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| Main Authors: | , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2410.01125 |
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| _version_ | 1866910628316184576 |
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| author | Molina, Isabella Chomiuk, Laura Linford, Justin D. Aydi, Elias Mioduszewski, Amy J. Mukai, Koji Sokolovsky, Kirill V. Strader, Jay Craig, Peter Dong, Dillon Harris, Chelsea E. Nyamai, Miriam M. Rupen, Michael P. Sokoloski, Jennifer L. Walter, Frederick M. Weston, Jennifer H. S. Williams, Montana N. |
| author_facet | Molina, Isabella Chomiuk, Laura Linford, Justin D. Aydi, Elias Mioduszewski, Amy J. Mukai, Koji Sokolovsky, Kirill V. Strader, Jay Craig, Peter Dong, Dillon Harris, Chelsea E. Nyamai, Miriam M. Rupen, Michael P. Sokoloski, Jennifer L. Walter, Frederick M. Weston, Jennifer H. S. Williams, Montana N. |
| contents | V745 Sco is a Galactic symbiotic recurrent nova with nova eruptions in 1937, 1989 and 2014. We study the behavior of V745 Sco at radio wavelengths (0.6-37,GHz), covering both its 1989 and 2014 eruptions and informed by optical, X-ray, and $γ$-ray data. The radio light curves are synchrotron-dominated. Surprisingly, compared to expectations for synchrotron emission from explosive transients such as radio supernovae, the light curves spanning 0.6-37 GHz all peak around the same time ($\sim$18-26 days after eruption) and with similar flux densities (5-9 mJy).We model the synchrotron light curves as interaction of the nova ejecta with the red giant wind, but find that simple spherically symmetric models with wind-like circumstellar material (CSM) cannot explain the radio light curve. Instead, we conclude that the shock suddenly breaks out of a dense CSM absorbing screen around 20 days after eruption, and then expands into a relatively low density wind ($\dot{M}_{out} \approx 10^{-9}-10^{-8}$ M$_{\odot}$ yr$^{-1}$ for $v_w = 10$ km s$^{-1}$) out to $\sim$1 year post-eruption. The dense, close-in CSM may be an equatorial density enhancement or a more spherical red giant wind with $\dot{M}_{in} \approx [5-10] \times 10^{-7}$ M$_{\odot}$ yr$^{-1}$, truncated beyond several $\times 10^{14}$ cm. The outer lower-density CSM would not be visible in typical radio observations of Type Ia supernovae: V745 Sco cannot be ruled out as a Type Ia progenitor based on CSM constraints alone.Complementary constraints from the free-free radio optical depth and the synchrotron luminosity imply the shock is efficient at accelerating relativistic electrons and amplifying magnetic fields, with $ε_e$ and $ε_B \approx 0.01-0.1$. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2410_01125 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The Symbiotic Recurrent Nova V745 Sco at Radio Wavelengths Molina, Isabella Chomiuk, Laura Linford, Justin D. Aydi, Elias Mioduszewski, Amy J. Mukai, Koji Sokolovsky, Kirill V. Strader, Jay Craig, Peter Dong, Dillon Harris, Chelsea E. Nyamai, Miriam M. Rupen, Michael P. Sokoloski, Jennifer L. Walter, Frederick M. Weston, Jennifer H. S. Williams, Montana N. High Energy Astrophysical Phenomena V745 Sco is a Galactic symbiotic recurrent nova with nova eruptions in 1937, 1989 and 2014. We study the behavior of V745 Sco at radio wavelengths (0.6-37,GHz), covering both its 1989 and 2014 eruptions and informed by optical, X-ray, and $γ$-ray data. The radio light curves are synchrotron-dominated. Surprisingly, compared to expectations for synchrotron emission from explosive transients such as radio supernovae, the light curves spanning 0.6-37 GHz all peak around the same time ($\sim$18-26 days after eruption) and with similar flux densities (5-9 mJy).We model the synchrotron light curves as interaction of the nova ejecta with the red giant wind, but find that simple spherically symmetric models with wind-like circumstellar material (CSM) cannot explain the radio light curve. Instead, we conclude that the shock suddenly breaks out of a dense CSM absorbing screen around 20 days after eruption, and then expands into a relatively low density wind ($\dot{M}_{out} \approx 10^{-9}-10^{-8}$ M$_{\odot}$ yr$^{-1}$ for $v_w = 10$ km s$^{-1}$) out to $\sim$1 year post-eruption. The dense, close-in CSM may be an equatorial density enhancement or a more spherical red giant wind with $\dot{M}_{in} \approx [5-10] \times 10^{-7}$ M$_{\odot}$ yr$^{-1}$, truncated beyond several $\times 10^{14}$ cm. The outer lower-density CSM would not be visible in typical radio observations of Type Ia supernovae: V745 Sco cannot be ruled out as a Type Ia progenitor based on CSM constraints alone.Complementary constraints from the free-free radio optical depth and the synchrotron luminosity imply the shock is efficient at accelerating relativistic electrons and amplifying magnetic fields, with $ε_e$ and $ε_B \approx 0.01-0.1$. |
| title | The Symbiotic Recurrent Nova V745 Sco at Radio Wavelengths |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2410.01125 |