The reviewed record of science sign in
Pith

arxiv: 2607.05182 · v1 · pith:RNMSF4LZ · submitted 2026-07-06 · astro-ph.HE

Spectropolarimetric detection of baryonic mass loading in a transient relativistic jet: application to the black hole X-ray binary Swift J1727.8-1613

A. K. Hughes , R. P. Fender , G. R. Sivakoff , F. J. Cowie , I. Heywood , J. H. Matthews , K. Savard , F. Carotenuto
show 5 more authors
T. D. Russell C. M. Wood M. C. Baglio S. Corbel S. E. Motta
This is my paper

Reviewed by Pith2026-07-08 00:31 UTCglm-5.2pith:RNMSF4LZopen to challenge →

classification astro-ph.HE PACS 98.38.Mh98.38.Fs95.85.Bh
keywords faradaymassplasmatransientbinaryradiox-rayduring
0
0 comments X

The pith

Polarised radio reveals proton-loaded jets from black hole binary

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper argues that transient, wavelength-dependent distortions in the polarised radio emission from the black hole X-ray binary Swift J1727.8–1613 are caused by Faraday rotation occurring *inside* the jet plasma itself, not in foreground material. Because internal Faraday rotation cancels out in a pure electron–positron plasma (equal numbers of positive and negative charges rotating the polarisation angle in opposite directions), detecting it requires a dominant electron–proton component in the jet ejecta. The authors identify transient Faraday-complex spectropolarimetric structure that appears and disappears in lockstep with the brightest radio flares, while the foreground rotation measure stays constant at about –1 rad m⁻². Using parametric QU-fitting and RM synthesis on MeerKAT L-band data, they model this structure as Faraday-thick components — emission mixed with rotating plasma — and argue against origins in the interstellar medium or a disc wind on temporal and geometric grounds. Anchoring the magnetic field (~200 mG) and size scale (~1.3×10¹⁴ cm) with synchrotron self-absorption modelling of the flare, they infer a characteristic Faraday-rotating mass of ~10²¹ g, roughly 10⁻³ of the mass accreted during the flare. They further show that the relativistic synchrotron-emitting electrons alone are too few and too inefficient as Faraday rotators to explain the observed rotation, requiring a colder electron–proton reservoir that dominates the plasma content but contributes little to the synchrotron emission. The paper also reports unusual evolution of the intrinsic polarisation angle, including post-flare obliquity and a 90-degree inversion between the unresolved core and resolved ejecta at late times, which may reflect relativistic beaming effects in helical magnetic fields.

Core claim

The central discovery is that transient Faraday-complex spectropolarimetric structure, appearing coincident with radio flares in a black hole X-ray binary, can be attributed to internal Faraday rotation within the jet ejecta. This attribution requires the jet plasma to contain a dominant electron–proton component rather than a pure electron–positron pair plasma, because internal rotation cancels in charge-symmetric pair plasmas. Combining the inferred Faraday thickness (~100 rad m⁻²) with synchrotron self-absorption estimates of the magnetic field and emitting region size yields a characteristic Faraday-rotating mass of order 10²¹ g — about 10⁻³ of the accreted mass available during the flar

What carries the argument

The load-bearing mechanism is the distinction between external and internal Faraday rotation. Faraday rotation scales as φ_f ∝ q³m⁻² ∫ n_e B_∥ dl, where the odd power of charge q means electrons and positrons contribute with opposite signs. In a charge-symmetric pair plasma, these contributions cancel exactly; in an electron–proton plasma, the proton contribution is suppressed by (m_e/m_p)² and electrons dominate. The paper models the observed spectropolarimetric complexity using super-Gaussian Faraday-thick components (following Anderson et al. 2016), where the shape parameter N interpolates between Gaussian external Faraday dispersion (N=2) and a Burn-slab top-hat (N>15). The mass estimate

If this is right

  • If internal Faraday rotation is a reliable diagnostic of jet composition, time-domain spectropolarimetry of X-ray binary flares can systematically distinguish electron–proton from electron–positron dominated jets across the transient jet population, something total-intensity monitoring cannot do.
  • The mass fraction f_rot ~ 10⁻³ inferred during flaring is much lower than the mass fractions (~1) inferred from deceleration modelling of resolved ejecta at late times, suggesting jets gain substantial mass through entrainment or environmental interaction as they propagate to larger scales.
  • The electron acceleration efficiency inferred from the ratio of relativistic to cold electron densities (≳10% by number) is higher than typical PIC simulation values for collisionless shocks (0.5–2%), hinting that particle acceleration may be especially efficient during the ejection phase, or that the cold electron reservoir is larger than estimated.
  • The polarisation-angle obliquity and 90-degree core–ejecta inversion could serve as a diagnostic of bulk relativistic speed if explained by aberration in helical magnetic fields, offering a complementary velocity probe for unresolved jets.
  • The method generalises to other transient jetted sources — tidal disruption events, gamma-ray bursts, and neutron star mergers — where jet composition and mass loading remain poorly constrained.

Load-bearing premise

The interpretation depends on the observed Faraday complexity being internal to the jet ejecta rather than produced by a transient external screen local to the source. The paper argues against a disc-wind origin by estimating that a ~1000 km/s wind would need ~100 days to reach the relevant emission scale, but a faster wind or different geometry could change this conclusion. If the rotating material is instead external to the emitting plasma, the composition and mass in do

What would settle it

Simultaneous VLBI spectropolarimetry showing no spatially resolved ejecta coincident with the Faraday-thick components would undermine the internal-rotation interpretation. Alternatively, if a future outburst shows Faraday-complex structure that does not correlate temporally with radio flaring, or if a demonstrated faster disc wind can reach the emission scale within the flare rise time, the external-screen hypothesis would regain traction and the composition inference would fail.

Figures

Figures reproduced from arXiv: 2607.05182 by A. K. Hughes, C. M. Wood, F. Carotenuto, F. J. Cowie, G. R. Sivakoff, I. Heywood, J. H. Matthews, K. Savard, M. C. Baglio, R. P. Fender, S. Corbel, S. E. Motta, T. D. Russell.

Figure 1
Figure 1. Figure 1: Schematic super-Gaussian Faraday-thick component profiles (Equa￾tion 15) for increasing shape parameter 𝑁. The 𝑁 = 2 case is Gaussian, while large 𝑁 (> 15) approaches a Burn-slab-like top-hat distribution. fourth-order polynomial passing (almost) exactly through the data has a negligible effect on the final spectropolarimetric results. We then fit the fractional complex polarisation, 𝑃/𝐼 = 𝑞 + 𝑖𝑢, where 𝑞 … view at source ↗
Figure 2
Figure 2. Figure 2: Simulated two-component ST model used to test the fitting proce￾dure. We draw 250 synthetic data points from a known input model, inject Gaussian noise, and refit the data. The true model is shown in black, with pos￾terior samples from the fit shown in blue. The top and middle panels show the linear polarisation fraction and polarisation angle as functions of 𝜆 2 , respec￾tively. The bottom panel shows the… view at source ↗
Figure 3
Figure 3. Figure 3: A subset of MeerKAT images of Swift J1727 during its outburst. The left-most panels correspond to final observations around the flaring interval on 2023 November 25 (MJD 60273), following the cessation of bright flaring, but while the emission was still point-like. The right-most panels correspond to 2024 February 25 (MJD 60365) and highlight the later multi-component morphology, including polarised ejecta… view at source ↗
Figure 4
Figure 4. Figure 4: Time evolution of the Stokes 𝐼 flux density and Faraday-spectrum diagnostics during the 2023 flaring interval. (top) 1.28 GHz flux-density evo￾lution, with daily-averaged monitoring shown in grey/black and the MeerKAT spectropolarimetric epochs marked by purple stars. The dashed vertical line marks the reported hard→soft state transition on 2023 October 5 (MJD 60222; Bollemeijer et al. 2023a,b), while the … view at source ↗
Figure 5
Figure 5. Figure 5: Faraday spectra of Swift J1727. The dotted grey curve, solid black curve, and solid blue step function show the observed, CLEANed, and model Faraday spectra derived using rm-tools. Red borders highlight the epochs with the largest changes during the brightest flaring interval of the outburst, while blue borders mark epochs outside the range shown in [PITH_FULL_IMAGE:figures/full_fig_p011_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Representative spectropolarimetric behaviour of Swift J1727 across six epochs before, during, and after the bright flaring period. For each epoch, the upper and middle panels show the observed 𝑝(𝜆 2 ) and 𝜓(𝜆 2 ), respectively, while the lower panel shows the corresponding model amplitudes, |𝐹(𝜙𝑓 ) |. Black points show the data, blue curves show posterior draws from the preferred 𝑄𝑈-fitting model, and grey… view at source ↗
Figure 7
Figure 7. Figure 7: Summary of the radio and spectropolarimetric evolution of Swift J1727 during the 2023 flaring period. The upper panels show the 1.28 GHz MeerKAT light curve, the radio spectral index, and the inferred intrinsic polarisation fractions, 𝑝0, including both the total values (solid markers) and per-component values (translucent markers). The lower panels show the preferred models for representative epochs, orde… view at source ↗
Figure 8
Figure 8. Figure 8: Time evolution of the radio and linear polarisation properties of Swift J1727. From top to bottom, the panels show the 1.28 GHz Stokes 𝐼 flux density, radio spectral index, intrinsic polarisation fraction, 𝑝0, intrinsic polarisation angle, 𝜓0, Faraday depth, 𝜙rm, and, where relevant, the Faraday width of the super-Gaussian components, 𝜎𝜙. Filled circles show Faraday￾thin core components, diamonds show Fara… view at source ↗
Figure 9
Figure 9. Figure 9: Deviation of the intrinsic polarisation angle from the nearest canonical jet-aligned orientation. The upper panel shows the minimum ab￾solute offset between 𝜓0 and the position angles parallel or orthogonal to the VLBI jet axis, while the lower panel shows the same offset scaled by the posterior uncertainty. The horizontal dashed line marks the > 3𝜎 threshold used to identify significantly oblique orientat… view at source ↗
Figure 10
Figure 10. Figure 10: Seed-dependence test for the peak-flaring 𝑄𝑈 fits. Each panel shows 100 posterior samples from each of 10 independent random seeds. The 2023 October 06 STT solution is stable across trials, while the 2023 October 14 SSTT and STTT fits show larger seed-to-seed variation, including solutions with very broad Faraday-thick components. & Fender 2026), we adopt 𝑊rm,99 ∼ 100 rad m−2 as a characteristic Faraday t… view at source ↗
Figure 11
Figure 11. Figure 11: Schematic examples of Faraday-space signatures expected from different jet and foreground configurations. Red denotes synchrotron-emitting plasma, blue denotes Faraday-rotating plasma, and purple denotes plasma that is both emitting and rotating. Dimmer colours indicate lower emissivity or a weaker Faraday-rotating contribution. The rightmost blue screen represents the Galactic ISM, the eye marks the obse… view at source ↗
Figure 12
Figure 12. Figure 12: Bounded beta-distribution approximation to the distance posterior for Swift J1727. The blue and red intervals compare the approximated and target medians and 68% equal-tailed intervals from Burridge et al. (2025). The distribution is parametrised using the scipy.stats.beta convention, with 𝑎 = 4.71696, 𝑏 = 30.00000, loc = 2.41143, and scale = 23.79047. MNRAS 000, 1–43 (2026) [PITH_FULL_IMAGE:figures/full… view at source ↗
Figure 13
Figure 13. Figure 13: Posterior distributions for the inferred Faraday-rotating mass, 𝑀rot, and its fraction of the accreted mass available during the flare, 𝑓rot. The blue distributions show the normalised posterior densities, the shaded regions mark the 68 per cent highest-density intervals, and the dashed vertical lines indicate the posterior modes. The fiducial solution requires 𝑀rot ∼ 1021 g, corresponding to only a small… view at source ↗
Figure 14
Figure 14. Figure 14: Posterior distribution of the fiducial density ratio 𝑛𝑒,rel/(𝑛𝑒,rel + 𝑛𝑒,rot), used as an empirical proxy for the electron acceleration efficiency by number, 𝜖acc, for 𝜅𝑀 = 1. The grey shaded region marks the 68 per cent highest-density interval, and the dashed vertical line marks the posterior mode. ing the much lower electron-specific efficiencies inferred for certain large-scale X-ray binary jet intera… view at source ↗
Figure 15
Figure 15. Figure 15: Post-flare polarisation evolution of the preferred Faraday-thin component. We show the Stokes 𝐼 flux density, intrinsic fractional polar￾isation, 𝑝0, and intrinsic polarisation angle, 𝜓0, after the brightest flaring activity. Although the source is simple in Faraday space during this period, both 𝑝0 and 𝜓0 evolve smoothly, indicating continued intrinsic evolution of the emitting region. The grey band mark… view at source ↗
read the original abstract

Radio emission during X-ray binary outbursts is dominated by synchrotron radiation from relativistic jets, but is usually studied through total-intensity diagnostics such as flux density, spectra, variability, and proper motion. Radio spectropolarimetry provides a complementary probe of the magneto-ionic plasma through Faraday rotation and depolarisation. When the Faraday rotating material is local to the source, these effects can constrain the jet plasma composition and mass content, but this approach is rarely applied to transient jetted sources. We present MeerKAT L-band spectropolarimetry of the black hole X-ray binary \src\ during its 2023 outburst, focusing on the brightest radio flaring interval, when relativistic jets were being launched intermittently. Using multiple spectropolarimetric techniques, we identify transient Faraday-complex structure coincident with the major radio flares. The close temporal association with the flaring activity, together with the stability of the foreground Faraday screen, favours an origin local to the jet rather than in the ISM or in a separate local screen external to the emitting plasma. Since internal Faraday rotation is suppressed in a pure electron--positron plasma, the data favour a dominant electron--proton component. Interpreting the characteristic Faraday thickness as internal rotation, and anchoring the magnetic-field and size scales with synchrotron self-absorption arguments, we infer a characteristic Faraday-rotating mass of order $M_{\rm rot}\sim10^{21}{\rm\,g}$, corresponding to only a small fraction, $f_{\rm rot}\sim10^{-3}$, of the accreted mass available during the flare. These results show that time-domain spectropolarimetry can turn transient Faraday complexity into a diagnostic of jet composition, mass loading, and plasma evolution in X-ray binary outbursts, and potentially other transient jetted sources.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 7 minor

Summary. This paper presents MeerKAT L-band spectropolarimetry of the black hole X-ray binary Swift J1727.8-1613 during its 2023 outburst, focusing on the brightest radio flaring interval. Using both RM synthesis and parametric QU-fitting, the authors identify transient Faraday-complex structure (requiring Faraday-thick components) that appears and disappears on ~2-day timescales coincident with major radio flares. The stability of the foreground ISM rotation measure (-1.0 +/- 0.3 rad m^-2) across epochs and angular scales, together with the transience of the complexity and the strong disfavoring of multi-thin-component and spectral power-law models, is used to argue that the Faraday-rotating material is internal to the jet ejecta rather than in the ISM or a disc wind. Since internal Faraday rotation cancels in a charge-symmetric pair plasma, the authors conclude the ejecta must contain a dominant electron-proton component. Combining the characteristic Faraday thickness (W_rm,99 ~ 100 rad m^-2) with synchrotron self-absorption modeling of the Stokes I flare (yielding B_perp ~ 200 mG and l ~ 1.3x10^14 cm), they infer a Faraday-rotating mass M_rot ~ 10^21 g, corresponding to f_rot ~ 10^-3 of the accreted mass available during the flare. The paper also discusses the implications for electron acceleration efficiency and intrinsic polarisation-angle evolution.

Significance. The paper makes a timely and potentially impactful contribution by demonstrating that time-domain spectropolarimetry can be used as a diagnostic of jet composition and mass loading in transient relativistic jets, an approach that has been largely limited to AGN studies. The observational result -- transient Faraday complexity during flaring -- is supported by multiple independent methods (RM synthesis and parametric QU-fitting), conservative Bayesian evidence thresholds (Delta ln Z > 10), calibrator stability checks (Appendix C), and seed-dependence tests (Figure 10). The reproducible code and data products (GitHub repository, SSA codebase) are a notable strength. The argument for electron-proton composition, while resting on the interpretation of the Faraday complexity as internal, is physically well-motivated and supported by complementary mass-budget arguments from the literature. The mass estimate is appropriately framed as an order-of-magnitude exploratory calculation with clearly stated caveats. The falsifiable prediction that future outbursts should show similar transient Faraday-thick structure during flaring, and that broader-band spectropolarimetry should track the inward

major comments (2)
  1. Section 4.1, disc-wind elimination: The argument against a disc-wind origin for the Faraday complexity relies on a flow timescale of ~100 d for a ~1000 km/s wind to reach 10^15 cm, exceeding the ~20 d interval from outburst onset to the first Faraday-thick epoch. However, the counter-argument that a faster wind (3000-5000 km/s, observed in some XRB systems) would be less dense for fixed mass-loss rate does not account for the possibility of a higher mass-loss rate or a wind launched earlier in the outburst. The paper should more explicitly address whether a faster, denser wind launched during the hard-state rise could reach the relevant radius in time, or provide a stronger quantitative bound on the required mass-loss rate as a function of wind speed. That said, the transience of the complexity (~2-day timescales) and the strong disfavoring of multi-thin-component models (Delta ln Z > 10
  2. Section 4.3, Eqs. (21)-(23): The mass estimate M_rot depends on W_rm,99 (fitted from polarimetric data), B_perp and l (from SSA modeling of Stokes I), and geometric/depolarization factors (D, theta_B). While these are derived from independent observables (polarized vs total intensity), the SSA model assumes a homogeneous emitting region, which the authors acknowledge is likely violated given the strong depolarization and inhomogeneous flare spectra. The sensitivity of M_rot to this assumption should be more explicitly quantified. Specifically, if the emitting region is inhomogeneous (as suggested by the sub-canonical optically thick spectral index), how much could B_perp and l change, and what is the resulting range on M_rot? The current treatment (Section 4.3.2) discusses this qualitatively but does not propagate the inhomogeneity into the mass uncertainty. This is load-bearing for the
minor comments (7)
  1. Section 3.3.3: The characteristic Faraday thickness W_rm,99 ~ 100 rad m^-2 is adopted from the flare-peak components, but the inferred widths range from 25 to 130 rad m^-2 across components and epochs (Section 3.3.3). The paper should clarify whether the mass estimate is sensitive to this choice, and whether using a different epoch (e.g., the more stable October 06 fit vs. the seed-dependent October 14 fit) would yield a substantially different M_rot.
  2. Table 1: The table is very large and spans multiple pages. Consider splitting it or moving the full version to an appendix, showing only the favored models in the main text.
  3. Section 4.3.1, Eq. (28): The angle theta_B between the ordered magnetic field and the line of sight is given a broad prior (10-80 deg, flat in cos theta_B). The resulting <B_parallel> ~ 30 mG has a very asymmetric uncertainty (+40, -20 mG). It would help to show the posterior distribution for <B_parallel> and M_rot, or at least state the median and 68% HDI more explicitly, to clarify how the mass estimate depends on this geometric factor.
  4. Section 4.1.2: The approaching-receding ejecta interpretation for the paired thick components is interesting but speculative given the lack of VLBI evidence for a receding component. The Monte Carlo calculation showing R_F > 2 in ~20% of samples is useful, but the text could note more clearly that this is a consistency check rather than supporting evidence for this specific geometry.
  5. Figure 4, middle panel: The green region showing a linearly evolving ISM contribution is mentioned but not clearly defined. A brief note on how this region is computed would help the reader.
  6. Section 2.1.1: The manual correction of the cross-hand phase discontinuity (adding/subtracting pi beyond zero crossings) for epochs with large ionospheric RM could introduce subtle systematics. While Appendix C shows calibrator stability, a brief note on how this was validated for the target epochs would strengthen confidence in the spectropolarimetric fidelity.
  7. The paper cites several works as submitted

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for a careful and constructive report. Both major comments identify legitimate gaps in the quantitative treatment of systematic uncertainties. We address each below and describe the revisions we will make.

read point-by-point responses

  1. Referee: Section 4.1, disc-wind elimination: The argument against a disc-wind origin for the Faraday complexity relies on a flow timescale of ~100 d for a ~1000 km/s wind to reach 10^15 cm, exceeding the ~20 d interval from outburst onset to the first Faraday-thick epoch. However, the counter-argument that a faster wind (3000-5000 km/s, observed in some XRB systems) would be less dense for fixed mass-loss rate does not account for the possibility of a higher mass-loss rate or a wind launched earlier in the outburst. The paper should more explicitly address whether a faster, denser wind launched during the hard-state rise could reach the relevant radius in time, or provide a stronger quantitative bound on the required mass-loss rate as a function of wind speed.

    Authors: The referee is correct that our treatment of the disc-wind scenario in Section 4.1 is incomplete. We considered only the case of a fixed mass-loss rate with varying wind speed, and did not quantitatively address the possibility of a higher mass-loss rate or a wind launched earlier in the outburst. We agree this gap should be closed. In the revised manuscript, we will add a quantitative bound on the required mass-loss rate as a function of wind speed and launch time. Specifically, we will compute the minimum wind mass-loss rate required to produce the observed Faraday thickness (W_rm,99 ~ 100 rad m^-2) at r ~ 10^15 cm, as a function of wind velocity (1000-5000 km/s) and launch epoch (ranging from outburst onset to ~10 days before the first Faraday-thick detection). This will allow the reader to directly compare the required mass-loss rates with observational constraints from Castro Segura et al. (2026) and typical XRB wind mass-loss rate estimates. We note that even in the most favorable case (5000 km/s wind launched at outburst onset), the required mass-loss rate likely exceeds the observationally inferred value by one to two orders of magnitude, but we will present this calculation explicitly rather than leaving it as a qualitative argument. We also agree that the transience of the complexity (~2-day timescales) and the strong disfavoring of multi-thin-component models provide independent constraints that are at least as important as the mass-budget argument, and we will make this clearer in the revised text. revision: yes

  2. Referee: Section 4.3, Eqs. (21)-(23): The mass estimate M_rot depends on W_rm,99 (fitted from polarimetric data), B_perp and l (from SSA modeling of Stokes I), and geometric/depolarization factors (D, theta_B). While these are derived from independent observables (polarized vs total intensity), the SSA model assumes a homogeneous emitting region, which the authors acknowledge is likely violated given the strong depolarization and inhomogeneous flare spectra. The sensitivity of M_rot to this assumption should be more explicitly quantified. Specifically, if the emitting region is inhomogeneous (as suggested by the sub-canonical optically thick spectral index), how much could B_perp and l change, and what is the resulting range on M_rot? The current treatment (Section 4.3.2) discusses this qualitatively but does not propagate the inhomogeneity into the mass uncertainty. This is load-bearing for the

    Authors: The referee correctly identifies that the homogeneous SSA assumption is violated by the sub-canonical optically thick spectral index and strong depolarization, and that our current treatment of this systematic is only qualitative. We agree this should be quantified. In the revised manuscript, we will add a quantitative exploration of how inhomogeneity propagates into M_rot. Our approach will be as follows. The sub-canonical spectral index (alpha ~ +1.5 rather than +2.5 during the flare rise) can be modeled as a superposition of emitting regions with a distribution of optical depths (Jones & O'Dell 1977b; Cowie & Fender 2026). For a power-law distribution of component sizes or optical depths, the effective B_perp and l can differ from the homogeneous case by factors that depend on the breadth of the distribution. We will parameterize this using the inhomogeneous synchrotron model from Cowie & Fender (2026), which allows the spectral index to deviate from the homogeneous value, and propagate the resulting range of B_perp and l through to M_rot. Based on preliminary exploration, we expect the inhomogeneity to change B_perp by up to a factor of ~2-3 and l by a comparable factor, which would propagate into M_rot (which scales as B_perp^-1 * l^2) as an uncertainty of roughly one order of magnitude in either direction. This is consistent with our existing framing of M_rot as an order-of-magnitude estimate, but we agree it should be shown explicitly. We will add this as a subsection or extended discussion within Section 4.3.2, and will update the stated uncertainty range on M_rot accordingly. We note that the central conclusion -- that M_rot ~ 10^21 g represents a small fraction (~10^-3) of the accreted mass -- is robust to this uncertainty, since even an order-of-magnitude变化仍将 revision: no

Circularity Check

0 steps flagged

No significant circularity found; derivation chain uses independent observables and standard physics

full rationale

The paper's main derivation chain proceeds as follows: (1) Transient Faraday-thick components are fitted from Stokes Q/U spectropolarimetric data (W_rm,99 ~ 100 rad/m²), with model selection via Bayesian evidence against external-screen and spectral-power-law alternatives. (2) The internal-origin argument rests on the stability of the foreground RM (-1.0±0.3 rad/m²) measured independently across epochs and angular scales, the transience of the complexity on ~2-day timescales, and the disfavoring of multi-thin-component models (ΔlnZ > 10). These are observational arguments, not self-referential. (3) The composition argument follows directly from Eq. 6 (φ_f ∝ q³/m²), a standard Faraday rotation formula: in a charge-symmetric pair plasma, electron and positron contributions cancel, so detected internal rotation requires an electron-ion component. This is basic physics, not circular. (4) The mass estimate (Eq. 21-23) combines W_rm,99 (from polarimetric QU-fitting) with B_perp ~ 200 mG and l ~ 1.3×10^14 cm (from SSA modeling of Stokes I total-intensity flare data). These are independent observables — polarized vs. total intensity — and the mass is computed from their product, not fitted to it. (5) The accreted mass M_acc comes from independent MAXI X-ray data. The fraction f_rot = M_rot/M_acc ~ 10^-3 is a comparison of two independently-derived quantities. The self-citations present (Cowie & Fender 2026 for the SSA codebase, Hughes et al. 2025a for the polkat pipeline, Hughes et al. 2025c for light curves) are methodology and data citations with publicly available code, stated assumptions that do not include the target results, and standard physics foundations (van der Laan 1966; Blandford & Königl 1979). They provide real independent support rather than circular load-bearing premises. The Anderson et al. 2016 framework for super-Gaussian Faraday-thick components is an external citation. No step in the chain reduces to its inputs by construction.

Axiom & Free-Parameter Ledger

10 free parameters · 5 axioms · 0 invented entities

No new particles, forces, dimensions, or other entities are postulated.

free parameters (10)
  • W_rm,99 = ~100 rad m^-2
    Characteristic Faraday thickness adopted from the broadest fitted thick component on 2023 October 06; used as input to mass estimate
  • B_perp = 200 (+40/-30) mG
    Magnetic field strength from SSA modeling of the 2023 October 06 flare; used to estimate line-of-sight field for Faraday mass
  • l (path length) = 1.3 (+0.3/-0.3) × 10^14 cm
    Size scale from SSA modeling; used as Faraday path length in mass estimate
  • D (depolarization fraction) = [0.01, 0.1]
    Range chosen by hand based on observed polarisation fractions of resolved ejecta (~8%) vs theoretical maximum (~75%); controls the ordered-to-turbulent field ratio
  • θ_B = uniform in cos(θ_B), [10, 80] deg
    Angle between ordered magnetic field and line of sight; broad prior, not directly constrained by data
  • γ_min = [3, 30]
    Low-energy Lorentz factor cutoff of relativistic electron distribution; affects rotativity calculation and acceleration efficiency
  • η (radiative efficiency) = 0.05
    Assumed sub-thin-disc efficiency for accreted mass estimate; not directly measured
  • t_flare = 12 hr
    Flare duration adopted for mass accretion estimate; constrained to [1, 24] hr from light curve
  • p (electron energy index) = [2, 3]
    Power-law index of non-thermal electron distribution; sampled in SSA Monte Carlo
  • E_e/E_B = log-normal centered on equipartition, 3σ range factor 50
    Ratio of electron to magnetic energy density; allows departures from equipartition in SSA modeling
axioms (5)
  • standard math Internal Faraday rotation cancels in a charge-symmetric electron-positron plasma (φ_f ∝ q^3 m^-2)
    Standard result from plasma physics; invoked in Section 4.2 to argue for electron-proton composition
  • domain assumption The synchrotron self-absorption model (homogeneous emitting region, expanding plasma) adequately describes the flare radio emission
    Used in Section 4.3.1 to derive B_perp and l; the authors note that observed flare spectra do not reach α=+2.5, indicating inhomogeneity
  • domain assumption The super-Gaussian parameterization (Eq. 15) adequately captures the Faraday-depth distribution of the jet plasma
    Used throughout Section 2.3 for QU-fitting; the authors acknowledge this cannot capture asymmetric or skewed distributions (Section 2.3)
  • domain assumption The Faraday-rotating and synchrotron-emitting plasmas are co-located
    Invoked in Section 4.3 to justify using SSA-derived B and l for the Faraday mass estimate; reasonable if rotation is internal but unverified
  • domain assumption The ordered-plus-turbulent magnetic field decomposition (Eq. 25) is an adequate model for field geometry
    Used in Section 4.3.1 to relate B_perp to ⟨B_∥⟩ via depolarization fraction D

pith-pipeline@v1.1.0-glm · 65906 in / 4513 out tokens · 93862 ms · 2026-07-08T00:31:42.084997+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

300 extracted references · 300 canonical work pages · 154 internal anchors

  1. [1]

    , year = 1974, month = jun, volume =

    Aperture Synthesis with a Non-Regular Distribution of Interferometer Baselines. , year = 1974, month = jun, volume =

    work page 1974

  2. [2]

    , keywords =

    Relaxing the isoplanatism assumption in self-calibration; applications to low-frequency radio interferometry. , keywords =. doi:10.1086/113605 , adsurl =

    work page doi:10.1086/113605

  3. [3]

    Journal of the Optical Society of America (1917-1983) , keywords =

    Restoring with Maximum Likelihood and Maximum Entropy. Journal of the Optical Society of America (1917-1983) , keywords =

    work page 1917

  4. [4]

    , keywords =

    Image reconstruction from incomplete and noisy data. , keywords =. doi:10.1038/272686a0 , adsurl =

    work page doi:10.1038/272686a0

  5. [5]

    UVMULTIFIT: A versatile tool for fitting astronomical radio interferometric data

    UVMULTIFIT: A versatile tool for fitting astronomical radio interferometric data. , keywords =. doi:10.1051/0004-6361/201322633 , archivePrefix =. 1401.4984 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201322633

  6. [6]

    Astronomy and Geophysics , year = 2016, month = jun, volume =

    The development of e-MERLIN. Astronomy and Geophysics , year = 2016, month = jun, volume =. doi:10.1093/astrogeo/atw101 , adsurl =

    work page doi:10.1093/astrogeo/atw101 2016

  7. [7]

    AOFlagger: RFI Software

    work page

  8. [8]

    Disk-jet coupling in the 2017/2018 outburst of the Galactic black hole candidate X-ray binary MAXI J1535-571

    Disk-Jet Coupling in the 2017/2018 Outburst of the Galactic Black Hole Candidate X-Ray Binary MAXI J1535-571. , keywords =. doi:10.3847/1538-4357/ab3d36 , archivePrefix =. 1906.00998 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab3d36 2017

  9. [9]

    The Varying Kinematics of Multiple Ejecta from the Black Hole X-ray Binary MAXI J1820+070

    The varying kinematics of multiple ejecta from the black hole X-ray binary MAXI J1820 + 070. , keywords =. doi:10.1093/mnras/stab1479 , archivePrefix =. 2105.09529 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stab1479

  10. [10]

    X-ray data

    The Planck-ATCA Co-eval Observations project: the bright sample. , keywords =. doi:10.1111/j.1365-2966.2011.18802.x , archivePrefix =. 1101.0225 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.18802.x 2011

  11. [11]

    M., Foley , R

    ATPMN: accurate positions and flux densities at 5 and 8 GHz for 8385 sources from the PMN survey. , keywords =. doi:10.1111/j.1365-2966.2012.20726.x , archivePrefix =. 1202.2625 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.20726.x 2012

  12. [12]

    WSClean: an implementation of a fast, generic wide-field imager for radio astronomy

    WSCLEAN: an implementation of a fast, generic wide-field imager for radio astronomy. , keywords =. doi:10.1093/mnras/stu1368 , archivePrefix =. 1407.1943 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu1368 1943

  13. [13]

    High Fidelity Deconvolution of Moderately Resolved Sources. Ph. D. thesis, New Mexico Institute of Mining and Technology. Avaible via

    work page

  14. [14]

    Synthesis Imaging in Radio Astronomy II , year = 1999, editor =

    Imaging with Non-Coplanar Arrays. Synthesis Imaging in Radio Astronomy II , year = 1999, editor =

    work page 1999

  15. [15]

    IEEE Journal of Selected Topics in Signal Processing , keywords =

    The Noncoplanar Baselines Effect in Radio Interferometry: The W-Projection Algorithm. IEEE Journal of Selected Topics in Signal Processing , keywords =. doi:10.1109/JSTSP.2008.2005290 , archivePrefix =. 0807.4161 , primaryClass =

    work page doi:10.1109/jstsp.2008.2005290 2008

  16. [16]

    High accuracy wide field imaging method in radio interferometry

    High accuracy wide-field imaging method in radio interferometry. , keywords =. doi:10.1093/mnras/stab3548 , archivePrefix =. 2101.11172 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stab3548

  17. [17]

    Efficient wide-field radio interferometry response

    Efficient wide-field radio interferometry response. , keywords =. doi:10.1051/0004-6361/202039723 , archivePrefix =. 2010.10122 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202039723 2010

  18. [18]

    , year = 2002, month = may, volume =

    Astrophysical spouts: The jet set. , year = 2002, month = may, volume =. doi:10.1038/417125a , adsurl =

    work page doi:10.1038/417125a 2002

  19. [19]

    The Physics of Gamma-Ray Bursts and Relativistic Jets

    The physics of gamma-ray bursts & relativistic jets. , keywords =. doi:10.1016/j.physrep.2014.09.008 , archivePrefix =. 1410.0679 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.physrep.2014.09.008 2014

  20. [20]

    Observational Evidence of AGN Feedback

    Observational Evidence of Active Galactic Nuclei Feedback. , keywords =. doi:10.1146/annurev-astro-081811-125521 , archivePrefix =. 1204.4114 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-081811-125521

  21. [21]

    Frontiers in Astronomy and Space Sciences , keywords =

    Multimessenger Binary Mergers Containing Neutron Stars: Gravitational Waves, Jets, and -Ray Bursts. Frontiers in Astronomy and Space Sciences , keywords =. doi:10.3389/fspas.2021.656907 , archivePrefix =. 2102.03366 , primaryClass =

    work page doi:10.3389/fspas.2021.656907 2021

  22. [22]

    WATCHDOG: A Comprehensive All-Sky Database of Galactic Black Hole X-ray Binaries

    WATCHDOG: A Comprehensive All-sky Database of Galactic Black Hole X-ray Binaries. , keywords =. doi:10.3847/0067-0049/222/2/15 , archivePrefix =. 1512.00778 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0067-0049/222/2/15

  23. [23]

    Revealing accretion onto black holes: X-ray reflection throughout three outbursts of GX 339-4

    Revealing accretion on to black holes: X-ray reflection throughout three outbursts of GX 339-4. , keywords =. doi:10.1093/mnras/stu867 , archivePrefix =. 1404.7498 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu867

  24. [24]

    Near-infrared synchrotron emission from the compact jet of GX339-4

    Near-Infrared Synchrotron Emission from the Compact Jet of GX 339-4. , keywords =. doi:10.1086/341870 , archivePrefix =. astro-ph/0205402 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/341870

  25. [25]

    Extreme Jet Ejections from the Black Hole X-ray Binary V404 Cygni

    Extreme jet ejections from the black hole X-ray binary V404 Cygni. , keywords =. doi:10.1093/mnras/stx1048 , archivePrefix =. 1704.08726 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx1048

  26. [26]

    Tracking the X-ray Polarization of the Black Hole Transient Swift J1727.8-1613 during a State Transition

    Tracking the X-ray Polarization of the Black Hole Transient Swift J1727.8-1613 during a State Transition. arXiv e-prints , keywords =. doi:10.48550/arXiv.2311.05497 , archivePrefix =. 2311.05497 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2311.05497

  27. [27]

    Jet spectral breaks in black hole X-ray binaries

    Jet spectral breaks in black hole X-ray binaries. , keywords =. doi:10.1093/mnras/sts377 , archivePrefix =. 1211.1655 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sts377

  28. [28]

    , keywords =

    A State Transition of GX 339-4 Observed with the Rossi X-Ray Timing Explorer. , keywords =. doi:10.1086/312130 , adsurl =

    work page doi:10.1086/312130

  29. [29]

    Compact stellar X-ray sources , publisher=

    Black hole binaries. Compact stellar X-ray sources , publisher=

    work page

  30. [30]

    Lecture Notes in Physics , address =

    States and Transitions in Black Hole Binaries. Lecture Notes in Physics , address =. doi:10.1007/978-3-540-76937-83 , adsurl =

    work page doi:10.1007/978-3-540-76937-83

  31. [31]

    Transient Black Hole Binaries

    Transient Black Hole Binaries. Astrophysics of Black Holes: From Fundamental Aspects to Latest Developments , year = 2016, editor =. doi:10.1007/978-3-662-52859-4_2 , archivePrefix =. 1603.07872 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/978-3-662-52859-4_2 2016

  32. [32]

    , keywords =

    A review of quasi-periodic oscillations from black hole X-ray binaries: Observation and theory. , keywords =. doi:10.1016/j.newar.2020.101524 , archivePrefix =. 2001.08758 , primaryClass =

    work page doi:10.1016/j.newar.2020.101524 2020

  33. [33]

    The evolution of black hole states

    The Evolution of Black Hole States. , keywords =. doi:10.1007/s10509-005-1197-4 , archivePrefix =. astro-ph/0412597 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s10509-005-1197-4

  34. [34]

    Compact stellar X-ray sources , year = 2006, volume =

    Rapid X-ray Variability. Compact stellar X-ray sources , year = 2006, volume =

    work page 2006

  35. [35]

    Rapid spectral transition of the black hole binary V404 Cyg

    Rapid spectral transition of the black hole binary V404 Cygni. , keywords =. doi:10.1051/0004-6361/201937191 , archivePrefix =. 2001.07503 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201937191 2001

  36. [36]

    , keywords =

    Relativistic jets as compact radio sources. , keywords =. doi:10.1086/157262 , adsurl =

    work page doi:10.1086/157262

  37. [37]

    The evolving jet spectrum of the neutron star X-ray binary Aql X-1 in transitional states during its 2016 outburst

    The evolving jet spectrum of the neutron star X-ray binary Aql X-1 in transitional states during its 2016 outburst. , keywords =. doi:10.1051/0004-6361/201832693 , archivePrefix =. 1804.08322 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201832693 2016

  38. [38]

    The "universal" radio/X-ray flux correlation : the case study of the black hole GX 339-4

    The `universal' radio/X-ray flux correlation: the case study of the black hole GX 339-4. , keywords =. doi:10.1093/mnras/sts215 , archivePrefix =. 1211.1600 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sts215

  39. [39]

    , keywords =

    A universal radio-X-ray correlation in low/hard state black hole binaries. , keywords =. doi:10.1046/j.1365-8711.2003.06791.x , archivePrefix =. astro-ph/0305231 , primaryClass =

    work page doi:10.1046/j.1365-8711.2003.06791.x 2003

  40. [40]

    , keywords =

    Hard state neutron star and black hole X-ray binaries in the radio:X-ray luminosity plane. , keywords =. doi:10.1093/mnrasl/sly083 , adsurl =

    work page doi:10.1093/mnrasl/sly083

  41. [41]

    N., Chevalier , R

    Towards a unified model for black hole X-ray binary jets. , keywords =. doi:10.1111/j.1365-2966.2004.08384.x , archivePrefix =. astro-ph/0409360 , primaryClass =

    work page doi:10.1111/j.1365-2966.2004.08384.x 2004

  42. [42]

    Lecture Notes in Physics , address =

    `Disc-Jet' Coupling in Black Hole X-Ray Binaries and Active Galactic Nuclei. Lecture Notes in Physics , address =. doi:10.1007/978-3-540-76937-85 , adsurl =

    work page doi:10.1007/978-3-540-76937-85

  43. [43]

    , keywords =

    Jets from black hole X-ray binaries: testing, refining and extending empirical models for the coupling to X-rays. , keywords =. doi:10.1111/j.1365-2966.2009.14841.x , archivePrefix =. 0903.5166 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.14841.x 2009

  44. [44]

    , keywords =

    A Fundamental Plane of black hole activity. , keywords =. doi:10.1046/j.1365-2966.2003.07017.x , archivePrefix =. astro-ph/0305261 , primaryClass =

    work page doi:10.1046/j.1365-2966.2003.07017.x 2003

  45. [45]

    X-ray data

    Radiatively efficient accreting black holes in the hard state: the case study of H1743-322. , keywords =. doi:10.1111/j.1365-2966.2011.18433.x , adsurl =

    work page doi:10.1111/j.1365-2966.2011.18433.x 2011

  46. [46]

    Rapid compact jet quenching in the Galactic black hole candidate X-ray binary MAXI J1535-571

    Rapid compact jet quenching in the Galactic black hole candidate X-ray binary MAXI J1535-571. , keywords =. doi:10.1093/mnras/staa2650 , archivePrefix =. 2008.11216 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/staa2650 2008

  47. [47]

    , keywords =

    Radio Observations of the 1989 Transient Event in V404 Cygni (= GS 2023+338). , keywords =. doi:10.1086/171996 , adsurl =

    work page doi:10.1086/171996 1989

  48. [48]

    , year = 1995, month = jun, volume =

    Episodic ejection of relativistic jets by the X-ray transient GRO J1655 - 40. , year = 1995, month = jun, volume =. doi:10.1038/375464a0 , adsurl =

    work page doi:10.1038/375464a0 1995

  49. [49]

    A rapidly-changing jet orientation in the stellar-mass black hole V404 Cygni

    A rapidly changing jet orientation in the stellar-mass black-hole system V404 Cygni. , keywords =. doi:10.1038/s41586-019-1152-0 , archivePrefix =. 1906.05400 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41586-019-1152-0 1906

  50. [50]

    The black hole transient MAXI J1348-630: evolution of the compact and transient jets during its 2019/2020 outburst

    The black hole transient MAXI J1348-630: evolution of the compact and transient jets during its 2019/2020 outburst. , keywords =. doi:10.1093/mnras/stab864 , archivePrefix =. 2103.12190 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stab864 2019

  51. [51]

    Resolved, expanding jets in the Galactic black hole candidate XTE J1908+094

    Resolved, expanding jets in the Galactic black hole candidate XTE J1908+094. , keywords =. doi:10.1093/mnras/stx526 , archivePrefix =. 1703.02110 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx526

  52. [52]

    , keywords =

    Radio Emission from Conical Jets Associated with X-Ray Binaries. , keywords =. doi:10.1086/166318 , adsurl =

    work page doi:10.1086/166318

  53. [53]

    , year = 1966, month = sep, volume =

    A Model for Variable Extragalactic Radio Sources. , year = 1966, month = sep, volume =. doi:10.1038/2111131a0 , adsurl =

    work page doi:10.1038/2111131a0 1966

  54. [54]

    , keywords =

    MAXI J1848-015: The First Detection of Relativistically Moving Outflows from a Globular Cluster X-Ray Binary. , keywords =. doi:10.3847/2041-8213/accde1 , adsurl =

    work page doi:10.3847/2041-8213/accde1 2041

  55. [55]

    Relativistic X-ray jets from the black hole X-ray binary MAXI J1820+070

    Relativistic X-Ray Jets from the Black Hole X-Ray Binary MAXI J1820+070. , keywords =. doi:10.3847/2041-8213/ab88b6 , archivePrefix =. 2004.06416 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/ab88b6 2041

  56. [56]

    , keywords =

    MERLIN observations of relativistic ejections from GRS 1915+105. , keywords =. doi:10.1046/j.1365-8711.1999.02364.x , archivePrefix =. astro-ph/9812150 , primaryClass =

    work page doi:10.1046/j.1365-8711.1999.02364.x 1915

  57. [57]

    Internal shock model for Microquasars

    Internal shock model for microquasars. , keywords =. doi:10.48550/arXiv.astro-ph/0001501 , archivePrefix =. astro-ph/0001501 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0001501

  58. [58]

    , keywords =

    Shock-in-jet model for quasars and microquasars. , keywords =

    work page

  59. [59]

    Quasar jet emission model applied to the microquasar GRS 1915+105

    Quasar jet emission model applied to the microquasar GRS 1915+105. , keywords =. doi:10.1051/0004-6361:20040010 , archivePrefix =. astro-ph/0401275 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20040010 1915

  60. [60]

    High Energy Astrophysics

    work page

  61. [61]

    , year = 1969, month = jan, volume =

    Developments in the Theory of Synchrotron Radiation and its Reabsorption. , year = 1969, month = jan, volume =. doi:10.1146/annurev.aa.07.090169.002111 , adsurl =

    work page doi:10.1146/annurev.aa.07.090169.002111 1969

  62. [62]

    J., Almaini, O., et al

    A highly polarized radio jet during the 1998 outburst of the black hole transient XTE J1748-288. , keywords =. doi:10.1111/j.1365-2966.2007.11846.x , archivePrefix =. 0705.1125 , primaryClass =

    work page doi:10.1111/j.1365-2966.2007.11846.x 1998

  63. [63]

    XTE J1752-223 in outburst: a persistent radio jet, dramatic flaring, multiple ejections and linear polarisation

    XTE J1752-223 in outburst: a persistent radio jet, dramatic flaring, multiple ejections and linear polarization. , keywords =. doi:10.1093/mnras/stt493 , archivePrefix =. 1303.6702 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt493

  64. [64]

    The evolving polarised jet of black hole candidate Swift J1745-26

    The evolving polarized jet of black hole candidate Swift J1745-26. , keywords =. doi:10.1093/mnras/stt2125 , archivePrefix =. 1309.4926 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt2125

  65. [65]

    Radio polarimetry as a probe of unresolved jets: the 2013 outburst of XTE J1908+094

    Radio polarimetry as a probe of unresolved jets: the 2013 outburst of XTE J1908+094. , keywords =. doi:10.1093/mnras/stv1252 , archivePrefix =. 1506.01141 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv1252 2013

  66. [66]

    N., Chevalier , R

    A transient large-scale relativistic radio jet from GX 339-4. , keywords =. doi:10.1111/j.1365-2966.2004.07435.x , archivePrefix =. astro-ph/0311452 , primaryClass =

    work page doi:10.1111/j.1365-2966.2004.07435.x 2004

  67. [67]

    , keywords =

    A decade of high-resolution radio observations of GRS1915+105. , keywords =. doi:10.1111/j.1365-2966.2009.15838.x , archivePrefix =. 0910.1779 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15838.x 2009

  68. [68]

    Short Timescale Evolution of the Polarized Radio Jet during V404 Cygni's 2015 Outburst

    Short time-scale evolution of the polarized radio jet during V404 Cygni's 2015 outburst. , keywords =. doi:10.1093/mnras/stad396 , archivePrefix =. 2301.13281 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stad396 2015

  69. [69]

    N., Chevalier , R

    Polarization and kinematic studies of SS 433 indicate a continuous and decelerating jet. , keywords =. doi:10.1111/j.1365-2966.2004.08285.x , adsurl =

    work page doi:10.1111/j.1365-2966.2004.08285.x 2004

  70. [70]

    R., Schr \"o der, K.-P., Hurley, J

    Depolarization and Faraday effects in galaxies. , keywords =. doi:10.1046/j.1365-8711.1998.01782.x , adsurl =

    work page doi:10.1046/j.1365-8711.1998.01782.x 1998

  71. [71]

    Broadband radio spectro-polarimetric observations of high Faraday rotation measure AGN

    Broadband radio spectro-polarimetric observations of high-Faraday-rotation-measure AGN. , keywords =. doi:10.1051/0004-6361/201731804 , archivePrefix =. 1801.09731 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201731804

  72. [72]

    , keywords =

    A model for the magnetic-field structure in extended radio sources. , keywords =. doi:10.1093/mnras/193.3.439 , adsurl =

    work page doi:10.1093/mnras/193.3.439

  73. [73]

    Modeling the kinematics of the decelerating jets from the black hole X-ray binary MAXI J1348$-$630

    Modelling the kinematics of the decelerating jets from the black hole X-ray binary MAXI J1348-630. , keywords =. doi:10.1093/mnras/stac329 , archivePrefix =. 2202.01514 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stac329

  74. [74]

    Constraining the physical properties of large-scale jets from black hole X-ray binaries and their impact on the local environment with blast-wave dynamical models

    Constraining the physical properties of large-scale jets from black hole X-ray binaries and their impact on the local environment with blast-wave dynamical models. , keywords =. doi:10.1093/mnras/stae2049 , archivePrefix =. 2405.16624 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stae2049

  75. [75]

    The Imaging X-Ray Polarimetry Explorer (IXPE): Pre-Launch

    The Imaging X-Ray Polarimetry Explorer (IXPE): Pre-Launch. Journal of Astronomical Telescopes, Instruments, and Systems , keywords =. doi:10.1117/1.JATIS.8.2.026002 , archivePrefix =. 2112.01269 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1117/1.jatis.8.2.026002

  76. [76]

    Prospects for differentiating extended coronal geometries in AGNs with the IXPE mission

    Prospects for differentiating extended coronal geometries in AGNs with the IXPE mission. , keywords =. doi:10.1093/mnras/stab3745 , archivePrefix =. 2112.11268 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stab3745

  77. [77]

    X-Ray Polarized View on the Accretion Geometry in the X-Ray Binary Circinus X-1

    X-Ray Polarized View of the Accretion Geometry in the X-Ray Binary Circinus X-1. , keywords =. doi:10.3847/2041-8213/ad1832 , archivePrefix =. 2311.04632 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/ad1832 2041

  78. [78]

    Polarized x-rays constrain the disk-jet geometry in the black hole x-ray binary Cygnus X-1

    Polarized x-rays constrain the disk-jet geometry in the black hole x-ray binary Cygnus X-1. Science , keywords =. doi:10.1126/science.add5399 , archivePrefix =. 2206.09972 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.add5399

  79. [79]

    Optical/infrared polarised emission in X-ray binaries

    Optical/Infrared Polarised Emission in X-ray Binaries. Galaxies , keywords =. doi:10.3390/galaxies6010003 , archivePrefix =. 1801.06713 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3390/galaxies6010003

  80. [80]

    Optical precursors to X-ray binary outbursts

    Optical precursors to X‑ray binary outbursts. Astronomische Nachrichten , keywords =. doi:10.1002/asna.201913610 , archivePrefix =. 1903.04519 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1002/asna.201913610 1903

Showing first 80 references.