AustralieFrV1, PascalFrancis, Corpus, bibRecord, 004910

On the properties of H I shells in the small magellanic cloud

Identifieur interne : 004910 ( PascalFrancis/Corpus ); précédent : 004909; suivant : 004911

On the properties of H I shells in the small magellanic cloud

Auteurs : D. Hatzidimitriou ; S. Stanimirovic ; F. Maragoudaki ; L. Staveley-Smith ; A. Dapergolas ; E. Bratsolis

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2005.

RBID : Pascal:05-0289632

Descripteurs français

Pascal (Inist)
- Petit Nuage Magellan, Hydrogène neutre, Age, Objet stellaire jeune, Catalogue astronomique, Association stellaire OB, Supergéante, Céphéide, Etoile type Wolf Rayet, Reste supernova, Amas stellaire, Méthode Monte Carlo, Vitesse expansion, Fonction distribution vitesse, Modèle standard, Vent stellaire, Explosion supernova, Loi puissance, Luminosité, Formation stellaire, Sursaut Rγ, Turbulence, Mécanisme formation, Cinématique, Dynamique, Nuages Magellan.

English descriptors

KwdEn :
- Age, Astronomical catalogues, Cepheids, Dynamics, Expansion velocity, Formation mechanism, Gamma ray burst, Kinematics, Luminosity, Magellanic Clouds, Monte Carlo methods, Neutral hydrogen, OB stellar association, Power law, Small Magellanic Cloud, Standard model, Star clusters, Star formation, Stellar winds, Supergiant stars, Supernova remnants, Supernovae explosion, Turbulence, Velocity distribution function, Wolf-Rayet stars, Young stellar object.

Abstract

There are 509 expanding neutral hydrogen shells catalogued in the Small Magellanic Cloud (SMC), all apparently very young, with dynamical ages of a few Myr. To examine their relationship with young stellar objects, we cross-correlated the shell catalogue with various catalogues of OB associations, supergiants, Cepheids, Wolf-Rayet stars, supernova remnants and star clusters. The incidence of chance line-ups was estimated via Monte Carlo simulations, and found to be high. However, it is important that there are 1.5 times more shells that are not spatially correlated to an OB association, than shells that are. Moreover, 59 of the 509 shells lie mainly in low stellar density fields and have no young stellar objects associated with them, and therefore no obvious energy source. It is shown that, on the whole, the properties of these 'empty' shells are very similar to the properties of the rest of the shells, once selection biases are taken into account. In both cases, the shell radius and expansion velocity distribution functions are consistent with the standard model, according to which shells are created by stellar winds and supernova explosions, as long as all shells were created in a single burst and with a power-law distribution of the input mechanical luminosity. This would indicate a burst of star formation. This interpretation, however, cannot explain why the 59 shells, with no young stellar counterparts, show almost exactly the same behaviour as shells with OB associations within their radius. Gamma-ray bursts could account for some but certainly not for the majority of the 'empty' shells. Many 'empty' shells, including most of the high-luminosity ones, are located in the north-western outer regions of the SMC, and may be associated with a chimney-like feature that is known to exist in that area. Finally, it is noted that turbulence is a promising mechanism for the formation of the shell-like structures, but direct comparison with the observations was not possible at this stage, due to lack of detailed models.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

A01	`01`	`1`		`@0 0035-8711`
A02	`01`			`@0 MNRAA4`
A03		`1`		`@0 Mon. Not. R. Astron. Soc.`
A05				`@2 360`
A06				`@2 3`
A08	`01`	`1`	`ENG`	`@1 On the properties of H I shells in the small magellanic cloud`
A11	`01`	`1`		`@1 HATZIDIMITRIOU (D.)`
A11	`02`	`1`		`@1 STANIMIROVIC (S.)`
A11	`03`	`1`		`@1 MARAGOUDAKI (F.)`
A11	`04`	`1`		`@1 STAVELEY-SMITH (L.)`
A11	`05`	`1`		`@1 DAPERGOLAS (A.)`
A11	`06`	`1`		`@1 BRATSOLIS (E.)`
A14	`01`			`@1 Physics Department, University of Crete, PO Box 2208 @2 710-03 Heraklion, Crete @3 GRC @Z 1 aut.`
A14	`02`			`@1 Radio Astronomy Laboratory, University of California, Berkeley, 601 Campbell Hall @2 Berkeley, CA 94720 @3 USA @Z 2 aut.`
A14	`03`			`@1 Section of Astrophysics, Astronomy and Mechanics, Department of Physics, University of Athens @2 15784 Athens @3 GRC @Z 3 aut.`
A14	`04`			`@1 Australia Telescope National Facility, CSIRO, PO Box 76 @2 Epping, NSW 1710 @3 AUS @Z 4 aut.`
A14	`05`			`@1 Astronomical Institute, National Observatory of Athens, PO Box 20048 @2 11810 Athens @3 GRC @Z 5 aut.`
A14	`06`			`@1 Department Traitement du Signal et des Images, Ecole Nationale Superieure des Telecommunications, Telecom Paris, 46 rue Barrault @2 75634 @3 FRA @Z 6 aut.`
A20				`@1 1171-1184`
A21				`@1 2005`
A23	`01`			`@0 ENG`
A43	`01`			`@1 INIST @2 2067 @5 354000138223830360`
A44				`@0 0000 @1 © 2005 INIST-CNRS. All rights reserved.`
A45				`@0 64 ref.`
A47	`01`	`1`		`@0 05-0289632`
A60				`@1 P`
A61				`@0 A`
A64	`01`	`1`		`@0 Monthly Notices of the Royal Astronomical Society`
A66	`01`			`@0 GBR`
C01	`01`		`ENG`	@0 There are 509 expanding neutral hydrogen shells catalogued in the Small Magellanic Cloud (SMC), all apparently very young, with dynamical ages of a few Myr. To examine their relationship with young stellar objects, we cross-correlated the shell catalogue with various catalogues of OB associations, supergiants, Cepheids, Wolf-Rayet stars, supernova remnants and star clusters. The incidence of chance line-ups was estimated via Monte Carlo simulations, and found to be high. However, it is important that there are 1.5 times more shells that are not spatially correlated to an OB association, than shells that are. Moreover, 59 of the 509 shells lie mainly in low stellar density fields and have no young stellar objects associated with them, and therefore no obvious energy source. It is shown that, on the whole, the properties of these 'empty' shells are very similar to the properties of the rest of the shells, once selection biases are taken into account. In both cases, the shell radius and expansion velocity distribution functions are consistent with the standard model, according to which shells are created by stellar winds and supernova explosions, as long as all shells were created in a single burst and with a power-law distribution of the input mechanical luminosity. This would indicate a burst of star formation. This interpretation, however, cannot explain why the 59 shells, with no young stellar counterparts, show almost exactly the same behaviour as shells with OB associations within their radius. Gamma-ray bursts could account for some but certainly not for the majority of the 'empty' shells. Many 'empty' shells, including most of the high-luminosity ones, are located in the north-western outer regions of the SMC, and may be associated with a chimney-like feature that is known to exist in that area. Finally, it is noted that turbulence is a promising mechanism for the formation of the shell-like structures, but direct comparison with the observations was not possible at this stage, due to lack of detailed models.
C02	`01`	`3`		`@0 001E03`
C03	`01`	`3`	`FRE`	`@0 Petit Nuage Magellan @5 26`
C03	`01`	`3`	`ENG`	`@0 Small Magellanic Cloud @5 26`
C03	`02`	`X`	`FRE`	`@0 Hydrogène neutre @5 27`
C03	`02`	`X`	`ENG`	`@0 Neutral hydrogen @5 27`
C03	`02`	`X`	`SPA`	`@0 Hidrógeno neutro @5 27`
C03	`03`	`X`	`FRE`	`@0 Age @5 28`
C03	`03`	`X`	`ENG`	`@0 Age @5 28`
C03	`03`	`X`	`SPA`	`@0 Edad @5 28`
C03	`04`	`X`	`FRE`	`@0 Objet stellaire jeune @2 NO @5 29`
C03	`04`	`X`	`ENG`	`@0 Young stellar object @2 NO @5 29`
C03	`04`	`X`	`SPA`	`@0 Objeto estelar joven @2 NO @5 29`
C03	`05`	`3`	`FRE`	`@0 Catalogue astronomique @5 30`
C03	`05`	`3`	`ENG`	`@0 Astronomical catalogues @5 30`
C03	`06`	`X`	`FRE`	`@0 Association stellaire OB @5 31`
C03	`06`	`X`	`ENG`	`@0 OB stellar association @5 31`
C03	`06`	`X`	`SPA`	`@0 Asociación estelar OB @5 31`
C03	`07`	`3`	`FRE`	`@0 Supergéante @5 32`
C03	`07`	`3`	`ENG`	`@0 Supergiant stars @5 32`
C03	`08`	`3`	`FRE`	`@0 Céphéide @5 33`
C03	`08`	`3`	`ENG`	`@0 Cepheids @5 33`
C03	`09`	`3`	`FRE`	`@0 Etoile type Wolf Rayet @5 34`
C03	`09`	`3`	`ENG`	`@0 Wolf-Rayet stars @5 34`
C03	`10`	`3`	`FRE`	`@0 Reste supernova @5 35`
C03	`10`	`3`	`ENG`	`@0 Supernova remnants @5 35`
C03	`11`	`3`	`FRE`	`@0 Amas stellaire @5 36`
C03	`11`	`3`	`ENG`	`@0 Star clusters @5 36`
C03	`12`	`3`	`FRE`	`@0 Méthode Monte Carlo @5 37`
C03	`12`	`3`	`ENG`	`@0 Monte Carlo methods @5 37`
C03	`13`	`X`	`FRE`	`@0 Vitesse expansion @5 38`
C03	`13`	`X`	`ENG`	`@0 Expansion velocity @5 38`
C03	`13`	`X`	`SPA`	`@0 Velocidad expansión @5 38`
C03	`14`	`X`	`FRE`	`@0 Fonction distribution vitesse @5 39`
C03	`14`	`X`	`ENG`	`@0 Velocity distribution function @5 39`
C03	`14`	`X`	`SPA`	`@0 Función distribución velocidad @5 39`
C03	`15`	`3`	`FRE`	`@0 Modèle standard @5 40`
C03	`15`	`3`	`ENG`	`@0 Standard model @5 40`
C03	`16`	`3`	`FRE`	`@0 Vent stellaire @5 41`
C03	`16`	`3`	`ENG`	`@0 Stellar winds @5 41`
C03	`17`	`X`	`FRE`	`@0 Explosion supernova @5 42`
C03	`17`	`X`	`ENG`	`@0 Supernovae explosion @5 42`
C03	`17`	`X`	`SPA`	`@0 Explosión supernova @5 42`
C03	`18`	`X`	`FRE`	`@0 Loi puissance @5 43`
C03	`18`	`X`	`ENG`	`@0 Power law @5 43`
C03	`18`	`X`	`SPA`	`@0 Ley poder @5 43`
C03	`19`	`3`	`FRE`	`@0 Luminosité @5 44`
C03	`19`	`3`	`ENG`	`@0 Luminosity @5 44`
C03	`20`	`3`	`FRE`	`@0 Formation stellaire @5 45`
C03	`20`	`3`	`ENG`	`@0 Star formation @5 45`
C03	`21`	`X`	`FRE`	`@0 Sursaut Rγ @5 46`
C03	`21`	`X`	`ENG`	`@0 Gamma ray burst @5 46`
C03	`21`	`X`	`SPA`	`@0 Arrebato Rγ @5 46`
C03	`22`	`3`	`FRE`	`@0 Turbulence @5 47`
C03	`22`	`3`	`ENG`	`@0 Turbulence @5 47`
C03	`23`	`X`	`FRE`	`@0 Mécanisme formation @5 48`
C03	`23`	`X`	`ENG`	`@0 Formation mechanism @5 48`
C03	`23`	`X`	`SPA`	`@0 Mecanismo formacion @5 48`
C03	`24`	`3`	`FRE`	`@0 Cinématique @5 49`
C03	`24`	`3`	`ENG`	`@0 Kinematics @5 49`
C03	`25`	`3`	`FRE`	`@0 Dynamique @5 50`
C03	`25`	`3`	`ENG`	`@0 Dynamics @5 50`
C03	`26`	`3`	`FRE`	`@0 Nuages Magellan @5 90`
C03	`26`	`3`	`ENG`	`@0 Magellanic Clouds @5 90`
N21				`@1 199`
N44	`01`			`@1 OTO`
N82				`@1 OTO`

Format Inist (serveur)

NO :	PASCAL 05-0289632 INIST
ET :	On the properties of H I shells in the small magellanic cloud
AU :	HATZIDIMITRIOU (D.); STANIMIROVIC (S.); MARAGOUDAKI (F.); STAVELEY-SMITH (L.); DAPERGOLAS (A.); BRATSOLIS (E.)
AF :	Physics Department, University of Crete, PO Box 2208/710-03 Heraklion, Crete/Grèce (1 aut.); Radio Astronomy Laboratory, University of California, Berkeley, 601 Campbell Hall/Berkeley, CA 94720/Etats-Unis (2 aut.); Section of Astrophysics, Astronomy and Mechanics, Department of Physics, University of Athens/15784 Athens/Grèce (3 aut.); Australia Telescope National Facility, CSIRO, PO Box 76/Epping, NSW 1710/Australie (4 aut.); Astronomical Institute, National Observatory of Athens, PO Box 20048/11810 Athens/Grèce (5 aut.); Department Traitement du Signal et des Images, Ecole Nationale Superieure des Telecommunications, Telecom Paris, 46 rue Barrault/75634/France (6 aut.)
DT :	Publication en série; Niveau analytique
SO :	Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2005; Vol. 360; No. 3; Pp. 1171-1184; Bibl. 64 ref.
LA :	Anglais
EA :	There are 509 expanding neutral hydrogen shells catalogued in the Small Magellanic Cloud (SMC), all apparently very young, with dynamical ages of a few Myr. To examine their relationship with young stellar objects, we cross-correlated the shell catalogue with various catalogues of OB associations, supergiants, Cepheids, Wolf-Rayet stars, supernova remnants and star clusters. The incidence of chance line-ups was estimated via Monte Carlo simulations, and found to be high. However, it is important that there are 1.5 times more shells that are not spatially correlated to an OB association, than shells that are. Moreover, 59 of the 509 shells lie mainly in low stellar density fields and have no young stellar objects associated with them, and therefore no obvious energy source. It is shown that, on the whole, the properties of these 'empty' shells are very similar to the properties of the rest of the shells, once selection biases are taken into account. In both cases, the shell radius and expansion velocity distribution functions are consistent with the standard model, according to which shells are created by stellar winds and supernova explosions, as long as all shells were created in a single burst and with a power-law distribution of the input mechanical luminosity. This would indicate a burst of star formation. This interpretation, however, cannot explain why the 59 shells, with no young stellar counterparts, show almost exactly the same behaviour as shells with OB associations within their radius. Gamma-ray bursts could account for some but certainly not for the majority of the 'empty' shells. Many 'empty' shells, including most of the high-luminosity ones, are located in the north-western outer regions of the SMC, and may be associated with a chimney-like feature that is known to exist in that area. Finally, it is noted that turbulence is a promising mechanism for the formation of the shell-like structures, but direct comparison with the observations was not possible at this stage, due to lack of detailed models.
CC :	001E03
FD :	Petit Nuage Magellan; Hydrogène neutre; Age; Objet stellaire jeune; Catalogue astronomique; Association stellaire OB; Supergéante; Céphéide; Etoile type Wolf Rayet; Reste supernova; Amas stellaire; Méthode Monte Carlo; Vitesse expansion; Fonction distribution vitesse; Modèle standard; Vent stellaire; Explosion supernova; Loi puissance; Luminosité; Formation stellaire; Sursaut Rγ; Turbulence; Mécanisme formation; Cinématique; Dynamique; Nuages Magellan
ED :	Small Magellanic Cloud; Neutral hydrogen; Age; Young stellar object; Astronomical catalogues; OB stellar association; Supergiant stars; Cepheids; Wolf-Rayet stars; Supernova remnants; Star clusters; Monte Carlo methods; Expansion velocity; Velocity distribution function; Standard model; Stellar winds; Supernovae explosion; Power law; Luminosity; Star formation; Gamma ray burst; Turbulence; Formation mechanism; Kinematics; Dynamics; Magellanic Clouds
SD :	Hidrógeno neutro; Edad; Objeto estelar joven; Asociación estelar OB; Velocidad expansión; Función distribución velocidad; Explosión supernova; Ley poder; Arrebato Rγ; Mecanismo formacion
LO :	INIST-2067.354000138223830360
ID :	05-0289632

Links to Exploration step

Pascal:05-0289632

Le document en format XML

<record><TEI><teiHeader><fileDesc><titleStmt><title xml:lang="en" level="a">On the properties of H I shells in the small magellanic cloud</title>
<author><name sortKey="Hatzidimitriou, D" sort="Hatzidimitriou, D" uniqKey="Hatzidimitriou D" first="D." last="Hatzidimitriou">D. Hatzidimitriou</name>
<affiliation><inist:fA14 i1="01"><s1>Physics Department, University of Crete, PO Box 2208</s1>
<s2>710-03 Heraklion, Crete</s2>
<s3>GRC</s3>
<sZ>1 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Stanimirovic, S" sort="Stanimirovic, S" uniqKey="Stanimirovic S" first="S." last="Stanimirovic">S. Stanimirovic</name>
<affiliation><inist:fA14 i1="02"><s1>Radio Astronomy Laboratory, University of California, Berkeley, 601 Campbell Hall</s1>
<s2>Berkeley, CA 94720</s2>
<s3>USA</s3>
<sZ>2 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Maragoudaki, F" sort="Maragoudaki, F" uniqKey="Maragoudaki F" first="F." last="Maragoudaki">F. Maragoudaki</name>
<affiliation><inist:fA14 i1="03"><s1>Section of Astrophysics, Astronomy and Mechanics, Department of Physics, University of Athens</s1>
<s2>15784 Athens</s2>
<s3>GRC</s3>
<sZ>3 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Staveley Smith, L" sort="Staveley Smith, L" uniqKey="Staveley Smith L" first="L." last="Staveley-Smith">L. Staveley-Smith</name>
<affiliation><inist:fA14 i1="04"><s1>Australia Telescope National Facility, CSIRO, PO Box 76</s1>
<s2>Epping, NSW 1710</s2>
<s3>AUS</s3>
<sZ>4 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Dapergolas, A" sort="Dapergolas, A" uniqKey="Dapergolas A" first="A." last="Dapergolas">A. Dapergolas</name>
<affiliation><inist:fA14 i1="05"><s1>Astronomical Institute, National Observatory of Athens, PO Box 20048</s1>
<s2>11810 Athens</s2>
<s3>GRC</s3>
<sZ>5 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Bratsolis, E" sort="Bratsolis, E" uniqKey="Bratsolis E" first="E." last="Bratsolis">E. Bratsolis</name>
<affiliation><inist:fA14 i1="06"><s1>Department Traitement du Signal et des Images, Ecole Nationale Superieure des Telecommunications, Telecom Paris, 46 rue Barrault</s1>
<s2>75634</s2>
<s3>FRA</s3>
<sZ>6 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
</titleStmt>
<publicationStmt><idno type="wicri:source">INIST</idno>
<idno type="inist">05-0289632</idno>
<date when="2005">2005</date>
<idno type="stanalyst">PASCAL 05-0289632 INIST</idno>
<idno type="RBID">Pascal:05-0289632</idno>
<idno type="wicri:Area/PascalFrancis/Corpus">004910</idno>
</publicationStmt>
<sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">On the properties of H I shells in the small magellanic cloud</title>
<author><name sortKey="Hatzidimitriou, D" sort="Hatzidimitriou, D" uniqKey="Hatzidimitriou D" first="D." last="Hatzidimitriou">D. Hatzidimitriou</name>
<affiliation><inist:fA14 i1="01"><s1>Physics Department, University of Crete, PO Box 2208</s1>
<s2>710-03 Heraklion, Crete</s2>
<s3>GRC</s3>
<sZ>1 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Stanimirovic, S" sort="Stanimirovic, S" uniqKey="Stanimirovic S" first="S." last="Stanimirovic">S. Stanimirovic</name>
<affiliation><inist:fA14 i1="02"><s1>Radio Astronomy Laboratory, University of California, Berkeley, 601 Campbell Hall</s1>
<s2>Berkeley, CA 94720</s2>
<s3>USA</s3>
<sZ>2 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Maragoudaki, F" sort="Maragoudaki, F" uniqKey="Maragoudaki F" first="F." last="Maragoudaki">F. Maragoudaki</name>
<affiliation><inist:fA14 i1="03"><s1>Section of Astrophysics, Astronomy and Mechanics, Department of Physics, University of Athens</s1>
<s2>15784 Athens</s2>
<s3>GRC</s3>
<sZ>3 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Staveley Smith, L" sort="Staveley Smith, L" uniqKey="Staveley Smith L" first="L." last="Staveley-Smith">L. Staveley-Smith</name>
<affiliation><inist:fA14 i1="04"><s1>Australia Telescope National Facility, CSIRO, PO Box 76</s1>
<s2>Epping, NSW 1710</s2>
<s3>AUS</s3>
<sZ>4 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Dapergolas, A" sort="Dapergolas, A" uniqKey="Dapergolas A" first="A." last="Dapergolas">A. Dapergolas</name>
<affiliation><inist:fA14 i1="05"><s1>Astronomical Institute, National Observatory of Athens, PO Box 20048</s1>
<s2>11810 Athens</s2>
<s3>GRC</s3>
<sZ>5 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Bratsolis, E" sort="Bratsolis, E" uniqKey="Bratsolis E" first="E." last="Bratsolis">E. Bratsolis</name>
<affiliation><inist:fA14 i1="06"><s1>Department Traitement du Signal et des Images, Ecole Nationale Superieure des Telecommunications, Telecom Paris, 46 rue Barrault</s1>
<s2>75634</s2>
<s3>FRA</s3>
<sZ>6 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
</analytic>
<series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title>
<title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title>
<idno type="ISSN">0035-8711</idno>
<imprint><date when="2005">2005</date>
</imprint>
</series>
</biblStruct>
</sourceDesc>
<seriesStmt><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title>
<title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title>
<idno type="ISSN">0035-8711</idno>
</seriesStmt>
</fileDesc>
<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Age</term>
<term>Astronomical catalogues</term>
<term>Cepheids</term>
<term>Dynamics</term>
<term>Expansion velocity</term>
<term>Formation mechanism</term>
<term>Gamma ray burst</term>
<term>Kinematics</term>
<term>Luminosity</term>
<term>Magellanic Clouds</term>
<term>Monte Carlo methods</term>
<term>Neutral hydrogen</term>
<term>OB stellar association</term>
<term>Power law</term>
<term>Small Magellanic Cloud</term>
<term>Standard model</term>
<term>Star clusters</term>
<term>Star formation</term>
<term>Stellar winds</term>
<term>Supergiant stars</term>
<term>Supernova remnants</term>
<term>Supernovae explosion</term>
<term>Turbulence</term>
<term>Velocity distribution function</term>
<term>Wolf-Rayet stars</term>
<term>Young stellar object</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Petit Nuage Magellan</term>
<term>Hydrogène neutre</term>
<term>Age</term>
<term>Objet stellaire jeune</term>
<term>Catalogue astronomique</term>
<term>Association stellaire OB</term>
<term>Supergéante</term>
<term>Céphéide</term>
<term>Etoile type Wolf Rayet</term>
<term>Reste supernova</term>
<term>Amas stellaire</term>
<term>Méthode Monte Carlo</term>
<term>Vitesse expansion</term>
<term>Fonction distribution vitesse</term>
<term>Modèle standard</term>
<term>Vent stellaire</term>
<term>Explosion supernova</term>
<term>Loi puissance</term>
<term>Luminosité</term>
<term>Formation stellaire</term>
<term>Sursaut Rγ</term>
<term>Turbulence</term>
<term>Mécanisme formation</term>
<term>Cinématique</term>
<term>Dynamique</term>
<term>Nuages Magellan</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front><div type="abstract" xml:lang="en">There are 509 expanding neutral hydrogen shells catalogued in the Small Magellanic Cloud (SMC), all apparently very young, with dynamical ages of a few Myr. To examine their relationship with young stellar objects, we cross-correlated the shell catalogue with various catalogues of OB associations, supergiants, Cepheids, Wolf-Rayet stars, supernova remnants and star clusters. The incidence of chance line-ups was estimated via Monte Carlo simulations, and found to be high. However, it is important that there are 1.5 times more shells that are not spatially correlated to an OB association, than shells that are. Moreover, 59 of the 509 shells lie mainly in low stellar density fields and have no young stellar objects associated with them, and therefore no obvious energy source. It is shown that, on the whole, the properties of these 'empty' shells are very similar to the properties of the rest of the shells, once selection biases are taken into account. In both cases, the shell radius and expansion velocity distribution functions are consistent with the standard model, according to which shells are created by stellar winds and supernova explosions, as long as all shells were created in a single burst and with a power-law distribution of the input mechanical luminosity. This would indicate a burst of star formation. This interpretation, however, cannot explain why the 59 shells, with no young stellar counterparts, show almost exactly the same behaviour as shells with OB associations within their radius. Gamma-ray bursts could account for some but certainly not for the majority of the 'empty' shells. Many 'empty' shells, including most of the high-luminosity ones, are located in the north-western outer regions of the SMC, and may be associated with a chimney-like feature that is known to exist in that area. Finally, it is noted that turbulence is a promising mechanism for the formation of the shell-like structures, but direct comparison with the observations was not possible at this stage, due to lack of detailed models.</div>
</front>
</TEI>
<inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0035-8711</s0>
</fA01>
<fA02 i1="01"><s0>MNRAA4</s0>
</fA02>
<fA03 i2="1"><s0>Mon. Not. R. Astron. Soc.</s0>
</fA03>
<fA05><s2>360</s2>
</fA05>
<fA06><s2>3</s2>
</fA06>
<fA08 i1="01" i2="1" l="ENG"><s1>On the properties of H I shells in the small magellanic cloud</s1>
</fA08>
<fA11 i1="01" i2="1"><s1>HATZIDIMITRIOU (D.)</s1>
</fA11>
<fA11 i1="02" i2="1"><s1>STANIMIROVIC (S.)</s1>
</fA11>
<fA11 i1="03" i2="1"><s1>MARAGOUDAKI (F.)</s1>
</fA11>
<fA11 i1="04" i2="1"><s1>STAVELEY-SMITH (L.)</s1>
</fA11>
<fA11 i1="05" i2="1"><s1>DAPERGOLAS (A.)</s1>
</fA11>
<fA11 i1="06" i2="1"><s1>BRATSOLIS (E.)</s1>
</fA11>
<fA14 i1="01"><s1>Physics Department, University of Crete, PO Box 2208</s1>
<s2>710-03 Heraklion, Crete</s2>
<s3>GRC</s3>
<sZ>1 aut.</sZ>
</fA14>
<fA14 i1="02"><s1>Radio Astronomy Laboratory, University of California, Berkeley, 601 Campbell Hall</s1>
<s2>Berkeley, CA 94720</s2>
<s3>USA</s3>
<sZ>2 aut.</sZ>
</fA14>
<fA14 i1="03"><s1>Section of Astrophysics, Astronomy and Mechanics, Department of Physics, University of Athens</s1>
<s2>15784 Athens</s2>
<s3>GRC</s3>
<sZ>3 aut.</sZ>
</fA14>
<fA14 i1="04"><s1>Australia Telescope National Facility, CSIRO, PO Box 76</s1>
<s2>Epping, NSW 1710</s2>
<s3>AUS</s3>
<sZ>4 aut.</sZ>
</fA14>
<fA14 i1="05"><s1>Astronomical Institute, National Observatory of Athens, PO Box 20048</s1>
<s2>11810 Athens</s2>
<s3>GRC</s3>
<sZ>5 aut.</sZ>
</fA14>
<fA14 i1="06"><s1>Department Traitement du Signal et des Images, Ecole Nationale Superieure des Telecommunications, Telecom Paris, 46 rue Barrault</s1>
<s2>75634</s2>
<s3>FRA</s3>
<sZ>6 aut.</sZ>
</fA14>
<fA20><s1>1171-1184</s1>
</fA20>
<fA21><s1>2005</s1>
</fA21>
<fA23 i1="01"><s0>ENG</s0>
</fA23>
<fA43 i1="01"><s1>INIST</s1>
<s2>2067</s2>
<s5>354000138223830360</s5>
</fA43>
<fA44><s0>0000</s0>
<s1>© 2005 INIST-CNRS. All rights reserved.</s1>
</fA44>
<fA45><s0>64 ref.</s0>
</fA45>
<fA47 i1="01" i2="1"><s0>05-0289632</s0>
</fA47>
<fA60><s1>P</s1>
</fA60>
<fA61><s0>A</s0>
</fA61>
<fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0>
</fA64>
<fA66 i1="01"><s0>GBR</s0>
</fA66>
<fC01 i1="01" l="ENG"><s0>There are 509 expanding neutral hydrogen shells catalogued in the Small Magellanic Cloud (SMC), all apparently very young, with dynamical ages of a few Myr. To examine their relationship with young stellar objects, we cross-correlated the shell catalogue with various catalogues of OB associations, supergiants, Cepheids, Wolf-Rayet stars, supernova remnants and star clusters. The incidence of chance line-ups was estimated via Monte Carlo simulations, and found to be high. However, it is important that there are 1.5 times more shells that are not spatially correlated to an OB association, than shells that are. Moreover, 59 of the 509 shells lie mainly in low stellar density fields and have no young stellar objects associated with them, and therefore no obvious energy source. It is shown that, on the whole, the properties of these 'empty' shells are very similar to the properties of the rest of the shells, once selection biases are taken into account. In both cases, the shell radius and expansion velocity distribution functions are consistent with the standard model, according to which shells are created by stellar winds and supernova explosions, as long as all shells were created in a single burst and with a power-law distribution of the input mechanical luminosity. This would indicate a burst of star formation. This interpretation, however, cannot explain why the 59 shells, with no young stellar counterparts, show almost exactly the same behaviour as shells with OB associations within their radius. Gamma-ray bursts could account for some but certainly not for the majority of the 'empty' shells. Many 'empty' shells, including most of the high-luminosity ones, are located in the north-western outer regions of the SMC, and may be associated with a chimney-like feature that is known to exist in that area. Finally, it is noted that turbulence is a promising mechanism for the formation of the shell-like structures, but direct comparison with the observations was not possible at this stage, due to lack of detailed models.</s0>
</fC01>
<fC02 i1="01" i2="3"><s0>001E03</s0>
</fC02>
<fC03 i1="01" i2="3" l="FRE"><s0>Petit Nuage Magellan</s0>
<s5>26</s5>
</fC03>
<fC03 i1="01" i2="3" l="ENG"><s0>Small Magellanic Cloud</s0>
<s5>26</s5>
</fC03>
<fC03 i1="02" i2="X" l="FRE"><s0>Hydrogène neutre</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="X" l="ENG"><s0>Neutral hydrogen</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="X" l="SPA"><s0>Hidrógeno neutro</s0>
<s5>27</s5>
</fC03>
<fC03 i1="03" i2="X" l="FRE"><s0>Age</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="X" l="ENG"><s0>Age</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="X" l="SPA"><s0>Edad</s0>
<s5>28</s5>
</fC03>
<fC03 i1="04" i2="X" l="FRE"><s0>Objet stellaire jeune</s0>
<s2>NO</s2>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="X" l="ENG"><s0>Young stellar object</s0>
<s2>NO</s2>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="X" l="SPA"><s0>Objeto estelar joven</s0>
<s2>NO</s2>
<s5>29</s5>
</fC03>
<fC03 i1="05" i2="3" l="FRE"><s0>Catalogue astronomique</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="3" l="ENG"><s0>Astronomical catalogues</s0>
<s5>30</s5>
</fC03>
<fC03 i1="06" i2="X" l="FRE"><s0>Association stellaire OB</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="X" l="ENG"><s0>OB stellar association</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="X" l="SPA"><s0>Asociación estelar OB</s0>
<s5>31</s5>
</fC03>
<fC03 i1="07" i2="3" l="FRE"><s0>Supergéante</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="3" l="ENG"><s0>Supergiant stars</s0>
<s5>32</s5>
</fC03>
<fC03 i1="08" i2="3" l="FRE"><s0>Céphéide</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="3" l="ENG"><s0>Cepheids</s0>
<s5>33</s5>
</fC03>
<fC03 i1="09" i2="3" l="FRE"><s0>Etoile type Wolf Rayet</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="3" l="ENG"><s0>Wolf-Rayet stars</s0>
<s5>34</s5>
</fC03>
<fC03 i1="10" i2="3" l="FRE"><s0>Reste supernova</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="3" l="ENG"><s0>Supernova remnants</s0>
<s5>35</s5>
</fC03>
<fC03 i1="11" i2="3" l="FRE"><s0>Amas stellaire</s0>
<s5>36</s5>
</fC03>
<fC03 i1="11" i2="3" l="ENG"><s0>Star clusters</s0>
<s5>36</s5>
</fC03>
<fC03 i1="12" i2="3" l="FRE"><s0>Méthode Monte Carlo</s0>
<s5>37</s5>
</fC03>
<fC03 i1="12" i2="3" l="ENG"><s0>Monte Carlo methods</s0>
<s5>37</s5>
</fC03>
<fC03 i1="13" i2="X" l="FRE"><s0>Vitesse expansion</s0>
<s5>38</s5>
</fC03>
<fC03 i1="13" i2="X" l="ENG"><s0>Expansion velocity</s0>
<s5>38</s5>
</fC03>
<fC03 i1="13" i2="X" l="SPA"><s0>Velocidad expansión</s0>
<s5>38</s5>
</fC03>
<fC03 i1="14" i2="X" l="FRE"><s0>Fonction distribution vitesse</s0>
<s5>39</s5>
</fC03>
<fC03 i1="14" i2="X" l="ENG"><s0>Velocity distribution function</s0>
<s5>39</s5>
</fC03>
<fC03 i1="14" i2="X" l="SPA"><s0>Función distribución velocidad</s0>
<s5>39</s5>
</fC03>
<fC03 i1="15" i2="3" l="FRE"><s0>Modèle standard</s0>
<s5>40</s5>
</fC03>
<fC03 i1="15" i2="3" l="ENG"><s0>Standard model</s0>
<s5>40</s5>
</fC03>
<fC03 i1="16" i2="3" l="FRE"><s0>Vent stellaire</s0>
<s5>41</s5>
</fC03>
<fC03 i1="16" i2="3" l="ENG"><s0>Stellar winds</s0>
<s5>41</s5>
</fC03>
<fC03 i1="17" i2="X" l="FRE"><s0>Explosion supernova</s0>
<s5>42</s5>
</fC03>
<fC03 i1="17" i2="X" l="ENG"><s0>Supernovae explosion</s0>
<s5>42</s5>
</fC03>
<fC03 i1="17" i2="X" l="SPA"><s0>Explosión supernova</s0>
<s5>42</s5>
</fC03>
<fC03 i1="18" i2="X" l="FRE"><s0>Loi puissance</s0>
<s5>43</s5>
</fC03>
<fC03 i1="18" i2="X" l="ENG"><s0>Power law</s0>
<s5>43</s5>
</fC03>
<fC03 i1="18" i2="X" l="SPA"><s0>Ley poder</s0>
<s5>43</s5>
</fC03>
<fC03 i1="19" i2="3" l="FRE"><s0>Luminosité</s0>
<s5>44</s5>
</fC03>
<fC03 i1="19" i2="3" l="ENG"><s0>Luminosity</s0>
<s5>44</s5>
</fC03>
<fC03 i1="20" i2="3" l="FRE"><s0>Formation stellaire</s0>
<s5>45</s5>
</fC03>
<fC03 i1="20" i2="3" l="ENG"><s0>Star formation</s0>
<s5>45</s5>
</fC03>
<fC03 i1="21" i2="X" l="FRE"><s0>Sursaut Rγ</s0>
<s5>46</s5>
</fC03>
<fC03 i1="21" i2="X" l="ENG"><s0>Gamma ray burst</s0>
<s5>46</s5>
</fC03>
<fC03 i1="21" i2="X" l="SPA"><s0>Arrebato Rγ</s0>
<s5>46</s5>
</fC03>
<fC03 i1="22" i2="3" l="FRE"><s0>Turbulence</s0>
<s5>47</s5>
</fC03>
<fC03 i1="22" i2="3" l="ENG"><s0>Turbulence</s0>
<s5>47</s5>
</fC03>
<fC03 i1="23" i2="X" l="FRE"><s0>Mécanisme formation</s0>
<s5>48</s5>
</fC03>
<fC03 i1="23" i2="X" l="ENG"><s0>Formation mechanism</s0>
<s5>48</s5>
</fC03>
<fC03 i1="23" i2="X" l="SPA"><s0>Mecanismo formacion</s0>
<s5>48</s5>
</fC03>
<fC03 i1="24" i2="3" l="FRE"><s0>Cinématique</s0>
<s5>49</s5>
</fC03>
<fC03 i1="24" i2="3" l="ENG"><s0>Kinematics</s0>
<s5>49</s5>
</fC03>
<fC03 i1="25" i2="3" l="FRE"><s0>Dynamique</s0>
<s5>50</s5>
</fC03>
<fC03 i1="25" i2="3" l="ENG"><s0>Dynamics</s0>
<s5>50</s5>
</fC03>
<fC03 i1="26" i2="3" l="FRE"><s0>Nuages Magellan</s0>
<s5>90</s5>
</fC03>
<fC03 i1="26" i2="3" l="ENG"><s0>Magellanic Clouds</s0>
<s5>90</s5>
</fC03>
<fN21><s1>199</s1>
</fN21>
<fN44 i1="01"><s1>OTO</s1>
</fN44>
<fN82><s1>OTO</s1>
</fN82>
</pA>
</standard>
<server><NO>PASCAL 05-0289632 INIST</NO>
<ET>On the properties of H I shells in the small magellanic cloud</ET>
<AU>HATZIDIMITRIOU (D.); STANIMIROVIC (S.); MARAGOUDAKI (F.); STAVELEY-SMITH (L.); DAPERGOLAS (A.); BRATSOLIS (E.)</AU>
<AF>Physics Department, University of Crete, PO Box 2208/710-03 Heraklion, Crete/Grèce (1 aut.); Radio Astronomy Laboratory, University of California, Berkeley, 601 Campbell Hall/Berkeley, CA 94720/Etats-Unis (2 aut.); Section of Astrophysics, Astronomy and Mechanics, Department of Physics, University of Athens/15784 Athens/Grèce (3 aut.); Australia Telescope National Facility, CSIRO, PO Box 76/Epping, NSW 1710/Australie (4 aut.); Astronomical Institute, National Observatory of Athens, PO Box 20048/11810 Athens/Grèce (5 aut.); Department Traitement du Signal et des Images, Ecole Nationale Superieure des Telecommunications, Telecom Paris, 46 rue Barrault/75634/France (6 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2005; Vol. 360; No. 3; Pp. 1171-1184; Bibl. 64 ref.</SO>
<LA>Anglais</LA>
<EA>There are 509 expanding neutral hydrogen shells catalogued in the Small Magellanic Cloud (SMC), all apparently very young, with dynamical ages of a few Myr. To examine their relationship with young stellar objects, we cross-correlated the shell catalogue with various catalogues of OB associations, supergiants, Cepheids, Wolf-Rayet stars, supernova remnants and star clusters. The incidence of chance line-ups was estimated via Monte Carlo simulations, and found to be high. However, it is important that there are 1.5 times more shells that are not spatially correlated to an OB association, than shells that are. Moreover, 59 of the 509 shells lie mainly in low stellar density fields and have no young stellar objects associated with them, and therefore no obvious energy source. It is shown that, on the whole, the properties of these 'empty' shells are very similar to the properties of the rest of the shells, once selection biases are taken into account. In both cases, the shell radius and expansion velocity distribution functions are consistent with the standard model, according to which shells are created by stellar winds and supernova explosions, as long as all shells were created in a single burst and with a power-law distribution of the input mechanical luminosity. This would indicate a burst of star formation. This interpretation, however, cannot explain why the 59 shells, with no young stellar counterparts, show almost exactly the same behaviour as shells with OB associations within their radius. Gamma-ray bursts could account for some but certainly not for the majority of the 'empty' shells. Many 'empty' shells, including most of the high-luminosity ones, are located in the north-western outer regions of the SMC, and may be associated with a chimney-like feature that is known to exist in that area. Finally, it is noted that turbulence is a promising mechanism for the formation of the shell-like structures, but direct comparison with the observations was not possible at this stage, due to lack of detailed models.</EA>
<CC>001E03</CC>
<FD>Petit Nuage Magellan; Hydrogène neutre; Age; Objet stellaire jeune; Catalogue astronomique; Association stellaire OB; Supergéante; Céphéide; Etoile type Wolf Rayet; Reste supernova; Amas stellaire; Méthode Monte Carlo; Vitesse expansion; Fonction distribution vitesse; Modèle standard; Vent stellaire; Explosion supernova; Loi puissance; Luminosité; Formation stellaire; Sursaut Rγ; Turbulence; Mécanisme formation; Cinématique; Dynamique; Nuages Magellan</FD>
<ED>Small Magellanic Cloud; Neutral hydrogen; Age; Young stellar object; Astronomical catalogues; OB stellar association; Supergiant stars; Cepheids; Wolf-Rayet stars; Supernova remnants; Star clusters; Monte Carlo methods; Expansion velocity; Velocity distribution function; Standard model; Stellar winds; Supernovae explosion; Power law; Luminosity; Star formation; Gamma ray burst; Turbulence; Formation mechanism; Kinematics; Dynamics; Magellanic Clouds</ED>
<SD>Hidrógeno neutro; Edad; Objeto estelar joven; Asociación estelar OB; Velocidad expansión; Función distribución velocidad; Explosión supernova; Ley poder; Arrebato Rγ; Mecanismo formacion</SD>
<LO>INIST-2067.354000138223830360</LO>
<ID>05-0289632</ID>
</server>
</inist>
</record>

Pour manipuler ce document sous Unix (Dilib)

EXPLOR_STEP=$WICRI_ROOT/Wicri/Asie/explor/AustralieFrV1/Data/PascalFrancis/Corpus

HfdSelect -h $EXPLOR_STEP/biblio.hfd -nk 004910 | SxmlIndent | more

HfdSelect -h $EXPLOR_AREA/Data/PascalFrancis/Corpus/biblio.hfd -nk 004910 | SxmlIndent | more

Pour mettre un lien sur cette page dans le réseau Wicri

{{Explor lien
   |wiki=    Wicri/Asie
   |area=    AustralieFrV1
   |flux=    PascalFrancis
   |étape=   Corpus
   |type=    RBID
   |clé=     Pascal:05-0289632
   |texte=   On the properties of H I shells in the small magellanic cloud
}}

This area was generated with Dilib version V0.6.33.
Data generation: Tue Dec 5 10:43:12 2017. Site generation: Tue Mar 5 14:07:20 2024

	Serveur d'exploration sur les relations entre la France et l'Australie
	Attention, ce site est en cours de développement ! Attention, site généré par des moyens informatiques à partir de corpus bruts. Les informations ne sont donc pas validées.

Serveur d'exploration sur les relations entre la France et l'Australie

On the properties of H I shells in the small magellanic cloud

On the properties of H I shells in the small magellanic cloud

Source :

Descripteurs français

English descriptors

Abstract

Notice en format standard (ISO 2709)

Format Inist (serveur)

Links to Exploration step

Le document en format XML

Pour manipuler ce document sous Unix (Dilib)

Pour mettre un lien sur cette page dans le réseau Wicri