A Principle of Corresponding States for Two-Component, Self-Gravitating Fluids

Macrogases are defined as two-component,large-scale celestial objects where the subsystems interact only via gravitation.The macrogas equation of state is formulated and compared to the van der Waals (VDW)equation of state for ordinary gases.By analogy, it is assumed that real macroisothermal curves in macrogases occur as real isothermal curves in ordinary gases, where a phase transition(vapour-liquid observed in ordinary gases and gas-stars assumed in macrogases) takesplace along a horizontal linein the macrovolume-macropressure{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane.The intersections between real and theoretical(deduced from the equation of state) macro isothermalcurves, make two regions of equal surface as for ordinary gases obeying the VDW equation of state.A numerical algorithm is developed for determining the following points of a selected theoretical macroisothermal curve on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane:the three intersections with the related real macroisothermal curve,and the two extremum points (one maximum and one minimum). Different kinds of macrogases are studied in detail: UU, where U density profiles are flat, to be conceived as a simple guidance case; HH, where H density profiles obey the Hernquist (1990) law, which satisfactorily fits the observed spheroidal components of galaxies; HN/NH, where N density profiles obey the Navarro-Frenk-White (1995,1996, 1997) law, which satisfactorily fits the simulated nonbaryonic dark matter haloes.A different trend is shown by theoretical macroisothermal curves on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane,according to whether density profiles are sufficiently mild (UU) or sufficiently steep (HH, HN/NH).In the former alternative, no critical macroisothermal curve exists, below or above which the trend is monotonous. In the latter alternative, a critical macroisothermal curve exists, as shown by VDW gases, where the critical point may be defined as the horizontal inflexion point. In any case, by analogy with VDW gases, the first quadrant of the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane may be divided into three parts: (i) The G region, where only gas exists; (ii) The S region,where only stars exist; (iii) The GS region,where both gas and stars, exist. With regard to HH and HN/NH macrogases, an application is made to a subsample ({small $N=16$}) of elliptical galaxies extracted from larger samples {small $(N=25,~N=48)$}of early type galaxies investigated within the SAURON project (Cappellari et al. 2006, 2007).Under the simplifying assumption of universal mass ratio of the two subsystems, {small $m$}, different models characterized by different scaled truncation radii, i.e. concentrations, {small $Xi_i$},{small $Xi_j$}, are considered and the related position of sample objects on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane is determined. Macrogases fitting to elliptical galaxies are expected to lie within the S region or slightly outside the boundary between the S and the GS region at most. Accordingly,models where sample objects lie outside the S region and far from its boundary, or cannot be positioned on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, are rejected. For each macrogas, twenty models are considered for different values of {small $(Xi_i,Xi_j, m)$}, namely {small $Xi_i, Xi_j=5,~ 10,~ 20,~+infty$} {small $(Xi_i, Xi_j,$} both either finite or infinite), and {small $m=10,~ 20$}. Acceptable models are {small $(10,~10,~20)$}, {small $(10,~20,~20)$},{small $(20,~10,~20)$}, {small $(20,~20,~20)$}, for HH macrogases,and {small $(10,~5,~10)$}, {small $(10,~10,~20)$}, {small $(20,~10,~20)$},for HN/NH macrogases. Tipically, fast rotators are found to lie within the S region, while slow rotators are close (from both sides) to the boundary between the S and the GS region. The net effect of the uncertainty affecting observed quantities, on the position of sample objects on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, is also investigated. Finally, a principle of corresponding states is formulated for macrogases with assigned density profiles and scaled truncation radii. Ausführliche Beschreibung

Gespeichert in:

Autor*in:	Caimmi, R. [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2010

Schlagwörter:	Galaxies: evolution Galaxies: halos Dark matter

Übergeordnetes Werk:	In: Serbian Astronomical Journal - Astronomical Observatory, Department of Astronomy, Belgrade, 2008, 180(2010), Seite 19-55
Übergeordnetes Werk:	volume:180 ; year:2010 ; pages:19-55

Links:	Link aufrufen Link aufrufen Journal toc

Katalog-ID:	DOAJ066069602

Internformat


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245	1	2	\|a A Principle of Corresponding States for Two-Component, Self-Gravitating Fluids
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520			\|a Macrogases are defined as two-component,large-scale celestial objects where the subsystems interact only via gravitation.The macrogas equation of state is formulated and compared to the van der Waals (VDW)equation of state for ordinary gases.By analogy, it is assumed that real macroisothermal curves in macrogases occur as real isothermal curves in ordinary gases, where a phase transition(vapour-liquid observed in ordinary gases and gas-stars assumed in macrogases) takesplace along a horizontal linein the macrovolume-macropressure{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane.The intersections between real and theoretical(deduced from the equation of state) macro isothermalcurves, make two regions of equal surface as for ordinary gases obeying the VDW equation of state.A numerical algorithm is developed for determining the following points of a selected theoretical macroisothermal curve on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane:the three intersections with the related real macroisothermal curve,and the two extremum points (one maximum and one minimum). Different kinds of macrogases are studied in detail: UU, where U density profiles are flat, to be conceived as a simple guidance case; HH, where H density profiles obey the Hernquist (1990) law, which satisfactorily fits the observed spheroidal components of galaxies; HN/NH, where N density profiles obey the Navarro-Frenk-White (1995,1996, 1997) law, which satisfactorily fits the simulated nonbaryonic dark matter haloes.A different trend is shown by theoretical macroisothermal curves on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane,according to whether density profiles are sufficiently mild (UU) or sufficiently steep (HH, HN/NH).In the former alternative, no critical macroisothermal curve exists, below or above which the trend is monotonous. In the latter alternative, a critical macroisothermal curve exists, as shown by VDW gases, where the critical point may be defined as the horizontal inflexion point. In any case, by analogy with VDW gases, the first quadrant of the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane may be divided into three parts: (i) The G region, where only gas exists; (ii) The S region,where only stars exist; (iii) The GS region,where both gas and stars, exist. With regard to HH and HN/NH macrogases, an application is made to a subsample ({small $N=16$}) of elliptical galaxies extracted from larger samples {small $(N=25,~N=48)$}of early type galaxies investigated within the SAURON project (Cappellari et al. 2006, 2007).Under the simplifying assumption of universal mass ratio of the two subsystems, {small $m$}, different models characterized by different scaled truncation radii, i.e. concentrations, {small $Xi_i$},{small $Xi_j$}, are considered and the related position of sample objects on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane is determined. Macrogases fitting to elliptical galaxies are expected to lie within the S region or slightly outside the boundary between the S and the GS region at most. Accordingly,models where sample objects lie outside the S region and far from its boundary, or cannot be positioned on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, are rejected. For each macrogas, twenty models are considered for different values of {small $(Xi_i,Xi_j, m)$}, namely {small $Xi_i, Xi_j=5,~ 10,~ 20,~+infty$} {small $(Xi_i, Xi_j,$} both either finite or infinite), and {small $m=10,~ 20$}. Acceptable models are {small $(10,~10,~20)$}, {small $(10,~20,~20)$},{small $(20,~10,~20)$}, {small $(20,~20,~20)$}, for HH macrogases,and {small $(10,~5,~10)$}, {small $(10,~10,~20)$}, {small $(20,~10,~20)$},for HN/NH macrogases. Tipically, fast rotators are found to lie within the S region, while slow rotators are close (from both sides) to the boundary between the S and the GS region. The net effect of the uncertainty affecting observed quantities, on the position of sample objects on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, is also investigated. Finally, a principle of corresponding states is formulated for macrogases with assigned density profiles and scaled truncation radii.
650		4	\|a Galaxies: evolution
650		4	\|a Galaxies: halos
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773	0	8	\|i In \|t Serbian Astronomical Journal \|d Astronomical Observatory, Department of Astronomy, Belgrade, 2008 \|g 180(2010), Seite 19-55 \|w (DE-627)538218460 \|w (DE-600)2378699-1 \|x 18209289 \|7 nnns
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allfields	(DE-627)DOAJ066069602 (DE-599)DOAJ194aa060541b427f9f45ee6a964314a0 DE-627 ger DE-627 rakwb eng QB1-991 Caimmi, R. verfasserin aut A Principle of Corresponding States for Two-Component, Self-Gravitating Fluids 2010 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Macrogases are defined as two-component,large-scale celestial objects where the subsystems interact only via gravitation.The macrogas equation of state is formulated and compared to the van der Waals (VDW)equation of state for ordinary gases.By analogy, it is assumed that real macroisothermal curves in macrogases occur as real isothermal curves in ordinary gases, where a phase transition(vapour-liquid observed in ordinary gases and gas-stars assumed in macrogases) takesplace along a horizontal linein the macrovolume-macropressure{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane.The intersections between real and theoretical(deduced from the equation of state) macro isothermalcurves, make two regions of equal surface as for ordinary gases obeying the VDW equation of state.A numerical algorithm is developed for determining the following points of a selected theoretical macroisothermal curve on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane:the three intersections with the related real macroisothermal curve,and the two extremum points (one maximum and one minimum). Different kinds of macrogases are studied in detail: UU, where U density profiles are flat, to be conceived as a simple guidance case; HH, where H density profiles obey the Hernquist (1990) law, which satisfactorily fits the observed spheroidal components of galaxies; HN/NH, where N density profiles obey the Navarro-Frenk-White (1995,1996, 1997) law, which satisfactorily fits the simulated nonbaryonic dark matter haloes.A different trend is shown by theoretical macroisothermal curves on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane,according to whether density profiles are sufficiently mild (UU) or sufficiently steep (HH, HN/NH).In the former alternative, no critical macroisothermal curve exists, below or above which the trend is monotonous. In the latter alternative, a critical macroisothermal curve exists, as shown by VDW gases, where the critical point may be defined as the horizontal inflexion point. In any case, by analogy with VDW gases, the first quadrant of the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane may be divided into three parts: (i) The G region, where only gas exists; (ii) The S region,where only stars exist; (iii) The GS region,where both gas and stars, exist. With regard to HH and HN/NH macrogases, an application is made to a subsample ({small $N=16$}) of elliptical galaxies extracted from larger samples {small $(N=25,~N=48)$}of early type galaxies investigated within the SAURON project (Cappellari et al. 2006, 2007).Under the simplifying assumption of universal mass ratio of the two subsystems, {small $m$}, different models characterized by different scaled truncation radii, i.e. concentrations, {small $Xi_i$},{small $Xi_j$}, are considered and the related position of sample objects on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane is determined. Macrogases fitting to elliptical galaxies are expected to lie within the S region or slightly outside the boundary between the S and the GS region at most. Accordingly,models where sample objects lie outside the S region and far from its boundary, or cannot be positioned on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, are rejected. For each macrogas, twenty models are considered for different values of {small $(Xi_i,Xi_j, m)$}, namely {small $Xi_i, Xi_j=5,~ 10,~ 20,~+infty$} {small $(Xi_i, Xi_j,$} both either finite or infinite), and {small $m=10,~ 20$}. Acceptable models are {small $(10,~10,~20)$}, {small $(10,~20,~20)$},{small $(20,~10,~20)$}, {small $(20,~20,~20)$}, for HH macrogases,and {small $(10,~5,~10)$}, {small $(10,~10,~20)$}, {small $(20,~10,~20)$},for HN/NH macrogases. Tipically, fast rotators are found to lie within the S region, while slow rotators are close (from both sides) to the boundary between the S and the GS region. The net effect of the uncertainty affecting observed quantities, on the position of sample objects on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, is also investigated. Finally, a principle of corresponding states is formulated for macrogases with assigned density profiles and scaled truncation radii. Galaxies: evolution Galaxies: halos Dark matter Astronomy In Serbian Astronomical Journal Astronomical Observatory, Department of Astronomy, Belgrade, 2008 180(2010), Seite 19-55 (DE-627)538218460 (DE-600)2378699-1 18209289 nnns volume:180 year:2010 pages:19-55 https://doaj.org/article/194aa060541b427f9f45ee6a964314a0 kostenfrei http://saj.matf.bg.ac.rs/180/pdf/019-055.pdf kostenfrei https://doaj.org/toc/1450-698X Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 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_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 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_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 180 2010 19-55
spelling	(DE-627)DOAJ066069602 (DE-599)DOAJ194aa060541b427f9f45ee6a964314a0 DE-627 ger DE-627 rakwb eng QB1-991 Caimmi, R. verfasserin aut A Principle of Corresponding States for Two-Component, Self-Gravitating Fluids 2010 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Macrogases are defined as two-component,large-scale celestial objects where the subsystems interact only via gravitation.The macrogas equation of state is formulated and compared to the van der Waals (VDW)equation of state for ordinary gases.By analogy, it is assumed that real macroisothermal curves in macrogases occur as real isothermal curves in ordinary gases, where a phase transition(vapour-liquid observed in ordinary gases and gas-stars assumed in macrogases) takesplace along a horizontal linein the macrovolume-macropressure{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane.The intersections between real and theoretical(deduced from the equation of state) macro isothermalcurves, make two regions of equal surface as for ordinary gases obeying the VDW equation of state.A numerical algorithm is developed for determining the following points of a selected theoretical macroisothermal curve on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane:the three intersections with the related real macroisothermal curve,and the two extremum points (one maximum and one minimum). Different kinds of macrogases are studied in detail: UU, where U density profiles are flat, to be conceived as a simple guidance case; HH, where H density profiles obey the Hernquist (1990) law, which satisfactorily fits the observed spheroidal components of galaxies; HN/NH, where N density profiles obey the Navarro-Frenk-White (1995,1996, 1997) law, which satisfactorily fits the simulated nonbaryonic dark matter haloes.A different trend is shown by theoretical macroisothermal curves on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane,according to whether density profiles are sufficiently mild (UU) or sufficiently steep (HH, HN/NH).In the former alternative, no critical macroisothermal curve exists, below or above which the trend is monotonous. In the latter alternative, a critical macroisothermal curve exists, as shown by VDW gases, where the critical point may be defined as the horizontal inflexion point. In any case, by analogy with VDW gases, the first quadrant of the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane may be divided into three parts: (i) The G region, where only gas exists; (ii) The S region,where only stars exist; (iii) The GS region,where both gas and stars, exist. With regard to HH and HN/NH macrogases, an application is made to a subsample ({small $N=16$}) of elliptical galaxies extracted from larger samples {small $(N=25,~N=48)$}of early type galaxies investigated within the SAURON project (Cappellari et al. 2006, 2007).Under the simplifying assumption of universal mass ratio of the two subsystems, {small $m$}, different models characterized by different scaled truncation radii, i.e. concentrations, {small $Xi_i$},{small $Xi_j$}, are considered and the related position of sample objects on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane is determined. Macrogases fitting to elliptical galaxies are expected to lie within the S region or slightly outside the boundary between the S and the GS region at most. Accordingly,models where sample objects lie outside the S region and far from its boundary, or cannot be positioned on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, are rejected. For each macrogas, twenty models are considered for different values of {small $(Xi_i,Xi_j, m)$}, namely {small $Xi_i, Xi_j=5,~ 10,~ 20,~+infty$} {small $(Xi_i, Xi_j,$} both either finite or infinite), and {small $m=10,~ 20$}. Acceptable models are {small $(10,~10,~20)$}, {small $(10,~20,~20)$},{small $(20,~10,~20)$}, {small $(20,~20,~20)$}, for HH macrogases,and {small $(10,~5,~10)$}, {small $(10,~10,~20)$}, {small $(20,~10,~20)$},for HN/NH macrogases. Tipically, fast rotators are found to lie within the S region, while slow rotators are close (from both sides) to the boundary between the S and the GS region. The net effect of the uncertainty affecting observed quantities, on the position of sample objects on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, is also investigated. Finally, a principle of corresponding states is formulated for macrogases with assigned density profiles and scaled truncation radii. Galaxies: evolution Galaxies: halos Dark matter Astronomy In Serbian Astronomical Journal Astronomical Observatory, Department of Astronomy, Belgrade, 2008 180(2010), Seite 19-55 (DE-627)538218460 (DE-600)2378699-1 18209289 nnns volume:180 year:2010 pages:19-55 https://doaj.org/article/194aa060541b427f9f45ee6a964314a0 kostenfrei http://saj.matf.bg.ac.rs/180/pdf/019-055.pdf kostenfrei https://doaj.org/toc/1450-698X Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 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_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 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_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 180 2010 19-55
allfields_unstemmed	(DE-627)DOAJ066069602 (DE-599)DOAJ194aa060541b427f9f45ee6a964314a0 DE-627 ger DE-627 rakwb eng QB1-991 Caimmi, R. verfasserin aut A Principle of Corresponding States for Two-Component, Self-Gravitating Fluids 2010 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Macrogases are defined as two-component,large-scale celestial objects where the subsystems interact only via gravitation.The macrogas equation of state is formulated and compared to the van der Waals (VDW)equation of state for ordinary gases.By analogy, it is assumed that real macroisothermal curves in macrogases occur as real isothermal curves in ordinary gases, where a phase transition(vapour-liquid observed in ordinary gases and gas-stars assumed in macrogases) takesplace along a horizontal linein the macrovolume-macropressure{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane.The intersections between real and theoretical(deduced from the equation of state) macro isothermalcurves, make two regions of equal surface as for ordinary gases obeying the VDW equation of state.A numerical algorithm is developed for determining the following points of a selected theoretical macroisothermal curve on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane:the three intersections with the related real macroisothermal curve,and the two extremum points (one maximum and one minimum). Different kinds of macrogases are studied in detail: UU, where U density profiles are flat, to be conceived as a simple guidance case; HH, where H density profiles obey the Hernquist (1990) law, which satisfactorily fits the observed spheroidal components of galaxies; HN/NH, where N density profiles obey the Navarro-Frenk-White (1995,1996, 1997) law, which satisfactorily fits the simulated nonbaryonic dark matter haloes.A different trend is shown by theoretical macroisothermal curves on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane,according to whether density profiles are sufficiently mild (UU) or sufficiently steep (HH, HN/NH).In the former alternative, no critical macroisothermal curve exists, below or above which the trend is monotonous. In the latter alternative, a critical macroisothermal curve exists, as shown by VDW gases, where the critical point may be defined as the horizontal inflexion point. In any case, by analogy with VDW gases, the first quadrant of the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane may be divided into three parts: (i) The G region, where only gas exists; (ii) The S region,where only stars exist; (iii) The GS region,where both gas and stars, exist. With regard to HH and HN/NH macrogases, an application is made to a subsample ({small $N=16$}) of elliptical galaxies extracted from larger samples {small $(N=25,~N=48)$}of early type galaxies investigated within the SAURON project (Cappellari et al. 2006, 2007).Under the simplifying assumption of universal mass ratio of the two subsystems, {small $m$}, different models characterized by different scaled truncation radii, i.e. concentrations, {small $Xi_i$},{small $Xi_j$}, are considered and the related position of sample objects on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane is determined. Macrogases fitting to elliptical galaxies are expected to lie within the S region or slightly outside the boundary between the S and the GS region at most. Accordingly,models where sample objects lie outside the S region and far from its boundary, or cannot be positioned on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, are rejected. For each macrogas, twenty models are considered for different values of {small $(Xi_i,Xi_j, m)$}, namely {small $Xi_i, Xi_j=5,~ 10,~ 20,~+infty$} {small $(Xi_i, Xi_j,$} both either finite or infinite), and {small $m=10,~ 20$}. Acceptable models are {small $(10,~10,~20)$}, {small $(10,~20,~20)$},{small $(20,~10,~20)$}, {small $(20,~20,~20)$}, for HH macrogases,and {small $(10,~5,~10)$}, {small $(10,~10,~20)$}, {small $(20,~10,~20)$},for HN/NH macrogases. Tipically, fast rotators are found to lie within the S region, while slow rotators are close (from both sides) to the boundary between the S and the GS region. The net effect of the uncertainty affecting observed quantities, on the position of sample objects on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, is also investigated. Finally, a principle of corresponding states is formulated for macrogases with assigned density profiles and scaled truncation radii. Galaxies: evolution Galaxies: halos Dark matter Astronomy In Serbian Astronomical Journal Astronomical Observatory, Department of Astronomy, Belgrade, 2008 180(2010), Seite 19-55 (DE-627)538218460 (DE-600)2378699-1 18209289 nnns volume:180 year:2010 pages:19-55 https://doaj.org/article/194aa060541b427f9f45ee6a964314a0 kostenfrei http://saj.matf.bg.ac.rs/180/pdf/019-055.pdf kostenfrei https://doaj.org/toc/1450-698X Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 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_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 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_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 180 2010 19-55
allfieldsGer	(DE-627)DOAJ066069602 (DE-599)DOAJ194aa060541b427f9f45ee6a964314a0 DE-627 ger DE-627 rakwb eng QB1-991 Caimmi, R. verfasserin aut A Principle of Corresponding States for Two-Component, Self-Gravitating Fluids 2010 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Macrogases are defined as two-component,large-scale celestial objects where the subsystems interact only via gravitation.The macrogas equation of state is formulated and compared to the van der Waals (VDW)equation of state for ordinary gases.By analogy, it is assumed that real macroisothermal curves in macrogases occur as real isothermal curves in ordinary gases, where a phase transition(vapour-liquid observed in ordinary gases and gas-stars assumed in macrogases) takesplace along a horizontal linein the macrovolume-macropressure{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane.The intersections between real and theoretical(deduced from the equation of state) macro isothermalcurves, make two regions of equal surface as for ordinary gases obeying the VDW equation of state.A numerical algorithm is developed for determining the following points of a selected theoretical macroisothermal curve on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane:the three intersections with the related real macroisothermal curve,and the two extremum points (one maximum and one minimum). Different kinds of macrogases are studied in detail: UU, where U density profiles are flat, to be conceived as a simple guidance case; HH, where H density profiles obey the Hernquist (1990) law, which satisfactorily fits the observed spheroidal components of galaxies; HN/NH, where N density profiles obey the Navarro-Frenk-White (1995,1996, 1997) law, which satisfactorily fits the simulated nonbaryonic dark matter haloes.A different trend is shown by theoretical macroisothermal curves on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane,according to whether density profiles are sufficiently mild (UU) or sufficiently steep (HH, HN/NH).In the former alternative, no critical macroisothermal curve exists, below or above which the trend is monotonous. In the latter alternative, a critical macroisothermal curve exists, as shown by VDW gases, where the critical point may be defined as the horizontal inflexion point. In any case, by analogy with VDW gases, the first quadrant of the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane may be divided into three parts: (i) The G region, where only gas exists; (ii) The S region,where only stars exist; (iii) The GS region,where both gas and stars, exist. With regard to HH and HN/NH macrogases, an application is made to a subsample ({small $N=16$}) of elliptical galaxies extracted from larger samples {small $(N=25,~N=48)$}of early type galaxies investigated within the SAURON project (Cappellari et al. 2006, 2007).Under the simplifying assumption of universal mass ratio of the two subsystems, {small $m$}, different models characterized by different scaled truncation radii, i.e. concentrations, {small $Xi_i$},{small $Xi_j$}, are considered and the related position of sample objects on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane is determined. Macrogases fitting to elliptical galaxies are expected to lie within the S region or slightly outside the boundary between the S and the GS region at most. Accordingly,models where sample objects lie outside the S region and far from its boundary, or cannot be positioned on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, are rejected. For each macrogas, twenty models are considered for different values of {small $(Xi_i,Xi_j, m)$}, namely {small $Xi_i, Xi_j=5,~ 10,~ 20,~+infty$} {small $(Xi_i, Xi_j,$} both either finite or infinite), and {small $m=10,~ 20$}. Acceptable models are {small $(10,~10,~20)$}, {small $(10,~20,~20)$},{small $(20,~10,~20)$}, {small $(20,~20,~20)$}, for HH macrogases,and {small $(10,~5,~10)$}, {small $(10,~10,~20)$}, {small $(20,~10,~20)$},for HN/NH macrogases. Tipically, fast rotators are found to lie within the S region, while slow rotators are close (from both sides) to the boundary between the S and the GS region. The net effect of the uncertainty affecting observed quantities, on the position of sample objects on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, is also investigated. Finally, a principle of corresponding states is formulated for macrogases with assigned density profiles and scaled truncation radii. Galaxies: evolution Galaxies: halos Dark matter Astronomy In Serbian Astronomical Journal Astronomical Observatory, Department of Astronomy, Belgrade, 2008 180(2010), Seite 19-55 (DE-627)538218460 (DE-600)2378699-1 18209289 nnns volume:180 year:2010 pages:19-55 https://doaj.org/article/194aa060541b427f9f45ee6a964314a0 kostenfrei http://saj.matf.bg.ac.rs/180/pdf/019-055.pdf kostenfrei https://doaj.org/toc/1450-698X Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 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_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 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_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 180 2010 19-55
allfieldsSound	(DE-627)DOAJ066069602 (DE-599)DOAJ194aa060541b427f9f45ee6a964314a0 DE-627 ger DE-627 rakwb eng QB1-991 Caimmi, R. verfasserin aut A Principle of Corresponding States for Two-Component, Self-Gravitating Fluids 2010 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Macrogases are defined as two-component,large-scale celestial objects where the subsystems interact only via gravitation.The macrogas equation of state is formulated and compared to the van der Waals (VDW)equation of state for ordinary gases.By analogy, it is assumed that real macroisothermal curves in macrogases occur as real isothermal curves in ordinary gases, where a phase transition(vapour-liquid observed in ordinary gases and gas-stars assumed in macrogases) takesplace along a horizontal linein the macrovolume-macropressure{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane.The intersections between real and theoretical(deduced from the equation of state) macro isothermalcurves, make two regions of equal surface as for ordinary gases obeying the VDW equation of state.A numerical algorithm is developed for determining the following points of a selected theoretical macroisothermal curve on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane:the three intersections with the related real macroisothermal curve,and the two extremum points (one maximum and one minimum). Different kinds of macrogases are studied in detail: UU, where U density profiles are flat, to be conceived as a simple guidance case; HH, where H density profiles obey the Hernquist (1990) law, which satisfactorily fits the observed spheroidal components of galaxies; HN/NH, where N density profiles obey the Navarro-Frenk-White (1995,1996, 1997) law, which satisfactorily fits the simulated nonbaryonic dark matter haloes.A different trend is shown by theoretical macroisothermal curves on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane,according to whether density profiles are sufficiently mild (UU) or sufficiently steep (HH, HN/NH).In the former alternative, no critical macroisothermal curve exists, below or above which the trend is monotonous. In the latter alternative, a critical macroisothermal curve exists, as shown by VDW gases, where the critical point may be defined as the horizontal inflexion point. In any case, by analogy with VDW gases, the first quadrant of the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane may be divided into three parts: (i) The G region, where only gas exists; (ii) The S region,where only stars exist; (iii) The GS region,where both gas and stars, exist. With regard to HH and HN/NH macrogases, an application is made to a subsample ({small $N=16$}) of elliptical galaxies extracted from larger samples {small $(N=25,~N=48)$}of early type galaxies investigated within the SAURON project (Cappellari et al. 2006, 2007).Under the simplifying assumption of universal mass ratio of the two subsystems, {small $m$}, different models characterized by different scaled truncation radii, i.e. concentrations, {small $Xi_i$},{small $Xi_j$}, are considered and the related position of sample objects on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane is determined. Macrogases fitting to elliptical galaxies are expected to lie within the S region or slightly outside the boundary between the S and the GS region at most. Accordingly,models where sample objects lie outside the S region and far from its boundary, or cannot be positioned on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, are rejected. For each macrogas, twenty models are considered for different values of {small $(Xi_i,Xi_j, m)$}, namely {small $Xi_i, Xi_j=5,~ 10,~ 20,~+infty$} {small $(Xi_i, Xi_j,$} both either finite or infinite), and {small $m=10,~ 20$}. Acceptable models are {small $(10,~10,~20)$}, {small $(10,~20,~20)$},{small $(20,~10,~20)$}, {small $(20,~20,~20)$}, for HH macrogases,and {small $(10,~5,~10)$}, {small $(10,~10,~20)$}, {small $(20,~10,~20)$},for HN/NH macrogases. Tipically, fast rotators are found to lie within the S region, while slow rotators are close (from both sides) to the boundary between the S and the GS region. The net effect of the uncertainty affecting observed quantities, on the position of sample objects on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, is also investigated. Finally, a principle of corresponding states is formulated for macrogases with assigned density profiles and scaled truncation radii. Galaxies: evolution Galaxies: halos Dark matter Astronomy In Serbian Astronomical Journal Astronomical Observatory, Department of Astronomy, Belgrade, 2008 180(2010), Seite 19-55 (DE-627)538218460 (DE-600)2378699-1 18209289 nnns volume:180 year:2010 pages:19-55 https://doaj.org/article/194aa060541b427f9f45ee6a964314a0 kostenfrei http://saj.matf.bg.ac.rs/180/pdf/019-055.pdf kostenfrei https://doaj.org/toc/1450-698X Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 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_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 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_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 180 2010 19-55
language	English
source	In Serbian Astronomical Journal 180(2010), Seite 19-55 volume:180 year:2010 pages:19-55
sourceStr	In Serbian Astronomical Journal 180(2010), Seite 19-55 volume:180 year:2010 pages:19-55
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	Galaxies: evolution Galaxies: halos Dark matter Astronomy
isfreeaccess_bool	true
container_title	Serbian Astronomical Journal
authorswithroles_txt_mv	Caimmi, R. @@aut@@
publishDateDaySort_date	2010-01-01T00:00:00Z
hierarchy_top_id	538218460
id	DOAJ066069602
language_de	englisch
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Different kinds of macrogases are studied in detail: UU, where U density profiles are flat, to be conceived as a simple guidance case; HH, where H density profiles obey the Hernquist (1990) law, which satisfactorily fits the observed spheroidal components of galaxies; HN/NH, where N density profiles obey the Navarro-Frenk-White (1995,1996, 1997) law, which satisfactorily fits the simulated nonbaryonic dark matter haloes.A different trend is shown by theoretical macroisothermal curves on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane,according to whether density profiles are sufficiently mild (UU) or sufficiently steep (HH, HN/NH).In the former alternative, no critical macroisothermal curve exists, below or above which the trend is monotonous. In the latter alternative, a critical macroisothermal curve exists, as shown by VDW gases, where the critical point may be defined as the horizontal inflexion point. In any case, by analogy with VDW gases, the first quadrant of the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane may be divided into three parts: (i) The G region, where only gas exists; (ii) The S region,where only stars exist; (iii) The GS region,where both gas and stars, exist. With regard to HH and HN/NH macrogases, an application is made to a subsample ({small $N=16$}) of elliptical galaxies extracted from larger samples {small $(N=25,~N=48)$}of early type galaxies investigated within the SAURON project (Cappellari et al. 2006, 2007).Under the simplifying assumption of universal mass ratio of the two subsystems, {small $m$}, different models characterized by different scaled truncation radii, i.e. concentrations, {small $Xi_i$},{small $Xi_j$}, are considered and the related position of sample objects on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane is determined. Macrogases fitting to elliptical galaxies are expected to lie within the S region or slightly outside the boundary between the S and the GS region at most. Accordingly,models where sample objects lie outside the S region and far from its boundary, or cannot be positioned on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, are rejected. For each macrogas, twenty models are considered for different values of {small $(Xi_i,Xi_j, m)$}, namely {small $Xi_i, Xi_j=5,~ 10,~ 20,~+infty$} {small $(Xi_i, Xi_j,$} both either finite or infinite), and {small $m=10,~ 20$}. Acceptable models are {small $(10,~10,~20)$}, {small $(10,~20,~20)$},{small $(20,~10,~20)$}, {small $(20,~20,~20)$}, for HH macrogases,and {small $(10,~5,~10)$}, {small $(10,~10,~20)$}, {small $(20,~10,~20)$},for HN/NH macrogases. Tipically, fast rotators are found to lie within the S region, while slow rotators are close (from both sides) to the boundary between the S and the GS region. The net effect of the uncertainty affecting observed quantities, on the position of sample objects on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, is also investigated. 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callnumber-first	Q - Science
author	Caimmi, R.
spellingShingle	Caimmi, R. misc QB1-991 misc Galaxies: evolution misc Galaxies: halos misc Dark matter misc Astronomy A Principle of Corresponding States for Two-Component, Self-Gravitating Fluids
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topic_title	QB1-991 A Principle of Corresponding States for Two-Component, Self-Gravitating Fluids Galaxies: evolution Galaxies: halos Dark matter
topic	misc QB1-991 misc Galaxies: evolution misc Galaxies: halos misc Dark matter misc Astronomy
topic_unstemmed	misc QB1-991 misc Galaxies: evolution misc Galaxies: halos misc Dark matter misc Astronomy
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title	A Principle of Corresponding States for Two-Component, Self-Gravitating Fluids
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title_full	A Principle of Corresponding States for Two-Component, Self-Gravitating Fluids
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title_sort	principle of corresponding states for two-component, self-gravitating fluids
callnumber	QB1-991
title_auth	A Principle of Corresponding States for Two-Component, Self-Gravitating Fluids
abstract	Macrogases are defined as two-component,large-scale celestial objects where the subsystems interact only via gravitation.The macrogas equation of state is formulated and compared to the van der Waals (VDW)equation of state for ordinary gases.By analogy, it is assumed that real macroisothermal curves in macrogases occur as real isothermal curves in ordinary gases, where a phase transition(vapour-liquid observed in ordinary gases and gas-stars assumed in macrogases) takesplace along a horizontal linein the macrovolume-macropressure{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane.The intersections between real and theoretical(deduced from the equation of state) macro isothermalcurves, make two regions of equal surface as for ordinary gases obeying the VDW equation of state.A numerical algorithm is developed for determining the following points of a selected theoretical macroisothermal curve on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane:the three intersections with the related real macroisothermal curve,and the two extremum points (one maximum and one minimum). Different kinds of macrogases are studied in detail: UU, where U density profiles are flat, to be conceived as a simple guidance case; HH, where H density profiles obey the Hernquist (1990) law, which satisfactorily fits the observed spheroidal components of galaxies; HN/NH, where N density profiles obey the Navarro-Frenk-White (1995,1996, 1997) law, which satisfactorily fits the simulated nonbaryonic dark matter haloes.A different trend is shown by theoretical macroisothermal curves on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane,according to whether density profiles are sufficiently mild (UU) or sufficiently steep (HH, HN/NH).In the former alternative, no critical macroisothermal curve exists, below or above which the trend is monotonous. In the latter alternative, a critical macroisothermal curve exists, as shown by VDW gases, where the critical point may be defined as the horizontal inflexion point. In any case, by analogy with VDW gases, the first quadrant of the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane may be divided into three parts: (i) The G region, where only gas exists; (ii) The S region,where only stars exist; (iii) The GS region,where both gas and stars, exist. With regard to HH and HN/NH macrogases, an application is made to a subsample ({small $N=16$}) of elliptical galaxies extracted from larger samples {small $(N=25,~N=48)$}of early type galaxies investigated within the SAURON project (Cappellari et al. 2006, 2007).Under the simplifying assumption of universal mass ratio of the two subsystems, {small $m$}, different models characterized by different scaled truncation radii, i.e. concentrations, {small $Xi_i$},{small $Xi_j$}, are considered and the related position of sample objects on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane is determined. Macrogases fitting to elliptical galaxies are expected to lie within the S region or slightly outside the boundary between the S and the GS region at most. Accordingly,models where sample objects lie outside the S region and far from its boundary, or cannot be positioned on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, are rejected. For each macrogas, twenty models are considered for different values of {small $(Xi_i,Xi_j, m)$}, namely {small $Xi_i, Xi_j=5,~ 10,~ 20,~+infty$} {small $(Xi_i, Xi_j,$} both either finite or infinite), and {small $m=10,~ 20$}. Acceptable models are {small $(10,~10,~20)$}, {small $(10,~20,~20)$},{small $(20,~10,~20)$}, {small $(20,~20,~20)$}, for HH macrogases,and {small $(10,~5,~10)$}, {small $(10,~10,~20)$}, {small $(20,~10,~20)$},for HN/NH macrogases. Tipically, fast rotators are found to lie within the S region, while slow rotators are close (from both sides) to the boundary between the S and the GS region. The net effect of the uncertainty affecting observed quantities, on the position of sample objects on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, is also investigated. Finally, a principle of corresponding states is formulated for macrogases with assigned density profiles and scaled truncation radii.
abstractGer	Macrogases are defined as two-component,large-scale celestial objects where the subsystems interact only via gravitation.The macrogas equation of state is formulated and compared to the van der Waals (VDW)equation of state for ordinary gases.By analogy, it is assumed that real macroisothermal curves in macrogases occur as real isothermal curves in ordinary gases, where a phase transition(vapour-liquid observed in ordinary gases and gas-stars assumed in macrogases) takesplace along a horizontal linein the macrovolume-macropressure{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane.The intersections between real and theoretical(deduced from the equation of state) macro isothermalcurves, make two regions of equal surface as for ordinary gases obeying the VDW equation of state.A numerical algorithm is developed for determining the following points of a selected theoretical macroisothermal curve on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane:the three intersections with the related real macroisothermal curve,and the two extremum points (one maximum and one minimum). Different kinds of macrogases are studied in detail: UU, where U density profiles are flat, to be conceived as a simple guidance case; HH, where H density profiles obey the Hernquist (1990) law, which satisfactorily fits the observed spheroidal components of galaxies; HN/NH, where N density profiles obey the Navarro-Frenk-White (1995,1996, 1997) law, which satisfactorily fits the simulated nonbaryonic dark matter haloes.A different trend is shown by theoretical macroisothermal curves on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane,according to whether density profiles are sufficiently mild (UU) or sufficiently steep (HH, HN/NH).In the former alternative, no critical macroisothermal curve exists, below or above which the trend is monotonous. In the latter alternative, a critical macroisothermal curve exists, as shown by VDW gases, where the critical point may be defined as the horizontal inflexion point. In any case, by analogy with VDW gases, the first quadrant of the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane may be divided into three parts: (i) The G region, where only gas exists; (ii) The S region,where only stars exist; (iii) The GS region,where both gas and stars, exist. With regard to HH and HN/NH macrogases, an application is made to a subsample ({small $N=16$}) of elliptical galaxies extracted from larger samples {small $(N=25,~N=48)$}of early type galaxies investigated within the SAURON project (Cappellari et al. 2006, 2007).Under the simplifying assumption of universal mass ratio of the two subsystems, {small $m$}, different models characterized by different scaled truncation radii, i.e. concentrations, {small $Xi_i$},{small $Xi_j$}, are considered and the related position of sample objects on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane is determined. Macrogases fitting to elliptical galaxies are expected to lie within the S region or slightly outside the boundary between the S and the GS region at most. Accordingly,models where sample objects lie outside the S region and far from its boundary, or cannot be positioned on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, are rejected. For each macrogas, twenty models are considered for different values of {small $(Xi_i,Xi_j, m)$}, namely {small $Xi_i, Xi_j=5,~ 10,~ 20,~+infty$} {small $(Xi_i, Xi_j,$} both either finite or infinite), and {small $m=10,~ 20$}. Acceptable models are {small $(10,~10,~20)$}, {small $(10,~20,~20)$},{small $(20,~10,~20)$}, {small $(20,~20,~20)$}, for HH macrogases,and {small $(10,~5,~10)$}, {small $(10,~10,~20)$}, {small $(20,~10,~20)$},for HN/NH macrogases. Tipically, fast rotators are found to lie within the S region, while slow rotators are close (from both sides) to the boundary between the S and the GS region. The net effect of the uncertainty affecting observed quantities, on the position of sample objects on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, is also investigated. Finally, a principle of corresponding states is formulated for macrogases with assigned density profiles and scaled truncation radii.
abstract_unstemmed	Macrogases are defined as two-component,large-scale celestial objects where the subsystems interact only via gravitation.The macrogas equation of state is formulated and compared to the van der Waals (VDW)equation of state for ordinary gases.By analogy, it is assumed that real macroisothermal curves in macrogases occur as real isothermal curves in ordinary gases, where a phase transition(vapour-liquid observed in ordinary gases and gas-stars assumed in macrogases) takesplace along a horizontal linein the macrovolume-macropressure{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane.The intersections between real and theoretical(deduced from the equation of state) macro isothermalcurves, make two regions of equal surface as for ordinary gases obeying the VDW equation of state.A numerical algorithm is developed for determining the following points of a selected theoretical macroisothermal curve on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane:the three intersections with the related real macroisothermal curve,and the two extremum points (one maximum and one minimum). Different kinds of macrogases are studied in detail: UU, where U density profiles are flat, to be conceived as a simple guidance case; HH, where H density profiles obey the Hernquist (1990) law, which satisfactorily fits the observed spheroidal components of galaxies; HN/NH, where N density profiles obey the Navarro-Frenk-White (1995,1996, 1997) law, which satisfactorily fits the simulated nonbaryonic dark matter haloes.A different trend is shown by theoretical macroisothermal curves on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane,according to whether density profiles are sufficiently mild (UU) or sufficiently steep (HH, HN/NH).In the former alternative, no critical macroisothermal curve exists, below or above which the trend is monotonous. In the latter alternative, a critical macroisothermal curve exists, as shown by VDW gases, where the critical point may be defined as the horizontal inflexion point. In any case, by analogy with VDW gases, the first quadrant of the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane may be divided into three parts: (i) The G region, where only gas exists; (ii) The S region,where only stars exist; (iii) The GS region,where both gas and stars, exist. With regard to HH and HN/NH macrogases, an application is made to a subsample ({small $N=16$}) of elliptical galaxies extracted from larger samples {small $(N=25,~N=48)$}of early type galaxies investigated within the SAURON project (Cappellari et al. 2006, 2007).Under the simplifying assumption of universal mass ratio of the two subsystems, {small $m$}, different models characterized by different scaled truncation radii, i.e. concentrations, {small $Xi_i$},{small $Xi_j$}, are considered and the related position of sample objects on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane is determined. Macrogases fitting to elliptical galaxies are expected to lie within the S region or slightly outside the boundary between the S and the GS region at most. Accordingly,models where sample objects lie outside the S region and far from its boundary, or cannot be positioned on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, are rejected. For each macrogas, twenty models are considered for different values of {small $(Xi_i,Xi_j, m)$}, namely {small $Xi_i, Xi_j=5,~ 10,~ 20,~+infty$} {small $(Xi_i, Xi_j,$} both either finite or infinite), and {small $m=10,~ 20$}. Acceptable models are {small $(10,~10,~20)$}, {small $(10,~20,~20)$},{small $(20,~10,~20)$}, {small $(20,~20,~20)$}, for HH macrogases,and {small $(10,~5,~10)$}, {small $(10,~10,~20)$}, {small $(20,~10,~20)$},for HN/NH macrogases. Tipically, fast rotators are found to lie within the S region, while slow rotators are close (from both sides) to the boundary between the S and the GS region. The net effect of the uncertainty affecting observed quantities, on the position of sample objects on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, is also investigated. Finally, a principle of corresponding states is formulated for macrogases with assigned density profiles and scaled truncation radii.
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title_short	A Principle of Corresponding States for Two-Component, Self-Gravitating Fluids
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fullrecord_marcxml	<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">DOAJ066069602</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230309054808.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">230228s2010 xx \|\|\|\|\|o 00\| \|\|eng c</controlfield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)DOAJ066069602</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-599)DOAJ194aa060541b427f9f45ee6a964314a0</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="050" ind1=" " ind2="0"><subfield code="a">QB1-991</subfield></datafield><datafield tag="100" ind1="0" ind2=" "><subfield code="a">Caimmi, R.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="2"><subfield code="a">A Principle of Corresponding States for Two-Component, Self-Gravitating Fluids</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2010</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">Macrogases are defined as two-component,large-scale celestial objects where the subsystems interact only via gravitation.The macrogas equation of state is formulated and compared to the van der Waals (VDW)equation of state for ordinary gases.By analogy, it is assumed that real macroisothermal curves in macrogases occur as real isothermal curves in ordinary gases, where a phase transition(vapour-liquid observed in ordinary gases and gas-stars assumed in macrogases) takesplace along a horizontal linein the macrovolume-macropressure{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane.The intersections between real and theoretical(deduced from the equation of state) macro isothermalcurves, make two regions of equal surface as for ordinary gases obeying the VDW equation of state.A numerical algorithm is developed for determining the following points of a selected theoretical macroisothermal curve on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane:the three intersections with the related real macroisothermal curve,and the two extremum points (one maximum and one minimum). Different kinds of macrogases are studied in detail: UU, where U density profiles are flat, to be conceived as a simple guidance case; HH, where H density profiles obey the Hernquist (1990) law, which satisfactorily fits the observed spheroidal components of galaxies; HN/NH, where N density profiles obey the Navarro-Frenk-White (1995,1996, 1997) law, which satisfactorily fits the simulated nonbaryonic dark matter haloes.A different trend is shown by theoretical macroisothermal curves on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane,according to whether density profiles are sufficiently mild (UU) or sufficiently steep (HH, HN/NH).In the former alternative, no critical macroisothermal curve exists, below or above which the trend is monotonous. In the latter alternative, a critical macroisothermal curve exists, as shown by VDW gases, where the critical point may be defined as the horizontal inflexion point. In any case, by analogy with VDW gases, the first quadrant of the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane may be divided into three parts: (i) The G region, where only gas exists; (ii) The S region,where only stars exist; (iii) The GS region,where both gas and stars, exist. With regard to HH and HN/NH macrogases, an application is made to a subsample ({small $N=16$}) of elliptical galaxies extracted from larger samples {small $(N=25,~N=48)$}of early type galaxies investigated within the SAURON project (Cappellari et al. 2006, 2007).Under the simplifying assumption of universal mass ratio of the two subsystems, {small $m$}, different models characterized by different scaled truncation radii, i.e. concentrations, {small $Xi_i$},{small $Xi_j$}, are considered and the related position of sample objects on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane is determined. Macrogases fitting to elliptical galaxies are expected to lie within the S region or slightly outside the boundary between the S and the GS region at most. Accordingly,models where sample objects lie outside the S region and far from its boundary, or cannot be positioned on the{small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, are rejected. For each macrogas, twenty models are considered for different values of {small $(Xi_i,Xi_j, m)$}, namely {small $Xi_i, Xi_j=5,~ 10,~ 20,~+infty$} {small $(Xi_i, Xi_j,$} both either finite or infinite), and {small $m=10,~ 20$}. Acceptable models are {small $(10,~10,~20)$}, {small $(10,~20,~20)$},{small $(20,~10,~20)$}, {small $(20,~20,~20)$}, for HH macrogases,and {small $(10,~5,~10)$}, {small $(10,~10,~20)$}, {small $(20,~10,~20)$},for HN/NH macrogases. Tipically, fast rotators are found to lie within the S region, while slow rotators are close (from both sides) to the boundary between the S and the GS region. The net effect of the uncertainty affecting observed quantities, on the position of sample objects on the {small $({sf O}sX_mathrm{V}sX_mathrm{p})$} plane, is also investigated. Finally, a principle of corresponding states is formulated for macrogases with assigned density profiles and scaled truncation radii.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Galaxies: evolution</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Galaxies: halos</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Dark matter</subfield></datafield><datafield tag="653" ind1=" " ind2="0"><subfield code="a">Astronomy</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">In</subfield><subfield code="t">Serbian Astronomical Journal</subfield><subfield code="d">Astronomical Observatory, Department of Astronomy, Belgrade, 2008</subfield><subfield code="g">180(2010), Seite 19-55</subfield><subfield code="w">(DE-627)538218460</subfield><subfield code="w">(DE-600)2378699-1</subfield><subfield code="x">18209289</subfield><subfield code="7">nnns</subfield></datafield><datafield 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A Principle of Corresponding States for Two-Component, Self-Gravitating Fluids

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