18354-0649S. This object is not associated with any known radio or far-IR source, though it appears in Spitzer IRAC data obtained as part of the GLIMPSE survey. At shorter wavelengths, this embedded source exhibits an extreme color, K - L' = 6.7. At an assumed distance of 5.7 kpc, this source has a near-IR luminosity of similar to 1000 L-circle dot. Its spectral energy distribution (SED) rises sharply from 2.1 mu m to 8 mu m, similar to that of a Class 0 young stellar object. Theoretical modeling of the SED indicates that the central star has a mass of 6-12 M-circle dot, with an optical extinction of more than 30. As both inflow and outflow motions are present in JCMT 18354-0649S, we suggest that this deeply embedded source is (1) a massive protostar in the early stages of accretion, and (2) the driving source of a massive molecular outflow evident in HCN J = 3-2 profiles observed toward this region.http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000294955700053&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=8e1609b174ce4e31116a60747a720701Astronomy & AstrophysicsSCI(E)1ARTICLE1null73
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