期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 379, 期 1, 页码 L35-L39出版社
OXFORD UNIV PRESS
DOI: 10.1111/j.1745-3933.2007.00328.x
关键词
stars : activity; stars : coronae; stars : magnetic fields; stars : pre-main sequence; X-rays : stars
资金
- Science and Technology Facilities Council [PP/D000890/1] Funding Source: researchfish
- STFC [PP/D000890/1] Funding Source: UKRI
Accreting T Tauri stars are observed to be less luminous in X-rays than non-accretors, an effect that has been detected in various star-forming regions. To explain this we have combined, for the first time, a radiative transfer code with an accretion model that considers magnetic fields extrapolated from surface magnetograms obtained from Zeeman-Doppler imaging. Such fields consist of compact magnetic regions close to the stellar surface, with extended field lines interacting with the disc. We study the propagation of coronal X-rays through the magnetosphere and demonstrate that they are strongly absorbed by the dense gas in accretion columns. The reduction in the observed X-ray emission depends on the field geometry, which may explain why accreting T Tauri stars show a larger scatter in their observed X-ray luminosity compared with non-accreting stars.
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