FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W4386163940> ?p ?o ?g. }

• W4386163940 endingPage "A86" @default.
• W4386163940 startingPage "A86" @default.
• W4386163940 abstract "Context. Classical T Tauri stars are thought to accrete material from their surrounding protoplanetary disks through funnel flows along their magnetic field lines. The classical T Tauri stars with high accretion rates (∼10 −7 M ⊙ yr −1 ) are ideal targets for testing this magnetospheric accretion scenario in a sustained regime. Aims. We constrained the accretion-ejection phenomena around the strongly accreting northern component of the S CrA young binary system (S CrA N) by deriving its magnetic field topology and its magnetospheric properties, and by detecting ejection signatures, if any. Methods. We led a two-week observing campaign on S CrA N with the ESPaDOnS optical spectropolarimeter at the Canada-France-Hawaii Telescope. We recorded 12 Stokes I and V spectra over 14 nights. We computed the corresponding least-squares deconvolution (LSD) profiles of the photospheric lines and performed Zeeman-Doppler imaging (ZDI). We analyzed the kinematics of noticeable emission lines, namely He I λ 5876 and the first four lines of the Balmer series, which are known to trace the accretion process. Results. We found that S CrA N is a low-mass (0.8 M ⊙ ) young (∼1 Myr) and fully convective object exhibiting strong and variable veiling (with a mean value of 7 ± 2), which suggests that the star is in a strong accretion regime. These findings could indicate a stellar evolutionary stage between Class I and Class II for S CrA N. We reconstructed an axisymmetric large-scale magnetic field (∼70% of the total energy) that is primarily located in the dipolar component, but has significant higher poloidal orders. From the narrow emission component radial velocity curve of He I λ 5876, we derived a stellar rotation period of P * = 7.3 ± 0.2 days. We found a magnetic truncation radius of ∼2 R * which is significantly closer to the star than the corotation radius of ∼6 R * , suggesting that S CrA N is in an unstable accretion regime. That the truncation radius is quite smaller than the size of the Br γ line emitting region, as measured with the GRAVITY interferometer (∼8 R * ), supports the presence of outflows, which is nicely corroborated by the line profiles presented in this work. Conclusions. The findings from spectropolarimetry are complementary to those provided by optical long-baseline interferometry, allowing us to construct a coherent view of the innermost regions of a young, strongly accreting star. The strong and complex magnetic field reconstructed for S CrA N is inconsistent with the observed magnetic signatures of the emission lines associated with the postshock region, however. We recommend a multitechnique synchronized campaign of several days to place more constrains on a system that varies on a timescale of about one day." @default.
• W4386163940 created "2023-08-26" @default.
• W4386163940 creator A5003303261 @default.
• W4386163940 creator A5015052564 @default.
• W4386163940 creator A5019246734 @default.
• W4386163940 creator A5026728474 @default.
• W4386163940 creator A5027753647 @default.
• W4386163940 creator A5033455882 @default.
• W4386163940 creator A5034866899 @default.
• W4386163940 creator A5037992182 @default.
• W4386163940 creator A5038720230 @default.
• W4386163940 creator A5038791583 @default.
• W4386163940 creator A5040642427 @default.
• W4386163940 creator A5044901272 @default.
• W4386163940 creator A5087374232 @default.
• W4386163940 creator A5089576682 @default.
• W4386163940 date "2023-10-01" @default.
• W4386163940 modified "2023-10-12" @default.
• W4386163940 title "Star-disk interactions in the strongly accreting T Tauri star S CrA N" @default.
• W4386163940 cites W1578951559 @default.
• W4386163940 cites W1642880642 @default.
• W4386163940 cites W1963670682 @default.
• W4386163940 cites W1972226679 @default.
• W4386163940 cites W1978391636 @default.
• W4386163940 cites W1979546591 @default.
• W4386163940 cites W1990494221 @default.
• W4386163940 cites W2003095861 @default.
• W4386163940 cites W2003639536 @default.
• W4386163940 cites W2011924956 @default.
• W4386163940 cites W2012894249 @default.
• W4386163940 cites W2015914151 @default.
• W4386163940 cites W2026679688 @default.
• W4386163940 cites W2027542103 @default.
• W4386163940 cites W2030435803 @default.
• W4386163940 cites W2047398779 @default.
• W4386163940 cites W2051850553 @default.
• W4386163940 cites W2053680061 @default.
• W4386163940 cites W2053987082 @default.
• W4386163940 cites W2055069090 @default.
• W4386163940 cites W2068843564 @default.
• W4386163940 cites W2070531397 @default.
• W4386163940 cites W2072218578 @default.
• W4386163940 cites W2074756552 @default.
• W4386163940 cites W2078188791 @default.
• W4386163940 cites W2091403096 @default.
• W4386163940 cites W2114515137 @default.
• W4386163940 cites W2129661673 @default.
• W4386163940 cites W2147364630 @default.
• W4386163940 cites W2167902545 @default.
• W4386163940 cites W2167911977 @default.
• W4386163940 cites W2170814103 @default.
• W4386163940 cites W2221977688 @default.
• W4386163940 cites W2511160231 @default.
• W4386163940 cites W2612686510 @default.
• W4386163940 cites W2768824768 @default.
• W4386163940 cites W2780773861 @default.
• W4386163940 cites W2953580156 @default.
• W4386163940 cites W2979352650 @default.
• W4386163940 cites W2991571672 @default.
• W4386163940 cites W3081754461 @default.
• W4386163940 cites W3087703040 @default.
• W4386163940 cites W3098088122 @default.
• W4386163940 cites W3099667223 @default.
• W4386163940 cites W3099799282 @default.
• W4386163940 cites W3099807012 @default.
• W4386163940 cites W3100150643 @default.
• W4386163940 cites W3100511326 @default.
• W4386163940 cites W3100985338 @default.
• W4386163940 cites W3102346326 @default.
• W4386163940 cites W3102637606 @default.
• W4386163940 cites W3102671280 @default.
• W4386163940 cites W3103060636 @default.
• W4386163940 cites W3103211289 @default.
• W4386163940 cites W3105112239 @default.
• W4386163940 cites W3105419345 @default.
• W4386163940 cites W3105607527 @default.
• W4386163940 cites W3106061258 @default.
• W4386163940 cites W3138636731 @default.
• W4386163940 cites W3140110770 @default.
• W4386163940 cites W3143071818 @default.
• W4386163940 cites W3152845924 @default.
• W4386163940 cites W3174201118 @default.
• W4386163940 cites W3198407191 @default.
• W4386163940 cites W3203180205 @default.
• W4386163940 cites W3209462728 @default.
• W4386163940 cites W4281694390 @default.
• W4386163940 cites W4288083755 @default.
• W4386163940 cites W4290079606 @default.
• W4386163940 cites W4292309267 @default.
• W4386163940 cites W4292399985 @default.
• W4386163940 cites W4292403025 @default.
• W4386163940 cites W4309879471 @default.
• W4386163940 cites W4313646725 @default.
• W4386163940 cites W4380590566 @default.
• W4386163940 doi "https://doi.org/10.1051/0004-6361/202347145" @default.
• W4386163940 hasPublicationYear "2023" @default.
• W4386163940 type Work @default.
• W4386163940 citedByCount "0" @default.

• next