Shock-driven synchrotron radio emission from the 2021 outburst of RS Ophiuchi
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arXiv
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| Autores principales: | , , , , , , |
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| Formato: | Preprint |
| Publicado: |
2024
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| _version_ | 1866910294210510848 |
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| author | Nayana, A. J. Anupama, G. C. Roy, Nirupam Banerjee, Dipankar P. K. Singh, Kulinder Pal S., Sonith L. Kamath, U. S. |
| author_facet | Nayana, A. J. Anupama, G. C. Roy, Nirupam Banerjee, Dipankar P. K. Singh, Kulinder Pal S., Sonith L. Kamath, U. S. |
| contents | We present low-frequency radio observations of the Galactic symbiotic recurrent nova RS Ophiuchi during its 2021 outburst. The observations were carried out with the upgraded Giant Metrewave Radio Telescope (uGMRT) spanning a frequency range of 0.15$-$1.4 GHz during 23$-$287 days post the outburst. The average value of the optically thin spectral index is $α\sim$ $-$0.4 ($F_ν \propto ν^α$), indicating a non-thermal origin of the radio emission at the observed frequencies. The radio light curves are best represented by shock-driven synchrotron emission, initially absorbed by a clumpy ionized circumbinary medium. We estimate the mass-loss rate of the red giant companion star to be $\dot{M} \sim$ 7.5 $\times$ 10$^{-8}$ $M_{\odot}$ yr$^{-1}$ for an assumed stellar wind velocity of 20 km/s. The 0.15--1.4 GHz radio light curves of the 2021 outburst are systematically brighter than those of the 2006 outburst. Considering similar shock properties between the two outbursts, this is indicative of a relatively higher particle number density in the synchrotron emitting plasma in the current outburst. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2401_05643 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Shock-driven synchrotron radio emission from the 2021 outburst of RS Ophiuchi Nayana, A. J. Anupama, G. C. Roy, Nirupam Banerjee, Dipankar P. K. Singh, Kulinder Pal S., Sonith L. Kamath, U. S. Solar and Stellar Astrophysics High Energy Astrophysical Phenomena We present low-frequency radio observations of the Galactic symbiotic recurrent nova RS Ophiuchi during its 2021 outburst. The observations were carried out with the upgraded Giant Metrewave Radio Telescope (uGMRT) spanning a frequency range of 0.15$-$1.4 GHz during 23$-$287 days post the outburst. The average value of the optically thin spectral index is $α\sim$ $-$0.4 ($F_ν \propto ν^α$), indicating a non-thermal origin of the radio emission at the observed frequencies. The radio light curves are best represented by shock-driven synchrotron emission, initially absorbed by a clumpy ionized circumbinary medium. We estimate the mass-loss rate of the red giant companion star to be $\dot{M} \sim$ 7.5 $\times$ 10$^{-8}$ $M_{\odot}$ yr$^{-1}$ for an assumed stellar wind velocity of 20 km/s. The 0.15--1.4 GHz radio light curves of the 2021 outburst are systematically brighter than those of the 2006 outburst. Considering similar shock properties between the two outbursts, this is indicative of a relatively higher particle number density in the synchrotron emitting plasma in the current outburst. |
| title | Shock-driven synchrotron radio emission from the 2021 outburst of RS Ophiuchi |
| topic | Solar and Stellar Astrophysics High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2401.05643 |