Young Stellar Groups, Runaway Stars, and Pulsars

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dc.creatorde Zeeuw, Tim
dc.creatorHoogerwerf, Ronnie
dc.creatorde Bruijne, Jos
dc.date2000-07-28
dc.date.accessioned2026-07-07T01:54:35Z
dc.date.available2026-07-07T01:54:35Z
dc.descriptionMilli-arcsecond astrometry provided by Hipparcos and by radio observations makes it possible to retrace the orbits of nearby runaway stars and pulsars with sufficient accuracy to identify their parent stellar cluster or association. For two cases it is even possible to deduce the specific formation scenario. The runaway star zeta Oph and PSR J1932+1059 are the result of a supernova explosion which took place 1 Myr ago in a massive binary in the Upper Scorpius association. The pulsar received a kick velocity of about 350 km/s in this event. The runaway stars mu Col and AE Aur and the isolated eccentric massive binary iota Ori result from a binary-binary encounter, most likely inside the Trapezium cluster, 2.5 Myr ago. Future astrometric missions such as DIVA, FAME and in particular GAIA will allow extension of these studies to a significant fraction of the Galactic disk, and will provide new constraints on the formation and evolution of massive stars.
dc.descriptionTo appear in: Dynamics of Starclusters and the Milky Way eds S. Deiters, B. Fuchs, A. Just, R. Spurzem, R. Wielen, ASP Conf. Ser
dc.identifierhttps://arxiv.org/abs/astro-ph/0007439
dc.identifierhttp://arxiv.org/abs/astro-ph/0007439
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/1408
dc.subjectAstrophysics
dc.titleYoung Stellar Groups, Runaway Stars, and Pulsars
dc.typetext

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