Magnetic field, activity, and companions of V410 Tau
ABSTRACT We report the analysis, conducted as part of the MaTYSSE programme, of a spectropolarimetric monitoring of the ∼0.8 Myr, ∼1.4 M⊙ disc-less weak-line T Tauri star V410 Tau with the ESPaDOnS instrument at the Canada–France–Hawaii Telescope and NARVAL at the Télescope Bernard Lyot, between 200...
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croxfordunivpr:10.1093/mnras/stz2481 2024-06-09T07:50:13+00:00 Magnetic field, activity, and companions of V410 Tau Yu, L Donati, J-F Grankin, K Collier Cameron, A Moutou, C Hussain, G Baruteau, C Jouve, L MaTYSSE collaboration, the Université Fédérale Toulouse Midi-Pyrénées European Southern Observatory European Research Council 2019 http://dx.doi.org/10.1093/mnras/stz2481 http://academic.oup.com/mnras/advance-article-pdf/doi/10.1093/mnras/stz2481/29603653/stz2481.pdf http://academic.oup.com/mnras/article-pdf/489/4/5556/30068118/stz2481.pdf en eng Oxford University Press (OUP) https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model Monthly Notices of the Royal Astronomical Society volume 489, issue 4, page 5556-5572 ISSN 0035-8711 1365-2966 journal-article 2019 croxfordunivpr https://doi.org/10.1093/mnras/stz2481 2024-05-10T13:14:36Z ABSTRACT We report the analysis, conducted as part of the MaTYSSE programme, of a spectropolarimetric monitoring of the ∼0.8 Myr, ∼1.4 M⊙ disc-less weak-line T Tauri star V410 Tau with the ESPaDOnS instrument at the Canada–France–Hawaii Telescope and NARVAL at the Télescope Bernard Lyot, between 2008 and 2016. With Zeeman-Doppler Imaging, we reconstruct the surface brightness and magnetic field of V410 Tau, and show that the star is heavily spotted and possesses a ∼550 G relatively toroidal magnetic field. We find that V410 Tau features a weak level of surface differential rotation between the equator and pole ∼5 times weaker than the solar differential rotation. The spectropolarimetric data exhibit intrinsic variability, beyond differential rotation, which points towards a dynamo-generated field rather than a fossil field. Long-term variations in the photometric data suggest that spots appear at increasing latitudes over the span of our data set, implying that, if V410 Tau has a magnetic cycle, it would have a period of more than 8 yr. Having derived raw radial velocities (RVs) from our spectra, we filter out the stellar activity jitter, modelled either from our Doppler maps or using Gaussian process regression. Thus filtered, our RVs exclude the presence of a hot Jupiter-mass companion below ∼0.1 au, which is suggestive that hot Jupiter formation may be inhibited by the early depletion of the circumstellar disc, which for V410 Tau may have been caused by the close (few tens of au) M dwarf stellar companion. Article in Journal/Newspaper narval narval Oxford University Press Canada Jupiter ENVELOPE(101.133,101.133,-66.117,-66.117) Monthly Notices of the Royal Astronomical Society 489 4 5556 5572 |
institution |
Open Polar |
collection |
Oxford University Press |
op_collection_id |
croxfordunivpr |
language |
English |
description |
ABSTRACT We report the analysis, conducted as part of the MaTYSSE programme, of a spectropolarimetric monitoring of the ∼0.8 Myr, ∼1.4 M⊙ disc-less weak-line T Tauri star V410 Tau with the ESPaDOnS instrument at the Canada–France–Hawaii Telescope and NARVAL at the Télescope Bernard Lyot, between 2008 and 2016. With Zeeman-Doppler Imaging, we reconstruct the surface brightness and magnetic field of V410 Tau, and show that the star is heavily spotted and possesses a ∼550 G relatively toroidal magnetic field. We find that V410 Tau features a weak level of surface differential rotation between the equator and pole ∼5 times weaker than the solar differential rotation. The spectropolarimetric data exhibit intrinsic variability, beyond differential rotation, which points towards a dynamo-generated field rather than a fossil field. Long-term variations in the photometric data suggest that spots appear at increasing latitudes over the span of our data set, implying that, if V410 Tau has a magnetic cycle, it would have a period of more than 8 yr. Having derived raw radial velocities (RVs) from our spectra, we filter out the stellar activity jitter, modelled either from our Doppler maps or using Gaussian process regression. Thus filtered, our RVs exclude the presence of a hot Jupiter-mass companion below ∼0.1 au, which is suggestive that hot Jupiter formation may be inhibited by the early depletion of the circumstellar disc, which for V410 Tau may have been caused by the close (few tens of au) M dwarf stellar companion. |
author2 |
Université Fédérale Toulouse Midi-Pyrénées European Southern Observatory European Research Council |
format |
Article in Journal/Newspaper |
author |
Yu, L Donati, J-F Grankin, K Collier Cameron, A Moutou, C Hussain, G Baruteau, C Jouve, L MaTYSSE collaboration, the |
spellingShingle |
Yu, L Donati, J-F Grankin, K Collier Cameron, A Moutou, C Hussain, G Baruteau, C Jouve, L MaTYSSE collaboration, the Magnetic field, activity, and companions of V410 Tau |
author_facet |
Yu, L Donati, J-F Grankin, K Collier Cameron, A Moutou, C Hussain, G Baruteau, C Jouve, L MaTYSSE collaboration, the |
author_sort |
Yu, L |
title |
Magnetic field, activity, and companions of V410 Tau |
title_short |
Magnetic field, activity, and companions of V410 Tau |
title_full |
Magnetic field, activity, and companions of V410 Tau |
title_fullStr |
Magnetic field, activity, and companions of V410 Tau |
title_full_unstemmed |
Magnetic field, activity, and companions of V410 Tau |
title_sort |
magnetic field, activity, and companions of v410 tau |
publisher |
Oxford University Press (OUP) |
publishDate |
2019 |
url |
http://dx.doi.org/10.1093/mnras/stz2481 http://academic.oup.com/mnras/advance-article-pdf/doi/10.1093/mnras/stz2481/29603653/stz2481.pdf http://academic.oup.com/mnras/article-pdf/489/4/5556/30068118/stz2481.pdf |
long_lat |
ENVELOPE(101.133,101.133,-66.117,-66.117) |
geographic |
Canada Jupiter |
geographic_facet |
Canada Jupiter |
genre |
narval narval |
genre_facet |
narval narval |
op_source |
Monthly Notices of the Royal Astronomical Society volume 489, issue 4, page 5556-5572 ISSN 0035-8711 1365-2966 |
op_rights |
https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model |
op_doi |
https://doi.org/10.1093/mnras/stz2481 |
container_title |
Monthly Notices of the Royal Astronomical Society |
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489 |
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4 |
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5556 |
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5572 |
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