Multi-wavelength detection of an ongoing FUOr-type outburst on a low-mass YSO
Fuente:
arXiv
Guardado en:
| Autores principales: | , , , , , , , , , , , , , , , |
|---|---|
| Formato: | Preprint |
| Publicado: |
2024
|
| Materias: | |
| Acceso en línea: | |
| Etiquetas: |
Agregar Etiqueta
Sin Etiquetas, Sea el primero en etiquetar este registro!
|
| _version_ | 1866913210023542784 |
|---|---|
| author | Guo, Zhen Lucas, P. W. Kurtev, R. G. Borissova, J. Elbakyan, V. Morris, C. Bayo, A. Smith, L. Garatti, A. Caratti o Peña, C. Contreras Minniti, D. Jose, J. Ashraf, M. Alonso-García, J. Miller, N. Muthu, H. D. S. |
| author_facet | Guo, Zhen Lucas, P. W. Kurtev, R. G. Borissova, J. Elbakyan, V. Morris, C. Bayo, A. Smith, L. Garatti, A. Caratti o Peña, C. Contreras Minniti, D. Jose, J. Ashraf, M. Alonso-García, J. Miller, N. Muthu, H. D. S. |
| contents | During the pre-main-sequence evolution, Young Stellar Objects (YSOs) assemble most of their mass during the episodic accretion process. The rarely seen FUOr-type events (FUOrs) are valuable laboratories to investigate the outbursting nature of YSOs. Here, we present multi-wavelength detection of a high-amplitude eruptive source in the young open cluster VdBH 221 with an ongoing outburst, including optical to mid-infrared time series and near-infrared spectra. The initial outburst has an exceptional amplitude of $>$6.3 mag in Gaia and 4.6 mag in $K_s$, with a peak luminosity up to 16 $L_{\odot}$ and a peak mass accretion rate of 1.4 $\times$ 10$^{-5}$ $M_\odot$ yr$^{-1}$. The optical to infrared spectral energy distribution (SED) of this object is consistent with a low-mass star (0.2$M_\odot$) with a modest extinction ($A_V < 2$ mag). A 100-d delay between optical and infrared rising stages is detected, suggesting an outside-in origin of the instability. The spectroscopic features of this object reveal a self-luminous accretion disc, very similar to FU Orionis, with a low line-of-sight extinction. Most recently, there has been a gradual increase in brightness throughout the wavelength range, possibly suggesting an enhancement of the mass accretion rate. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2401_14470 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Multi-wavelength detection of an ongoing FUOr-type outburst on a low-mass YSO Guo, Zhen Lucas, P. W. Kurtev, R. G. Borissova, J. Elbakyan, V. Morris, C. Bayo, A. Smith, L. Garatti, A. Caratti o Peña, C. Contreras Minniti, D. Jose, J. Ashraf, M. Alonso-García, J. Miller, N. Muthu, H. D. S. Solar and Stellar Astrophysics Astrophysics of Galaxies During the pre-main-sequence evolution, Young Stellar Objects (YSOs) assemble most of their mass during the episodic accretion process. The rarely seen FUOr-type events (FUOrs) are valuable laboratories to investigate the outbursting nature of YSOs. Here, we present multi-wavelength detection of a high-amplitude eruptive source in the young open cluster VdBH 221 with an ongoing outburst, including optical to mid-infrared time series and near-infrared spectra. The initial outburst has an exceptional amplitude of $>$6.3 mag in Gaia and 4.6 mag in $K_s$, with a peak luminosity up to 16 $L_{\odot}$ and a peak mass accretion rate of 1.4 $\times$ 10$^{-5}$ $M_\odot$ yr$^{-1}$. The optical to infrared spectral energy distribution (SED) of this object is consistent with a low-mass star (0.2$M_\odot$) with a modest extinction ($A_V < 2$ mag). A 100-d delay between optical and infrared rising stages is detected, suggesting an outside-in origin of the instability. The spectroscopic features of this object reveal a self-luminous accretion disc, very similar to FU Orionis, with a low line-of-sight extinction. Most recently, there has been a gradual increase in brightness throughout the wavelength range, possibly suggesting an enhancement of the mass accretion rate. |
| title | Multi-wavelength detection of an ongoing FUOr-type outburst on a low-mass YSO |
| topic | Solar and Stellar Astrophysics Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2401.14470 |