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dc.contributor.authorKastner, Joelen_US
dc.contributor.authorRichmond, Michaelen_US
dc.contributor.authorGrosso, Nicolasen_US
dc.contributor.authorWeintraub, Daviden_US
dc.contributor.authorSimon, Theodoreen_US
dc.contributor.authorFrank, Adamen_US
dc.contributor.authorHamaguchi, Kenjien_US
dc.contributor.authorOzawa, Hidekien_US
dc.contributor.authorHenden, Arneen_US
dc.identifier.citationNature 430 (2004) 429-431en_US
dc.descriptionRIT community members may access full-text via RIT Libraries licensed databases:
dc.description.abstractYoung, low-mass stars are luminous X-ray sources1 whose powerful X-ray flares^(2-6) may exert a profound influence over the process of planet formation^(7). The origin of such emission is uncertain. Although many or perhaps most recently formed, low-mass stars emit X-rays as a consequence of solar-like coronal activity^(1,8,9), it has also been suggested that X-ray emission may be a direct result of mass accretion onto the forming star^(10-12). Here we report X-ray imaging spectroscopy observations which reveal a factor ~50 increase in the X-ray flux from a young star that is presently undergoing a spectacular optical/IR outburst^(13,14). The outburst is thought to be due to the sudden onset of a phase of rapid accretion^(14-16). The coincidence of a surge in X-ray brightness with the optical/IR eruption demonstrates that strongly enhanced high-energy emission from young stars can occur as a consequence of high accretion rates. We suggest that such accretion enhanced X-ray emission from erupting young stars may be short-lived, because intense star-disk magnetospheric interactions are quenched rapidly by the subsequent accretion flood (Refer to PDF file for exact formulas).en_US
dc.description.sponsorshipCXO observations of the erupting object in L1630 acquired in March 2004 were obtained under allocations of CXC Director’s Discretionary Time. XSPEC software is maintained by NASA’s High Energy Astrophysics Science Archive Research Center. The archival optical image in Fig. 2 was obtained with ESO’s VLTat the Paranal Observatories under program ID 272.C-5045. We thank B. L. Gary for communicating results of I-band monitoring of the source.en_US
dc.format.extent235589 bytesen_US
dc.relation.ispartofseriesvol. 430en_US
dc.relation.ispartofseriesno. 6998en_US
dc.subjectMass accretionen_US
dc.subjectX-rays - outburstsen_US
dc.subjectX-rays - starsen_US
dc.titleAn X-ray outburst from the rapidly accreting young star that illuminates McNeil's Nebulaen_US

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