On the causes of brightness variability of the young star BP Tau
Fuente:
arXiv
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| Autori principali: | , , , , , , , , |
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| Natura: | Preprint |
| Pubblicazione: |
2025
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| _version_ | 1866910910562435072 |
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| author | Burlak, M. A. Grankin, K. N. Dodin, A. V. Zharova, A. V. Ikonnikova, N. P. Kiryukhina, V. A. Lamzin, S. A. Safonov, B. S. Strakhov, I. A. |
| author_facet | Burlak, M. A. Grankin, K. N. Dodin, A. V. Zharova, A. V. Ikonnikova, N. P. Kiryukhina, V. A. Lamzin, S. A. Safonov, B. S. Strakhov, I. A. |
| contents | We have constructed and analysed the secular light curve of BP Tau, a classical T Tauri-type star. Wave-like variations in the average brightness were detected, with an amplitude of $ΔB\approx 0.2$ and characteristic time-scales of several decades. We argue that three deep dimming events $(ΔB \sim 1.5)$, lasting from 1 hour to several days, are caused by the eclipse of a hot (accretion) spot by dust falling onto the star together with gas. Such eclipses, albeit with smaller amplitudes, may explain the absence of a strictly defined periodicity in the brightness variations of BP Tau associated with axial rotation. We also show that within the distance range of 0.1 to 200 AU, BP Tau does not have a companion with a mass exceeding 0.2M$_\odot.$ The causes of brightness and colour index variations on different time-scales are discussed. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_09290 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | On the causes of brightness variability of the young star BP Tau Burlak, M. A. Grankin, K. N. Dodin, A. V. Zharova, A. V. Ikonnikova, N. P. Kiryukhina, V. A. Lamzin, S. A. Safonov, B. S. Strakhov, I. A. Solar and Stellar Astrophysics We have constructed and analysed the secular light curve of BP Tau, a classical T Tauri-type star. Wave-like variations in the average brightness were detected, with an amplitude of $ΔB\approx 0.2$ and characteristic time-scales of several decades. We argue that three deep dimming events $(ΔB \sim 1.5)$, lasting from 1 hour to several days, are caused by the eclipse of a hot (accretion) spot by dust falling onto the star together with gas. Such eclipses, albeit with smaller amplitudes, may explain the absence of a strictly defined periodicity in the brightness variations of BP Tau associated with axial rotation. We also show that within the distance range of 0.1 to 200 AU, BP Tau does not have a companion with a mass exceeding 0.2M$_\odot.$ The causes of brightness and colour index variations on different time-scales are discussed. |
| title | On the causes of brightness variability of the young star BP Tau |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2504.09290 |