Modeling of large-scale disk perturbation eclipses of UX Ori stars with the puffed-up inner disks
Eclipses of UX Ori stars by compact gas–dust clouds and large-scale circumstellar disk perturbations are modeled. A flared disk and a disk with a puffing-up in the dust sublimation zone are considered. The disk puffing-up explains several observed features of eclipses. The linear polarization degree...
| Main Authors: | , |
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| Format: | Article |
| Language: | English |
| Published: |
De Gruyter
2022-02-01
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| Series: | Open Astronomy |
| Subjects: | |
| Online Access: | https://doi.org/10.1515/astro-2022-0010 |
| _version_ | 1811203750648348672 |
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| author | Shulman Sergey Grinin Vladimir |
| author_facet | Shulman Sergey Grinin Vladimir |
| author_sort | Shulman Sergey |
| collection | DOAJ |
| description | Eclipses of UX Ori stars by compact gas–dust clouds and large-scale circumstellar disk perturbations are modeled. A flared disk and a disk with a puffing-up in the dust sublimation zone are considered. The disk puffing-up explains several observed features of eclipses. The linear polarization degree can remain unchanged during the eclipse. There might be no star reddening in the blue and ultraviolet spectral regions. Strong changes (up to 90°90\text{°}) in the positional angle of the linear polarization may happen when passing from one spectral band to another. An eclipse by a large-scale disk perturbation can be noticeably deeper than an eclipse by a compact gas–dust cloud. The polarization degree in such an eclipse can also be significantly higher. In addition, an eclipse by a large-scale perturbation of a star with a puffed-up disk explains the significant scatter of eclipse parameters at the same fading level. A significant change in the positional angle of the linear polarization may occur during a large-scale disk perturbation eclipse minimum and after it. We attempted parametric identification of long-lasted deep minima of UX Ori and WW Vul. The considered simple model can only partially explain the observed phenomena and need further development. |
| first_indexed | 2024-04-12T03:00:28Z |
| format | Article |
| id | doaj.art-30bd35b2553b4ee78d2dd49fc363e827 |
| institution | Directory Open Access Journal |
| issn | 2543-6376 |
| language | English |
| last_indexed | 2024-04-12T03:00:28Z |
| publishDate | 2022-02-01 |
| publisher | De Gruyter |
| record_format | Article |
| series | Open Astronomy |
| spelling | doaj.art-30bd35b2553b4ee78d2dd49fc363e8272022-12-22T03:50:40ZengDe GruyterOpen Astronomy2543-63762022-02-01311677910.1515/astro-2022-0010Modeling of large-scale disk perturbation eclipses of UX Ori stars with the puffed-up inner disksShulman Sergey0Grinin Vladimir1Mathematics & Mechanics Faculty, St. Petersburg State University, Universitetskii pr. 28, St. Petersburg, 198504, RussiaMathematics & Mechanics Faculty, St. Petersburg State University, Universitetskii pr. 28, St. Petersburg, 198504, RussiaEclipses of UX Ori stars by compact gas–dust clouds and large-scale circumstellar disk perturbations are modeled. A flared disk and a disk with a puffing-up in the dust sublimation zone are considered. The disk puffing-up explains several observed features of eclipses. The linear polarization degree can remain unchanged during the eclipse. There might be no star reddening in the blue and ultraviolet spectral regions. Strong changes (up to 90°90\text{°}) in the positional angle of the linear polarization may happen when passing from one spectral band to another. An eclipse by a large-scale disk perturbation can be noticeably deeper than an eclipse by a compact gas–dust cloud. The polarization degree in such an eclipse can also be significantly higher. In addition, an eclipse by a large-scale perturbation of a star with a puffed-up disk explains the significant scatter of eclipse parameters at the same fading level. A significant change in the positional angle of the linear polarization may occur during a large-scale disk perturbation eclipse minimum and after it. We attempted parametric identification of long-lasted deep minima of UX Ori and WW Vul. The considered simple model can only partially explain the observed phenomena and need further development.https://doi.org/10.1515/astro-2022-0010radiative transferstars: variables: t tauriherbig ae/becircumstellar matterpolarization |
| spellingShingle | Shulman Sergey Grinin Vladimir Modeling of large-scale disk perturbation eclipses of UX Ori stars with the puffed-up inner disks Open Astronomy radiative transfer stars: variables: t tauri herbig ae/be circumstellar matter polarization |
| title | Modeling of large-scale disk perturbation eclipses of UX Ori stars with the puffed-up inner disks |
| title_full | Modeling of large-scale disk perturbation eclipses of UX Ori stars with the puffed-up inner disks |
| title_fullStr | Modeling of large-scale disk perturbation eclipses of UX Ori stars with the puffed-up inner disks |
| title_full_unstemmed | Modeling of large-scale disk perturbation eclipses of UX Ori stars with the puffed-up inner disks |
| title_short | Modeling of large-scale disk perturbation eclipses of UX Ori stars with the puffed-up inner disks |
| title_sort | modeling of large scale disk perturbation eclipses of ux ori stars with the puffed up inner disks |
| topic | radiative transfer stars: variables: t tauri herbig ae/be circumstellar matter polarization |
| url | https://doi.org/10.1515/astro-2022-0010 |
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