Pith. sign in

REVIEW 2 major objections 5 minor 86 references

At low luminosities, magnetospheric accretion in X-ray pulsars runs through partially ionized plasma, not the fully ionized flow usually assumed.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · grok-4.5

2026-07-14 12:28 UTC pith:MMI7S4CM

load-bearing objection Solid first quantitative thermal-balance calculation showing partial recombination in low-L magnetospheric flows; pure-H LTE is the real soft spot, but the temperature drop itself looks robust. the 2 major comments →

arxiv 2607.10342 v1 pith:MMI7S4CM submitted 2026-07-11 astro-ph.HE astro-ph.SR

Magnetospheric flows in X-ray pulsars II: Heating, cooling and ionization degree at sub-critical accretion

Alexander A. Mushtukov , Alexander Y. Potekhin , Valery F. Suleimanov , Andrew Yu , Sergey S. Tsygankov This is my paper
classification astro-ph.HE astro-ph.SR
keywords X-ray pulsarsmagnetospheric accretionpartial ionizationCompton heatingfree-free coolingcyclotron emissionsub-critical accretionneutron stars
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

X-ray pulsars accrete through a magnetosphere that is usually treated as fully ionized plasma. This paper calculates the thermal balance of that flow at sub-critical luminosities, balancing Compton heating by surface X-rays, compressional heating, and free-free plus cyclotron cooling. The calculation shows that the flow cools efficiently near the neutron star: at L less than about 10^35 erg/s the temperature can drop to a few tens of eV. In the strong surface fields of these objects, that temperature allows partial recombination of pure hydrogen into neutral atoms. External illumination re-ionizes only a geometrically thin layer just above the surface, so most of the channel remains weakly ionized. The result matters because ionization controls how the plasma couples to the magnetic field, how it brakes near the surface, and how cyclotron and polarization signals form.

Core claim

In the sub-critical regime the interplay of Compton heating, compressional heating, and free-free (plus cyclotron) cooling drives the magnetospheric flow temperature near the stellar surface down to a few tens of eV at L < 10^35 erg s^{-1}. At those temperatures and B ~ 10^{12}–10^{13} G, pure-hydrogen plasma partially recombines; photoionization restores a higher ionization fraction only inside a thin layer of thickness comparable to the channel width. Magnetospheric accretion at low luminosity therefore proceeds through a partially ionized medium rather than a fully ionized flow.

What carries the argument

The thermal-balance equation along dipole field lines: dT/dt = (2 m_p / 3) (Q+ − Q−)/Σ, with Q+ from Compton scattering of surface X-rays plus compressional heating and Q− from free-free and cyclotron emission, solved on a pre-computed dynamical structure and closed with a strong-field Saha ionization equilibrium (partial LTE) plus a Monte-Carlo photoionization layer.

Load-bearing premise

The ionization state is taken from pure-hydrogen local thermodynamic equilibrium with recombination treated as instantaneous once the Saha estimate gives a substantial neutral fraction; if metals, molecules, or non-equilibrium timescales keep the plasma more ionized, the partial-recombination claim fails.

What would settle it

A simultaneous measurement of near-surface temperature (or free-electron density) and cyclotron-line strength or polarization degree at L ≲ 10^{34}–10^{35} erg s^{-1}: if the plasma remains fully ionized or the re-ionized layer is much thicker than the channel width, the central claim is ruled out.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Cyclotron scattering features at low luminosity form in a medium whose free-electron density is lower than the fully ionized assumption, altering line optical depth and Doppler shift.
  • Incomplete magnetic coupling via ambipolar diffusion of neutrals can modify flow geometry and dynamics near the surface.
  • A thin partially recombined layer changes the dielectric tensor and therefore the polarization of emergent X-rays.
  • Radiative braking efficiency in the upper atmosphere is reduced when free electrons are scarce, changing the structure of the deceleration region.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The luminosity threshold for partial recombination scales with surface field strength, so sources with different B should show the transition at different L, offering a clean multi-source test.
  • If metals are present they would raise line cooling and lower the recombination threshold luminosity, making partial ionization even more widespread than the pure-H calculation indicates.
  • Pulse-profile and aperiodic-variability models that assume fully ionized Thomson opacity need re-examination below ~10^{35} erg s^{-1}.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

2 major / 5 minor

Summary. The paper models the thermal balance of magnetospheric accretion flows in sub-critical X-ray pulsars (L ≲ 10^37 erg s^{-1}). Dynamics are taken from a prior dipole-channel calculation; the energy equation includes Compton heating by surface X-rays (Monte Carlo), compressional heating, free-free cooling, and an approximate cyclotron term. Temperature profiles are computed as functions of L, Bp and beaming parameter ξ. Near the surface T falls to a few tens of eV at L ≲ 10^35 erg s^{-1}. For pure hydrogen in B ∼ 10^{12}–10^{13} G the magnetic Saha equation then yields a substantial neutral fraction over an extended radial range, while photoionization re-ionizes only a geometrically thin layer of thickness ∼ d immediately above the surface. The central claim is that low-luminosity magnetospheric accretion proceeds through a partially ionized medium rather than the fully ionized flow usually assumed.

Significance. If the result holds, it changes the microphysical boundary conditions used for cyclotron-line formation, radiative braking, polarization and magnetic coupling at low accretion rates. The work is constructive: the energy equation is built from standard rates, the dynamical structure is imported from an independent calculation, and the two most uncertain pieces (LTE cyclotron cooling and resonant magnetic scattering) are stress-tested in Appendices C and D and shown not to control the near-surface temperature minimum. The pure-H magnetic Saha calculation and the photoionization Monte Carlo supply a concrete, falsifiable prediction (partial recombination below a luminosity that rises with Bp; thin re-ionized skin of thickness ∼ d). That combination of first-principles rates, sensitivity tests and a clear observational implication makes the paper a useful contribution even if later work with metals or non-LTE kinetics revises the neutral fraction.

major comments (2)
  1. The ionization claim rests on pure-hydrogen partial LTE (magnetic Saha, eqs. 60–61; §2.3.1–2.3.2) with recombination treated as instantaneous once the LTE estimate gives substantial f_H. Timescale arguments (tc,e-e, tneut, Γ_rec^{-1} ≪ free-fall) are given and free-free cooling is shown to set the temperature minimum (Appendix C), so the temperature drop itself is robust. However, metals and molecules are omitted, and free-free is already noted as a lower bound on cooling (§2.2.1). A short quantitative estimate of how line cooling or a solar-composition Saha solution would shift the recombination luminosity (or an explicit statement that the pure-H case is a limiting lower bound on ionization) is needed before the claim can be taken as generic for XRPs.
  2. Photoionization is treated by a Monte Carlo that forbids recombination inside h_max = 10d and enforces I(h_j) ≥ I(h_{j+1}) (§3.2, eq. 67). The resulting skin thickness ∼ d is therefore partly by construction. A brief check that the recombination time remains longer than the free-fall time across that layer (or a run that allows local recombination) would confirm that the thin re-ionized layer is physical rather than an artifact of the no-recombination assumption.
minor comments (5)
  1. Fig. 3 caption refers to beaming parameter “x”; the text and eq. (29) use ξ. Align notation.
  2. Eq. (35) for channel thickness H ≈ Hd sin^{2} heta sin χ is used throughout; a one-sentence justification that the result is insensitive to order-unity changes in H would strengthen the free-free cooling estimates.
  3. The abstract states “a few tens of eV at L < 10^{35}”; Fig. 3a shows a few eV at 10^{34}. A single clarifying sentence on the luminosity range would avoid over-reading the abstract.
  4. Appendix E shows that a cutoff power-law spectrum raises near-surface T by at most a factor ∼2. Mentioning this bound once in the main text (§4.1) would help readers who skip the appendices.
  5. The discussion of cyclotron-line correlations (§5) correctly notes that the observed transition luminosities are higher than the recombination threshold found here; the caveat is already present and should be retained.

Circularity Check

1 steps flagged

No significant circularity: temperature and ionization follow from independent heating/cooling rates on fixed dynamics imported from prior work.

specific steps
  1. self citation load bearing [§2 (Model) and §3.1]
    "The dynamical structure of the magnetospheric flow adopted in this work follows our previous studies (Mushtukov et al. 2024). ... Calculating dynamical structure of the flow (i.e., distributions of the surface density and velocity along magnetic field lines), we follow Mushtukov et al. (2024)."

    The velocity and surface-density profiles that enter the energy equation and the ionization calculation are taken wholesale from the authors' own prior paper rather than re-derived. This is ordinary modular reuse and does not force the temperature or ionization results (which are computed independently once the dynamics are fixed), so the circularity is minor and non-load-bearing for the central claim.

full rationale

The paper's central claim (near-surface T falling to tens of eV at L ≲ 10^35 erg s^{-1}, permitting partial H recombination under strong B, with only a thin photoionized layer) is obtained by solving the energy equation with explicit Compton, compressional, free-free and (approximate) cyclotron terms, then feeding the resulting T(ρ) into the magnetic Saha equation under partial LTE. Dynamics (v, Σ, A(s)) are pre-computed and held fixed from Mushtukov et al. (2024); that import is ordinary modular reuse of an independent dynamical calculation, not a re-statement of the thermal or ionization result. No free parameters are fitted to the ionization degree or to any observational proxy of it; the Monte-Carlo Compton maps and Saha evaluation are forward calculations. Sensitivity tests (Appendix C removing cyclotron cooling; Appendix D/E varying resonant scattering and spectral shape) confirm the near-surface T minimum is robust. The pure-H LTE idealization is an assumption, not a circular step. Score 1 only for the single non-load-bearing self-citation of the dynamical structure.

Axiom & Free-Parameter Ledger

3 free parameters · 5 axioms · 0 invented entities

The central claim rests on standard plasma microphysics plus a handful of modeling choices (pure H, partial LTE, dipole geometry, dynamics imported from prior work). No new particles or forces are introduced; free parameters are limited to conventional astrophysical inputs (L, Bp, beam pattern ξ) that are scanned rather than fitted to the ionization result.

free parameters (3)
  • beaming parameter ξ
    Controls the angular distribution of surface X-rays (Eq. 29); scanned over 0.5–2 but not fitted to data.
  • surface magnetic field Bp
    Scanned over 5e12–1e14 G; sets magnetospheric size and binding energies.
  • accretion luminosity L
    Primary control parameter; scanned over 1e33–1e36 erg/s.
axioms (5)
  • domain assumption Partial LTE (Boltzmann populations of particles and atoms) holds because collisional and recombination timescales are much shorter than free-fall time through the strong-field zone.
    Stated and estimated in §2.3.1; underpins the entire ionization calculation.
  • domain assumption Plasma is pure hydrogen; metals and molecules are neglected.
    Explicit throughout; line cooling and molecular formation would alter the cooling function and Saha balance.
  • domain assumption Radiative force is negligible and dynamics can be pre-computed independently of the thermal structure.
    Justified for L ≲ 1e37 erg/s in §2 and §3; allows separation of dynamics and thermal balance.
  • domain assumption Dipole magnetic field geometry with α=0 (aligned rotator).
    Adopted for simplicity in §2.1.1; sets the mapping from θ to r and B.
  • domain assumption Magnetic free-free (rather than LTE cyclotron) is the dominant true photon production channel in the strongly quantizing regime; the LTE cyclotron term is only an upper bound.
    Discussed in Appendix C; the paper shows the near-surface temperature is insensitive to removing the term.

pith-pipeline@v1.1.0-grok45 · 34930 in / 2805 out tokens · 32614 ms · 2026-07-14T12:28:35.471265+00:00 · methodology

0 comments
read the original abstract

Magnetospheric accretion flows in X-ray pulsars shape their spectra, polarization, and variability. We model the thermal balance of the flow enveloping the neutron star magnetosphere in the sub-critical regime ($L \lesssim 10^{37}\,\mathrm{erg\,s^{-1}}$), where radiation forces do not control the dynamics and single Compton scatterings dominate. The energy budget includes Compton heating by surface X-rays, compressional (adiabatic) heating in the converging flow, and radiative cooling dominated by free-free emission and contributed also by cyclotron emission. We show that the interplay of these processes leads to efficient cooling of the flow in the inner magnetosphere. We compute the flow temperature profile as a function of luminosity and find that near the stellar surface the temperature can fall to a few tens of eV at $L < 10^{35}\,\mathrm{erg\,s^{-1}}$. Under such conditions, the accreting plasma, modelled here as pure hydrogen, is no longer fully ionized. In the strong magnetic fields typical for X-ray pulsars, such temperatures permit partial recombination of electrons and protons into neutral hydrogen. As a result, a significant fraction of the flow becomes weakly ionized, while external illumination ionizes this gas only partially within a geometrically thin layer immediately above the neutron star surface. This implies that magnetospheric accretion at low luminosities proceeds through a partially ionized medium, in contrast to the commonly assumed fully ionized flow.

Figures

Figures reproduced from arXiv: 2607.10342 by Alexander A. Mushtukov, Alexander Y. Potekhin, Andrew Yu, Sergey S. Tsygankov, Valery F. Suleimanov.

Figure 1
Figure 1. Figure 1: The schematic representation of the dipole magnetic field lines, where Rm denotes the inner disc radius, θ is the magnetic colatitude of a given point and χ is the angle between the position vector of this point and the tangent to the field line (19). Panel A illustrates the global geometry of the magnetosphere and the main forces acting on the accretion flow, including gravita￾tional, centrifugal and pres… view at source ↗
Figure 2
Figure 2. Figure 2: Profiles of the thermal balance in the magnetospheric ac￾cretion flow. Panel a: temperature of the flow as a function of the coordinate θ along the magnetic field line. For the reference, the upper horizontal axis shows the radial coordinate in units of NS radii. Panel b: the mass density (solid black line) and local B-field strength (dashed red line) in accretion channel. Panel c: heating and cooling rate… view at source ↗
Figure 3
Figure 3. Figure 3: Temperature distribution along the accretion flux trajec￾tory in the magnetosphere of an XRP, parametrized by the mag￾netic colatitude θ (see Fig. 1A). The fiducial case is given by solid red line and corresponds to the accretion luminosity L = 1035 erg s−1 , magnetic field at the pole Bp = 1013 G and beaming parameter in equation (29) x. NS mass and radius are fixed at M = 1.4M⊙ and R = 106 cm. Panel (a) … view at source ↗
Figure 4
Figure 4. Figure 4: Ionization degree of the accretion flow above the NS sur￾face (at height h ∼ 3d), computed assuming the Boltzmann distri￾bution, as a function of accretion luminosity. Curves correspond to different surface magnetic fields: Bp = 5×1012 G (solid), 1×1013 G (dashed), 2 × 1013 G (dotted), and 1 × 1014 G (dash–dot). At suffi￾ciently low luminosities the flow remains weakly ionized. Above a characteristic trans… view at source ↗
Figure 6
Figure 6. Figure 6: Ionization structure of the flow at intermediate dis￾tances from the NS. The calculations are shown for a fixed sur￾face magnetic field Bp = 1013 G and four accretion luminosi￾ties: L = 1034 erg s−1 (solid line), 2 × 1034 erg s−1 (dashed), 5 × 1034 erg s−1 (dashed-dotted), and 1035 erg s−1 (dotted). The upper panel shows the ionization degree calculated from the lo￾cal temperature and density along the mag… view at source ↗

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

86 extracted references · 38 canonical work pages · 26 internal anchors

  1. [1]

    Outburst of GX 304-1 monitored with INTEGRAL: positive correlation between the cyclotron line energy and flux

    Outburst of GX 304-1 monitored with INTEGRAL: positive correlation between the cyclotron line energy and flux. , keywords =. doi:10.1051/0004-6361/201219385 , archivePrefix =. 1205.5475 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201219385

  2. [2]

    Discovery of a flux-related change of the cyclotron line energy in Her X-1

    Discovery of a flux-related change of the cyclotron line energy in Hercules X-1. , keywords =. doi:10.1051/0004-6361:20077098 , archivePrefix =. astro-ph/0702490 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20077098

  3. [3]

    The quiescent X-ray emission of three transient X-ray pulsars

    The Quiescent X-Ray Emission of Three Transient X-Ray Pulsars. , keywords =. doi:10.1086/343074 , archivePrefix =. astro-ph/0207422 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/343074

  4. [4]

    Cyclotron line evolution revealed with pulse-to-pulse analysis in the 2020 outburst of 1A 0535+262

    Cyclotron line evolution revealed with pulse-to-pulse analysis in the 2020 outburst of 1A 0535+262. , keywords =. doi:10.1093/mnras/stae352 , archivePrefix =. 2403.11815 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stae352 2020

  5. [5]

    Relation of cyclotron resonant energy and luminosity in a strongly magnetized neutron star GRO J1008-57 observed by Insight-HXMT

    Relation of Cyclotron Resonant Energy and Luminosity in a Strongly Magnetized Neutron Star GRO J1008-57 Observed by Insight-HXMT. , keywords =. doi:10.3847/1538-4357/ac1268 , archivePrefix =. 2107.03267 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ac1268

  6. [6]

    Physics Uspekhi , keywords =

    Atmospheres and radiating surfaces of neutron stars. Physics Uspekhi , keywords =. doi:10.3367/UFNe.0184.201408a.0793 , archivePrefix =. 1403.0074 , primaryClass =

    doi:10.3367/ufne.0184.201408a.0793

  7. [8]

    , keywords =

    Study of the X-ray pulsar IGR J19294+1816 with NuSTAR: Detection of cyclotron line and transition to accretion from the cold disk. , keywords =. doi:10.1051/0004-6361/201833786 , archivePrefix =. 1811.08912 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201833786

  8. [9]

    , keywords =

    Stable accretion from a cold disc in highly magnetized neutron stars. , keywords =. doi:10.1051/0004-6361/201630248 , archivePrefix =. 1703.04528 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201630248

  9. [10]

    Cyclotron emission, absorption, and the two faces of X-ray pulsar A 0535+262

    Cyclotron emission, absorption, and the two faces of X-ray pulsar A 0535+262. , keywords =. doi:10.1093/mnrasl/slz079 , archivePrefix =. 1905.09496 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnrasl/slz079 1905

  10. [11]

    , keywords =

    SRG/ART-XC and NuSTAR Observations of the X-Ray pulsar GRO J1008-57 in the Lowest Luminosity State. , keywords =. doi:10.3847/1538-4357/abec43 , archivePrefix =. 2103.05728 , primaryClass =

    work page doi:10.3847/1538-4357/abec43

  11. [12]

    Dramatic spectral transition of X-ray pulsar GX 304-1 in low luminous state

    Dramatic spectral transition of X-ray pulsar GX 304-1 in low luminous state. , keywords =. doi:10.1093/mnrasl/sly236 , archivePrefix =. 1810.13307 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnrasl/sly236

  12. [13]

    , keywords =

    Collisional Plasma Models with APEC/APED: Emission-Line Diagnostics of Hydrogen-like and Helium-like Ions. , keywords =. doi:10.1086/322992 , archivePrefix =. astro-ph/0106478 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/322992

  13. [14]

    Astrophysical Bulletin , keywords =

    Ultraluminous X-Ray Sources. Astrophysical Bulletin , keywords =. doi:10.1134/S1990341321010077 , archivePrefix =. 2105.10537 , primaryClass =

    Pith/arXiv arXiv doi:10.1134/s1990341321010077

  14. [15]

    Photoionization of hydrogen in atmospheres of magnetic neutron stars

    Photoionization of Hydrogen in Atmospheres of Magnetic Neutron Stars. , keywords =. doi:10.1086/304250 , archivePrefix =. astro-ph/9702004 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/304250

  15. [16]

    , keywords =

    Photoionization of the Hydrogen Atom in Strong Magnetic Fields. , keywords =. doi:10.1086/172515 , adsurl =

    work page doi:10.1086/172515

  16. [17]

    Magnetospheric Flows in X-ray Pulsars I: Instability at super-Eddington regime of accretion

    Magnetospheric flows in X-ray Pulsars I : Instability at super-Eddington regime of accretion. , keywords =. doi:10.1093/mnras/stae781 , archivePrefix =. 2402.12965 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stae781

  17. [18]

    , keywords =

    The critical accretion luminosity for magnetized neutron stars. , keywords =. doi:10.1093/mnras/stu2484 , archivePrefix =. 1409.6457 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stu2484

  18. [19]

    GK Per and EX Hya: Intermediate polars with small magnetospheres

    GK Persei and EX Hydrae: Intermediate polars with small magnetospheres. , keywords =. doi:10.1051/0004-6361/201628301 , archivePrefix =. 1604.00232 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201628301

  19. [20]

    Partially Ionized Plasmas in Astrophysics

    Partially Ionized Plasmas in Astrophysics. , keywords =. doi:10.1007/s11214-018-0485-6 , archivePrefix =. 1707.07975 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s11214-018-0485-6

  20. [21]

    , keywords =

    Electromagnetic Polarization in Partially Ionized Plasmas with Strong Magnetic Fields and Neutron Star Atmosphere Models. , keywords =. doi:10.1086/422679 , archivePrefix =. astro-ph/0405383 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/422679

  21. [22]

    On the maximum accretion luminosity of magnetized neutron stars: connecting X-ray pulsars and ultraluminous X-ray sources

    On the maximum accretion luminosity of magnetized neutron stars: connecting X-ray pulsars and ultraluminous X-ray sources. , keywords =. doi:10.1093/mnras/stv2087 , archivePrefix =. 1506.03600 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv2087

  22. [23]

    Astronomy Reports , keywords =

    The thickness of accretion -disks: Theory and observations. Astronomy Reports , keywords =. doi:10.1134/S1063772907070049 , adsurl =

    doi:10.1134/s1063772907070049

  23. [24]

    Volume II: Gas Dynamics

    The Physics of Astrophysics. Volume II: Gas Dynamics

  24. [25]

    , keywords =

    Positive correlation between the cyclotron line energy and luminosity in sub-critical X-ray pulsars: Doppler effect in the accretion channel. , keywords =. doi:10.1093/mnras/stv2182 , archivePrefix =. 1509.05628 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stv2182

  25. [26]

    X-ray emission from magnetized neutron star atmospheres at low mass-accretion rates. I. Phase-averaged spectrum. , keywords =. doi:10.1051/0004-6361/202040228 , archivePrefix =. 2104.06802 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202040228

  26. [27]

    , keywords =

    Spectrum formation in X-ray pulsars at very low mass accretion rate: Monte Carlo approach. , keywords =. doi:10.1093/mnras/stab811 , archivePrefix =. 2006.13596 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stab811 2006

  27. [28]

    Observational appearance

    Black holes in binary systems. Observational appearance. , year = 1973, month = jan, volume =

    1973

  28. [29]

    Radiative Processes in Astrophysics

  29. [30]

    , keywords =

    Statistical features of multiple Compton scattering in a strong magnetic field. , keywords =. doi:10.1103/PhysRevD.105.103027 , archivePrefix =. 2204.12271 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevd.105.103027

  30. [31]

    The X-ray polarimetry view of the accreting pulsar Cen X-3

    The X-Ray Polarimetry View of the Accreting Pulsar Cen X-3. , keywords =. doi:10.3847/2041-8213/aca486 , archivePrefix =. 2209.02447 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aca486 2041

  31. [32]

    Soviet Astronomy Letters , keywords =

    Plasma and radiation processes at the Alfven surface of an accreting neutron star. Soviet Astronomy Letters , keywords =

  32. [33]

    , keywords =

    Observational properties of accreting neutron stars with an optically thick envelope. , keywords =. doi:10.1093/mnras/stad2391 , adsurl =

    work page doi:10.1093/mnras/stad2391

  33. [34]

    , keywords =

    Timing properties of ULX pulsars: optically thick envelopes and outflows. , keywords =. doi:10.1093/mnras/sty3525 , archivePrefix =. 1811.02049 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/sty3525

  34. [35]

    , keywords =

    Optically thick envelopes around ULXs powered by accreating neutron stars. , keywords =. doi:10.1093/mnras/stx141 , archivePrefix =. 1612.00964 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stx141

  35. [36]

    Wind accretion: Theory and Observations

    Wind accretion: Theory and observations. Astronomy Reports , keywords =. doi:10.1134/S1063772915070112 , archivePrefix =. 1407.3163 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1134/s1063772915070112

  36. [37]

    , keywords =

    Theory of quasi-spherical accretion in X-ray pulsars. , keywords =. doi:10.1111/j.1365-2966.2011.20026.x , archivePrefix =. 1110.3701 , primaryClass =

    doi:10.1111/j.1365-2966.2011.20026.x 2011

  37. [38]

    Hard Spectra of X-Ray Pulsars from INTEGRAL Data

    Hard Spectra of X-ray Pulsars from INTEGRAL Data. Astronomy Letters , keywords =. doi:10.1134/1.2123288 , archivePrefix =. astro-ph/0509525 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1134/1.2123288

  38. [39]

    , keywords =

    Radiative Widths and Splitting of Cyclotron Lines in Superstrong Magnetic Fields. , keywords =. doi:10.1086/170611 , adsurl =

    doi:10.1086/170611

  39. [40]

    A new radiative cooling curve based on an up to date plasma emission code

    A new radiative cooling curve based on an up-to-date plasma emission code. , keywords =. doi:10.1051/0004-6361/200912495 , archivePrefix =. 0909.5204 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200912495

  40. [41]

    arXiv e-prints , keywords =

    Propeller effect in action: Unveiling quenched accretion in the transient X-ray pulsar 4U 0115+63. arXiv e-prints , keywords =. doi:10.48550/arXiv.2509.09860 , archivePrefix =. 2509.09860 , primaryClass =

    work page doi:10.48550/arxiv.2509.09860

  41. [42]

    , keywords =

    Quantum Effects in Cyclotron Plasma Absorption. , keywords =. doi:10.1007/BF00642366 , adsurl =

    doi:10.1007/bf00642366

  42. [43]

    Magnetized neutron star atmospheres: beyond cold plasma approximation

    Magnetized Neutron Star Atmospheres: Beyond the Cold Plasma Approximation. , keywords =. doi:10.1088/0004-637X/751/1/15 , archivePrefix =. 1201.5527 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/751/1/15

  43. [44]

    Propagation and Polarisation of Radiation in Cosmic Media

  44. [45]

    , year = 1975, month = feb, volume =

    Why the Number of Galactic X-ray Stars Is so Small?. , year = 1975, month = feb, volume =

    1975

  45. [46]

    "Propeller" Regime of Disk Accretion to Rapidly Rotating Stars

    ``Propeller'' Regime of Disk Accretion to Rapidly Rotating Stars. , keywords =. doi:10.1086/503379 , archivePrefix =. astro-ph/0603249 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/503379

  46. [47]

    Propeller effect in two brightest transient X-ray pulsars: 4U 0115+63 and V 0332+53

    Propeller effect in two brightest transient X-ray pulsars: 4U 0115+63 and V 0332+53. , keywords =. doi:10.1051/0004-6361/201628236 , archivePrefix =. 1602.03177 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201628236

  47. [48]

    , keywords =

    Cyclotron lines in highly magnetized neutron stars. , keywords =. doi:10.1051/0004-6361/201834479 , archivePrefix =. 1812.03461 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201834479

  48. [49]

    , keywords =

    Ultraluminous X-ray sources. , keywords =. doi:10.1016/j.newar.2022.101672 , archivePrefix =. 2302.10605 , primaryClass =

    doi:10.1016/j.newar.2022.101672 2022

  49. [50]

    Accretion Power in Astrophysics

  50. [51]

    arXiv e-prints , keywords =

    Accreting strongly magnetised neutron stars: X-ray pulsars. arXiv e-prints , keywords =. doi:10.1007/978-981-19-6960-7 , archivePrefix =. 2204.14185 , primaryClass =

    Pith/arXiv arXiv doi:10.1007/978-981-19-6960-7

  51. [52]

    On gravitational collapse of a magnetic stars , journal =

  52. [53]

    Polarization of Thermal X-rays from Isolated Neutron Stars

    Polarization of Thermal X-Rays from Isolated Neutron Stars. , keywords =. doi:10.1086/308313 , archivePrefix =. astro-ph/9909326 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/308313

  53. [54]

    , keywords =

    Finite-Velocity Effects on Atoms in Strong Magnetic Fields and Implications for Neutron Star Atmospheres. , keywords =. doi:10.1086/173274 , adsurl =

    work page doi:10.1086/173274

  54. [55]

    Journal of Physics B Atomic Molecular Physics , keywords =

    Centre-of-mass effects on the hydrogen atom in a magnetic field. Journal of Physics B Atomic Molecular Physics , keywords =. doi:10.1088/0953-4075/21/13/009 , adsurl =

    work page doi:10.1088/0953-4075/21/13/009

  55. [56]

    arXiv e-prints , keywords =

    Maximum Accretion Efficiency in General Theory of Relativity. arXiv e-prints , keywords =. doi:10.48550/arXiv.astro-ph/9811402 , archivePrefix =. astro-ph/9811402 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9811402

  56. [57]

    Journal of Physics G Nuclear Physics , keywords =

    Nuclear physics of the outer layers of accreting neutron stars. Journal of Physics G Nuclear Physics , keywords =. doi:10.1088/1361-6471/aad171 , archivePrefix =. 1807.01150 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/1361-6471/aad171

  57. [58]

    Partially ionized hydrogen plasma in strong magnetic fields

    Partially ionized hydrogen plasma in strong magnetic fields. , keywords =. doi:10.1103/PhysRevE.60.2193 , archivePrefix =. astro-ph/9907006 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physreve.60.2193

  58. [59]

    Physics of Plasmas , keywords =

    Ionization equilibrium and equation of state in strongly coupled plasmas. Physics of Plasmas , keywords =. doi:10.1063/1.873815 , adsurl =

    work page doi:10.1063/1.873815

  59. [60]

    Reviews of Modern Physics , year = 1983, month = jan, volume =

    Interaction of atoms, molecules, and ions with constant electric and magnetic fields. Reviews of Modern Physics , year = 1983, month = jan, volume =. doi:10.1103/RevModPhys.55.109 , adsurl =

    work page doi:10.1103/revmodphys.55.109 1983

  60. [61]

    Equation of state and opacities for hydrogen atmospheres of neutron stars with strong magnetic fields

    Equation of State and Opacities for Hydrogen Atmospheres of Neutron Stars with Strong Magnetic Fields. , keywords =. doi:10.1086/346150 , archivePrefix =. astro-ph/0212062 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/346150

  61. [62]

    The Equation of State for Stellar Envelopes. I. an Occupation Probability Formalism for the Truncation of Internal Partition Functions. , keywords =. doi:10.1086/166600 , adsurl =

    doi:10.1086/166600

  62. [63]

    , year = 1939, month = oct, volume =

    Ionic Depression of Series Limits in One-Electron Spectra. , year = 1939, month = oct, volume =. doi:10.1086/144118 , adsurl =

    doi:10.1086/144118 1939

  63. [64]

    , keywords =

    Statistical Mechanics of Partially Ionized Stellar Plasmas: The Planck-Larkin Partition Function, Polarization Shifts, and Simulations of Optical Spectra. , keywords =. doi:10.1086/165446 , adsurl =

    work page doi:10.1086/165446

  64. [65]

    Ionization equilibrium of hot hydrogen plasma

    Ionization equilibrium of hot hydrogen plasma. Physics of Plasmas , keywords =. doi:10.1063/1.871547 , archivePrefix =. plasm-ph/9607001 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1063/1.871547

  65. [66]

    Equation of state for magnetized Coulomb plasmas

    Equation of state for magnetized Coulomb plasmas. , keywords =. doi:10.1051/0004-6361/201220082 , archivePrefix =. 1212.3405 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201220082

  66. [67]

    Matter Radiat

    Statistical and quantum photoionization cross sections in plasmas: Analytical approaches for any configurations including inner shells. Matter Radiat. Extremes , year = 2020, month = nov, volume =

    2020

  67. [68]

    Influence of vacuum polarization by a magnetic field on the propagation of electromagnetic waves in a plasma. Sov. Phys. -- JETP , year = 1979, month = may, volume =

    1979

  68. [69]

    Physics of Fully Ionized Gases

  69. [70]

    Reports on Progress in Physics , keywords =

    Physics of strongly magnetized neutron stars. Reports on Progress in Physics , keywords =. doi:10.1088/0034-4885/69/9/R03 , archivePrefix =. astro-ph/0606674 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0034-4885/69/9/r03

  70. [71]

    Compton scattering S-matrix and cross section in strong magnetic field

    Compton scattering S matrix and cross section in strong magnetic field. , keywords =. doi:10.1103/PhysRevD.93.105003 , archivePrefix =. 1512.06681 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.93.105003

  71. [72]

    High-energy radiation from magnetized neutron stars

  72. [73]

    doi:10.1007/978-94-009-0201-5 , adsurl =

    Radiation in Astrophysical Plasmas. doi:10.1007/978-94-009-0201-5 , adsurl =

    doi:10.1007/978-94-009-0201-5

  73. [74]

    , keywords =

    Statistical equilibrium and ion cyclotron absorption/emission in strongly magnetized plasmas. , keywords =. doi:10.1111/j.1365-2966.2007.11474.x , archivePrefix =. astro-ph/0701285 , primaryClass =

    doi:10.1111/j.1365-2966.2007.11474.x 2007

  74. [75]

    , keywords =

    Scattering of light in a strongly magnetized plasma. , keywords =. doi:10.1103/PhysRevD.19.1684 , adsurl =

    doi:10.1103/physrevd.19.1684

  75. [76]

    The propagation of electromagnetic waves in plasmas

  76. [77]

    , keywords =

    Dynamic effects on cyclotron scattering in pulsar accretion columns. , keywords =. doi:10.1086/169749 , adsurl =

    work page doi:10.1086/169749

  77. [78]

    , keywords =

    Coulomb bremsstrahlung and cyclotron emissivity in hot magnetized plasmas. , keywords =

  78. [79]

    , keywords =

    Cyclotron line formation in the accretion column of an X-ray pulsar. , keywords =. doi:10.1086/157817 , adsurl =

    doi:10.1086/157817

  79. [80]

    X-ray pulsar models. I. Angle-dependent cyclotron line formation and comptonization. , keywords =. doi:10.1086/163594 , adsurl =

    doi:10.1086/163594

  80. [81]

    Sov.\ Sci.\ Rev

    Vacuum polarization by a magnetic field and its astrophysical manifestations. Sov.\ Sci.\ Rev. E: Astrophys.\ Space Phys.\ Rev. , year = 1984, month = jan, volume =

    1984

Showing first 80 references.