AustralieFrV1, PascalFrancis, Corpus, bibRecord, 001B67

The effect of the regular solution model in the condensation of protoplanetary dust

Identifieur interne : 001B67 ( PascalFrancis/Corpus ); précédent : 001B66; suivant : 001B68

The effect of the regular solution model in the condensation of protoplanetary dust

Auteurs : F. C. Pignatale ; S. T. Maddison ; V. Taquet ; G. Brooks ; K. Liffman

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011.

RBID : Pascal:11-0292146

Descripteurs français

Pascal (Inist)
- Solution régulière, Modèle, Condensation, Equilibre chimique, Thermodynamique, Energie libre Gibbs, Haute température, Abondance, Basse température, Matière circumstellaire.

English descriptors

KwdEn :
- Abundance, Chemical equilibrium, Circumstellar matter, Gibbs free energy, High temperature, Low temperature, Models, Regular solution, Thermodynamics, Vapor condensation.

Abstract

We utilize a chemical equilibrium code in order to study the condensation process which occurs in protoplanetary discs during the formation of the first solids. The model specifically focuses on the thermodynamic behaviour on the solid species assuming the regular solution model. For each solution, we establish the relationship between the activity of the species, the composition and the temperature using experimental data from the literature. We then apply the Gibbs free energy minimization method and study the resulting condensation sequence for a range of temperatures and pressures within a protoplanetary disc. Our results using the regular solution model show that grains condense over a large temperature range and therefore throughout a large portion of the disc. In the high-temperature region (T > 1400 K) hibonite and gehlenite dominate, and we find that the formation of corundum is sensitive to the pressure. The mid-temperature region is dominated by Fe(s) and silicates such as Mg₂SiO₄ and MgSiO₃. The chemistry of forsterite and that of enstatite are strictly related, and our simulations show a sequence of forsterite-enstatite-forsterite with decreasing temperature and the abundance of the first high-temperature peak of forsterite is also pressure sensitive. In the low-temperature regions (T ≤ 600 K), a range of iron compounds (FeS, Fe₂SiO₃, FeAl₂O₃) form. We find that all the condensation sequences move towards lower temperature as the pressure decreases. We also run simulations using the ideal solution model and see clear differences in the resulting condensation sequences with changing solution model. In particular, we find that the turning point in which forsterite replaces enstatite in the low-temperature region is sensitive to the solution model. In this same temperature region, fayalite is the most stable compound for the regular solution, while magnetite replaces fayalite in the ideal solution model at the lowest values of temperature. Our results show that the ideal solution model is often a poor approximation to experimental data at most temperatures important in protoplanetary discs. We find some important differences in the resulting condensation sequences when using the regular solution model and suggest that this model should provide a more realistic condensation sequence.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

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A11	`01`	`1`		`@1 PIGNATALE (F. C.)`
A11	`02`	`1`		`@1 MADDISON (S. T.)`
A11	`03`	`1`		`@1 TAQUET (V.)`
A11	`04`	`1`		`@1 BROOKS (G.)`
A11	`05`	`1`		`@1 LIFFMAN (K.)`
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A14	`04`			`@1 Mathematics Discipline, FEIS, Swinburne University, H38, PO Box 218 @2 Hawthorn, VIC 3122 @3 AUS @Z 4 aut.`
A14	`05`			`@1 CSIRO/MSE, PO Box 56 @2 Heighett, VIC 3190 @3 AUS @Z 5 aut.`
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A44				`@0 0000 @1 © 2011 INIST-CNRS. All rights reserved.`
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C01	`01`		`ENG`	@0 We utilize a chemical equilibrium code in order to study the condensation process which occurs in protoplanetary discs during the formation of the first solids. The model specifically focuses on the thermodynamic behaviour on the solid species assuming the regular solution model. For each solution, we establish the relationship between the activity of the species, the composition and the temperature using experimental data from the literature. We then apply the Gibbs free energy minimization method and study the resulting condensation sequence for a range of temperatures and pressures within a protoplanetary disc. Our results using the regular solution model show that grains condense over a large temperature range and therefore throughout a large portion of the disc. In the high-temperature region (T > 1400 K) hibonite and gehlenite dominate, and we find that the formation of corundum is sensitive to the pressure. The mid-temperature region is dominated by Fe(s) and silicates such as Mg₂SiO₄ and MgSiO₃. The chemistry of forsterite and that of enstatite are strictly related, and our simulations show a sequence of forsterite-enstatite-forsterite with decreasing temperature and the abundance of the first high-temperature peak of forsterite is also pressure sensitive. In the low-temperature regions (T ≤ 600 K), a range of iron compounds (FeS, Fe₂SiO₃, FeAl₂O₃) form. We find that all the condensation sequences move towards lower temperature as the pressure decreases. We also run simulations using the ideal solution model and see clear differences in the resulting condensation sequences with changing solution model. In particular, we find that the turning point in which forsterite replaces enstatite in the low-temperature region is sensitive to the solution model. In this same temperature region, fayalite is the most stable compound for the regular solution, while magnetite replaces fayalite in the ideal solution model at the lowest values of temperature. Our results show that the ideal solution model is often a poor approximation to experimental data at most temperatures important in protoplanetary discs. We find some important differences in the resulting condensation sequences when using the regular solution model and suggest that this model should provide a more realistic condensation sequence.
C02	`01`	`3`		`@0 001E03`
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C03	`02`	`X`	`FRE`	`@0 Modèle @5 27`
C03	`02`	`X`	`ENG`	`@0 Models @5 27`
C03	`02`	`X`	`SPA`	`@0 Modelo @5 27`
C03	`03`	`3`	`FRE`	`@0 Condensation @5 28`
C03	`03`	`3`	`ENG`	`@0 Vapor condensation @5 28`
C03	`04`	`3`	`FRE`	`@0 Equilibre chimique @5 29`
C03	`04`	`3`	`ENG`	`@0 Chemical equilibrium @5 29`
C03	`05`	`3`	`FRE`	`@0 Thermodynamique @5 30`
C03	`05`	`3`	`ENG`	`@0 Thermodynamics @5 30`
C03	`06`	`X`	`FRE`	`@0 Energie libre Gibbs @5 31`
C03	`06`	`X`	`ENG`	`@0 Gibbs free energy @5 31`
C03	`06`	`X`	`SPA`	`@0 Energía libre Gibbs @5 31`
C03	`07`	`X`	`FRE`	`@0 Haute température @5 32`
C03	`07`	`X`	`ENG`	`@0 High temperature @5 32`
C03	`07`	`X`	`SPA`	`@0 Alta temperatura @5 32`
C03	`08`	`3`	`FRE`	`@0 Abondance @5 33`
C03	`08`	`3`	`ENG`	`@0 Abundance @5 33`
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N21				`@1 199`
N44	`01`			`@1 OTO`
N82				`@1 OTO`

Format Inist (serveur)

NO :	PASCAL 11-0292146 INIST
ET :	The effect of the regular solution model in the condensation of protoplanetary dust
AU :	PIGNATALE (F. C.); MADDISON (S. T.); TAQUET (V.); BROOKS (G.); LIFFMAN (K.)
AF :	Centre for Astrophysics & Supercomputing, Swinburne University, H39, PO Box 218/Hawthorn, VIC 3122/Australie (1 aut., 2 aut., 3 aut.); Laboratoire d'Astrophysique de Grenoble, UMR 5571 Université Joseph Fourier/CNRS. BP 53/38041 Grenoble/France (2 aut., 3 aut.); Mngistere de Physique Fondamentale d'Orsay, Universite Paris-11/France (3 aut.); Mathematics Discipline, FEIS, Swinburne University, H38, PO Box 218/Hawthorn, VIC 3122/Australie (4 aut.); CSIRO/MSE, PO Box 56/Heighett, VIC 3190/Australie (5 aut.)
DT :	Publication en série; Niveau analytique
SO :	Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Etats-Unis; Da. 2011; Vol. 414; No. 3; Pp. 2386-2405; Bibl. 3/4 p.
LA :	Anglais
EA :	We utilize a chemical equilibrium code in order to study the condensation process which occurs in protoplanetary discs during the formation of the first solids. The model specifically focuses on the thermodynamic behaviour on the solid species assuming the regular solution model. For each solution, we establish the relationship between the activity of the species, the composition and the temperature using experimental data from the literature. We then apply the Gibbs free energy minimization method and study the resulting condensation sequence for a range of temperatures and pressures within a protoplanetary disc. Our results using the regular solution model show that grains condense over a large temperature range and therefore throughout a large portion of the disc. In the high-temperature region (T > 1400 K) hibonite and gehlenite dominate, and we find that the formation of corundum is sensitive to the pressure. The mid-temperature region is dominated by Fe(s) and silicates such as Mg₂SiO₄ and MgSiO₃. The chemistry of forsterite and that of enstatite are strictly related, and our simulations show a sequence of forsterite-enstatite-forsterite with decreasing temperature and the abundance of the first high-temperature peak of forsterite is also pressure sensitive. In the low-temperature regions (T ≤ 600 K), a range of iron compounds (FeS, Fe₂SiO₃, FeAl₂O₃) form. We find that all the condensation sequences move towards lower temperature as the pressure decreases. We also run simulations using the ideal solution model and see clear differences in the resulting condensation sequences with changing solution model. In particular, we find that the turning point in which forsterite replaces enstatite in the low-temperature region is sensitive to the solution model. In this same temperature region, fayalite is the most stable compound for the regular solution, while magnetite replaces fayalite in the ideal solution model at the lowest values of temperature. Our results show that the ideal solution model is often a poor approximation to experimental data at most temperatures important in protoplanetary discs. We find some important differences in the resulting condensation sequences when using the regular solution model and suggest that this model should provide a more realistic condensation sequence.
CC :	001E03
FD :	Solution régulière; Modèle; Condensation; Equilibre chimique; Thermodynamique; Energie libre Gibbs; Haute température; Abondance; Basse température; Matière circumstellaire
ED :	Regular solution; Models; Vapor condensation; Chemical equilibrium; Thermodynamics; Gibbs free energy; High temperature; Abundance; Low temperature; Circumstellar matter
SD :	Solución regular; Modelo; Energía libre Gibbs; Alta temperatura; Baja temperatura
LO :	INIST-2067.354000190369470450
ID :	11-0292146

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Pascal:11-0292146

Le document en format XML

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<front><div type="abstract" xml:lang="en">We utilize a chemical equilibrium code in order to study the condensation process which occurs in protoplanetary discs during the formation of the first solids. The model specifically focuses on the thermodynamic behaviour on the solid species assuming the regular solution model. For each solution, we establish the relationship between the activity of the species, the composition and the temperature using experimental data from the literature. We then apply the Gibbs free energy minimization method and study the resulting condensation sequence for a range of temperatures and pressures within a protoplanetary disc. Our results using the regular solution model show that grains condense over a large temperature range and therefore throughout a large portion of the disc. In the high-temperature region (T > 1400 K) hibonite and gehlenite dominate, and we find that the formation of corundum is sensitive to the pressure. The mid-temperature region is dominated by Fe(s) and silicates such as Mg<sub>2</sub>
SiO<sub>4</sub>
 and MgSiO<sub>3</sub>
. The chemistry of forsterite and that of enstatite are strictly related, and our simulations show a sequence of forsterite-enstatite-forsterite with decreasing temperature and the abundance of the first high-temperature peak of forsterite is also pressure sensitive. In the low-temperature regions (T ≤ 600 K), a range of iron compounds (FeS, Fe<sub>2</sub>
SiO<sub>3</sub>
, FeAl<sub>2</sub>
O<sub>3</sub>
) form. We find that all the condensation sequences move towards lower temperature as the pressure decreases. We also run simulations using the ideal solution model and see clear differences in the resulting condensation sequences with changing solution model. In particular, we find that the turning point in which forsterite replaces enstatite in the low-temperature region is sensitive to the solution model. In this same temperature region, fayalite is the most stable compound for the regular solution, while magnetite replaces fayalite in the ideal solution model at the lowest values of temperature. Our results show that the ideal solution model is often a poor approximation to experimental data at most temperatures important in protoplanetary discs. We find some important differences in the resulting condensation sequences when using the regular solution model and suggest that this model should provide a more realistic condensation sequence.</div>
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<s3>AUS</s3>
<sZ>5 aut.</sZ>
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<fA20><s1>2386-2405</s1>
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<s1>© 2011 INIST-CNRS. All rights reserved.</s1>
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<fA47 i1="01" i2="1"><s0>11-0292146</s0>
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<fA61><s0>A</s0>
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<fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0>
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<fC01 i1="01" l="ENG"><s0>We utilize a chemical equilibrium code in order to study the condensation process which occurs in protoplanetary discs during the formation of the first solids. The model specifically focuses on the thermodynamic behaviour on the solid species assuming the regular solution model. For each solution, we establish the relationship between the activity of the species, the composition and the temperature using experimental data from the literature. We then apply the Gibbs free energy minimization method and study the resulting condensation sequence for a range of temperatures and pressures within a protoplanetary disc. Our results using the regular solution model show that grains condense over a large temperature range and therefore throughout a large portion of the disc. In the high-temperature region (T > 1400 K) hibonite and gehlenite dominate, and we find that the formation of corundum is sensitive to the pressure. The mid-temperature region is dominated by Fe(s) and silicates such as Mg<sub>2</sub>
SiO<sub>4</sub>
 and MgSiO<sub>3</sub>
. The chemistry of forsterite and that of enstatite are strictly related, and our simulations show a sequence of forsterite-enstatite-forsterite with decreasing temperature and the abundance of the first high-temperature peak of forsterite is also pressure sensitive. In the low-temperature regions (T ≤ 600 K), a range of iron compounds (FeS, Fe<sub>2</sub>
SiO<sub>3</sub>
, FeAl<sub>2</sub>
O<sub>3</sub>
) form. We find that all the condensation sequences move towards lower temperature as the pressure decreases. We also run simulations using the ideal solution model and see clear differences in the resulting condensation sequences with changing solution model. In particular, we find that the turning point in which forsterite replaces enstatite in the low-temperature region is sensitive to the solution model. In this same temperature region, fayalite is the most stable compound for the regular solution, while magnetite replaces fayalite in the ideal solution model at the lowest values of temperature. Our results show that the ideal solution model is often a poor approximation to experimental data at most temperatures important in protoplanetary discs. We find some important differences in the resulting condensation sequences when using the regular solution model and suggest that this model should provide a more realistic condensation sequence.</s0>
</fC01>
<fC02 i1="01" i2="3"><s0>001E03</s0>
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<s5>31</s5>
</fC03>
<fC03 i1="07" i2="X" l="FRE"><s0>Haute température</s0>
<s5>32</s5>
</fC03>
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<s5>32</s5>
</fC03>
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<s5>32</s5>
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<fC03 i1="08" i2="3" l="FRE"><s0>Abondance</s0>
<s5>33</s5>
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<s5>33</s5>
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<s5>34</s5>
</fC03>
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<s5>34</s5>
</fC03>
<fC03 i1="09" i2="X" l="SPA"><s0>Baja temperatura</s0>
<s5>34</s5>
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<s5>35</s5>
</fC03>
<fC03 i1="10" i2="3" l="ENG"><s0>Circumstellar matter</s0>
<s5>35</s5>
</fC03>
<fN21><s1>199</s1>
</fN21>
<fN44 i1="01"><s1>OTO</s1>
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<server><NO>PASCAL 11-0292146 INIST</NO>
<ET>The effect of the regular solution model in the condensation of protoplanetary dust</ET>
<AU>PIGNATALE (F. C.); MADDISON (S. T.); TAQUET (V.); BROOKS (G.); LIFFMAN (K.)</AU>
<AF>Centre for Astrophysics & Supercomputing, Swinburne University, H39, PO Box 218/Hawthorn, VIC 3122/Australie (1 aut., 2 aut., 3 aut.); Laboratoire d'Astrophysique de Grenoble, UMR 5571 Université Joseph Fourier/CNRS. BP 53/38041 Grenoble/France (2 aut., 3 aut.); Mngistere de Physique Fondamentale d'Orsay, Universite Paris-11/France (3 aut.); Mathematics Discipline, FEIS, Swinburne University, H38, PO Box 218/Hawthorn, VIC 3122/Australie (4 aut.); CSIRO/MSE, PO Box 56/Heighett, VIC 3190/Australie (5 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Etats-Unis; Da. 2011; Vol. 414; No. 3; Pp. 2386-2405; Bibl. 3/4 p.</SO>
<LA>Anglais</LA>
<EA>We utilize a chemical equilibrium code in order to study the condensation process which occurs in protoplanetary discs during the formation of the first solids. The model specifically focuses on the thermodynamic behaviour on the solid species assuming the regular solution model. For each solution, we establish the relationship between the activity of the species, the composition and the temperature using experimental data from the literature. We then apply the Gibbs free energy minimization method and study the resulting condensation sequence for a range of temperatures and pressures within a protoplanetary disc. Our results using the regular solution model show that grains condense over a large temperature range and therefore throughout a large portion of the disc. In the high-temperature region (T > 1400 K) hibonite and gehlenite dominate, and we find that the formation of corundum is sensitive to the pressure. The mid-temperature region is dominated by Fe(s) and silicates such as Mg<sub>2</sub>
SiO<sub>4</sub>
 and MgSiO<sub>3</sub>
. The chemistry of forsterite and that of enstatite are strictly related, and our simulations show a sequence of forsterite-enstatite-forsterite with decreasing temperature and the abundance of the first high-temperature peak of forsterite is also pressure sensitive. In the low-temperature regions (T ≤ 600 K), a range of iron compounds (FeS, Fe<sub>2</sub>
SiO<sub>3</sub>
, FeAl<sub>2</sub>
O<sub>3</sub>
) form. We find that all the condensation sequences move towards lower temperature as the pressure decreases. We also run simulations using the ideal solution model and see clear differences in the resulting condensation sequences with changing solution model. In particular, we find that the turning point in which forsterite replaces enstatite in the low-temperature region is sensitive to the solution model. In this same temperature region, fayalite is the most stable compound for the regular solution, while magnetite replaces fayalite in the ideal solution model at the lowest values of temperature. Our results show that the ideal solution model is often a poor approximation to experimental data at most temperatures important in protoplanetary discs. We find some important differences in the resulting condensation sequences when using the regular solution model and suggest that this model should provide a more realistic condensation sequence.</EA>
<CC>001E03</CC>
<FD>Solution régulière; Modèle; Condensation; Equilibre chimique; Thermodynamique; Energie libre Gibbs; Haute température; Abondance; Basse température; Matière circumstellaire</FD>
<ED>Regular solution; Models; Vapor condensation; Chemical equilibrium; Thermodynamics; Gibbs free energy; High temperature; Abundance; Low temperature; Circumstellar matter</ED>
<SD>Solución regular; Modelo; Energía libre Gibbs; Alta temperatura; Baja temperatura</SD>
<LO>INIST-2067.354000190369470450</LO>
<ID>11-0292146</ID>
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The effect of the regular solution model in the condensation of protoplanetary dust

The effect of the regular solution model in the condensation of protoplanetary dust

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