Magnetar Formation Channels

• Magnetar formation channels are distinct evolutionary pathways, including isolated core-collapse, binary interactions, and exotic mergers, that produce highly magnetized neutron stars.
• Key mechanisms such as the Tayler–Spruit dynamo, MRI, and disk dynamos rapidly amplify magnetic fields, setting the stage for observable magnetar properties.
• Population synthesis, MHD modeling, and observational surveys collectively constrain birth spins, delay times, and channel contributions to magnetar demographics.

Magnetars are neutron stars exhibiting persistent and variable X-ray luminosities and surface dipole magnetic fields in excess of $10^{14}$–$10^{15}$ G. Their formation channels are central to understanding fundamental aspects of stellar evolution, binary interactions, and compact-object astrophysics. Recent observational surveys, population-synthesis calculations, and magnetohydrodynamic (MHD) modeling have revealed that multiple evolutionary pathways, each characterized by distinct physical mechanisms, contribute to the observed magnetar population.

1. Isolated Core-Collapse and Fallback-Driven Dynamos

Core-collapse of massive isolated stars ($M_i \approx 5$–$21\,M_\odot$) remains a principal magnetar formation channel. After iron-core collapse, a fraction of the ejecta falls back ($M_\mathrm{fb} \gtrsim 10^{-2}\,M_\odot$), spinning up the proto-neutron star (PNS) and triggering the Tayler–Spruit dynamo (Barrère et al., 2022, Hu et al., 9 Nov 2025).

Amplification processes:

• Differential rotation in the post-bounce PNS supports strong shear, serving as the $\Omega$-effect in a Tayler–Spruit loop.
• Magnetic field amplification proceeds via nonaxisymmetric $m=1$ Tayler instabilities once the toroidal field $B_\phi$ locally exceeds a resistive cutoff $B_{\phi,c}$.
• Saturation field values scale as $$B_r^\mathrm{S} \simeq \sqrt{4\pi\rho r^2}q\Omega^2/N$$ (Spruit 2002) or $$B_r^\mathrm{F} \simeq \sqrt{4\pi\rho r^2}\Omega(q^2\Omega^5/N^5)^{1/3}$$ (Fuller et al. 2019).
• Magnetar-like fields ($B_r \gtrsim 10^{14}$–$10^{15}$ G) are reached within $20$–$40$ s for $M_\mathrm{fb} \gtrsim 0.01\,M_\odot$.

Observational implications:

• Magnetars formed by this channel are expected to be young ($t_{\mathrm{delay}} \sim 3$–$30$ Myr) and typically isolated, as single-star core-collapse SNe receive strong natal kicks ($v_k \sim 250$ km s$^{-1}$) (Hu et al., 9 Nov 2025).
• Magnetic-field decay (Ohmic, Hall, ambipolar) occurs over $\tau_B \sim 10^4$ yr, yielding $B_0\simeq 3\times10^{14}$–$10^{15}$ G and periods $P_\mathrm{max} \approx 13$ s (Beniamini et al., 2019).

2. Binary Interaction Channels: Tidal Spin-Up, Mass Transfer, and Stellar Mergers

Tidal Spin-Up in Binaries

Binary interactions significantly augment the core's angular momentum, enhancing conditions for rapid rotation and in situ magnetic amplification (Roy et al., 3 Jul 2025, Hu et al., 2023, Popov, 2015). Key routes include:

• Stable mass transfer or common-envelope (CE) evolution that produces a stripped helium star in a close orbit.
• Strong tidal torques synchronize the companion-upgraded helium star core ($P_{\mathrm{orb}} \lesssim 1$–$2$ d).
• At collapse, the core rotates sufficiently fast for convective/MRI-driven magnetar formation, producing surface fields $B_p \sim 10^{14}$–$10^{16}$ G and birth spin periods $P_0 \sim 1$–$20$ ms (Hu et al., 2023, Clark et al., 2014, Song et al., 2023).

Stellar and Core Mergers

Merger-driven channels entail:

• Merger of two evolved stars in a tight binary prior to core collapse, accompanied by hydrodynamical mixing and rapid rotation (Shenar et al., 2023, Popov, 2015).
• Disk–dynamo episodes in which a post-CE in-spiraling companion is shredded and accreted, creating a turbulent, magnetized disk around a pre-collapse core. This process is highly efficient at generating surface fields $B_\mathrm{core} \sim 10^{13}$–$10^{15}$ G and yields ms-spinning proto-magnetars (Nordhaus, 2011).

Binary Fraction and Observational Disruption

Population-synthesis calculations show that $79$–$90$\% of surviving binary magnetars have OB main-sequence companions, with eccentricities $e$ up to $0.9$ and periods $P_{\mathrm{orb}} \approx 0.1$–$100$ d (Hu et al., 9 Nov 2025). However, most magnetars are now single, reflecting high disruption rates by SN kicks and merger processes (Sherman et al., 8 Apr 2024). Observational constraints indicate that only $5$–$24$\% of Galactic magnetars retain unbound companions, a fraction far below population-synthesis predictions, implying a high pre-CCSN merger rate ($f_m \approx 48$–$86$\%) and/or substantial non-CCSN channels.

3. Exotic and Delayed Channels: White Dwarf Mergers, Accretion-Induced Collapse, and Globular Cluster Dynamics

Accretion-Induced Collapse (AIC) of Magnetized WDs

AIC of highly magnetized ONeMg white dwarfs in binaries with red giants can yield long-lived, highly magnetized neutron stars ($B_\mathrm{NS} > 10^{14}$ G) via magnetic flux conservation (Ablimit, 2022). Magnetic confinement enhances mass accumulation efficiency, pushing low-rate systems into the stable burning regime and narrowing the initial RG mass and period parameter space for successful AIC.

WD–WD and WD–NS Mergers in Dense Stellar Environments

Dynamical channels in globular clusters become relevant at late times ($t > 9$ Gyr) due to high densities, producing NSs via WD–WD or WD–NS mergers at rates $R_\mathrm{vol} \lesssim 45$ Gpc$^{-3}$ yr$^{-1}$ (Kremer et al., 2021). Typically, these NSs have $B \lesssim 10^{12}$ G, but a minority could reach magnetar strengths via shear-driven dynamo amplification.

Core Merger-Induced Collapse (CMIC)

The CMIC model involves mergers between ONeMg WDs and non-degenerate cores in CE episodes, forming proto-magnetars with rapid rotation ($P_0 \sim 0.6$–$6$ ms) and potentially $B \sim 10^{14}$–$10^{15}$ G via an $\alpha$–$\Omega$ dynamo (Ablimit et al., 2021).

4. Strong-Interaction Phase Transitions in Massive Cores

For NSs with central densities $\rho_\mathrm{center} \gtrsim 3\,\rho_0$, a strong-interaction-driven phase transition produces a neutral pion condensate that aligns nucleon spins (Dass et al., 2010). Core magnetization $M \sim n_N\,\mu_N$ gives internal fields $B_{\mathrm{core}} \sim 10^{16}$–$10^{17}$ G, shielded initially but reaching the surface as $$B_{\mathrm{surf}} \simeq B_{\mathrm{core}} (R_c/R)^3$$ over ambipolar and crustal diffusion timescales ($\tau_\mathrm{amb} \sim 10^4$ yr, $\tau_\mathrm{crust} \sim 10^5$ yr).

5. Observational Diagnostics, Channel Yields, and Population Synthesis

Population Yields and Delay Times

Comprehensive simulations (e.g., COMPAS, MESA, BSE) and observational constraints reveal that:

• $57$\% of magnetars originate as binaries disrupted by SN kicks or merger (“S2” channel), $19$\% from truly isolated single stars (“S1”), $19$\% from main-sequence mergers, and $\lesssim 1$\% from core-merger CE and AIC (Hu et al., 9 Nov 2025).
• Delay times range from “prompt” ($\sim$10 Myr for CCSN, tidal spin-up, binary mergers) to delayed ($\sim$0.1–1 Gyr for core merger channels, WD–WD mergers in clusters).
• Surviving binaries are characterized by distinct $P_{\mathrm{orb}}$–$e$ distributions and companion spectral types: majority OB stars, minority He stars or compact objects (Hu et al., 9 Nov 2025).

Observational Signatures

• Magnetar formation in broad-lined Type Ic SNe and SLSNe is tightly associated with ms magnetar birth periods and surface dipole fields $B_p \sim 10^{15}$–$10^{16}$ G (Wang et al., 2016, Hu et al., 2023).
• Association with cluster and host metallicity tracks the formation channel: binary-dominated routes favor star-forming galaxies and low-to-intermediate $Z$, while delayed mergers can populate older environments (Roy et al., 3 Jul 2025, Kremer et al., 2021).
• High proper-motion runaways and the presence (or absence) of associated supernova remnants (SNRs) diagnose channel disruption fractions and merger rates (Sherman et al., 8 Apr 2024).
• Distinctive features such as carbon pollution of runaway companions and delayed field emergence are unique markers for specific channels, e.g. Westerlund 1 (Wd1-5) (Clark et al., 2014).

Table: Dominant Physical Mechanisms Across Channels

Channel	Magnetic Field Amplification	Birth Spin (ms)
Isolated CCSN (fallback)	Tayler–Spruit dynamo via differential rot.	$8$–$28$
Binary tidal-spin-up / mass transfer	Tidal+convective dynamo/MRI at collapse	$1$–$20$
Merger (MS/MS, He/He, core mergers)	Disk dynamo; core merger; fossil field	$1$–$20$
Strong-interaction phase transition	Nucleon spin alignment in $\pi^0$ condens.	$10$–$100$
WD–WD, WD–NS mergers, AIC	Shear-driven/flux conservation from progenitor	$2$–$10$

6. Channel-Specific Limitations and Open Problems

Multiple channels are required to satisfy both empirical rates ($2.3$–$20$ kyr$^{-1}$) and observed magnetar birth fractions ($0.4^{+0.6}_{-0.28}$ of all NSs) (Beniamini et al., 2019). Single-channel models (e.g., high-$M$ single stars, pure CHE) under-predict observed rates given the underlying initial mass function and metallicity constraints.

Current controversies and uncertainties include:

• The exact role of pre-collapse mergers in boosting “fossil” fields and resolving the observed companion deficit in disrupted binaries (Sherman et al., 8 Apr 2024).
• The efficiency of angular momentum transport prescriptions (e.g., Spruit–Taylor, Fuller dynamo) in setting birth spins (Hu et al., 2023, Roy et al., 3 Jul 2025).
• The contribution of delayed channels (AIC, cluster mergers) at late times and their detectability.

7. Future Prospects: Breakthrough Diagnostics and Population Constraints

Planned multi-epoch VLBI proper-motion campaigns, deep SNR searches (e.g., DSA-2000, SKA), and high-cadence IR surveys (JWST, NGRST) will tighten constraints on channel yields, disruption fractions, and birth locations (Sherman et al., 8 Apr 2024).

The signatures of magnetar-driven transients (e.g., superluminous SNe, FBOTs, long-duration GRBs) are quantitatively linked to channel spin and magnetic field distributions, providing probe diagnostics for progenitor evolution (Hu et al., 2023, Song et al., 2023, Wang et al., 2016, Ablimit et al., 2021).

In conclusion, the formation of magnetars is governed by a convolution of channels involving isolated core-collapse, binary interactions (including mass transfer, tidal spin-up, and mergers), exotic delayed episodes, and phase transitions in extremely dense nucleonic matter. The relative contribution of each pathway shapes the demographics and observational signatures of the Galactic and extragalactic magnetar population, and continued integration of simulations, high-precision astrometry, and transient surveys is essential for quantitative channel discrimination.