pith. machine review for the scientific record. sign in

arxiv: 2604.06591 · v2 · submitted 2026-04-08 · 🌌 astro-ph.HE · hep-ex

Recognition: 1 theorem link

· Lean Theorem

Plasma Dynamics of Radiative Cooling Accretion Flow in AM Herculis with XRISM

(10) University of Cape Town, (11) Istanbul University, (12) Kadir Has University, (13) Tokyo Metropolitan University, (14) Toyama University, (15) Armagh Observatory, (16) California Institute of Technology), (2) ISAS/JAXA, (3) Columbia University, (4) Kyoto University, (5) Leibniz-Institut fur Astrophysik Potsdam, (6) Kanazawa University, (7) Nara University of Education, (8) South African Astronomical Observatory, (9) University of the Free State, Antonio Rodriguez (16), Atsuto Matsumura (13)(2), Axel D. Schwope (5), Charles J. Hailey (3), David A. H. Buckley (8)(9)(10), Gabriel L. Bridges (3), Gavin Ramsay (15), Kaya Mori (3), Mai Takeo (14), Manabu Ishida (2), Mariko Kimura (6), Masayoshi Nobukawa (7), Planetarium, Samantha Walker (3) ((1) Saitama University, Solen Balman (11)(12), Taichi Ichikawa (1), Takayuki Hayashi (4), Yukikatsu Terada (1)(2)

Authors on Pith no claims yet

Pith reviewed 2026-05-10 18:33 UTC · model grok-4.3

classification 🌌 astro-ph.HE hep-ex
keywords AM HerculisXRISMaccretion columnX-ray spectroscopymagnetic cataclysmic variableshock temperatureradiative coolingplasma diagnostics
0
0 comments X

The pith

XRISM spectra fix the accretion shock in AM Herculis at 24 keV temperature and 1116 km/s velocity.

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

High-resolution X-ray spectroscopy from XRISM resolves the emission lines from the plasma in AM Herculis, revealing both thermal widths and additional bulk Doppler broadening that varies with spin phase. The authors combine these line profiles with simultaneous broadband data and plasma models to extract a consistent set of post-shock conditions. This approach matters because it turns the observed line shapes and intensities into quantitative measures of temperature, velocity, density, and physical size inside the radiating column. A sympathetic reader would see this as a direct empirical map of how infalling matter cools and settles onto a strongly magnetized white dwarf.

Core claim

The paper establishes that the radiative cooling accretion flow onto the white dwarf in AM Herculis produces a shock with temperature 24.0 plus or minus 0.1 keV and inflow velocity 1116 plus or minus 2 km/s. Radiative transfer calculations applied to the resolved resonance lines give a post-shock density of 5 to 6 times 10 to the 15 per cubic centimeter. These values together imply an accretion column 200 to 300 km tall and 200 to 400 km wide. The same spectra confirm the predicted viewing-angle dependence of resonance-line equivalent widths and show intrinsic velocity and temperature gradients once orbital motion is removed.

What carries the argument

Phase-resolved Doppler shifts and intrinsic widths of the Fe XXV and Fe XXVI lines, interpreted through PSAC/MCVSPEC plasma models and radiative transfer simulations, which convert observed line properties into the temperature-velocity-density structure of the cooling flow.

If this is right

  • The shock temperature and velocity are recovered self-consistently from two independent instruments and modeling pipelines.
  • Resonance-line equivalent widths increase by factors of 1.30 to 1.35 at pole-on phases, matching the anisotropy expected from the oscillator strengths.
  • The resonance lines supply a new density diagnostic that constrains the post-shock plasma to 5-6 times 10^15 cm^{-3}.
  • The inferred column geometry supplies concrete length scales for the region where the plasma cools radiatively.

Where Pith is reading between the lines

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

  • The same line-profile technique can be applied to other magnetic cataclysmic variables once comparable high-resolution spectra become available.
  • The measured density and column height may be used to test how the accretion flow couples to the white dwarf's magnetic field and atmosphere.
  • If the derived column dimensions are typical, they set a benchmark for comparing radiative cooling lengths across different classes of accreting compact objects.

Load-bearing premise

The plasma emission and radiative transfer models correctly reproduce the temperature, velocity, and line-formation physics inside the accretion column without large unmodeled effects.

What would settle it

Future spectra showing line widths, velocity amplitudes, or resonance-line equivalent-width ratios that are incompatible with a 24 keV shock at 1116 km/s and the stated density and column dimensions.

Figures

Figures reproduced from arXiv: 2604.06591 by (10) University of Cape Town, (11) Istanbul University, (12) Kadir Has University, (13) Tokyo Metropolitan University, (14) Toyama University, (15) Armagh Observatory, (16) California Institute of Technology), (2) ISAS/JAXA, (3) Columbia University, (4) Kyoto University, (5) Leibniz-Institut fur Astrophysik Potsdam, (6) Kanazawa University, (7) Nara University of Education, (8) South African Astronomical Observatory, (9) University of the Free State, Antonio Rodriguez (16), Atsuto Matsumura (13)(2), Axel D. Schwope (5), Charles J. Hailey (3), David A. H. Buckley (8)(9)(10), Gabriel L. Bridges (3), Gavin Ramsay (15), Kaya Mori (3), Mai Takeo (14), Manabu Ishida (2), Mariko Kimura (6), Masayoshi Nobukawa (7), Planetarium, Samantha Walker (3) ((1) Saitama University, Solen Balman (11)(12), Taichi Ichikawa (1), Takayuki Hayashi (4), Yukikatsu Terada (1)(2).

Figure 1
Figure 1. Figure 1: A schematic illustration of the hot plasma in an accretion column on a magnetized white dwarf of an MCV is shown. The multi-temperature plasma structure and the mechanism of resonance anisotropy are also represented. Brinkmann et al. 1989; I. Hatsukade et al. 1990 etc) and non magnetic CVs (Ş. Balman et al. 2025 and references therein). For example, a key open question in MHD plasma physics is how electron… view at source ↗
Figure 2
Figure 2. Figure 2: The phase-averaged X-ray spectrum of AM Her￾culis observed with XRISM/Resolve is plotted as red crosses. In the upper panel, the best-fit ’bvcempow’ model with three Gaussian components and the non X-ray background model (see the text) are indicated by blue and gray lines, respec￾tively. The middle and bottom panels show the residuals with respect to the ’bremsstrahlung’ model and the ’bvcem￾pow’ model wit… view at source ↗
Figure 3
Figure 3. Figure 3: (Upper) The phase-averaged X-ray spectrum of AM Herculis with XRISM, focusing on the Fe-K lines, is shown in red crosses. The optimal Gaussian models representing Fe-K fluorescence, Fe XXV, and Fe XXVI lines are illustrated with black dotted lines. (Lower) A two-dimensional plot of photon energy versus spin phases is presented, computed using the ephemeris from equation (1) in A. D. Schwope et al. (2020). … view at source ↗
Figure 4
Figure 4. Figure 4: Same as [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: (Left) The Doppler velocities of highly-ionized Fe lines are displayed in polar coordinates as a function of phase, with the Fe XXV lines in blue and the Fe XXVI lines in red. The spin-orbital phase is calculated using the ephemeris given by equation (1) in A. D. Schwope et al. (2020), with phase zero defined at the inferior conjunction of the secondary star. The radial and angular dimensions represent the… view at source ↗
Figure 6
Figure 6. Figure 6: The demodulated X-ray spectra for Fe XXV and Fe XXVI lines are shown in the left and right panels, respectively, accompanied by the best-fit Gaussian models and the bremsstrahlung continuum. The bulk Doppler shifts of X-ray energies across phases are demodulated using the best-fit modulation functions, represented by the cyan and magenta dashed lines in [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: (Left) The upper and lower panels illustrate the equivalent widths of resonance lines and other lines across different phases, respectively. The data definitions are indicated by labels in matching colors: r, r1, and r2 denote resonance lines, while f and ic denote the forbidden and intercombination lines, respectively. The errors are provided at a 1.0 σ confidence level. (Right) The scatter plot shows the… view at source ↗
Figure 8
Figure 8. Figure 8: The illustration shows a scatter plot correlat￾ing the oscillator strengths of line transitions with the phase amplitude of the enhancement in equivalent widths. It in￾cludes Fe XXV forbidden, intercombination 1 and 2, and resonance lines, alongside Fe XXVI resonance 1 and 2 lines, represented in green, cyan, blue, magenta, red, and black, respectively, with error bars indicating 1 σ significance. The osci… view at source ↗
Figure 9
Figure 9. Figure 9: The position distributions of a) temperature, b) density, and c) velocity in the accretion column, as computed with the PSAC model (T. Hayashi & M. Ishida 2014a) and MCVSPEC (L. W. Filor et al. 2025) for MWD = 0.63M⊙ and B = 13.6 MG, are plotted in red and blue, respectively. For comparison, the Aizu model is also plotted in cyan. The x-axis represents the spatial coordinate scaled by the column height h. … view at source ↗
Figure 11
Figure 11. Figure 11: (top) The amplitudes of the EW enhancement factors, derived from RT simulations (Y. Terada et al. 2001) for the AM Herculis observation (EM=6.55 × 1054 cm−3 ), are displayed in relation to n sh e . Observed line amplitudes in [PITH_FULL_IMAGE:figures/full_fig_p012_11.png] view at source ↗
read the original abstract

We present XRISM/Resolve high-resolution X-ray spectroscopy of the prototypical magnetic cataclysmic variable AM Herculis. All satellite lines of highly ionized Fe are fully resolved. Lighter element lines (Si, S, Ca) show 2 - 3 eV widths consistent with purely thermal broadening, while the broader 6 - 7 eV Fe lines require additional bulk Doppler broadening. Spin-phase-resolved modulations are clearly detected in the Fe XXV and Fe XXVI lines, with semi-amplitudes of $81.8\pm6$ km s$^{-1}$ and $132.5\pm9$ km s$^{-1}$, and mean velocities of $143.6\pm6$ km s$^{-1}$ and $225.6\pm8$ km s$^{-1}$, respectively. After removing these bulk Doppler shifts, we obtain intrinsic Doppler widths of $5.23_{-0.15}^{+0.16}$ eV for Fe XXV and $6.23_{-0.18}^{+0.19}$ eV for Fe XXVI, directly revealing gradients of bulk velocity and temperature in the cooling-flow plasma. We additionally examined the resonance anisotropy predicted by Terada et al. (1999, 2001): the equivalent widths of the Fe XXV and Fe XXVI resonance lines increase at the pole-on phase by factors of 1.30 - 1.35, in positive correlation with their oscillator strengths. Combining XRISM with simultaneous NuSTAR data and PSAC/MCVSPEC plasma models, we derive a self-consistent shock temperature of $24.0\pm0.1$ keV and shock velocity of $1,116\pm2$ km s$^{-1}$. Radiative transfer simulations of the resonance lines further constrain the shock density to about $(5 - 6)\times10^{15}$ cm$^{-3}$, providing a new density diagnostic for accretion columns. The resulting accretion column geometry has a height of 200 - 300 km and a radius of 200 - 400 km.

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

1 major / 2 minor

Summary. The manuscript presents XRISM/Resolve high-resolution X-ray spectroscopy of the magnetic cataclysmic variable AM Herculis. It reports fully resolved satellite lines of highly ionized Fe, thermal widths of 2-3 eV for Si/S/Ca lines, additional bulk Doppler broadening in Fe lines, and spin-phase modulations in Fe XXV/XXVI resonance lines with measured semi-amplitudes and mean velocities. Combining XRISM with simultaneous NuSTAR data and PSAC/MCVSPEC plasma models yields a self-consistent shock temperature of 24.0±0.1 keV and shock velocity of 1,116±2 km s^{-1}; radiative-transfer simulations of resonance lines constrain post-shock density to (5-6)×10^{15} cm^{-3}, implying an accretion column with height 200-300 km and radius 200-400 km.

Significance. If the PSAC/MCVSPEC models and radiative-transfer assumptions hold without significant unmodeled effects, the work delivers direct observational constraints on velocity and temperature gradients in a radiative cooling accretion column, plus a new density diagnostic via resonance-line equivalent-width anisotropy. The phase-resolved line measurements and combined high-resolution/broadband fitting provide a valuable benchmark for theoretical models of post-shock plasma in magnetic cataclysmic variables.

major comments (1)
  1. [modeling and spectral fitting results (text following the PSAC/MCVSPEC description)] The central claim of self-consistent shock parameters (temperature 24.0±0.1 keV and velocity 1,116±2 km s^{-1} from PSAC/MCVSPEC fits to XRISM+NuSTAR spectra) is not reconciled with strong-shock jump conditions. Standard post-shock temperature kT = (3/16) μ m_H v_pre² with μ≈0.6 and v_pre=1116 km s^{-1} yields ~2 keV, while the reported temperature implies v_pre~3500 km s^{-1}. The manuscript does not define whether the quoted 'shock velocity' is pre-shock, immediate post-shock, or a flow-averaged quantity in the cooling column, nor demonstrate consistency via the jump conditions or model internals. This linkage is load-bearing for the self-consistency assertion and the subsequent density/geometry results.
minor comments (2)
  1. [Abstract] The abstract states that 'all satellite lines of highly ionized Fe are fully resolved' without listing the specific transitions (e.g., Fe XXV w, x, y, z or Fe XXVI Lyα) or tabulating their measured widths and uncertainties.
  2. [line width analysis] The reported intrinsic Doppler widths (5.23 eV for Fe XXV, 6.23 eV for Fe XXVI) after removal of bulk shifts would benefit from an explicit statement of the thermal vs. non-thermal decomposition and the assumed ion temperatures used in the conversion.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the careful reading of our manuscript and the constructive comment on the shock parameter consistency. We address the major comment point by point below.

read point-by-point responses

  1. Referee: [modeling and spectral fitting results (text following the PSAC/MCVSPEC description)] The central claim of self-consistent shock parameters (temperature 24.0±0.1 keV and velocity 1,116±2 km s^{-1} from PSAC/MCVSPEC fits to XRISM+NuSTAR spectra) is not reconciled with strong-shock jump conditions. Standard post-shock temperature kT = (3/16) μ m_H v_pre² with μ≈0.6 and v_pre=1116 km s^{-1} yields ~2 keV, while the reported temperature implies v_pre~3500 km s^{-1}. The manuscript does not define whether the quoted 'shock velocity' is pre-shock, immediate post-shock, or a flow-averaged quantity in the cooling column, nor demonstrate consistency via the jump conditions or model internals. This linkage is load-bearing for the self-consistency assertion and the subsequent density/geometry results.

    Authors: We agree that the manuscript should have explicitly defined the 'shock velocity' and demonstrated consistency with the strong-shock jump conditions. In the PSAC/MCVSPEC framework used here, the fitted shock velocity of 1,116 km s^{-1} corresponds to the immediate post-shock velocity (v_post), not the pre-shock velocity. For a strong shock with compression ratio 4, the pre-shock velocity is v_pre = 4 × v_post ≈ 4,464 km s^{-1}. Substituting into the jump-condition formula kT_post = (3/16) μ m_H v_pre² with μ ≈ 0.6 yields kT_post ≈ 23–24 keV, which is fully consistent with the fitted shock temperature of 24.0 ± 0.1 keV. The observed line widths and phase-dependent Doppler shifts reflect the velocity gradient through the cooling column, where velocity decreases from v_post toward zero at the white-dwarf surface. We will revise the text (in the modeling section and discussion of self-consistency) to state this definition explicitly, include the jump-condition calculation, and note that the pre-shock velocity implied by the temperature is the free-fall velocity appropriate for the white-dwarf mass in AM Herculis. This clarification does not alter the derived density or geometry results. revision: yes

Circularity Check

0 steps flagged

No significant circularity in the derivation chain

full rationale

The paper obtains the shock temperature (24.0±0.1 keV) and velocity (1,116±2 km s^{-1}) by fitting the external PSAC/MCVSPEC plasma models directly to the combined XRISM+NuSTAR spectra; the density ((5-6)×10^{15} cm^{-3}) follows from separate radiative-transfer simulations matched to the observed resonance-line equivalent widths. These steps apply independent models to observational data rather than re-deriving quantities from the same inputs by construction. The resonance-anisotropy check references prior work by the lead author (Terada et al. 1999, 2001) but is presented only as an additional examination and is not used to constrain the central temperature, velocity, density, or column geometry. The overall chain therefore remains data-driven and self-contained against external spectral benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claims rest on standard astrophysical plasma emission models and radiative transfer calculations whose parameters are adjusted to match the new spectra. No new physical entities are introduced.

free parameters (2)
  • shock density = (5-6) x 10^15 cm^-3
    Adjusted in radiative transfer simulations to reproduce observed resonance-line equivalent widths.
  • accretion column dimensions = height 200-300 km, radius 200-400 km
    Inferred from the fitted density together with shock velocity and temperature.
axioms (2)
  • domain assumption The accretion flow follows the radiative cooling structure described by the PSAC/MCVSPEC plasma code.
    Invoked to convert observed line profiles into shock temperature and velocity.
  • domain assumption Resonance-line anisotropy follows the predictions of Terada et al. (1999, 2001).
    Used to interpret the observed phase-dependent increase in equivalent widths.

pith-pipeline@v0.9.0 · 5926 in / 1758 out tokens · 120479 ms · 2026-05-10T18:33:31.240620+00:00 · methodology

discussion (0)

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

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

  • IndisputableMonolith/Foundation/RealityFromDistinction.lean reality_from_one_distinction unclear

    Combining XRISM with simultaneous NuSTAR data and PSAC/MCVSPEC plasma models, we derive a self-consistent shock temperature of 24.0±0.1 keV and shock velocity of 1,116±2 km s^{-1}. Radiative transfer simulations of the resonance lines further constrain the shock density to about (5 - 6)×10^{15} cm^{-3}... The resulting accretion column geometry has a height of 200 - 300 km and a radius of 200 - 400 km.

Reference graph

Works this paper leans on

55 extracted references · 51 canonical work pages

  1. [1]

    1973, Progress of Theoretical Physics, 49, 1184, doi: 10.1143/PTP.49.1184 Álvarez-Hernández, A., Torres, M

    Aizu, K. 1973, Progress of Theoretical Physics, 49, 1184, doi: 10.1143/PTP.49.1184 Álvarez-Hernández, A., Torres, M. A. P., Rodríguez-Gil, P., et al. 2023, MNRAS, 524, 3314, doi: 10.1093/mnras/stad2010 Álvarez-Hernández, A., Torres, M. A. P., Shahbaz, T., et al. 2024, A&A, 690, A218, doi: 10.1051/0004-6361/202451094

    work page doi:10.1143/ptp.49.1184 1973

  2. [2]

    Arnaud, K. A. 1996, in Astronomical Society of the Pacific Conference Series, Vol. 101, Astronomical Data Analysis Software and Systems V, ed. G. H. Jacoby & J. Barnes, 17

    1996

  3. [3]

    2025, PASJ, doi: 10.1093/pasj/psaf109 Balman, Ş., Orio, M., & Luna, G

    Audard, M., Awaki, H., Ballhausen, R., et al. 2025, PASJ, doi: 10.1093/pasj/psaf109 Balman, Ş., Orio, M., & Luna, G. J. M. 2025, Universe, 11, 105, doi: 10.3390/universe11040105

    work page doi:10.1093/pasj/psaf109 2025

  4. [4]

    H., Smith, A., & Haberl, F

    Brinkmann, W., Fink, H. H., Smith, A., & Haberl, F. 1989, A&A, 221, 385

    1989

  5. [5]

    1988, MNRAS, 231, 597, doi: 10.1093/mnras/231.3.597

    Cropper, M. 1988, MNRAS, 231, 597, doi: 10.1093/mnras/231.3.597

    work page doi:10.1093/mnras/231.3.597 1988

  6. [6]

    1990, SSRv, 54, 195, doi: 10.1007/BF00177799

    Cropper, M. 1990, SSRv, 54, 195, doi: 10.1007/BF00177799

    work page doi:10.1007/bf00177799 1990

  7. [7]

    1998, MNRAS, 299, 433, doi: 10.1046/j.1365-8711.1998.01828.x

    Cropper, M., Ramsay, G., & Wu, K. 1998, MNRAS, 293, 222, doi: 10.1046/j.1365-8711.1998.00610.x

    work page doi:10.1046/j.1365-8711.1998.00610.x 1998

  8. [8]

    P., & Beardmore, A

    Done, C., Osborne, J. P., & Beardmore, A. P. 1995, MNRAS, 276, 483, doi: 10.1093/mnras/276.2.483

    work page doi:10.1093/mnras/276.2.483 1995

  9. [9]

    1999, ApJS, 120, 277, doi: 10.1086/313181

    Ezuka, H., & Ishida, M. 1999, ApJS, 120, 277, doi: 10.1086/313181

    work page doi:10.1086/313181 1999

  10. [10]

    W., Mori, K., Bridges, G., et al

    Filor, L. W., Mori, K., Bridges, G., et al. 2025, ApJ, 987, 53, doi: 10.3847/1538-4357/add403

    work page doi:10.3847/1538-4357/add403 2025

  11. [11]

    1997, ApJ, 474, 774, doi: 10.1086/303483

    Fujimoto, R., & Ishida, M. 1997, ApJ, 474, 774, doi: 10.1086/303483

    work page doi:10.1086/303483 1997

  12. [12]

    H., & Jordan, C

    Gabriel, A. H., & Jordan, C. 1969, MNRAS, 145, 241, doi: 10.1093/mnras/145.2.241 Gänsicke, B. T., Beuermann, K., & de Martino, D. 1995, A&A, 303, 127

    work page doi:10.1093/mnras/145.2.241 1969

  13. [13]

    R., & Singh, K

    Girish, V., Rana, V. R., & Singh, K. P. 2007, ApJ, 658, 525, doi: 10.1086/510894

    work page doi:10.1086/510894 2007

  14. [14]

    J., Mori, K., Perez, K., Canipe, A

    Hailey, C. J., Mori, K., Perez, K., Canipe, A. M., & Hong et al., J. 2016, ApJ, 826, 160, doi: 10.3847/0004-637X/826/2/160

    work page doi:10.3847/0004-637x/826/2/160 2016

  15. [15]

    A., Craig, W

    Harrison, F. A., Craig, W. W., Christensen, F. E., et al. 2013, ApJ, 770, 103, doi: 10.1088/0004-637X/770/2/103

    work page doi:10.1088/0004-637x/770/2/103 2013

  16. [16]

    1990, PASJ, 42, 279, doi: 10.1093/pasj/42.2.279

    Hatsukade, I., Tsunemi, H., Yamashita, K., et al. 1990, PASJ, 42, 279, doi: 10.1093/pasj/42.2.279

    work page doi:10.1093/pasj/42.2.279 1990

  17. [17]

    2025, Journal of Astronomical Telescopes, Instruments, and Systems, 11, 042017, doi: 10.1117/1.JATIS.11.4.042017

    Hayashi, K., Tashiro, M., Terada, Y., & et al. . 2025, Journal of Astronomical Telescopes, Instruments, and Systems, 11, 042017, doi: 10.1117/1.JATIS.11.4.042017

    work page doi:10.1117/1.jatis.11.4.042017 2025

  18. [18]

    2014a, MNRAS, 441, 3718, doi: 10.1093/mnras/stu766

    Hayashi, T., & Ishida, M. 2014a, MNRAS, 441, 3718, doi: 10.1093/mnras/stu766

    work page doi:10.1093/mnras/stu766

  19. [19]

    2014b, MNRAS, 438, 2267, doi: 10.1093/mnras/stt2342 Hitomi Collaboration, Aharonian, F., Akamatsu, H., et al

    Hayashi, T., & Ishida, M. 2014b, MNRAS, 438, 2267, doi: 10.1093/mnras/stt2342 Hitomi Collaboration, Aharonian, F., Akamatsu, H., et al. 2016, Nature, 535, 117, doi: 10.1038/nature18627 Hōshi, R. 1973, Progress of Theoretical Physics, 49, 776, doi: 10.1143/PTP.49.776

    work page doi:10.1093/mnras/stt2342 2016

  20. [20]

    2025, Journal of Astronomical Telescopes, Instruments, and Systems, 11, 042021, doi: 10.1117/1.JATIS.11.4.042021

    Ishisaki, Y., Kelley, R., Awaki, H., & et al. . 2025, Journal of Astronomical Telescopes, Instruments, and Systems, 11, 042021, doi: 10.1117/1.JATIS.11.4.042021

    work page doi:10.1117/1.jatis.11.4.042021 2025

  21. [21]

    2006, ApJ, 639, 397, doi: 10.1086/499152

    Itoh, K., Okada, S., Ishida, M., & Kunieda, H. 2006, ApJ, 639, 397, doi: 10.1086/499152

    work page doi:10.1086/499152 2006

  22. [22]

    2025, Journal of Astronomical Telescopes, Instruments, and Systems, 11, 042026, doi: 10.1117/1.JATIS.11.4.042026

    Kelley, R., Ishisaki, Y., Costantini, E., & et al. . 2025, Journal of Astronomical Telescopes, Instruments, and Systems, 11, 042026, doi: 10.1117/1.JATIS.11.4.042026

    work page doi:10.1117/1.jatis.11.4.042026 2025

  23. [23]

    2018, PASJ, 70, R1, doi: 10.1093/pasj/psx084

    Koyama, K. 2018, PASJ, 70, R1, doi: 10.1093/pasj/psx084

    work page doi:10.1093/pasj/psx084 2018

  24. [24]

    2024, ApJ, 961, 205, doi: 10.3847/1538-4357/ad0dff

    Koyama, K., & Nobukawa, M. 2024, ApJ, 961, 205, doi: 10.3847/1538-4357/ad0dff

    work page doi:10.3847/1538-4357/ad0dff 2024

  25. [25]

    W., & Suleimanov, V

    Mauche, C. W., & Suleimanov, V. 2015, A&A, 578, A15, doi: 10.1051/0004-6361/201525755

    work page doi:10.1051/0004-6361/201525755 2015

  26. [26]

    1984, Ap&SS, 98, 367, doi: 10.1007/BF00651415

    Masai, K. 1984, Ap&SS, 98, 367, doi: 10.1007/BF00651415

    work page doi:10.1007/bf00651415 1984

  27. [27]

    Mewe, R., Gronenschild, E. H. B. M., & van den Oord, G. H. J. 1985, A&AS, 62, 197

    1985

  28. [28]

    Mukai, K., & Charles, P. A. 1987, MNRAS, 226, 209, doi: 10.1093/mnras/226.1.209

    work page doi:10.1093/mnras/226.1.209 1987

  29. [29]

    P., Bauer, F

    Muno, M. P., Bauer, F. E., Baganoff, F. K., Band yopadhyay, R. M., & Bower et al., G. C. 2009, ApJS, 181, 110, doi: 10.1088/0067-0049/181/1/110

    work page doi:10.1088/0067-0049/181/1/110 2009

  30. [30]

    N., & Pradhan, A

    Nahar, S. N., & Pradhan, A. K. 1999, A&AS, 135, 347, doi: 10.1051/aas:1999447

    work page doi:10.1051/aas:1999447 1999

  31. [31]

    Ness, J.-U., Mewe, R., Schmitt, J. H. M. M., et al. 2001, A&A, 367, 282, doi: 10.1051/0004-6361:20000419

    work page doi:10.1051/0004-6361:20000419 2001

  32. [32]

    F., G¨ ansicke, B

    Pala, A. F., Gänsicke, B. T., Breedt, E., et al. 2020, MNRAS, 494, 3799, doi: 10.1093/mnras/staa764

    work page doi:10.1093/mnras/staa764 2020

  33. [33]

    F., Gänsicke, B

    Pala, A. F., Gänsicke, B. T., Belloni, D., et al. 2022, MNRAS, 510, 6110, doi: 10.1093/mnras/stab3449

    work page doi:10.1093/mnras/stab3449 2022

  34. [34]

    J., Bauer, F

    Perez, K., Hailey, C. J., Bauer, F. E., Krivonos, R. A., & Mori et al., K. 2015, Nature, 520, 646, doi: 10.1038/nature14353

    work page doi:10.1038/nature14353 2015

  35. [35]

    Kaastra, J. S. 2001, A&A, 376, 1113, doi: 10.1051/0004-6361:20010959

    work page doi:10.1051/0004-6361:20010959 2001

  36. [36]

    K., & Shull, J

    Pradhan, A. K., & Shull, J. M. 1981, ApJ, 249, 821, doi: 10.1086/159340 17

    work page doi:10.1086/159340 1981

  37. [37]

    2006, A&A, 452, 169, doi: 10.1051/0004-6361:20054268

    Sunyaev, R. 2006, A&A, 452, 169, doi: 10.1051/0004-6361:20054268

    work page doi:10.1051/0004-6361:20054268 2006

  38. [38]

    2008, A&A, 489, 1121, doi: 10.1051/0004-6361:200810213

    Sunyaev, R. 2008, A&A, 489, 1121, doi: 10.1051/0004-6361:200810213

    work page doi:10.1051/0004-6361:200810213 2008

  39. [39]

    2026, arXiv e-prints, arXiv:2603.04679, doi: 10.48550/arXiv.2603.04679

    Sameshima, N., Tsujimoto, M., & Uemura, M. 2026, arXiv e-prints, arXiv:2603.04679, doi: 10.48550/arXiv.2603.04679

    work page doi:10.48550/arxiv.2603.04679 2026

  40. [40]

    Schwarz, R., Hedelt, P., Rau, A., Staude, A., & Schwope, A. D. 2002, in Astronomical Society of the Pacific Conference Series, Vol. 261, The Physics of Cataclysmic Variables and Related Objects, ed. B. T. Gänsicke, K. Beuermann, & K. Reinsch, 167

    2002

  41. [41]

    Schwope, A. D. 2025, A&A, 698, A106, doi: 10.1051/0004-6361/202554519

    work page doi:10.1051/0004-6361/202554519 2025

  42. [42]

    D., Worpel, H., Traulsen, I., & Sablowski, D

    Schwope, A. D., Worpel, H., Traulsen, I., & Sablowski, D. 2020, A&A, 642, A134, doi: 10.1051/0004-6361/202037714

    work page doi:10.1051/0004-6361/202037714 2020

  43. [43]

    W., Heinke, C

    Shaw, A. W., Heinke, C. O., Mukai, K., et al. 2020, MNRAS, 498, 3457, doi: 10.1093/mnras/staa2592

    work page doi:10.1093/mnras/staa2592 2020

  44. [44]

    Raymond, J. C. 2001, ApJL, 556, L91, doi: 10.1086/322992

    work page doi:10.1086/322992 2001

  45. [45]

    F., Doroshenko, V., & Werner, K

    Suleimanov, V. F., Doroshenko, V., & Werner, K. 2019, MNRAS, 482, 3622, doi: 10.1093/mnras/sty2952

    work page doi:10.1093/mnras/sty2952 2019

  46. [46]

    2025, PASJ, 77, S1, doi: 10.1093/pasj/psaf023

    Tashiro, M., Kelley, R., Watanabe, S., et al. 2025, PASJ, 77, S1, doi: 10.1093/pasj/psaf023

    work page doi:10.1093/pasj/psaf023 2025

  47. [47]

    G., Staveley-Smith, L., de Blok, W

    Terada, Y., Ishida, M., Makishima, K., et al. 2001, MNRAS, 328, 112, doi: 10.1046/j.1365-8711.2001.04878.x

    work page doi:10.1046/j.1365-8711.2001.04878.x 2001

  48. [48]

    1999, PASJ, 51, 39, doi: 10.1093/pasj/51.1.39

    Terada, Y., Kaneda, H., Makishima, K., et al. 1999, PASJ, 51, 39, doi: 10.1093/pasj/51.1.39

    work page doi:10.1093/pasj/51.1.39 1999

  49. [49]

    2025, Journal of Astronomical Telescopes, Instruments, and Systems, 11, 042007, doi: 10.1117/1.JATIS.11.4.042007

    Terada, Y., Shidatsu, M., Sawada, M., & et al. . 2025, Journal of Astronomical Telescopes, Instruments, and Systems, 11, 042007, doi: 10.1117/1.JATIS.11.4.042007

    work page doi:10.1117/1.jatis.11.4.042007 2025

  50. [50]

    2021, Journal of Astronomical Telescopes, Instruments, and Systems, 7, 037001, doi: 10.1117/1.JATIS.7.3.037001 Van Box Som, L., Falize, E., Koenig, M., et al

    Terada, Y., Holland, M., Loewenstein, M., et al. 2021, Journal of Astronomical Telescopes, Instruments, and Systems, 7, 037001, doi: 10.1117/1.JATIS.7.3.037001 Van Box Som, L., Falize, E., Koenig, M., et al. 2018, High Power Laser Science and Engineering, 6, e35, doi: 10.1017/hpl.2018.32

    work page doi:10.1117/1.jatis.7.3.037001 2021

  51. [51]

    A., Verner, E

    Verner, D. A., Verner, E. M., & Ferland, G. J. 1996, Atomic Data and Nuclear Data Tables, 64, 1, doi: 10.1006/adnd.1996.0018

    work page doi:10.1006/adnd.1996.0018 1996

  52. [52]

    1995, ApJ, 455, 260, doi: 10.1086/176574 XRISM Collaboration, Audard, M., Awaki, H., et al

    Wu, K., Chanmugam, G., & Shaviv, G. 1995, ApJ, 455, 260, doi: 10.1086/176574 XRISM Collaboration, Audard, M., Awaki, H., et al. 2024a, ApJL, 977, L34, doi: 10.3847/2041-8213/ad8ed0 XRISM Collaboration, Audard, M., Awaki, H., et al. 2024b, ApJL, 973, L25, doi: 10.3847/2041-8213/ad7397 XRISM Collaboration, Audard, M., Awaki, H., et al. 2024c, PASJ, 76, 1186...

    work page doi:10.1086/176574 1995

  53. [54]

    D., & Li, X.-D

    Xu, X.-j., Wang, Q. D., & Li, X.-D. 2016b, ApJ, 818, 136, doi: 10.3847/0004-637X/818/2/136

    work page doi:10.3847/0004-637x/818/2/136

  54. [55]

    2012, ApJ, 753, 129, doi: 10.1088/0004-637X/753/2/129

    Yuasa, T., Makishima, K., & Nakazawa, K. 2012, ApJ, 753, 129, doi: 10.1088/0004-637X/753/2/129

    work page doi:10.1088/0004-637x/753/2/129 2012

  55. [56]

    2010, A&A, 520, A25, doi: 10.1051/0004-6361/201014542

    Yuasa, T., Nakazawa, K., Makishima, K., et al. 2010, A&A, 520, A25, doi: 10.1051/0004-6361/201014542

    work page doi:10.1051/0004-6361/201014542 2010