Chemical evolution of two-component galaxies

Abstract In order to confirm and refine the results obtained in a previous paper (hereafter referred to as Paper II), the chemical evolution of two-component (spheroid+disk) galaxies is derived rejecting the instantaneous recycling approximation, by means of numerical computations, accouting for (i) the collapse phase of the gas, assumed to be uniform in density and composition, and (ii) a birth-rate stellar function where μ can be related to the usual density term whilex is a volume term first introduced in Paper II; computations are performed relatively to the solar neighbourhood and to model galaxies which closely resemble the real morphological sequence: in both cases, numerical results are compared with analytical ones. As regards the solar neighbourhood, we find the parametersn andq changed to about the value 10–20% with respect to the analytical one, andZ(t) (i.e., metallicity curve) values lowered to about the value≲25% with respect to the analytical one; moreover, spheroid star birth is intermediate between an initial burst and an uniform generation, while more than 90% with respect to the present-day (gas+star) disk is primary. As regards other galaxies, we find that when the disk component is dominant (i.e., in late-type spirals or irregulars) the numerical present-day values of the gas mass-fraction μ(T) and of the metallicityZ(T) differ by a few per cent from the corresponding analytical ones, while the main part of present-day disks is primary; on the contrary, when the spheroid component is dominant, μ(T) andZ(T) are ≈50% different from the corresponding analytical ones, while a substantial fraction of present-day disks is secondary: moreover, super-metallic effect takes place, as a direct consequence of rejecting instantaneous recycling. However, the qualitative conclusions of Paper II continue to hold, so we can state that analytical models constitute a zero-th order approximation in describing the chemical evolution of both solar neighbourhood and other galaxies; numerical models of this paper constitute a first-order approximation, while higher order approximations could be made by rejecting the hypothesis of uniform density and composition, and making use of detailed dynamical models. Ausführliche Beschreibung

Gespeichert in:

Autor*in:	Caimmi, R. [verfasserIn]

Format:	Artikel
Sprache:	Englisch

Erschienen:	1978

Schlagwörter:	Order Approximation Chemical Evolution High Order Approximation Solar Neighbourhood Usual Density

Anmerkung:	© D. Reidel Publishing Company 1978

Übergeordnetes Werk:	Enthalten in: Astrophysics and space science - Kluwer Academic Publishers, 1968, 59(1978), 2 vom: Dez., Seite 413-429
Übergeordnetes Werk:	volume:59 ; year:1978 ; number:2 ; month:12 ; pages:413-429

Links:	Volltext

DOI / URN:	10.1007/BF01023928

Katalog-ID:	OLC2066134422

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650		4	\|a Order Approximation
650		4	\|a Chemical Evolution
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650		4	\|a Solar Neighbourhood
650		4	\|a Usual Density
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allfields	10.1007/BF01023928 doi (DE-627)OLC2066134422 (DE-He213)BF01023928-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Caimmi, R. verfasserin aut Chemical evolution of two-component galaxies 1978 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1978 Abstract In order to confirm and refine the results obtained in a previous paper (hereafter referred to as Paper II), the chemical evolution of two-component (spheroid+disk) galaxies is derived rejecting the instantaneous recycling approximation, by means of numerical computations, accouting for (i) the collapse phase of the gas, assumed to be uniform in density and composition, and (ii) a birth-rate stellar function where μ can be related to the usual density term whilex is a volume term first introduced in Paper II; computations are performed relatively to the solar neighbourhood and to model galaxies which closely resemble the real morphological sequence: in both cases, numerical results are compared with analytical ones. As regards the solar neighbourhood, we find the parametersn andq changed to about the value 10–20% with respect to the analytical one, andZ(t) (i.e., metallicity curve) values lowered to about the value≲25% with respect to the analytical one; moreover, spheroid star birth is intermediate between an initial burst and an uniform generation, while more than 90% with respect to the present-day (gas+star) disk is primary. As regards other galaxies, we find that when the disk component is dominant (i.e., in late-type spirals or irregulars) the numerical present-day values of the gas mass-fraction μ(T) and of the metallicityZ(T) differ by a few per cent from the corresponding analytical ones, while the main part of present-day disks is primary; on the contrary, when the spheroid component is dominant, μ(T) andZ(T) are ≈50% different from the corresponding analytical ones, while a substantial fraction of present-day disks is secondary: moreover, super-metallic effect takes place, as a direct consequence of rejecting instantaneous recycling. However, the qualitative conclusions of Paper II continue to hold, so we can state that analytical models constitute a zero-th order approximation in describing the chemical evolution of both solar neighbourhood and other galaxies; numerical models of this paper constitute a first-order approximation, while higher order approximations could be made by rejecting the hypothesis of uniform density and composition, and making use of detailed dynamical models. Order Approximation Chemical Evolution High Order Approximation Solar Neighbourhood Usual Density Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 59(1978), 2 vom: Dez., Seite 413-429 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:59 year:1978 number:2 month:12 pages:413-429 https://doi.org/10.1007/BF01023928 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OLC-DE-84 SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 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_4035 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4700 AR 59 1978 2 12 413-429
spelling	10.1007/BF01023928 doi (DE-627)OLC2066134422 (DE-He213)BF01023928-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Caimmi, R. verfasserin aut Chemical evolution of two-component galaxies 1978 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1978 Abstract In order to confirm and refine the results obtained in a previous paper (hereafter referred to as Paper II), the chemical evolution of two-component (spheroid+disk) galaxies is derived rejecting the instantaneous recycling approximation, by means of numerical computations, accouting for (i) the collapse phase of the gas, assumed to be uniform in density and composition, and (ii) a birth-rate stellar function where μ can be related to the usual density term whilex is a volume term first introduced in Paper II; computations are performed relatively to the solar neighbourhood and to model galaxies which closely resemble the real morphological sequence: in both cases, numerical results are compared with analytical ones. As regards the solar neighbourhood, we find the parametersn andq changed to about the value 10–20% with respect to the analytical one, andZ(t) (i.e., metallicity curve) values lowered to about the value≲25% with respect to the analytical one; moreover, spheroid star birth is intermediate between an initial burst and an uniform generation, while more than 90% with respect to the present-day (gas+star) disk is primary. As regards other galaxies, we find that when the disk component is dominant (i.e., in late-type spirals or irregulars) the numerical present-day values of the gas mass-fraction μ(T) and of the metallicityZ(T) differ by a few per cent from the corresponding analytical ones, while the main part of present-day disks is primary; on the contrary, when the spheroid component is dominant, μ(T) andZ(T) are ≈50% different from the corresponding analytical ones, while a substantial fraction of present-day disks is secondary: moreover, super-metallic effect takes place, as a direct consequence of rejecting instantaneous recycling. However, the qualitative conclusions of Paper II continue to hold, so we can state that analytical models constitute a zero-th order approximation in describing the chemical evolution of both solar neighbourhood and other galaxies; numerical models of this paper constitute a first-order approximation, while higher order approximations could be made by rejecting the hypothesis of uniform density and composition, and making use of detailed dynamical models. Order Approximation Chemical Evolution High Order Approximation Solar Neighbourhood Usual Density Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 59(1978), 2 vom: Dez., Seite 413-429 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:59 year:1978 number:2 month:12 pages:413-429 https://doi.org/10.1007/BF01023928 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OLC-DE-84 SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 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_4035 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4700 AR 59 1978 2 12 413-429
allfields_unstemmed	10.1007/BF01023928 doi (DE-627)OLC2066134422 (DE-He213)BF01023928-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Caimmi, R. verfasserin aut Chemical evolution of two-component galaxies 1978 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1978 Abstract In order to confirm and refine the results obtained in a previous paper (hereafter referred to as Paper II), the chemical evolution of two-component (spheroid+disk) galaxies is derived rejecting the instantaneous recycling approximation, by means of numerical computations, accouting for (i) the collapse phase of the gas, assumed to be uniform in density and composition, and (ii) a birth-rate stellar function where μ can be related to the usual density term whilex is a volume term first introduced in Paper II; computations are performed relatively to the solar neighbourhood and to model galaxies which closely resemble the real morphological sequence: in both cases, numerical results are compared with analytical ones. As regards the solar neighbourhood, we find the parametersn andq changed to about the value 10–20% with respect to the analytical one, andZ(t) (i.e., metallicity curve) values lowered to about the value≲25% with respect to the analytical one; moreover, spheroid star birth is intermediate between an initial burst and an uniform generation, while more than 90% with respect to the present-day (gas+star) disk is primary. As regards other galaxies, we find that when the disk component is dominant (i.e., in late-type spirals or irregulars) the numerical present-day values of the gas mass-fraction μ(T) and of the metallicityZ(T) differ by a few per cent from the corresponding analytical ones, while the main part of present-day disks is primary; on the contrary, when the spheroid component is dominant, μ(T) andZ(T) are ≈50% different from the corresponding analytical ones, while a substantial fraction of present-day disks is secondary: moreover, super-metallic effect takes place, as a direct consequence of rejecting instantaneous recycling. However, the qualitative conclusions of Paper II continue to hold, so we can state that analytical models constitute a zero-th order approximation in describing the chemical evolution of both solar neighbourhood and other galaxies; numerical models of this paper constitute a first-order approximation, while higher order approximations could be made by rejecting the hypothesis of uniform density and composition, and making use of detailed dynamical models. Order Approximation Chemical Evolution High Order Approximation Solar Neighbourhood Usual Density Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 59(1978), 2 vom: Dez., Seite 413-429 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:59 year:1978 number:2 month:12 pages:413-429 https://doi.org/10.1007/BF01023928 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OLC-DE-84 SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 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_4035 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4700 AR 59 1978 2 12 413-429
allfieldsGer	10.1007/BF01023928 doi (DE-627)OLC2066134422 (DE-He213)BF01023928-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Caimmi, R. verfasserin aut Chemical evolution of two-component galaxies 1978 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1978 Abstract In order to confirm and refine the results obtained in a previous paper (hereafter referred to as Paper II), the chemical evolution of two-component (spheroid+disk) galaxies is derived rejecting the instantaneous recycling approximation, by means of numerical computations, accouting for (i) the collapse phase of the gas, assumed to be uniform in density and composition, and (ii) a birth-rate stellar function where μ can be related to the usual density term whilex is a volume term first introduced in Paper II; computations are performed relatively to the solar neighbourhood and to model galaxies which closely resemble the real morphological sequence: in both cases, numerical results are compared with analytical ones. As regards the solar neighbourhood, we find the parametersn andq changed to about the value 10–20% with respect to the analytical one, andZ(t) (i.e., metallicity curve) values lowered to about the value≲25% with respect to the analytical one; moreover, spheroid star birth is intermediate between an initial burst and an uniform generation, while more than 90% with respect to the present-day (gas+star) disk is primary. As regards other galaxies, we find that when the disk component is dominant (i.e., in late-type spirals or irregulars) the numerical present-day values of the gas mass-fraction μ(T) and of the metallicityZ(T) differ by a few per cent from the corresponding analytical ones, while the main part of present-day disks is primary; on the contrary, when the spheroid component is dominant, μ(T) andZ(T) are ≈50% different from the corresponding analytical ones, while a substantial fraction of present-day disks is secondary: moreover, super-metallic effect takes place, as a direct consequence of rejecting instantaneous recycling. However, the qualitative conclusions of Paper II continue to hold, so we can state that analytical models constitute a zero-th order approximation in describing the chemical evolution of both solar neighbourhood and other galaxies; numerical models of this paper constitute a first-order approximation, while higher order approximations could be made by rejecting the hypothesis of uniform density and composition, and making use of detailed dynamical models. Order Approximation Chemical Evolution High Order Approximation Solar Neighbourhood Usual Density Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 59(1978), 2 vom: Dez., Seite 413-429 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:59 year:1978 number:2 month:12 pages:413-429 https://doi.org/10.1007/BF01023928 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OLC-DE-84 SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 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_4035 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4700 AR 59 1978 2 12 413-429
allfieldsSound	10.1007/BF01023928 doi (DE-627)OLC2066134422 (DE-He213)BF01023928-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Caimmi, R. verfasserin aut Chemical evolution of two-component galaxies 1978 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1978 Abstract In order to confirm and refine the results obtained in a previous paper (hereafter referred to as Paper II), the chemical evolution of two-component (spheroid+disk) galaxies is derived rejecting the instantaneous recycling approximation, by means of numerical computations, accouting for (i) the collapse phase of the gas, assumed to be uniform in density and composition, and (ii) a birth-rate stellar function where μ can be related to the usual density term whilex is a volume term first introduced in Paper II; computations are performed relatively to the solar neighbourhood and to model galaxies which closely resemble the real morphological sequence: in both cases, numerical results are compared with analytical ones. As regards the solar neighbourhood, we find the parametersn andq changed to about the value 10–20% with respect to the analytical one, andZ(t) (i.e., metallicity curve) values lowered to about the value≲25% with respect to the analytical one; moreover, spheroid star birth is intermediate between an initial burst and an uniform generation, while more than 90% with respect to the present-day (gas+star) disk is primary. As regards other galaxies, we find that when the disk component is dominant (i.e., in late-type spirals or irregulars) the numerical present-day values of the gas mass-fraction μ(T) and of the metallicityZ(T) differ by a few per cent from the corresponding analytical ones, while the main part of present-day disks is primary; on the contrary, when the spheroid component is dominant, μ(T) andZ(T) are ≈50% different from the corresponding analytical ones, while a substantial fraction of present-day disks is secondary: moreover, super-metallic effect takes place, as a direct consequence of rejecting instantaneous recycling. However, the qualitative conclusions of Paper II continue to hold, so we can state that analytical models constitute a zero-th order approximation in describing the chemical evolution of both solar neighbourhood and other galaxies; numerical models of this paper constitute a first-order approximation, while higher order approximations could be made by rejecting the hypothesis of uniform density and composition, and making use of detailed dynamical models. Order Approximation Chemical Evolution High Order Approximation Solar Neighbourhood Usual Density Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 59(1978), 2 vom: Dez., Seite 413-429 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:59 year:1978 number:2 month:12 pages:413-429 https://doi.org/10.1007/BF01023928 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OLC-DE-84 SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 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_4035 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4700 AR 59 1978 2 12 413-429
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source	Enthalten in Astrophysics and space science 59(1978), 2 vom: Dez., Seite 413-429 volume:59 year:1978 number:2 month:12 pages:413-429
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Reidel Publishing Company 1978</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract In order to confirm and refine the results obtained in a previous paper (hereafter referred to as Paper II), the chemical evolution of two-component (spheroid+disk) galaxies is derived rejecting the instantaneous recycling approximation, by means of numerical computations, accouting for (i) the collapse phase of the gas, assumed to be uniform in density and composition, and (ii) a birth-rate stellar function where μ can be related to the usual density term whilex is a volume term first introduced in Paper II; computations are performed relatively to the solar neighbourhood and to model galaxies which closely resemble the real morphological sequence: in both cases, numerical results are compared with analytical ones. 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author	Caimmi, R.
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topic_title	520 530 620 VZ 16,12 ssgn Chemical evolution of two-component galaxies Order Approximation Chemical Evolution High Order Approximation Solar Neighbourhood Usual Density
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title	Chemical evolution of two-component galaxies
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title_full	Chemical evolution of two-component galaxies
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title_sort	chemical evolution of two-component galaxies
title_auth	Chemical evolution of two-component galaxies
abstract	Abstract In order to confirm and refine the results obtained in a previous paper (hereafter referred to as Paper II), the chemical evolution of two-component (spheroid+disk) galaxies is derived rejecting the instantaneous recycling approximation, by means of numerical computations, accouting for (i) the collapse phase of the gas, assumed to be uniform in density and composition, and (ii) a birth-rate stellar function where μ can be related to the usual density term whilex is a volume term first introduced in Paper II; computations are performed relatively to the solar neighbourhood and to model galaxies which closely resemble the real morphological sequence: in both cases, numerical results are compared with analytical ones. As regards the solar neighbourhood, we find the parametersn andq changed to about the value 10–20% with respect to the analytical one, andZ(t) (i.e., metallicity curve) values lowered to about the value≲25% with respect to the analytical one; moreover, spheroid star birth is intermediate between an initial burst and an uniform generation, while more than 90% with respect to the present-day (gas+star) disk is primary. As regards other galaxies, we find that when the disk component is dominant (i.e., in late-type spirals or irregulars) the numerical present-day values of the gas mass-fraction μ(T) and of the metallicityZ(T) differ by a few per cent from the corresponding analytical ones, while the main part of present-day disks is primary; on the contrary, when the spheroid component is dominant, μ(T) andZ(T) are ≈50% different from the corresponding analytical ones, while a substantial fraction of present-day disks is secondary: moreover, super-metallic effect takes place, as a direct consequence of rejecting instantaneous recycling. However, the qualitative conclusions of Paper II continue to hold, so we can state that analytical models constitute a zero-th order approximation in describing the chemical evolution of both solar neighbourhood and other galaxies; numerical models of this paper constitute a first-order approximation, while higher order approximations could be made by rejecting the hypothesis of uniform density and composition, and making use of detailed dynamical models. © D. Reidel Publishing Company 1978
abstractGer	Abstract In order to confirm and refine the results obtained in a previous paper (hereafter referred to as Paper II), the chemical evolution of two-component (spheroid+disk) galaxies is derived rejecting the instantaneous recycling approximation, by means of numerical computations, accouting for (i) the collapse phase of the gas, assumed to be uniform in density and composition, and (ii) a birth-rate stellar function where μ can be related to the usual density term whilex is a volume term first introduced in Paper II; computations are performed relatively to the solar neighbourhood and to model galaxies which closely resemble the real morphological sequence: in both cases, numerical results are compared with analytical ones. As regards the solar neighbourhood, we find the parametersn andq changed to about the value 10–20% with respect to the analytical one, andZ(t) (i.e., metallicity curve) values lowered to about the value≲25% with respect to the analytical one; moreover, spheroid star birth is intermediate between an initial burst and an uniform generation, while more than 90% with respect to the present-day (gas+star) disk is primary. As regards other galaxies, we find that when the disk component is dominant (i.e., in late-type spirals or irregulars) the numerical present-day values of the gas mass-fraction μ(T) and of the metallicityZ(T) differ by a few per cent from the corresponding analytical ones, while the main part of present-day disks is primary; on the contrary, when the spheroid component is dominant, μ(T) andZ(T) are ≈50% different from the corresponding analytical ones, while a substantial fraction of present-day disks is secondary: moreover, super-metallic effect takes place, as a direct consequence of rejecting instantaneous recycling. However, the qualitative conclusions of Paper II continue to hold, so we can state that analytical models constitute a zero-th order approximation in describing the chemical evolution of both solar neighbourhood and other galaxies; numerical models of this paper constitute a first-order approximation, while higher order approximations could be made by rejecting the hypothesis of uniform density and composition, and making use of detailed dynamical models. © D. Reidel Publishing Company 1978
abstract_unstemmed	Abstract In order to confirm and refine the results obtained in a previous paper (hereafter referred to as Paper II), the chemical evolution of two-component (spheroid+disk) galaxies is derived rejecting the instantaneous recycling approximation, by means of numerical computations, accouting for (i) the collapse phase of the gas, assumed to be uniform in density and composition, and (ii) a birth-rate stellar function where μ can be related to the usual density term whilex is a volume term first introduced in Paper II; computations are performed relatively to the solar neighbourhood and to model galaxies which closely resemble the real morphological sequence: in both cases, numerical results are compared with analytical ones. As regards the solar neighbourhood, we find the parametersn andq changed to about the value 10–20% with respect to the analytical one, andZ(t) (i.e., metallicity curve) values lowered to about the value≲25% with respect to the analytical one; moreover, spheroid star birth is intermediate between an initial burst and an uniform generation, while more than 90% with respect to the present-day (gas+star) disk is primary. As regards other galaxies, we find that when the disk component is dominant (i.e., in late-type spirals or irregulars) the numerical present-day values of the gas mass-fraction μ(T) and of the metallicityZ(T) differ by a few per cent from the corresponding analytical ones, while the main part of present-day disks is primary; on the contrary, when the spheroid component is dominant, μ(T) andZ(T) are ≈50% different from the corresponding analytical ones, while a substantial fraction of present-day disks is secondary: moreover, super-metallic effect takes place, as a direct consequence of rejecting instantaneous recycling. However, the qualitative conclusions of Paper II continue to hold, so we can state that analytical models constitute a zero-th order approximation in describing the chemical evolution of both solar neighbourhood and other galaxies; numerical models of this paper constitute a first-order approximation, while higher order approximations could be made by rejecting the hypothesis of uniform density and composition, and making use of detailed dynamical models. © D. Reidel Publishing Company 1978
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