The eruptive young star IRAS 21204+4913
Fuente:
arXiv
Guardado en:
| Autores principales: | , , , , , , , , , |
|---|---|
| Formato: | Preprint |
| Publicado: |
2026
|
| Materias: | |
| Acceso en línea: | |
| Etiquetas: |
Agregar Etiqueta
Sin Etiquetas, Sea el primero en etiquetar este registro!
|
| _version_ | 1866914383900180480 |
|---|---|
| author | Burlak, M. A. Dodin, A. V. Zharova, A. V. Zheltoukhov, S. G. Ikonnikova, N. P. Lamzin, S. A. Safonov, B. S. Strakhov, I. A. Tatarnikov, A. A. Tatarnikov, A. M. |
| author_facet | Burlak, M. A. Dodin, A. V. Zharova, A. V. Zheltoukhov, S. G. Ikonnikova, N. P. Lamzin, S. A. Safonov, B. S. Strakhov, I. A. Tatarnikov, A. A. Tatarnikov, A. M. |
| contents | The results of photometric, polarimetric, and spectroscopic observations are presented for the young star IRAS 21204+4913, whose visible brightness has increased by $\approx 5^{\rm m}$ since October 2025. The star's absorption spectrum in the $0.36 - 0.75 μ$m range resembles those of A - F giants and supergiants, but it also exhibits molecular TiO bands. The brightening was accompanied by a significant increase in the degree of polarization of the stellar radiation (to $\approx 16 \%$ in the I-band), likely due to scattering by dust in an expanding circumstellar shell. The P Cygni profile of the H$α$ line implies a dusty wind velocity of $\approx 300$ km/s. We believe that the outburst of IRAS 21204+4913 is caused by an increase in the accretion rate of protoplanetary disk's matter onto the young star with a mass of $\lesssim 0.5$ M$_\odot$ to $\gtrsim 3\times 10^{-5}$ M$_\odot$ yr$^{-1}$. Furthermore, IRAS 21204+4913 displays several unusual features: the dependence of the width and radial velocity of absorption lines on the excitation potential, emission in the TiO molecular bands, and a comparably bright outburst that occured in 1948. Several T Tauri stars and a group of Herbig-Haro objects are found in the vicinity of the star. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2602_15157 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | The eruptive young star IRAS 21204+4913 Burlak, M. A. Dodin, A. V. Zharova, A. V. Zheltoukhov, S. G. Ikonnikova, N. P. Lamzin, S. A. Safonov, B. S. Strakhov, I. A. Tatarnikov, A. A. Tatarnikov, A. M. Solar and Stellar Astrophysics The results of photometric, polarimetric, and spectroscopic observations are presented for the young star IRAS 21204+4913, whose visible brightness has increased by $\approx 5^{\rm m}$ since October 2025. The star's absorption spectrum in the $0.36 - 0.75 μ$m range resembles those of A - F giants and supergiants, but it also exhibits molecular TiO bands. The brightening was accompanied by a significant increase in the degree of polarization of the stellar radiation (to $\approx 16 \%$ in the I-band), likely due to scattering by dust in an expanding circumstellar shell. The P Cygni profile of the H$α$ line implies a dusty wind velocity of $\approx 300$ km/s. We believe that the outburst of IRAS 21204+4913 is caused by an increase in the accretion rate of protoplanetary disk's matter onto the young star with a mass of $\lesssim 0.5$ M$_\odot$ to $\gtrsim 3\times 10^{-5}$ M$_\odot$ yr$^{-1}$. Furthermore, IRAS 21204+4913 displays several unusual features: the dependence of the width and radial velocity of absorption lines on the excitation potential, emission in the TiO molecular bands, and a comparably bright outburst that occured in 1948. Several T Tauri stars and a group of Herbig-Haro objects are found in the vicinity of the star. |
| title | The eruptive young star IRAS 21204+4913 |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2602.15157 |