Doppler images of V1358 Ori
Abstract We present Doppler images of the active dwarf star V1358 Ori using high-resolution spectra from the NARVAL spectropolarimeter mounted on the Bernard Lyot Telescope. The spectra were taken between 09-20 Dec, 2013 with a resolution of R=80000. Doppler imaging was carried out with our new gene...
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Online Access: | http://dx.doi.org/10.1017/s1743921319003855 https://www.cambridge.org/core/services/aop-cambridge-core/content/view/S1743921319003855 |
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crcambridgeupr:10.1017/s1743921319003855 2023-05-15T18:50:47+02:00 Doppler images of V1358 Ori Kriskovics, Levente Kövári, Zsolt Vida, Krisztián Oláh, Katalin Carroll, Thorsten A. 2018 http://dx.doi.org/10.1017/s1743921319003855 https://www.cambridge.org/core/services/aop-cambridge-core/content/view/S1743921319003855 en eng Cambridge University Press (CUP) https://www.cambridge.org/core/terms Proceedings of the International Astronomical Union volume 14, issue A30, page 135-135 ISSN 1743-9213 1743-9221 Astronomy and Astrophysics Space and Planetary Science journal-article 2018 crcambridgeupr https://doi.org/10.1017/s1743921319003855 2022-04-07T08:05:10Z Abstract We present Doppler images of the active dwarf star V1358 Ori using high-resolution spectra from the NARVAL spectropolarimeter mounted on the Bernard Lyot Telescope. The spectra were taken between 09-20 Dec, 2013 with a resolution of R=80000. Doppler imaging was carried out with our new generation multi-line Dopper imaging code iMap (Carroll et al. 2012). 40 individual photospheric lines were selected by line depth, temperature sensitivity and blends. Two data subsets were formed to get two consecutive Doppler images. Prominent cool spots at lower latitudes are found on both maps. At 0.5 phase there is a prominent equatorial feature on both maps. Weaker polar features can be seen on the first map, which somewhat diminishes for the second map. On the first image there is a cool surface feature at 30 degrees latitude which seems to fade greatly on the second map. Around 0.75 phase, a new spot seems to form. These changes suggest a rapid surface evolution. Spot displacements may also indicate surface differential rotation, which was derived by cross-correlating the two subsequent Doppler images (see e.g. Kővári et al. 2012). We fit the latitudinal correlation peaks with a sine-squared law. The fit suggests solar-type surface differential rotation with a shear parameter of α=0.02±0.02. The shear parameter fits the ${P_{{\rm{rot}}}} - |\alpha | $ diagram in Kővári et al. (2017) quite well. Article in Journal/Newspaper narval narval Cambridge University Press (via Crossref) Proceedings of the International Astronomical Union 14 A30 135 135 |
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Open Polar |
collection |
Cambridge University Press (via Crossref) |
op_collection_id |
crcambridgeupr |
language |
English |
topic |
Astronomy and Astrophysics Space and Planetary Science |
spellingShingle |
Astronomy and Astrophysics Space and Planetary Science Kriskovics, Levente Kövári, Zsolt Vida, Krisztián Oláh, Katalin Carroll, Thorsten A. Doppler images of V1358 Ori |
topic_facet |
Astronomy and Astrophysics Space and Planetary Science |
description |
Abstract We present Doppler images of the active dwarf star V1358 Ori using high-resolution spectra from the NARVAL spectropolarimeter mounted on the Bernard Lyot Telescope. The spectra were taken between 09-20 Dec, 2013 with a resolution of R=80000. Doppler imaging was carried out with our new generation multi-line Dopper imaging code iMap (Carroll et al. 2012). 40 individual photospheric lines were selected by line depth, temperature sensitivity and blends. Two data subsets were formed to get two consecutive Doppler images. Prominent cool spots at lower latitudes are found on both maps. At 0.5 phase there is a prominent equatorial feature on both maps. Weaker polar features can be seen on the first map, which somewhat diminishes for the second map. On the first image there is a cool surface feature at 30 degrees latitude which seems to fade greatly on the second map. Around 0.75 phase, a new spot seems to form. These changes suggest a rapid surface evolution. Spot displacements may also indicate surface differential rotation, which was derived by cross-correlating the two subsequent Doppler images (see e.g. Kővári et al. 2012). We fit the latitudinal correlation peaks with a sine-squared law. The fit suggests solar-type surface differential rotation with a shear parameter of α=0.02±0.02. The shear parameter fits the ${P_{{\rm{rot}}}} - |\alpha | $ diagram in Kővári et al. (2017) quite well. |
format |
Article in Journal/Newspaper |
author |
Kriskovics, Levente Kövári, Zsolt Vida, Krisztián Oláh, Katalin Carroll, Thorsten A. |
author_facet |
Kriskovics, Levente Kövári, Zsolt Vida, Krisztián Oláh, Katalin Carroll, Thorsten A. |
author_sort |
Kriskovics, Levente |
title |
Doppler images of V1358 Ori |
title_short |
Doppler images of V1358 Ori |
title_full |
Doppler images of V1358 Ori |
title_fullStr |
Doppler images of V1358 Ori |
title_full_unstemmed |
Doppler images of V1358 Ori |
title_sort |
doppler images of v1358 ori |
publisher |
Cambridge University Press (CUP) |
publishDate |
2018 |
url |
http://dx.doi.org/10.1017/s1743921319003855 https://www.cambridge.org/core/services/aop-cambridge-core/content/view/S1743921319003855 |
genre |
narval narval |
genre_facet |
narval narval |
op_source |
Proceedings of the International Astronomical Union volume 14, issue A30, page 135-135 ISSN 1743-9213 1743-9221 |
op_rights |
https://www.cambridge.org/core/terms |
op_doi |
https://doi.org/10.1017/s1743921319003855 |
container_title |
Proceedings of the International Astronomical Union |
container_volume |
14 |
container_issue |
A30 |
container_start_page |
135 |
op_container_end_page |
135 |
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1766244545782087680 |