AustralieFrV1, PascalFrancis, Curation, bibRecord, 004317

Very Large Telescope Interferometer observations of the dust geometry around R Coronae Borealis stars

Identifieur interne : 004317 ( PascalFrancis/Curation ); précédent : 004316; suivant : 004318

Very Large Telescope Interferometer observations of the dust geometry around R Coronae Borealis stars

Auteurs : S. N. Bright [Australie] ; O. Chesneau [France] ; G. C. Clayton [États-Unis] ; O. De Marco [Australie] ; I. C. Leao [Brésil] ; J. Nordhaus [États-Unis] ; J. S. Gallagher [États-Unis]

Source :

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

RBID : Pascal:11-0287625

Descripteurs français

Pascal (Inist)
- Etoile type R Coronae Borealis, Supergéante, Observation interférométrique, Modèle géométrique, Transfert radiatif, Symétrie sphérique, Série temporelle, Masse stellaire, Perte masse.

English descriptors

KwdEn :
- Geometrical model, Interferometric observation, Mass loss, R Coronae Borealis stars, Radiative transfer, Spherical symmetry, Stellar mass, Supergiant stars, Time series.

Abstract

We are investigating the formation and evolution of dust around the hydrogen-deficient supergiants known as R Coronae Borealis (RCB) stars. We aim to determine the connection between the probable merger past of these stars and their current dust-production activities. We carried out high angular resolution interferometric observations of three RCB stars, namely RY Sgr, V CrA and V854 Cen, with the mid-infrared interferometer (MIDI) on the Very Large Telescope Interferometer (VLTI), using two telescope pairs. The baselines ranged from 30 to 60 m, allowing us to probe the dusty environment at very small spatial scales (˜50 mas or 400R_*). The observations of the RCB star dust environments were interpreted using both geometrical models and one-dimensional radiative transfer codes. From our analysis, we find that asymmetric circumstellar material is apparent in RY Sgr, may also exist in V CrA and is possible for V854 Cen. Overall, we find that our observations are consistent with dust forming in clumps ejected randomly around the RCB star so that over time they create a spherically symmetric distribution of dust. However, we conclude that the determination of whether there is a preferred plane of dust ejection must wait until a time series of observations are obtained.

A01	`01`	`1`		`@0 0035-8711`
A02	`01`			`@0 MNRAA4`
A03		`1`		`@0 Mon. Not. R. Astron. Soc.`
A05				`@2 414`
A06				`@2 2`
A08	`01`	`1`	`ENG`	`@1 Very Large Telescope Interferometer observations of the dust geometry around R Coronae Borealis stars`
A11	`01`	`1`		`@1 BRIGHT (S. N.)`
A11	`02`	`1`		`@1 CHESNEAU (O.)`
A11	`03`	`1`		`@1 CLAYTON (G. C.)`
A11	`04`	`1`		`@1 DE MARCO (O.)`
A11	`05`	`1`		`@1 LEAO (I. C.)`
A11	`06`	`1`		`@1 NORDHAUS (J.)`
A11	`07`	`1`		`@1 GALLAGHER (J. S.)`
A14	`01`			`@1 Department of Physics and Astronomy, Macquarie University @2 Sydney, NSW 2109 @3 AUS @Z 1 aut. @Z 4 aut.`
A14	`02`			`@1 UMR 6525 H. Fizeau, Univ. Nice Sophia Antipolis, CNRS, Observatoire de la Côte d'Azur, Av. Copernic @2 06130 Grasse @3 FRA @Z 2 aut.`
A14	`03`			`@1 Department of Physics and Astronomy, Louisiana State University @2 Baton Rouge, LA 70803 @3 USA @Z 3 aut. @Z 7 aut.`
A14	`04`			`@1 Departamento de Física, Universidade Federal do Rio Grande do Norte @2 59072-970 Natal, RN @3 BRA @Z 5 aut.`
A14	`05`			`@1 Department of Astrophysical Sciences, Princeton University @2 Princeton, NJ 08544 @3 USA @Z 6 aut.`
A20				`@1 1195-1206`
A21				`@1 2011`
A23	`01`			`@0 ENG`
A43	`01`			`@1 INIST @2 2067 @5 354000190355760280`
A44				`@0 0000 @1 © 2011 INIST-CNRS. All rights reserved.`
A45				`@0 3/4 p.`
A47	`01`	`1`		`@0 11-0287625`
A60				`@1 P`
A61				`@0 A`
A64	`01`	`1`		`@0 Monthly Notices of the Royal Astronomical Society`
A66	`01`			`@0 USA`
C01	`01`		`ENG`	@0 We are investigating the formation and evolution of dust around the hydrogen-deficient supergiants known as R Coronae Borealis (RCB) stars. We aim to determine the connection between the probable merger past of these stars and their current dust-production activities. We carried out high angular resolution interferometric observations of three RCB stars, namely RY Sgr, V CrA and V854 Cen, with the mid-infrared interferometer (MIDI) on the Very Large Telescope Interferometer (VLTI), using two telescope pairs. The baselines ranged from 30 to 60 m, allowing us to probe the dusty environment at very small spatial scales (˜50 mas or 400R_*). The observations of the RCB star dust environments were interpreted using both geometrical models and one-dimensional radiative transfer codes. From our analysis, we find that asymmetric circumstellar material is apparent in RY Sgr, may also exist in V CrA and is possible for V854 Cen. Overall, we find that our observations are consistent with dust forming in clumps ejected randomly around the RCB star so that over time they create a spherically symmetric distribution of dust. However, we conclude that the determination of whether there is a preferred plane of dust ejection must wait until a time series of observations are obtained.
C02	`01`	`3`		`@0 001E03`
C03	`01`	`3`	`FRE`	`@0 Etoile type R Coronae Borealis @5 26`
C03	`01`	`3`	`ENG`	`@0 R Coronae Borealis stars @5 26`
C03	`02`	`3`	`FRE`	`@0 Supergéante @5 27`
C03	`02`	`3`	`ENG`	`@0 Supergiant stars @5 27`
C03	`03`	`X`	`FRE`	`@0 Observation interférométrique @5 28`
C03	`03`	`X`	`ENG`	`@0 Interferometric observation @5 28`
C03	`03`	`X`	`SPA`	`@0 Observación interferométrica @5 28`
C03	`04`	`X`	`FRE`	`@0 Modèle géométrique @5 29`
C03	`04`	`X`	`ENG`	`@0 Geometrical model @5 29`
C03	`04`	`X`	`SPA`	`@0 Modelo geométrico @5 29`
C03	`05`	`3`	`FRE`	`@0 Transfert radiatif @5 30`
C03	`05`	`3`	`ENG`	`@0 Radiative transfer @5 30`
C03	`06`	`X`	`FRE`	`@0 Symétrie sphérique @5 31`
C03	`06`	`X`	`ENG`	`@0 Spherical symmetry @5 31`
C03	`06`	`X`	`SPA`	`@0 Simetría esférica @5 31`
C03	`07`	`3`	`FRE`	`@0 Série temporelle @5 32`
C03	`07`	`3`	`ENG`	`@0 Time series @5 32`
C03	`08`	`3`	`FRE`	`@0 Masse stellaire @5 33`
C03	`08`	`3`	`ENG`	`@0 Stellar mass @5 33`
C03	`09`	`3`	`FRE`	`@0 Perte masse @5 34`
C03	`09`	`3`	`ENG`	`@0 Mass loss @5 34`
N21				`@1 192`
N44	`01`			`@1 OTO`
N82				`@1 OTO`

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Le document en format XML

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<front><div type="abstract" xml:lang="en">We are investigating the formation and evolution of dust around the hydrogen-deficient supergiants known as R Coronae Borealis (RCB) stars. We aim to determine the connection between the probable merger past of these stars and their current dust-production activities. We carried out high angular resolution interferometric observations of three RCB stars, namely RY Sgr, V CrA and V854 Cen, with the mid-infrared interferometer (MIDI) on the Very Large Telescope Interferometer (VLTI), using two telescope pairs. The baselines ranged from 30 to 60 m, allowing us to probe the dusty environment at very small spatial scales (˜50 mas or 400R<sub>*</sub>
). The observations of the RCB star dust environments were interpreted using both geometrical models and one-dimensional radiative transfer codes. From our analysis, we find that asymmetric circumstellar material is apparent in RY Sgr, may also exist in V CrA and is possible for V854 Cen. Overall, we find that our observations are consistent with dust forming in clumps ejected randomly around the RCB star so that over time they create a spherically symmetric distribution of dust. However, we conclude that the determination of whether there is a preferred plane of dust ejection must wait until a time series of observations are obtained.</div>
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<fC01 i1="01" l="ENG"><s0>We are investigating the formation and evolution of dust around the hydrogen-deficient supergiants known as R Coronae Borealis (RCB) stars. We aim to determine the connection between the probable merger past of these stars and their current dust-production activities. We carried out high angular resolution interferometric observations of three RCB stars, namely RY Sgr, V CrA and V854 Cen, with the mid-infrared interferometer (MIDI) on the Very Large Telescope Interferometer (VLTI), using two telescope pairs. The baselines ranged from 30 to 60 m, allowing us to probe the dusty environment at very small spatial scales (˜50 mas or 400R<sub>*</sub>
). The observations of the RCB star dust environments were interpreted using both geometrical models and one-dimensional radiative transfer codes. From our analysis, we find that asymmetric circumstellar material is apparent in RY Sgr, may also exist in V CrA and is possible for V854 Cen. Overall, we find that our observations are consistent with dust forming in clumps ejected randomly around the RCB star so that over time they create a spherically symmetric distribution of dust. However, we conclude that the determination of whether there is a preferred plane of dust ejection must wait until a time series of observations are obtained.</s0>
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<fC03 i1="06" i2="X" l="FRE"><s0>Symétrie sphérique</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="X" l="ENG"><s0>Spherical symmetry</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="X" l="SPA"><s0>Simetría esférica</s0>
<s5>31</s5>
</fC03>
<fC03 i1="07" i2="3" l="FRE"><s0>Série temporelle</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="3" l="ENG"><s0>Time series</s0>
<s5>32</s5>
</fC03>
<fC03 i1="08" i2="3" l="FRE"><s0>Masse stellaire</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="3" l="ENG"><s0>Stellar mass</s0>
<s5>33</s5>
</fC03>
<fC03 i1="09" i2="3" l="FRE"><s0>Perte masse</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="3" l="ENG"><s0>Mass loss</s0>
<s5>34</s5>
</fC03>
<fN21><s1>192</s1>
</fN21>
<fN44 i1="01"><s1>OTO</s1>
</fN44>
<fN82><s1>OTO</s1>
</fN82>
</pA>
</standard>
</inist>
</record>

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	Serveur d'exploration sur les relations entre la France et l'Australie
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Very Large Telescope Interferometer observations of the dust geometry around R Coronae Borealis stars

Very Large Telescope Interferometer observations of the dust geometry around R Coronae Borealis stars

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