A multicomponent model for computing the thermal structure of collapsing protostellar clouds
Abstract A model for simulating the thermal and dynamical evolution of protostellar clouds is presented. In the model, the dust and gas temperatures are treated separately, making it possible to more precisely describe the initial stages of the cloud’s gravitational contraction and collapse. The mod...
Ausführliche Beschreibung
Autor*in: |
Pavlyuchenkov, Ya. N. [verfasserIn] Zhilkin, A. G. [verfasserIn] |
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Format: |
E-Artikel |
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Sprache: |
Englisch |
Erschienen: |
2013 |
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Schlagwörter: |
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Übergeordnetes Werk: |
Enthalten in: Astronomy reports - Moscow : MAIK Nauka/Interperiodika, 1993, 57(2013), 9 vom: Sept., Seite 641-656 |
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Übergeordnetes Werk: |
volume:57 ; year:2013 ; number:9 ; month:09 ; pages:641-656 |
Links: |
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DOI / URN: |
10.1134/S1063772913090035 |
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Katalog-ID: |
SPR019428596 |
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520 | |a Abstract A model for simulating the thermal and dynamical evolution of protostellar clouds is presented. In the model, the dust and gas temperatures are treated separately, making it possible to more precisely describe the initial stages of the cloud’s gravitational contraction and collapse. The model is fast enough to be applied in hydrodynamical computations, and has a high enough accuracy for the results to be used to compute emission spectra and comparing them with observational data. Two problems are considered as test examples and simple applications: calculation of the structure of clouds in thermal and hydrostatic equilibrium, and modeling the evolution of a protostellar cloud in a spherically symmetric approximation, including the formation of the first hydrostatic core. | ||
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10.1134/S1063772913090035 doi (DE-627)SPR019428596 (SPR)S1063772913090035-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Pavlyuchenkov, Ya. N. verfasserin aut A multicomponent model for computing the thermal structure of collapsing protostellar clouds 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract A model for simulating the thermal and dynamical evolution of protostellar clouds is presented. In the model, the dust and gas temperatures are treated separately, making it possible to more precisely describe the initial stages of the cloud’s gravitational contraction and collapse. The model is fast enough to be applied in hydrodynamical computations, and has a high enough accuracy for the results to be used to compute emission spectra and comparing them with observational data. Two problems are considered as test examples and simple applications: calculation of the structure of clouds in thermal and hydrostatic equilibrium, and modeling the evolution of a protostellar cloud in a spherically symmetric approximation, including the formation of the first hydrostatic core. Dust (dpeaa)DE-He213 Astronomy Report (dpeaa)DE-He213 Source Function (dpeaa)DE-He213 Thermal Structure (dpeaa)DE-He213 Bold Solid Line (dpeaa)DE-He213 Zhilkin, A. G. verfasserin aut Enthalten in Astronomy reports Moscow : MAIK Nauka/Interperiodika, 1993 57(2013), 9 vom: Sept., Seite 641-656 (DE-627)312182287 (DE-600)2010316-5 1562-6881 nnns volume:57 year:2013 number:9 month:09 pages:641-656 https://dx.doi.org/10.1134/S1063772913090035 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_647 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 57 2013 9 09 641-656 |
spelling |
10.1134/S1063772913090035 doi (DE-627)SPR019428596 (SPR)S1063772913090035-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Pavlyuchenkov, Ya. N. verfasserin aut A multicomponent model for computing the thermal structure of collapsing protostellar clouds 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract A model for simulating the thermal and dynamical evolution of protostellar clouds is presented. In the model, the dust and gas temperatures are treated separately, making it possible to more precisely describe the initial stages of the cloud’s gravitational contraction and collapse. The model is fast enough to be applied in hydrodynamical computations, and has a high enough accuracy for the results to be used to compute emission spectra and comparing them with observational data. Two problems are considered as test examples and simple applications: calculation of the structure of clouds in thermal and hydrostatic equilibrium, and modeling the evolution of a protostellar cloud in a spherically symmetric approximation, including the formation of the first hydrostatic core. Dust (dpeaa)DE-He213 Astronomy Report (dpeaa)DE-He213 Source Function (dpeaa)DE-He213 Thermal Structure (dpeaa)DE-He213 Bold Solid Line (dpeaa)DE-He213 Zhilkin, A. G. verfasserin aut Enthalten in Astronomy reports Moscow : MAIK Nauka/Interperiodika, 1993 57(2013), 9 vom: Sept., Seite 641-656 (DE-627)312182287 (DE-600)2010316-5 1562-6881 nnns volume:57 year:2013 number:9 month:09 pages:641-656 https://dx.doi.org/10.1134/S1063772913090035 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_647 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 57 2013 9 09 641-656 |
allfields_unstemmed |
10.1134/S1063772913090035 doi (DE-627)SPR019428596 (SPR)S1063772913090035-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Pavlyuchenkov, Ya. N. verfasserin aut A multicomponent model for computing the thermal structure of collapsing protostellar clouds 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract A model for simulating the thermal and dynamical evolution of protostellar clouds is presented. In the model, the dust and gas temperatures are treated separately, making it possible to more precisely describe the initial stages of the cloud’s gravitational contraction and collapse. The model is fast enough to be applied in hydrodynamical computations, and has a high enough accuracy for the results to be used to compute emission spectra and comparing them with observational data. Two problems are considered as test examples and simple applications: calculation of the structure of clouds in thermal and hydrostatic equilibrium, and modeling the evolution of a protostellar cloud in a spherically symmetric approximation, including the formation of the first hydrostatic core. Dust (dpeaa)DE-He213 Astronomy Report (dpeaa)DE-He213 Source Function (dpeaa)DE-He213 Thermal Structure (dpeaa)DE-He213 Bold Solid Line (dpeaa)DE-He213 Zhilkin, A. G. verfasserin aut Enthalten in Astronomy reports Moscow : MAIK Nauka/Interperiodika, 1993 57(2013), 9 vom: Sept., Seite 641-656 (DE-627)312182287 (DE-600)2010316-5 1562-6881 nnns volume:57 year:2013 number:9 month:09 pages:641-656 https://dx.doi.org/10.1134/S1063772913090035 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_647 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 57 2013 9 09 641-656 |
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10.1134/S1063772913090035 doi (DE-627)SPR019428596 (SPR)S1063772913090035-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Pavlyuchenkov, Ya. N. verfasserin aut A multicomponent model for computing the thermal structure of collapsing protostellar clouds 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract A model for simulating the thermal and dynamical evolution of protostellar clouds is presented. In the model, the dust and gas temperatures are treated separately, making it possible to more precisely describe the initial stages of the cloud’s gravitational contraction and collapse. The model is fast enough to be applied in hydrodynamical computations, and has a high enough accuracy for the results to be used to compute emission spectra and comparing them with observational data. Two problems are considered as test examples and simple applications: calculation of the structure of clouds in thermal and hydrostatic equilibrium, and modeling the evolution of a protostellar cloud in a spherically symmetric approximation, including the formation of the first hydrostatic core. Dust (dpeaa)DE-He213 Astronomy Report (dpeaa)DE-He213 Source Function (dpeaa)DE-He213 Thermal Structure (dpeaa)DE-He213 Bold Solid Line (dpeaa)DE-He213 Zhilkin, A. G. verfasserin aut Enthalten in Astronomy reports Moscow : MAIK Nauka/Interperiodika, 1993 57(2013), 9 vom: Sept., Seite 641-656 (DE-627)312182287 (DE-600)2010316-5 1562-6881 nnns volume:57 year:2013 number:9 month:09 pages:641-656 https://dx.doi.org/10.1134/S1063772913090035 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_647 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 57 2013 9 09 641-656 |
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10.1134/S1063772913090035 doi (DE-627)SPR019428596 (SPR)S1063772913090035-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Pavlyuchenkov, Ya. N. verfasserin aut A multicomponent model for computing the thermal structure of collapsing protostellar clouds 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract A model for simulating the thermal and dynamical evolution of protostellar clouds is presented. In the model, the dust and gas temperatures are treated separately, making it possible to more precisely describe the initial stages of the cloud’s gravitational contraction and collapse. The model is fast enough to be applied in hydrodynamical computations, and has a high enough accuracy for the results to be used to compute emission spectra and comparing them with observational data. Two problems are considered as test examples and simple applications: calculation of the structure of clouds in thermal and hydrostatic equilibrium, and modeling the evolution of a protostellar cloud in a spherically symmetric approximation, including the formation of the first hydrostatic core. Dust (dpeaa)DE-He213 Astronomy Report (dpeaa)DE-He213 Source Function (dpeaa)DE-He213 Thermal Structure (dpeaa)DE-He213 Bold Solid Line (dpeaa)DE-He213 Zhilkin, A. G. verfasserin aut Enthalten in Astronomy reports Moscow : MAIK Nauka/Interperiodika, 1993 57(2013), 9 vom: Sept., Seite 641-656 (DE-627)312182287 (DE-600)2010316-5 1562-6881 nnns volume:57 year:2013 number:9 month:09 pages:641-656 https://dx.doi.org/10.1134/S1063772913090035 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_647 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 57 2013 9 09 641-656 |
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Pavlyuchenkov, Ya. N. ddc 520 bkl 39.00 misc Dust misc Astronomy Report misc Source Function misc Thermal Structure misc Bold Solid Line A multicomponent model for computing the thermal structure of collapsing protostellar clouds |
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520 ASE 39.00 bkl A multicomponent model for computing the thermal structure of collapsing protostellar clouds Dust (dpeaa)DE-He213 Astronomy Report (dpeaa)DE-He213 Source Function (dpeaa)DE-He213 Thermal Structure (dpeaa)DE-He213 Bold Solid Line (dpeaa)DE-He213 |
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multicomponent model for computing the thermal structure of collapsing protostellar clouds |
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A multicomponent model for computing the thermal structure of collapsing protostellar clouds |
abstract |
Abstract A model for simulating the thermal and dynamical evolution of protostellar clouds is presented. In the model, the dust and gas temperatures are treated separately, making it possible to more precisely describe the initial stages of the cloud’s gravitational contraction and collapse. The model is fast enough to be applied in hydrodynamical computations, and has a high enough accuracy for the results to be used to compute emission spectra and comparing them with observational data. Two problems are considered as test examples and simple applications: calculation of the structure of clouds in thermal and hydrostatic equilibrium, and modeling the evolution of a protostellar cloud in a spherically symmetric approximation, including the formation of the first hydrostatic core. |
abstractGer |
Abstract A model for simulating the thermal and dynamical evolution of protostellar clouds is presented. In the model, the dust and gas temperatures are treated separately, making it possible to more precisely describe the initial stages of the cloud’s gravitational contraction and collapse. The model is fast enough to be applied in hydrodynamical computations, and has a high enough accuracy for the results to be used to compute emission spectra and comparing them with observational data. Two problems are considered as test examples and simple applications: calculation of the structure of clouds in thermal and hydrostatic equilibrium, and modeling the evolution of a protostellar cloud in a spherically symmetric approximation, including the formation of the first hydrostatic core. |
abstract_unstemmed |
Abstract A model for simulating the thermal and dynamical evolution of protostellar clouds is presented. In the model, the dust and gas temperatures are treated separately, making it possible to more precisely describe the initial stages of the cloud’s gravitational contraction and collapse. The model is fast enough to be applied in hydrodynamical computations, and has a high enough accuracy for the results to be used to compute emission spectra and comparing them with observational data. Two problems are considered as test examples and simple applications: calculation of the structure of clouds in thermal and hydrostatic equilibrium, and modeling the evolution of a protostellar cloud in a spherically symmetric approximation, including the formation of the first hydrostatic core. |
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A multicomponent model for computing the thermal structure of collapsing protostellar clouds |
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N.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="2"><subfield code="a">A multicomponent model for computing the thermal structure of collapsing protostellar clouds</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2013</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract A model for simulating the thermal and dynamical evolution of protostellar clouds is presented. In the model, the dust and gas temperatures are treated separately, making it possible to more precisely describe the initial stages of the cloud’s gravitational contraction and collapse. The model is fast enough to be applied in hydrodynamical computations, and has a high enough accuracy for the results to be used to compute emission spectra and comparing them with observational data. Two problems are considered as test examples and simple applications: calculation of the structure of clouds in thermal and hydrostatic equilibrium, and modeling the evolution of a protostellar cloud in a spherically symmetric approximation, including the formation of the first hydrostatic core.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Dust</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Astronomy Report</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Source Function</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Thermal Structure</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Bold Solid Line</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Zhilkin, A. 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