Spectral Variability of the Star HD 141569A
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arXiv
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| Main Authors: | , , , |
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| Format: | Preprint |
| Published: |
2026
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| _version_ | 1866914268708864000 |
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| author | Adigozalzade, H. N. Ismailov, N. Z. Bashirova, U. Z. Alishov, S. A. |
| author_facet | Adigozalzade, H. N. Ismailov, N. Z. Bashirova, U. Z. Alishov, S. A. |
| contents | The paper presents the results of long-term homogeneous spectroscopic studies of the Herbig Ae/Be star HD 141569A obtained in the optical range. We detect spectral variability on timescales of months to years, including changes in the spectrophotometric parameters of the Halpha emission line, as well as other hydrogen absorption lines. Based on the derived physical parameters and age, the star appears to be in a transitional evolutionary stage from a protoplanetary disk to a debris disk. We determine that the star axial rotation period is approximately 12 hours, and its equatorial velocity is significantly below the critical rotation velocity. The observed spectral variability is likely caused by partial obscuration of the central star radiation by extended fragments of the disrupted disk. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2601_14539 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Spectral Variability of the Star HD 141569A Adigozalzade, H. N. Ismailov, N. Z. Bashirova, U. Z. Alishov, S. A. Solar and Stellar Astrophysics 85A04, 85A05 F.2.2; I.2.7 The paper presents the results of long-term homogeneous spectroscopic studies of the Herbig Ae/Be star HD 141569A obtained in the optical range. We detect spectral variability on timescales of months to years, including changes in the spectrophotometric parameters of the Halpha emission line, as well as other hydrogen absorption lines. Based on the derived physical parameters and age, the star appears to be in a transitional evolutionary stage from a protoplanetary disk to a debris disk. We determine that the star axial rotation period is approximately 12 hours, and its equatorial velocity is significantly below the critical rotation velocity. The observed spectral variability is likely caused by partial obscuration of the central star radiation by extended fragments of the disrupted disk. |
| title | Spectral Variability of the Star HD 141569A |
| topic | Solar and Stellar Astrophysics 85A04, 85A05 F.2.2; I.2.7 |
| url | https://arxiv.org/abs/2601.14539 |