X-ray emission line profile modeling of hot stars
نویسندگان
چکیده
منابع مشابه
Modeling O-Star X-Ray Emission-Line Profiles
X-ray emission from hot (Oand B-type) stars is a long-standing astrophysical puzzle. High-resolution x-ray spectroscopy of hot stars resolves emission line profile shapes, offering direct insight into the dynamics and spatial distribution of the x-ray-emitting plasma. The O supergiant ζ Puppis shows broad, blueshifted, and asymmetric line profiles, generally consistent with the wind-shock pictu...
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We have modelled the X-ray emission of T Tauri stars assuming that they have isothermal, magnetically-confined coronae. These coronae extend outwards until either the pressure of the hot coronal gas overcomes the magnetic field, or, if the corona interacts with a disk before this happens, by the action of the disk itself. This work is motivated by the results of the Chandra Orion Ultradeep Proj...
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Young O stars are strong, hard, and variable X-ray sources; properties that strongly affect their circumstellar and galactic environments. After ≈ 1 Myr, these stars settle down to become steady sources of soft X-rays. I will use high-resolution X-ray spectroscopy and MHD modeling to show that young O stars like θ Ori C are well explained by the magnetically channeled wind shock scenario. After...
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We present new optical and X-ray observations to show that the X-ray source 1WGA J1346.5−6255 previously associated with the SNR G309.2-0.6 can be unequivocally identified with the emission line star HD 119682 located in the foreground open cluster NGC 5281. Images from Chandra in the X-ray band as well as from Magellan in the narrow optical Hα band show a coincidence of the source positions wi...
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ژورنال
عنوان ژورنال: Review of Scientific Instruments
سال: 2003
ISSN: 0034-6748,1089-7623
DOI: 10.1063/1.1535240