Parsec-scale X-ray Flows in High-mass Star-forming Regions

Simple item page
dc.creatorTownsley, L.
dc.creatorFeigelson, E.
dc.creatorMontmerle, T.
dc.creatorBroos, P.
dc.creatorChu, Y. -H.
dc.creatorGarmire, G.
dc.creatorGetman, K.
dc.date2004-06-15
dc.date.accessioned2026-07-07T02:13:32Z
dc.date.available2026-07-07T02:13:32Z
dc.descriptionWe present Chandra/ACIS images of several high-mass star-forming regions. The massive stellar clusters powering these HII regions are resolved at the arcsecond level into hundreds of stellar sources, similar to those seen in closer young stellar clusters. However, we also detect diffuse X-ray emission on parsec scales that is spatially and spectrally distinct from the point source population. For nearby regions (e.g. M17 and Rosette) the emission is soft, with plasma temperatures less than 10 million degrees, in contrast to what is seen in more distant complexes (e.g. RCW49, W51). This extended emission most likely arises from the fast O-star winds thermalized either by wind-wind collisions or by a termination shock against the surrounding media. We have established that only a small portion of the wind energy and mass appears in the observed diffuse X-ray plasma; in the blister HII regions, we suspect that most of it flows without cooling into the low-density interstellar medium through blow-outs or fissures in the surrounding neutral material. These data provide compelling observational evidence that strong wind shocks are present in HII regions.
dc.description10 pages, 14 figures, to appear in the Proceedings of "X-Ray and Radio Connections," Santa Fe, NM, 3-6 February, 2004
dc.identifierhttps://arxiv.org/abs/astro-ph/0406349
dc.identifierhttp://arxiv.org/abs/astro-ph/0406349
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/7845
dc.subjectAstrophysics
dc.titleParsec-scale X-ray Flows in High-mass Star-forming Regions
dc.typetext

Files

Collections

arXiv