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Article: On the formation of Perseus OB1 at high galactic latitudes

TitleOn the formation of Perseus OB1 at high galactic latitudes
Authors
KeywordsIsm: Clouds
Ism: Molecules
Open Clusters And Associations: Individual (Per Ob1)
Stars: Formation
Issue Date2008
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2008, v. 679 n. 2, p. 1352-1363 How to Cite?
AbstractThe Per OB1 association, which contains the remarkable double cluster h and χ Per, is unusual in not having a giant molecular cloud in its vicinity. We show from Hipparcos data that the luminous members of this association exhibit a bulk motion away from the Galactic plane, such that their average velocity increases with height above the Galactic plane. We find HAeBe and T Tauri stars toward probable remnant molecular clouds associated with Per OB1. These star-forming regions lie well beyond the location of the luminous member stars at heights of 280-400 pc above the Galactic plane, far higher than that previously found for embedded clusters. We argue that the observed motion of the luminous member stars is most naturally explained if many formed from molecular gas pushed and accelerated outward by an expanding superbubble, driven presumably by stellar winds and perhaps also by supernova explosions. A large shell of atomic hydrogen gas and dust that lies just beyond the remnant molecular clouds, believed to be driven by just such a superbubble, may comprise the swept-up remains of the parental giant molecular cloud from which this association formed. In support of this picture, we find a weak trend for the younger O star members to lie at higher Galactic latitudes than the older supergiant members. The star-forming regions located at even larger heights above the Galactic plane presumably correspond to more recent episodes of star formation at or near the periphery of this superbubble. © 2008. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/175147
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorLee, HTen_US
dc.contributor.authorLim, Jen_US
dc.date.accessioned2012-11-26T08:49:25Z-
dc.date.available2012-11-26T08:49:25Z-
dc.date.issued2008en_US
dc.identifier.citationAstrophysical Journal Letters, 2008, v. 679 n. 2, p. 1352-1363en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/175147-
dc.description.abstractThe Per OB1 association, which contains the remarkable double cluster h and χ Per, is unusual in not having a giant molecular cloud in its vicinity. We show from Hipparcos data that the luminous members of this association exhibit a bulk motion away from the Galactic plane, such that their average velocity increases with height above the Galactic plane. We find HAeBe and T Tauri stars toward probable remnant molecular clouds associated with Per OB1. These star-forming regions lie well beyond the location of the luminous member stars at heights of 280-400 pc above the Galactic plane, far higher than that previously found for embedded clusters. We argue that the observed motion of the luminous member stars is most naturally explained if many formed from molecular gas pushed and accelerated outward by an expanding superbubble, driven presumably by stellar winds and perhaps also by supernova explosions. A large shell of atomic hydrogen gas and dust that lies just beyond the remnant molecular clouds, believed to be driven by just such a superbubble, may comprise the swept-up remains of the parental giant molecular cloud from which this association formed. In support of this picture, we find a weak trend for the younger O star members to lie at higher Galactic latitudes than the older supergiant members. The star-forming regions located at even larger heights above the Galactic plane presumably correspond to more recent episodes of star formation at or near the periphery of this superbubble. © 2008. The American Astronomical Society. All rights reserved.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectIsm: Cloudsen_US
dc.subjectIsm: Moleculesen_US
dc.subjectOpen Clusters And Associations: Individual (Per Ob1)en_US
dc.subjectStars: Formationen_US
dc.titleOn the formation of Perseus OB1 at high galactic latitudesen_US
dc.typeArticleen_US
dc.identifier.emailLim, J: jjlim@hku.hken_US
dc.identifier.authorityLim, J=rp00745en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1086/587801en_US
dc.identifier.scopuseid_2-s2.0-46349110923en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-46349110923&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume679en_US
dc.identifier.issue2en_US
dc.identifier.spage1352en_US
dc.identifier.epage1363en_US
dc.identifier.isiWOS:000256315500030-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridLee, HT=8650502900en_US
dc.identifier.scopusauthoridLim, J=7403453870en_US

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