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| Main Authors: | , , , , |
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| Format: | Artículo Open Access |
| Published: |
Wiley
2024
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| Online Access: | https://onlinelibrary.wiley.com/doi/10.1002/asna.20249013 |
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| _version_ | 1867008105148055552 |
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| author | Manfred Küker S. P. Järvinen S. Hubrig Ilya Ilyin M. Schöller |
| author_facet | Manfred Küker S. P. Järvinen S. Hubrig Ilya Ilyin M. Schöller Manfred Küker S. P. Järvinen S. Hubrig Ilya Ilyin M. Schöller |
| collection | Wiley Open Access |
| contents | Cover Picture: Astron. Nachr. 4/2024 Manfred Küker S. P. Järvinen S. Hubrig Ilya Ilyin M. Schöller Astronomische Nachrichten Variability of the Hα emission line profile of the magnetic O‐type star HD 54897 over one decade, from 2014 to 2024. In the left panels, each profile is plotted with a different color as is indicated in the legend, showing the corresponding observing date and instrument used: H: HARPS, E: ESPaDOnS, U: UVES, and P: PEPSI. The upper panel shows the profiles based on the spectra observed recently, while the bottom panel shows all available profiles published previously. The right panel shows the same data in a color scale plot. The red color corresponds to the strongest emission, while the blue color shows the Hα line wings appearing in absorption. The observed Hα emission is thought to originatein a disk of increased gas density in the equatorial plane of the magnetic field. For details see the article by Küker et al., this issue, e230169. image 10.1002/asna.20249013 http://onlinelibrary.wiley.com/termsAndConditions#vor |
| doi_str_mv | 10.1002/asna.20249013 |
| format | Artículo Open Access |
| id | wiley_oa_10_1002_asna_20249013 |
| institution | Wiley Open Access |
| license_str_mv | http://onlinelibrary.wiley.com/termsAndConditions#vor |
| publishDate | 2024 |
| publisher | Wiley |
| record_format | wiley_oa |
| spellingShingle | Cover Picture: Astron. Nachr. 4/2024 Manfred Küker S. P. Järvinen S. Hubrig Ilya Ilyin M. Schöller Astronomische Nachrichten Cover Picture: Astron. Nachr. 4/2024 Manfred Küker S. P. Järvinen S. Hubrig Ilya Ilyin M. Schöller Astronomische Nachrichten Variability of the Hα emission line profile of the magnetic O‐type star HD 54897 over one decade, from 2014 to 2024. In the left panels, each profile is plotted with a different color as is indicated in the legend, showing the corresponding observing date and instrument used: H: HARPS, E: ESPaDOnS, U: UVES, and P: PEPSI. The upper panel shows the profiles based on the spectra observed recently, while the bottom panel shows all available profiles published previously. The right panel shows the same data in a color scale plot. The red color corresponds to the strongest emission, while the blue color shows the Hα line wings appearing in absorption. The observed Hα emission is thought to originatein a disk of increased gas density in the equatorial plane of the magnetic field. For details see the article by Küker et al., this issue, e230169. image 10.1002/asna.20249013 http://onlinelibrary.wiley.com/termsAndConditions#vor |
| title | Cover Picture: Astron. Nachr. 4/2024 |
| topic | Astronomische Nachrichten |
| url | https://onlinelibrary.wiley.com/doi/10.1002/asna.20249013 |