Persistent radio sources associated with fast radio bursts: Implications from magnetar progenitors
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2025
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| author | Rahaman, Sk. Minhajur Acharya, Sandeep Kumar Beniamini, Paz Granot, Jonathan |
| author_facet | Rahaman, Sk. Minhajur Acharya, Sandeep Kumar Beniamini, Paz Granot, Jonathan |
| contents | The rare association of three persistent radio sources (confirmed PRS1 and PRS2, candidate PRS3) with repeating fast radio bursts (FRB 20121102A, 20190520B, 20201124A) offers a unique probe into their magneto-ionic environments. PRSs are attributed to synchrotron emission from relativistic charged particles of magnetar wind nebula (MWN) powered by spin-down magnetohydrodynamic wind or internal magnetic field decay. Using a multizone hydrodynamic model, we track MWN evolution to constrain magnetar progenitor properties. For PRS1 and PRS2, we find an equipartition radius $R_\mathrm{eq} \sim 0.1 $ pc that is consistent with the radio scintillation estimates ($> 0.03$ pc) and radio imaging limits ($<0.7$ pc). This compact size favors low expansion speeds and large initial spin periods, $P_\mathrm{i} \gtrsim 10$ ms, ruling out millisecond magnetar progenitors. Given $P_\mathrm{i} \gtrsim 10$ ms, a current size of $\sim 0.1$ pc, a supernova kinetic energy $E_\mathrm{ SN} \sim 10^{50}-10^{51}$ erg and an ejecta mass $M \sim 3-10 \; M_{\odot}$, the PRS age is $t \sim 10-10^{2}$ yr. PRSs with $t>20$ years require an internal field ($B_\mathrm{int} \sim 10^{16}-10^{16.5}\;$G) with a decay timescale $t_\mathrm{d} \sim 10-10^{2.5}$ yr. The slowest field decay ($t_\mathrm{d,max} \sim 500$ yr) favors sub-energetic supernovae ($E_\mathrm{SN} \sim 10^{50}$ erg) with massive ejecta ($M \gtrsim 10\; M_{\odot}$) and low ionization fraction ($\sim 3\% $). For the sub-energetic scenario for the confirmed PRSs, we predict a cooling break at $100-150$ gigahertz at $20-40 \; μ\text{Jy}$ and self-absorption near 200 megahertz at $180\; μ\text{Jy}$. For PRS3, a rotation-powered MWN is viable only if $t \sim 10$ yr; an inverted spectrum beyond 150 gigahertz would rule out this scenario. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_01125 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Persistent radio sources associated with fast radio bursts: Implications from magnetar progenitors Rahaman, Sk. Minhajur Acharya, Sandeep Kumar Beniamini, Paz Granot, Jonathan High Energy Astrophysical Phenomena The rare association of three persistent radio sources (confirmed PRS1 and PRS2, candidate PRS3) with repeating fast radio bursts (FRB 20121102A, 20190520B, 20201124A) offers a unique probe into their magneto-ionic environments. PRSs are attributed to synchrotron emission from relativistic charged particles of magnetar wind nebula (MWN) powered by spin-down magnetohydrodynamic wind or internal magnetic field decay. Using a multizone hydrodynamic model, we track MWN evolution to constrain magnetar progenitor properties. For PRS1 and PRS2, we find an equipartition radius $R_\mathrm{eq} \sim 0.1 $ pc that is consistent with the radio scintillation estimates ($> 0.03$ pc) and radio imaging limits ($<0.7$ pc). This compact size favors low expansion speeds and large initial spin periods, $P_\mathrm{i} \gtrsim 10$ ms, ruling out millisecond magnetar progenitors. Given $P_\mathrm{i} \gtrsim 10$ ms, a current size of $\sim 0.1$ pc, a supernova kinetic energy $E_\mathrm{ SN} \sim 10^{50}-10^{51}$ erg and an ejecta mass $M \sim 3-10 \; M_{\odot}$, the PRS age is $t \sim 10-10^{2}$ yr. PRSs with $t>20$ years require an internal field ($B_\mathrm{int} \sim 10^{16}-10^{16.5}\;$G) with a decay timescale $t_\mathrm{d} \sim 10-10^{2.5}$ yr. The slowest field decay ($t_\mathrm{d,max} \sim 500$ yr) favors sub-energetic supernovae ($E_\mathrm{SN} \sim 10^{50}$ erg) with massive ejecta ($M \gtrsim 10\; M_{\odot}$) and low ionization fraction ($\sim 3\% $). For the sub-energetic scenario for the confirmed PRSs, we predict a cooling break at $100-150$ gigahertz at $20-40 \; μ\text{Jy}$ and self-absorption near 200 megahertz at $180\; μ\text{Jy}$. For PRS3, a rotation-powered MWN is viable only if $t \sim 10$ yr; an inverted spectrum beyond 150 gigahertz would rule out this scenario. |
| title | Persistent radio sources associated with fast radio bursts: Implications from magnetar progenitors |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2504.01125 |