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| Autori principali: | , , , , , , , |
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| Natura: | Preprint |
| Pubblicazione: |
2024
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| Soggetti: | |
| Accesso online: | https://arxiv.org/abs/2409.19112 |
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| _version_ | 1866915112209612800 |
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| author | Birney, M. Whelan, E. T. Dougados, C. Pascucci, I. Murphy, A. Flores-Rivera, L. Flock, M. Kirwan, A. |
| author_facet | Birney, M. Whelan, E. T. Dougados, C. Pascucci, I. Murphy, A. Flores-Rivera, L. Flock, M. Kirwan, A. |
| contents | The first images of the jet and low velocity component (LVC) from the strongly accreting classical T Tauri star RU Lupi are presented. Adaptive optics assisted spectro-imaging of forbidden emission lines was used. The main aim of the observations was to test the conclusion from a recent spectro-astrometric study that the narrow component of the LVC is tracing an MHD disk wind, and to estimate the mass loss rate in the wind. The structure and morphology of the component supports a wind origin for the NC. An upper limit to the launch radius and semi-opening angle of the wind in [O I]λ6300 emission are estimated to be 2 au and 19° in agreement with MHD wind models for high accretors. The height of the [O I]λ6300 wind emitting region, a key parameter for the derivation of the mass loss rate, is estimated for the first time at approximately 35 au giving M_out = 2.6 x 10^-11 M_sun/yr. When compared to the derived mass accretion rate of M_acc = 1.6 x 10^-7 M_sun/yr, the efficiency in the wind is too low for the wind to be significantly contributing to angular momentum removal. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2409_19112 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Forbidden Emission Line spectro-imaging of the RU Lupi jet and Low Velocity Component Birney, M. Whelan, E. T. Dougados, C. Pascucci, I. Murphy, A. Flores-Rivera, L. Flock, M. Kirwan, A. Solar and Stellar Astrophysics The first images of the jet and low velocity component (LVC) from the strongly accreting classical T Tauri star RU Lupi are presented. Adaptive optics assisted spectro-imaging of forbidden emission lines was used. The main aim of the observations was to test the conclusion from a recent spectro-astrometric study that the narrow component of the LVC is tracing an MHD disk wind, and to estimate the mass loss rate in the wind. The structure and morphology of the component supports a wind origin for the NC. An upper limit to the launch radius and semi-opening angle of the wind in [O I]λ6300 emission are estimated to be 2 au and 19° in agreement with MHD wind models for high accretors. The height of the [O I]λ6300 wind emitting region, a key parameter for the derivation of the mass loss rate, is estimated for the first time at approximately 35 au giving M_out = 2.6 x 10^-11 M_sun/yr. When compared to the derived mass accretion rate of M_acc = 1.6 x 10^-7 M_sun/yr, the efficiency in the wind is too low for the wind to be significantly contributing to angular momentum removal. |
| title | Forbidden Emission Line spectro-imaging of the RU Lupi jet and Low Velocity Component |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2409.19112 |