On the properties of elliptical and spiral galaxies in a CDM scenario
Abstract This paper aims to investigate what kind of density perturbations did lead to elliptical galaxies and what kind to spiral galaxies, in the context of a CDM scenario. Previous work by HP (Heavens and Peacock, 1988) is reviewed and extended; more particularly: (i) a theoreticalJ∼Mξ relation i...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Caimmi, R. [verfasserIn] |
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| Format: |
Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
1990 |
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| Schlagwörter: |
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| Anmerkung: |
© Kluwer Academic Publishers 1990 |
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| Übergeordnetes Werk: |
Enthalten in: Astrophysics and space science - Kluwer Academic Publishers, 1968, 168(1990), 1 vom: Juni, Seite 131-152 |
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| Übergeordnetes Werk: |
volume:168 ; year:1990 ; number:1 ; month:06 ; pages:131-152 |
| Links: |
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| DOI / URN: |
10.1007/BF00654599 |
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| Katalog-ID: |
OLC2066180041 |
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| 245 | 1 | 0 | |a On the properties of elliptical and spiral galaxies in a CDM scenario |
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| 520 | |a Abstract This paper aims to investigate what kind of density perturbations did lead to elliptical galaxies and what kind to spiral galaxies, in the context of a CDM scenario. Previous work by HP (Heavens and Peacock, 1988) is reviewed and extended; more particularly: (i) a theoreticalJ∼Mξ relation is derived for virialized configurations, with a slope increasing with the mass, in the range 5/3<ξ<2, and compared with its counterpart deduced by HP for expanding configurations; (ii) an non-dimensional angular momentum Λ=J/(G2M5tff)1/3; withtfffree-fall time at turnaround, is calculated explicitly and compared with the usual spin parameter λ=J(−E)1/2/(GM5/2), in the special case of polytropic spheres and for different peak heights; (iii) a model is built up where the ellipsoidal density perturbations described by HP are approximated as spherical density perturbations with the same mass and the same rate of acquisition of angular momentum, and the contribution of the latter to the expansion is also taken into account. The calculations are limited to the special case of Einstein-de Sitter universes (of dust only), in the whole range of HP distributions of angular momenta. If a massM=$ 10^{12} $m⊙ is typical for galaxies, the results are consistent with both an inferred difference roughly in a factor of six times between angular momenta of ellipticals and spirals, and a continuous transition from the former to the latter, for each peak height. It is argued that star formation together with angular momentum, instead of peak height alone, makes the fate of a given proto-object; more specifically, if star formation is high enough and/or angular momentum is low enough, the system will be frozen as an elliptical galaxy; if, on the other hand, the rate of star formation is low enough, and/or angular momentum is high enough, the system will be frozen as a spiral galaxy. In addition, the results lead to an obvious trend: more ellipticals are associated with higher peak heights and more spirals with lower peak heights. | ||
| 650 | 4 | |a Dust | |
| 650 | 4 | |a Angular Momentum | |
| 650 | 4 | |a Peak Height | |
| 650 | 4 | |a High Peak | |
| 650 | 4 | |a Star Formation | |
| 700 | 1 | |a Andriani, E. |4 aut | |
| 700 | 1 | |a Secco, L. |4 aut | |
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10.1007/BF00654599 doi (DE-627)OLC2066180041 (DE-He213)BF00654599-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Caimmi, R. verfasserin aut On the properties of elliptical and spiral galaxies in a CDM scenario 1990 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1990 Abstract This paper aims to investigate what kind of density perturbations did lead to elliptical galaxies and what kind to spiral galaxies, in the context of a CDM scenario. Previous work by HP (Heavens and Peacock, 1988) is reviewed and extended; more particularly: (i) a theoreticalJ∼Mξ relation is derived for virialized configurations, with a slope increasing with the mass, in the range 5/3<ξ<2, and compared with its counterpart deduced by HP for expanding configurations; (ii) an non-dimensional angular momentum Λ=J/(G2M5tff)1/3; withtfffree-fall time at turnaround, is calculated explicitly and compared with the usual spin parameter λ=J(−E)1/2/(GM5/2), in the special case of polytropic spheres and for different peak heights; (iii) a model is built up where the ellipsoidal density perturbations described by HP are approximated as spherical density perturbations with the same mass and the same rate of acquisition of angular momentum, and the contribution of the latter to the expansion is also taken into account. The calculations are limited to the special case of Einstein-de Sitter universes (of dust only), in the whole range of HP distributions of angular momenta. If a massM=$ 10^{12} $m⊙ is typical for galaxies, the results are consistent with both an inferred difference roughly in a factor of six times between angular momenta of ellipticals and spirals, and a continuous transition from the former to the latter, for each peak height. It is argued that star formation together with angular momentum, instead of peak height alone, makes the fate of a given proto-object; more specifically, if star formation is high enough and/or angular momentum is low enough, the system will be frozen as an elliptical galaxy; if, on the other hand, the rate of star formation is low enough, and/or angular momentum is high enough, the system will be frozen as a spiral galaxy. In addition, the results lead to an obvious trend: more ellipticals are associated with higher peak heights and more spirals with lower peak heights. Dust Angular Momentum Peak Height High Peak Star Formation Andriani, E. aut Secco, L. aut Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 168(1990), 1 vom: Juni, Seite 131-152 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:168 year:1990 number:1 month:06 pages:131-152 https://doi.org/10.1007/BF00654599 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_24 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4306 GBV_ILN_4700 AR 168 1990 1 06 131-152 |
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10.1007/BF00654599 doi (DE-627)OLC2066180041 (DE-He213)BF00654599-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Caimmi, R. verfasserin aut On the properties of elliptical and spiral galaxies in a CDM scenario 1990 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1990 Abstract This paper aims to investigate what kind of density perturbations did lead to elliptical galaxies and what kind to spiral galaxies, in the context of a CDM scenario. Previous work by HP (Heavens and Peacock, 1988) is reviewed and extended; more particularly: (i) a theoreticalJ∼Mξ relation is derived for virialized configurations, with a slope increasing with the mass, in the range 5/3<ξ<2, and compared with its counterpart deduced by HP for expanding configurations; (ii) an non-dimensional angular momentum Λ=J/(G2M5tff)1/3; withtfffree-fall time at turnaround, is calculated explicitly and compared with the usual spin parameter λ=J(−E)1/2/(GM5/2), in the special case of polytropic spheres and for different peak heights; (iii) a model is built up where the ellipsoidal density perturbations described by HP are approximated as spherical density perturbations with the same mass and the same rate of acquisition of angular momentum, and the contribution of the latter to the expansion is also taken into account. The calculations are limited to the special case of Einstein-de Sitter universes (of dust only), in the whole range of HP distributions of angular momenta. If a massM=$ 10^{12} $m⊙ is typical for galaxies, the results are consistent with both an inferred difference roughly in a factor of six times between angular momenta of ellipticals and spirals, and a continuous transition from the former to the latter, for each peak height. It is argued that star formation together with angular momentum, instead of peak height alone, makes the fate of a given proto-object; more specifically, if star formation is high enough and/or angular momentum is low enough, the system will be frozen as an elliptical galaxy; if, on the other hand, the rate of star formation is low enough, and/or angular momentum is high enough, the system will be frozen as a spiral galaxy. In addition, the results lead to an obvious trend: more ellipticals are associated with higher peak heights and more spirals with lower peak heights. Dust Angular Momentum Peak Height High Peak Star Formation Andriani, E. aut Secco, L. aut Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 168(1990), 1 vom: Juni, Seite 131-152 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:168 year:1990 number:1 month:06 pages:131-152 https://doi.org/10.1007/BF00654599 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_24 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4306 GBV_ILN_4700 AR 168 1990 1 06 131-152 |
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10.1007/BF00654599 doi (DE-627)OLC2066180041 (DE-He213)BF00654599-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Caimmi, R. verfasserin aut On the properties of elliptical and spiral galaxies in a CDM scenario 1990 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1990 Abstract This paper aims to investigate what kind of density perturbations did lead to elliptical galaxies and what kind to spiral galaxies, in the context of a CDM scenario. Previous work by HP (Heavens and Peacock, 1988) is reviewed and extended; more particularly: (i) a theoreticalJ∼Mξ relation is derived for virialized configurations, with a slope increasing with the mass, in the range 5/3<ξ<2, and compared with its counterpart deduced by HP for expanding configurations; (ii) an non-dimensional angular momentum Λ=J/(G2M5tff)1/3; withtfffree-fall time at turnaround, is calculated explicitly and compared with the usual spin parameter λ=J(−E)1/2/(GM5/2), in the special case of polytropic spheres and for different peak heights; (iii) a model is built up where the ellipsoidal density perturbations described by HP are approximated as spherical density perturbations with the same mass and the same rate of acquisition of angular momentum, and the contribution of the latter to the expansion is also taken into account. The calculations are limited to the special case of Einstein-de Sitter universes (of dust only), in the whole range of HP distributions of angular momenta. If a massM=$ 10^{12} $m⊙ is typical for galaxies, the results are consistent with both an inferred difference roughly in a factor of six times between angular momenta of ellipticals and spirals, and a continuous transition from the former to the latter, for each peak height. It is argued that star formation together with angular momentum, instead of peak height alone, makes the fate of a given proto-object; more specifically, if star formation is high enough and/or angular momentum is low enough, the system will be frozen as an elliptical galaxy; if, on the other hand, the rate of star formation is low enough, and/or angular momentum is high enough, the system will be frozen as a spiral galaxy. In addition, the results lead to an obvious trend: more ellipticals are associated with higher peak heights and more spirals with lower peak heights. Dust Angular Momentum Peak Height High Peak Star Formation Andriani, E. aut Secco, L. aut Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 168(1990), 1 vom: Juni, Seite 131-152 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:168 year:1990 number:1 month:06 pages:131-152 https://doi.org/10.1007/BF00654599 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_24 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4306 GBV_ILN_4700 AR 168 1990 1 06 131-152 |
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10.1007/BF00654599 doi (DE-627)OLC2066180041 (DE-He213)BF00654599-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Caimmi, R. verfasserin aut On the properties of elliptical and spiral galaxies in a CDM scenario 1990 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1990 Abstract This paper aims to investigate what kind of density perturbations did lead to elliptical galaxies and what kind to spiral galaxies, in the context of a CDM scenario. Previous work by HP (Heavens and Peacock, 1988) is reviewed and extended; more particularly: (i) a theoreticalJ∼Mξ relation is derived for virialized configurations, with a slope increasing with the mass, in the range 5/3<ξ<2, and compared with its counterpart deduced by HP for expanding configurations; (ii) an non-dimensional angular momentum Λ=J/(G2M5tff)1/3; withtfffree-fall time at turnaround, is calculated explicitly and compared with the usual spin parameter λ=J(−E)1/2/(GM5/2), in the special case of polytropic spheres and for different peak heights; (iii) a model is built up where the ellipsoidal density perturbations described by HP are approximated as spherical density perturbations with the same mass and the same rate of acquisition of angular momentum, and the contribution of the latter to the expansion is also taken into account. The calculations are limited to the special case of Einstein-de Sitter universes (of dust only), in the whole range of HP distributions of angular momenta. If a massM=$ 10^{12} $m⊙ is typical for galaxies, the results are consistent with both an inferred difference roughly in a factor of six times between angular momenta of ellipticals and spirals, and a continuous transition from the former to the latter, for each peak height. It is argued that star formation together with angular momentum, instead of peak height alone, makes the fate of a given proto-object; more specifically, if star formation is high enough and/or angular momentum is low enough, the system will be frozen as an elliptical galaxy; if, on the other hand, the rate of star formation is low enough, and/or angular momentum is high enough, the system will be frozen as a spiral galaxy. In addition, the results lead to an obvious trend: more ellipticals are associated with higher peak heights and more spirals with lower peak heights. Dust Angular Momentum Peak Height High Peak Star Formation Andriani, E. aut Secco, L. aut Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 168(1990), 1 vom: Juni, Seite 131-152 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:168 year:1990 number:1 month:06 pages:131-152 https://doi.org/10.1007/BF00654599 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_24 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4306 GBV_ILN_4700 AR 168 1990 1 06 131-152 |
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10.1007/BF00654599 doi (DE-627)OLC2066180041 (DE-He213)BF00654599-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Caimmi, R. verfasserin aut On the properties of elliptical and spiral galaxies in a CDM scenario 1990 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1990 Abstract This paper aims to investigate what kind of density perturbations did lead to elliptical galaxies and what kind to spiral galaxies, in the context of a CDM scenario. Previous work by HP (Heavens and Peacock, 1988) is reviewed and extended; more particularly: (i) a theoreticalJ∼Mξ relation is derived for virialized configurations, with a slope increasing with the mass, in the range 5/3<ξ<2, and compared with its counterpart deduced by HP for expanding configurations; (ii) an non-dimensional angular momentum Λ=J/(G2M5tff)1/3; withtfffree-fall time at turnaround, is calculated explicitly and compared with the usual spin parameter λ=J(−E)1/2/(GM5/2), in the special case of polytropic spheres and for different peak heights; (iii) a model is built up where the ellipsoidal density perturbations described by HP are approximated as spherical density perturbations with the same mass and the same rate of acquisition of angular momentum, and the contribution of the latter to the expansion is also taken into account. The calculations are limited to the special case of Einstein-de Sitter universes (of dust only), in the whole range of HP distributions of angular momenta. If a massM=$ 10^{12} $m⊙ is typical for galaxies, the results are consistent with both an inferred difference roughly in a factor of six times between angular momenta of ellipticals and spirals, and a continuous transition from the former to the latter, for each peak height. It is argued that star formation together with angular momentum, instead of peak height alone, makes the fate of a given proto-object; more specifically, if star formation is high enough and/or angular momentum is low enough, the system will be frozen as an elliptical galaxy; if, on the other hand, the rate of star formation is low enough, and/or angular momentum is high enough, the system will be frozen as a spiral galaxy. In addition, the results lead to an obvious trend: more ellipticals are associated with higher peak heights and more spirals with lower peak heights. Dust Angular Momentum Peak Height High Peak Star Formation Andriani, E. aut Secco, L. aut Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 168(1990), 1 vom: Juni, Seite 131-152 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:168 year:1990 number:1 month:06 pages:131-152 https://doi.org/10.1007/BF00654599 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_24 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4306 GBV_ILN_4700 AR 168 1990 1 06 131-152 |
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Enthalten in Astrophysics and space science 168(1990), 1 vom: Juni, Seite 131-152 volume:168 year:1990 number:1 month:06 pages:131-152 |
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on the properties of elliptical and spiral galaxies in a cdm scenario |
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On the properties of elliptical and spiral galaxies in a CDM scenario |
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Abstract This paper aims to investigate what kind of density perturbations did lead to elliptical galaxies and what kind to spiral galaxies, in the context of a CDM scenario. Previous work by HP (Heavens and Peacock, 1988) is reviewed and extended; more particularly: (i) a theoreticalJ∼Mξ relation is derived for virialized configurations, with a slope increasing with the mass, in the range 5/3<ξ<2, and compared with its counterpart deduced by HP for expanding configurations; (ii) an non-dimensional angular momentum Λ=J/(G2M5tff)1/3; withtfffree-fall time at turnaround, is calculated explicitly and compared with the usual spin parameter λ=J(−E)1/2/(GM5/2), in the special case of polytropic spheres and for different peak heights; (iii) a model is built up where the ellipsoidal density perturbations described by HP are approximated as spherical density perturbations with the same mass and the same rate of acquisition of angular momentum, and the contribution of the latter to the expansion is also taken into account. The calculations are limited to the special case of Einstein-de Sitter universes (of dust only), in the whole range of HP distributions of angular momenta. If a massM=$ 10^{12} $m⊙ is typical for galaxies, the results are consistent with both an inferred difference roughly in a factor of six times between angular momenta of ellipticals and spirals, and a continuous transition from the former to the latter, for each peak height. It is argued that star formation together with angular momentum, instead of peak height alone, makes the fate of a given proto-object; more specifically, if star formation is high enough and/or angular momentum is low enough, the system will be frozen as an elliptical galaxy; if, on the other hand, the rate of star formation is low enough, and/or angular momentum is high enough, the system will be frozen as a spiral galaxy. In addition, the results lead to an obvious trend: more ellipticals are associated with higher peak heights and more spirals with lower peak heights. © Kluwer Academic Publishers 1990 |
| abstractGer |
Abstract This paper aims to investigate what kind of density perturbations did lead to elliptical galaxies and what kind to spiral galaxies, in the context of a CDM scenario. Previous work by HP (Heavens and Peacock, 1988) is reviewed and extended; more particularly: (i) a theoreticalJ∼Mξ relation is derived for virialized configurations, with a slope increasing with the mass, in the range 5/3<ξ<2, and compared with its counterpart deduced by HP for expanding configurations; (ii) an non-dimensional angular momentum Λ=J/(G2M5tff)1/3; withtfffree-fall time at turnaround, is calculated explicitly and compared with the usual spin parameter λ=J(−E)1/2/(GM5/2), in the special case of polytropic spheres and for different peak heights; (iii) a model is built up where the ellipsoidal density perturbations described by HP are approximated as spherical density perturbations with the same mass and the same rate of acquisition of angular momentum, and the contribution of the latter to the expansion is also taken into account. The calculations are limited to the special case of Einstein-de Sitter universes (of dust only), in the whole range of HP distributions of angular momenta. If a massM=$ 10^{12} $m⊙ is typical for galaxies, the results are consistent with both an inferred difference roughly in a factor of six times between angular momenta of ellipticals and spirals, and a continuous transition from the former to the latter, for each peak height. It is argued that star formation together with angular momentum, instead of peak height alone, makes the fate of a given proto-object; more specifically, if star formation is high enough and/or angular momentum is low enough, the system will be frozen as an elliptical galaxy; if, on the other hand, the rate of star formation is low enough, and/or angular momentum is high enough, the system will be frozen as a spiral galaxy. In addition, the results lead to an obvious trend: more ellipticals are associated with higher peak heights and more spirals with lower peak heights. © Kluwer Academic Publishers 1990 |
| abstract_unstemmed |
Abstract This paper aims to investigate what kind of density perturbations did lead to elliptical galaxies and what kind to spiral galaxies, in the context of a CDM scenario. Previous work by HP (Heavens and Peacock, 1988) is reviewed and extended; more particularly: (i) a theoreticalJ∼Mξ relation is derived for virialized configurations, with a slope increasing with the mass, in the range 5/3<ξ<2, and compared with its counterpart deduced by HP for expanding configurations; (ii) an non-dimensional angular momentum Λ=J/(G2M5tff)1/3; withtfffree-fall time at turnaround, is calculated explicitly and compared with the usual spin parameter λ=J(−E)1/2/(GM5/2), in the special case of polytropic spheres and for different peak heights; (iii) a model is built up where the ellipsoidal density perturbations described by HP are approximated as spherical density perturbations with the same mass and the same rate of acquisition of angular momentum, and the contribution of the latter to the expansion is also taken into account. The calculations are limited to the special case of Einstein-de Sitter universes (of dust only), in the whole range of HP distributions of angular momenta. If a massM=$ 10^{12} $m⊙ is typical for galaxies, the results are consistent with both an inferred difference roughly in a factor of six times between angular momenta of ellipticals and spirals, and a continuous transition from the former to the latter, for each peak height. It is argued that star formation together with angular momentum, instead of peak height alone, makes the fate of a given proto-object; more specifically, if star formation is high enough and/or angular momentum is low enough, the system will be frozen as an elliptical galaxy; if, on the other hand, the rate of star formation is low enough, and/or angular momentum is high enough, the system will be frozen as a spiral galaxy. In addition, the results lead to an obvious trend: more ellipticals are associated with higher peak heights and more spirals with lower peak heights. © Kluwer Academic Publishers 1990 |
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