X-ray emission from Orion Nebula Cluster stars with circumstellar disks and jets

Show simple item record

dc.contributor.author Kastner, Joel en_US
dc.contributor.author Franz, Geoffrey en_US
dc.contributor.author Grosso, Nicolas en_US
dc.contributor.author Bally, John en_US
dc.contributor.author McCaughrean, Mark en_US
dc.contributor.author Getman, Konstantin en_US
dc.contributor.author Feigelson, Eric en_US
dc.contributor.author Schulz, Norbert en_US
dc.date.accessioned 2006-05-18T18:46:04Z en_US
dc.date.available 2006-05-18T18:46:04Z en_US
dc.date.issued 2005-10 en_US
dc.identifier.citation Astrophys.J.S. 160 (2005) 511-529 en_US
dc.identifier.issn 1538-4365 en_US
dc.identifier.uri http://hdl.handle.net/1850/1822 en_US
dc.description Also archived in: arXiv: astro-ph/0506650 v1 27 Jun 2005 en_US
dc.description.abstract We investigate the X-ray and near-infrared emission properties of a sample of pre-main sequence (PMS) stellar systems in the Orion Nebula Cluster (ONC) that display evidence for circumstellar disks (“proplyds”) and optical jets in Hubble Space Telescope (HST) imaging. Our study uses X-ray data acquired during Chandra Orion Ultradeep Program (COUP) observations, as well as complementary optical and near-infrared data recently acquired with HST and the Very Large Telescope (VLT), respectively. Approximately 70% of ~140 proplyds were detected as X-ray sources in the 838 ks COUP observation of the ONC, including ~25% of proplyds that do not display central stars in HST imaging. In nearinfrared imaging, the detection rate of proplyd central stars is > 90%. Many proplyds display near-infrared excesses, suggesting disk accretion is ongoing onto the central, PMS stars. About 50% of circumstellar disks that are detected in absorption in HST imaging contain X-ray sources. For these sources, we find that X-ray absorbing column and apparent disk inclination are well correlated, providing insight into the disk scale heights and metal abundances of UV- and X-ray-irradiated protoplanetary disks. Approximately 2/3 of the ~30 proplyds and PMS stars exhibiting jets in Hubble images have COUP X-ray counterparts. These jet sources display some of the largest near-infrared excesses among the proplyds, suggesting that the origin of the jets is closely related to ongoing, PMS stellar accretion. One morphologically complex jet source, d181–825, displays a double-peaked X-ray spectral energy distribution with a prominent soft component that is indicative of strong shocks in the jet collimation region. A handful of similar objects also display X-ray spectra that are suggestive of shocks near the jet source. These results support models in which circumstellar disks collimate and/or launch jets from young stellar objects and, furthermore, demonstrate that star-disk-jet interactions may contribute to PMS X-ray emission (Refer to PDF file for exact formulas). en_US
dc.description.sponsorship COUP is supported by Chandra Guest Observer grant SAO GO3-4009A (E. D. Feigelson, PI) as well as by the Chandra ACIS Team contract NAS8-38252. Additional support for the work described in this paper was provided by Chandra Guest Observer grant GO4-5012X to RIT. en_US
dc.format.extent 546712 bytes en_US
dc.format.mimetype application/pdf en_US
dc.language.iso en_US en_US
dc.publisher Astrophysical Journal Supplement en_US
dc.relation RIT Scholars content from RIT Digital Media Library has moved from http://ritdml.rit.edu/handle/1850/1822 to RIT Scholar Works http://scholarworks.rit.edu/article/862, please update your feeds & links!
dc.relation.ispartofseries vol. 160 en_US
dc.relation.ispartofseries no. 2 en_US
dc.subject Circumstellar matter en_US
dc.subject ISM - Herbig-Haro objects en_US
dc.subject Open clusters and associations - individual (Orion Nebula Cluster) en_US
dc.subject Planetary systems - protoplanetary disks en_US
dc.subject Stars - pre-main sequence en_US
dc.subject X-rays - stars en_US
dc.title X-ray emission from Orion Nebula Cluster stars with circumstellar disks and jets en_US
dc.type Article en_US

Files in this item

Files Size Format View
JKastnerArticle10-2005.pdf 546.7Kb PDF View/Open

This item appears in the following Collection(s)

Show simple item record

Search RIT DML

Advanced Search