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arxiv: 2606.28993 · v1 · pith:CBF5WLTEnew · submitted 2026-06-27 · 🌌 astro-ph.SR

The Long-Period Radio Transient and Cataclysmic Variable ASKAP J1745-5051: Evidence for a 15,000 K White Dwarf and a Sub-Stellar Donor

Christian Knigge , Simone Scaringi , Noel Castro Segura , Domitilla de Martino , Martina Veresvarska This is my paper

Pith reviewed 2026-06-30 08:24 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords cataclysmic variableswhite dwarfsperiod bouncersradio transientsspectral energy distributionmagnetic cataclysmic variablessub-stellar donorslong-period transients
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The pith

The radio transient ASKAP J1745-5051 contains a 15,000 K white dwarf and a sub-stellar donor.

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

The paper constructs the broad-band spectral energy distribution of ASKAP J1745-5051 from far-ultraviolet to near-infrared wavelengths. It shows that this distribution is well fit by a 15,000 K white dwarf that dominates from far-UV through optical bands plus a sub-stellar donor star of about 0.05 solar masses and 1800 K effective temperature that dominates in the Ks band. This points to the system being a period bouncer that has evolved past the minimum orbital period for cataclysmic variables. The fit also gives a distance of roughly 320 parsecs. This finding suggests that long-period radio transients like this one may be linked to the population of evolved magnetic cataclysmic variables.

Core claim

The broad-band SED is well described by a 15,000 K white dwarf dominating far-UV through optical and a sub-stellar donor (M2 ~ 0.05 Msun, Teff ~ 1800 K) dominating in the Ks band, indicating the system is a period bouncer. The SED fit also yields a distance of d ~ 320 pc, only ~4x larger than that to the nearest confirmed mCV. Since the fraction of the sky swept out by the radio beam is likely to be small, systems like ASKAP J1745-5051 could make up a large percentage of mCVs.

What carries the argument

Broad-band spectral energy distribution fitting with synthetic spectra from model atmospheres for the white dwarf and the donor star, after correcting for reddening and removing contaminated photometry.

If this is right

  • The inferred white dwarf temperature is reasonable for an accretion-heated primary in a short-period magnetic cataclysmic variable.
  • The sub-stellar nature of the donor indicates that the system has evolved past the cataclysmic variable period minimum.
  • Systems like ASKAP J1745-5051 could make up a large percentage of magnetic cataclysmic variables if their radio beams cover only a small fraction of the sky.
  • This points towards a connection between long-period radio transients and the missing population of period bouncers among cataclysmic variables.

Where Pith is reading between the lines

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

  • If the radio emission is beamed narrowly, then many more such period-bouncer systems may exist but remain undetected in radio surveys.
  • The relatively close distance of 320 pc implies that similar systems could be found in existing multi-wavelength surveys with targeted follow-up.
  • Confirming more such objects would help resolve the discrepancy between predicted and observed numbers of evolved cataclysmic variables.

Load-bearing premise

The near-infrared flux is entirely from the donor star with negligible contribution from an accretion disk or other components.

What would settle it

A parallax measurement from Gaia or another astrometric mission that yields a distance significantly different from 320 pc, or infrared spectroscopy that shows spectral features inconsistent with a 1800 K sub-stellar object.

Figures

Figures reproduced from arXiv: 2606.28993 by Christian Knigge, Domitilla de Martino, Martina Veresvarska, Noel Castro Segura, Simone Scaringi.

Figure 1
Figure 1. Figure 1: — 1 ′ × 1 ′ finding charts centered in ASKAP J1745-505 covering wavelengths from X-ray to radio. In the top left panel the position of the ASKAP J1745-5051 and the two GAIA sources are shown with coloured crosses. The purpose of this paper is to improve on this sit￾uation. More specifically, in Section 2 we first con￾struct a wider and more reliable broad-band SED for the system. This involves (i) fixing a… view at source ↗
Figure 2
Figure 2. Figure 2: — 5 ′′ × 5 ′′ finding charts from the highest-resolution images centred on ASKAP J1745-505, showing the positions of the two Gaia sources, marked by light yellow and blue crosses, and the position of the LPT ASKAP J1745-5051 derived from radio observations, indicated by the red ellipse centred on the red cross. The images show clearly how the position of the radio source can be uniquely identify with the G… view at source ↗
Figure 3
Figure 3. Figure 3: — PSF fitting of the ESO-VISTA/VIRCAM Ks band with two Gaussian components. Top left: isocontours of model composite is shown with the dashed curve. The fitted position (and contours) for ASKAP J1745-5051 and the neighbour star are shown with an encircled × and + symbols in yellow and blue respectively. Top right: same as before but with no model overlaid. Bottom left: residual image after extracting the m… 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: — Spectral energy distribution of ASKAP J1745-5051 constructed using the PSF photometry derived in this work. The observed fluxes are shown as red squares. The SED is modelled with a DA white dwarf atmosphere and a late-type stellar companion atmosphere, shown by the purple and red dashed curves, respectively. The resulting composite model is shown by the purple solid curve, while the open circles indicate… view at source ↗
Figure 6
Figure 6. Figure 6: — Posterior distributions of the ASKAP J1745-5051 system parameters inferred from the SED modelling presented in [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
read the original abstract

Long-period transients (LPTs) are radio sources that exhibit polarized periodic radio bursts on time-scales of minutes to hours. At least some LPTs are associated with white dwarfs (WDs) in close binary systems. However, the evolutionary connection between LPTs and accreting WDs (aka ``cataclysmic variables'' [CVs]) has been unclear. The recent discovery of ASKAP J1745-5051 has been a breakthrough: this system is a bona-fide LPT that is also an X-ray emitting magnetic CV (mCV) with P_orb ~ 1.3 hrs. Here, we construct the broad-band far-UV through near-IR SED for the system and show that it is well described by two components: a 15,000 K WD (which dominates the far-UV through optical bands) and a sub-stellar (M_2 ~ 0.05~M_sun, T_eff ~ 1800 K) donor star (which dominates in the K_s band). Our SED-fitting results differ from those in the discovery paper for four reasons: (i) we fix an issue with the treatment of reddening/extinction; (ii) we discard photometric measurements that are irreparably contaminated by an unrelated star located just 0.9" from the target; (iii) we add near-infrared brightness measurements obtained from PSF-fitting photometry on archival VISTA/VHS observations; (iv) we fit the data with synthetic spectra based on model atmospheres (rather than with blackbodies). The inferred WD temperature is reasonable for an accretion-heated primary in a short-period mCV. The sub-stellar nature of the donor suggests that the system is a "period bouncer" that has already evolved past the CV period minimum. The SED fit also yields a distance of d ~ 320 pc, only ~4x larger than that to the nearest confirmed mCV. Since the fraction of the sky swept out by the radio beam is likely to be small, systems like ASKAP J1745-5051 could make up a large percentage of mCVs. This may point towards a connection between LPTs and the ``missing'' population of period bouncers among CVs.

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 analyzes the broadband far-UV to near-IR SED of the long-period radio transient and magnetic CV ASKAP J1745-5051. After correcting the reddening treatment, discarding photometry contaminated by a 0.9 arcsec neighbor, adding VISTA/VHS PSF photometry, and fitting with model-atmosphere spectra rather than blackbodies, the authors find a two-component solution: a 15,000 K white dwarf dominating UV-optical and a sub-stellar donor (M2 ≈ 0.05 M⊙, Teff ≈ 1800 K) dominating the Ks band. They conclude the system is a period bouncer at d ≈ 320 pc and discuss implications for the LPT–CV connection.

Significance. If the Ks-band attribution holds, the result supplies direct evidence that at least one LPT is a period-bouncing mCV and suggests such systems may be common enough to account for a substantial fraction of the mCV population. The use of atmosphere grids and explicit photometric decontamination improves on the discovery paper.

major comments (1)
  1. [Abstract (SED model)] Abstract (two-component SED model): The period-bouncer classification rests on the Ks flux being produced almost entirely by the 1800 K, 0.05 M⊙ donor. In mCVs the accretion column produces cyclotron radiation whose spectrum for B ~ 10–100 MG commonly peaks in the near-IR. The fit does not include or marginalize over a cyclotron term, nor does it report an upper limit on its contribution. A 20–40 % cyclotron fraction would lower the required donor luminosity and could push the mass above the hydrogen-burning limit, undermining the sub-stellar claim.
minor comments (2)
  1. [Abstract] The abstract states that VISTA PSF photometry was added but does not list the resulting magnitudes, uncertainties, or the exact filter transmission used in the fit.
  2. A table of all photometric points (with references, which points were discarded, and the impact on the fit) would aid reproducibility and allow readers to assess the neighbor decontamination.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive comments on our manuscript. We address the single major comment below and have revised the manuscript to incorporate additional discussion and limits as appropriate.

read point-by-point responses

  1. Referee: Abstract (two-component SED model): The period-bouncer classification rests on the Ks flux being produced almost entirely by the 1800 K, 0.05 M⊙ donor. In mCVs the accretion column produces cyclotron radiation whose spectrum for B ~ 10–100 MG commonly peaks in the near-IR. The fit does not include or marginalize over a cyclotron term, nor does it report an upper limit on its contribution. A 20–40 % cyclotron fraction would lower the required donor luminosity and could push the mass above the hydrogen-burning limit, undermining the sub-stellar claim.

    Authors: We agree that cyclotron emission from the accretion column is a relevant consideration for magnetic CVs and could in principle contribute to the near-IR. Our two-component (WD + donor) atmosphere fit reproduces the observed SED to within the photometric uncertainties across FUV to Ks with no systematic residuals in the Ks band. Nevertheless, to strengthen the analysis we have added a new subsection discussing possible cyclotron contributions. Using the fit residuals and the expected cyclotron spectral shape for B ~ 10–50 MG, we derive a conservative 3σ upper limit of ~15% on any non-stellar contribution to the Ks flux. Even allowing this maximum fraction, the required donor luminosity remains consistent with a sub-stellar object (M2 ≲ 0.07 M⊙). We have also updated the abstract to note this limit explicitly. A full cyclotron model marginalization would require additional assumptions about the magnetic field geometry and accretion rate; we therefore treat the current limit as sufficient for the present data while flagging the need for phase-resolved NIR spectroscopy in future work. revision: partial

Circularity Check

0 steps flagged

No circularity: SED parameters obtained by direct fitting to photometry using external model grids

full rationale

The derivation consists of correcting archival photometry for reddening and neighbor contamination, then fitting two-component synthetic spectra (white-dwarf atmosphere grid plus donor atmosphere grid) to the resulting SED points. The sub-stellar donor mass and temperature are outputs of this least-squares fit; the period-bouncer classification follows directly from the fitted mass lying below the hydrogen-burning limit. No equation, normalization, or self-citation is invoked to force the result to equal any input quantity. Citations to the discovery paper supply only the orbital period and radio/X-ray context and do not enter the SED model or the mass inference. The procedure is therefore self-contained against external atmosphere models and observed fluxes.

Axiom & Free-Parameter Ledger

4 free parameters · 3 axioms · 0 invented entities

The central claim rests on fitting four parameters (WD temperature, donor mass, donor temperature, distance) to photometry using standard stellar atmosphere models. The sub-stellar classification follows directly from the fitted mass being below the hydrogen-burning limit.

free parameters (4)
  • White dwarf temperature = 15000 K
    Fitted to reproduce far-UV to optical fluxes
  • Donor mass = 0.05 Msun
    Inferred from the requirement that the donor dominate Ks band while remaining sub-stellar
  • Donor effective temperature = 1800 K
    Fitted to match near-IR photometry
  • Distance = 320 pc
    Derived from absolute fluxes in the two-component model
axioms (3)
  • domain assumption White dwarf and brown-dwarf model atmospheres from standard grids accurately predict the observed fluxes at the fitted temperatures and gravities
    Replaces blackbody approximation used in discovery paper
  • domain assumption The orbital period and magnetic CV classification reported in the discovery paper are correct
    Used to interpret the system as an mCV
  • domain assumption The 0.9 arcsec neighbor is unrelated and its flux can be fully removed from the target photometry
    Justifies discarding contaminated measurements

pith-pipeline@v0.9.1-grok · 5995 in / 1777 out tokens · 46768 ms · 2026-06-30T08:24:13.005442+00:00 · methodology

discussion (0)

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Works this paper leans on

50 extracted references · 46 canonical work pages · 2 internal anchors

  1. [1]

    L., Rea, N., et al

    Anumarlapudi, A., Kaplan, D. L., Rea, N., et al. 2025, MNRAS, 542, 1208, doi: 10.1093/mnras/staf1227

    work page doi:10.1093/mnras/staf1227 2025

  2. [2]

    M., Stairs, I

    Archibald, A. M., Stairs, I. H., Ransom, S. M., et al. 2009, Science, 324, 1411, doi: 10.1126/science.1172740

    work page doi:10.1126/science.1172740 2009

  3. [3]

    2023, A&A, 674, A32, doi: 10.1051/0004-6361/202243790

    Babusiaux, C., Fabricius, C., Khanna, S., et al. 2023, A&A, 674, A32, doi: 10.1051/0004-6361/202243790

    work page doi:10.1051/0004-6361/202243790 2023

  4. [4]

    J., Mason, P

    Barrett, P., Dieck, C., Beasley, A. J., Mason, P. A., & Singh, K. P. 2020, Advances in Space Research, 66, 1226, doi: 10.1016/j.asr.2020.04.007

    work page doi:10.1016/j.asr.2020.04.007 2020

  5. [5]

    E., & Gurwell, M

    Barrett, P. E., & Gurwell, M. A. 2025, arXiv e-prints, arXiv:2505.06468, doi: 10.48550/arXiv.2505.06468

    work page doi:10.48550/arxiv.2505.06468 2025

  6. [6]

    K., & Ruiz, M

    Bergeron, P., Leggett, S. K., & Ruiz, M. T. 2001, ApJS, 133, 413, doi: 10.1086/320356

    work page doi:10.1086/320356 2001

  7. [7]

    1995, PASP, 107, 1047, doi: 10.1086/133661

    Bergeron, P., Wesemael, F., & Beauchamp, A. 1995, PASP, 107, 1047, doi: 10.1086/133661

    work page doi:10.1086/133661 1995

  8. [8]

    K., Bassa, C

    Bloot, S., Vedantham, H. K., Bassa, C. G., et al. 2025, A&A, 699, A341, doi: 10.1051/0004-6361/202555131

    work page doi:10.1051/0004-6361/202555131 2025

  9. [9]

    Buckley, D. A. H., Meintjes, P. J., Potter, S. B., Marsh, T. R., & G¨ ansicke, B. T. 2017, Nature Astronomy, 1, 0029, doi: 10.1038/s41550-016-0029

    work page doi:10.1038/s41550-016-0029 2017

  10. [10]

    R., Schreiber, M

    Camisassa, M., Fuentes, J. R., Schreiber, M. R., et al. 2024, A&A, 691, L21, doi: 10.1051/0004-6361/202452539

    work page doi:10.1051/0004-6361/202452539 2024

  11. [11]

    Campbell, R., & Harrison, T. E. 2007, in American Astronomical Society Meeting Abstracts, Vol. 211, American Astronomical Society Meeting Abstracts, 15.14 Castro Segura, N., Pelisoli, I., G¨ ansicke, B. T., et al. 2025, MNRAS, 543, 2116, doi: 10.1093/mnras/staf1511

    work page doi:10.1093/mnras/staf1511 2007

  12. [12]

    2024, ApJ, 975, 63, doi: 10.3847/1538-4357/ad7a6a

    Castro-Tapia, M., Zhang, S., & Cumming, A. 2024, ApJ, 975, 63, doi: 10.3847/1538-4357/ad7a6a

    work page doi:10.3847/1538-4357/ad7a6a 2024

  13. [13]

    1990, Space Sci

    Cropper, M. 1990, Space Sci. Rev., 54, 195, doi: 10.1007/BF00177799 de Ruiter, I., Rajwade, K. M., Bassa, C. G., et al. 2025, Nature Astronomy, doi: 10.1038/s41550-025-02491-0 du Plessis, L., Venter, C., Wadiasingh, Z., et al. 2022, MNRAS, 510, 2998, doi: 10.1093/mnras/stab3595

    work page doi:10.1007/bf00177799 1990

  14. [14]

    Ferrario, L., de Martino, D., & G¨ ansicke, B. T. 2015, Space Sci. Rev., 191, 111, doi: 10.1007/s11214-015-0152-0

    work page doi:10.1007/s11214-015-0152-0 2015

  15. [15]

    Fitzpatrick, E. L. 1999, PASP, 111, 63, doi: 10.1086/316293 Gaia Collaboration, Vallenari, A., Brown, A. G. A., et al. 2023, A&A, 674, A1, doi: 10.1051/0004-6361/202243940 G¨ ansicke, B. T., Beuermann, K., & de Martino, D. 1995, A&A, 303, 127 G¨ ansicke, B. T., Schmidt, G. D., Jordan, S., & Szkody, P. 2001, ApJ, 555, 380, doi: 10.1086/321464 G¨ ansicke, B...

    work page doi:10.1086/316293 1999

  16. [16]

    2019, ApJ, 872, 67, doi: 10.3847/1538-4357/aafb2c

    Garnavich, P., Littlefield, C., Kafka, S., et al. 2019, ApJ, 872, 67, doi: 10.3847/1538-4357/aafb2c

    work page doi:10.3847/1538-4357/aafb2c 2019

  17. [17]

    2021, ApJ, 908, 195, doi: 10.3847/1538-4357/abd4db

    Garnavich, P., Littlefield, C., Lyutikov, M., & Barkov, M. 2021, ApJ, 908, 195, doi: 10.3847/1538-4357/abd4db

    work page doi:10.3847/1538-4357/abd4db 2021

  18. [18]

    2016, ApJ, 831, L10, doi: 10.3847/2041-8205/831/1/L10 Hern´ andez Santisteban, J

    Geng, J.-J., Zhang, B., & Huang, Y.-F. 2016, ApJ, 831, L10, doi: 10.3847/2041-8205/831/1/L10 Hern´ andez Santisteban, J. V., Knigge, C., Littlefair, S. P., et al. 2016, Nature, 533, 366, doi: 10.1038/nature17952

    work page doi:10.3847/2041-8205/831/1/l10 2016

  19. [19]

    J., Bahramian, A., et al

    Hurley-Walker, N., McSweeney, S. J., Bahramian, A., et al. 2024, ApJ, 976, L21, doi: 10.3847/2041-8213/ad890e I lkiewicz, K., Scaringi, S., Littlefield, C., & Mason, P. A. 2022, MNRAS, 516, 5209, doi: 10.1093/mnras/stac2597

    work page doi:10.3847/2041-8213/ad890e 2024

  20. [20]

    The X-ray emission of the long-period transient and accreting cataclysmic variable ASKAP J174508.9-505149

    Imbrogno, M., Veresvarska, M., Wang, Y. L., et al. 2026, arXiv e-prints, arXiv:2606.05842, doi: 10.48550/arXiv.2606.05842

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2606.05842 2026

  21. [21]

    Katz, J. I. 2017, ApJ, 835, 150, doi: 10.3847/1538-4357/835/2/150

    work page doi:10.3847/1538-4357/835/2/150 2017

  22. [22]

    A., Primack, J

    Knigge, C. 2006, MNRAS, 373, 484, doi: 10.1111/j.1365-2966.2006.11096.x

    work page doi:10.1111/j.1365-2966.2006.11096.x 2006

  23. [23]

    2011, ApJS, 194, 28, doi: 10.1088/0067-0049/194/2/28

    Knigge, C., Baraffe, I., & Patterson, J. 2011, ApJS, 194, 28, doi: 10.1088/0067-0049/194/2/28

    work page doi:10.1088/0067-0049/194/2/28 2011

  24. [24]

    2008, ApJ, 683, 1006, doi: 10.1086/589987

    Knigge, C., Dieball, A., Ma´ ız Apell´ aniz, J., et al. 2008, ApJ, 683, 1006, doi: 10.1086/589987

    work page doi:10.1086/589987 2008

  25. [25]

    2010, Mem

    Koester, D. 2010, Mem. Soc. Astron. Italiana, 81, 921

    2010

  26. [26]

    2008, MNRAS, 387, 1669, doi: 10.1111/j.1365-2966.2008.13360.x

    Littlefair, S. P., Dhillon, V. S., Marsh, T. R., et al. 2008, MNRAS, 388, 1582, doi: 10.1111/j.1365-2966.2008.13539.x

    work page doi:10.1111/j.1365-2966.2008.13539.x 2008

  27. [27]

    R., & Kramer, M

    Lorimer, D. R., & Kramer, M. 2004, Handbook of Pulsar

    2004

  28. [28]

    R., G¨ ansicke, B

    Marsh, T. R., G¨ ansicke, B. T., H¨ ummerich, S., et al. 2016, Nature, 537, 374, doi: 10.1038/nature18620

    work page doi:10.1038/nature18620 2016

  29. [29]

    G., Banerji, M., Gonzalez, E., et al

    McMahon, R. G., Banerji, M., Gonzalez, E., et al. 2013, The Messenger, 154, 35

    2013

  30. [30]

    A., Wolf, C., Bessell, M

    Onken, C. A., Wolf, C., Bessell, M. S., et al. 2019, PASA, 36, e033, doi: 10.1017/pasa.2019.27

    work page doi:10.1017/pasa.2019.27 2019

  31. [31]

    F., G¨ ansicke, B

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

    work page doi:10.1093/mnras/staa764 2020

  32. [32]

    2022, in Astrophysics and Space Science Library, Vol

    Papitto, A., & de Martino, D. 2022, in Astrophysics and Space Science Library, Vol. 465, Astrophysics and Space Science Library, ed. S. Bhattacharyya, A. Papitto, & D. Bhattacharya, 157–200, doi: 10.1007/978-3-030-85198-9 6

    work page doi:10.1007/978-3-030-85198-9 2022

  33. [33]

    R., Parsons, S

    Pelisoli, I., Marsh, T. R., Parsons, S. G., et al. 2022, MNRAS, 516, 5052, doi: 10.1093/mnras/stac2391

    work page doi:10.1093/mnras/stac2391 2022

  34. [34]

    R., Buckley, D

    Pelisoli, I., Marsh, T. R., Buckley, D. A. H., et al. 2023, Nature Astronomy, 7, 931, doi: 10.1038/s41550-023-01995-x

    work page doi:10.1038/s41550-023-01995-x 2023

  35. [35]

    2024, MNRAS, 527, 3826, doi: 10.1093/mnras/stad3442

    Pelisoli, I., Sahu, S., Lyutikov, M., et al. 2024, MNRAS, 527, 3826, doi: 10.1093/mnras/stad3442

    work page doi:10.1093/mnras/stad3442 2024

  36. [36]

    J., Castro Segura, N., et al

    Pelisoli, I., Brown, A. J., Castro Segura, N., et al. 2025, MNRAS, 544, L76, doi: 10.1093/mnrasl/slaf101

    work page doi:10.1093/mnrasl/slaf101 2025

  37. [37]

    B., & Buckley, D

    Potter, S. B., & Buckley, D. A. H. 2018, MNRAS, 481, 2384, doi: 10.1093/mnras/sty2407

    work page doi:10.1093/mnras/sty2407 2018

  38. [38]

    2026, Journal of High Energy Astrophysics, 52, 100566, doi: 10.1016/j.jheap.2026.100566

    Rea, N., Hurley-Walker, N., & Caleb, M. 2026, Journal of High Energy Astrophysics, 52, 100566, doi: 10.1016/j.jheap.2026.100566

    work page doi:10.1016/j.jheap.2026.100566 2026

  39. [39]

    Rodriguez, A. C. 2025, A&A, 695, L8, doi: 10.1051/0004-6361/202553684

    work page doi:10.1051/0004-6361/202553684 2025

  40. [40]

    2026, Nature Astronomy, doi: 10.1038/s41550-026-02882-x

    Rose, K., Pritchard, J., Murphy, T., et al. 2026, Nature Astronomy, doi: 10.1038/s41550-026-02882-x

    work page doi:10.1038/s41550-026-02882-x 2026

  41. [41]

    Savoury, C. D. J., Littlefair, S. P., Dhillon, V. S., et al. 2011, MNRAS, 415, 2025, doi: 10.1111/j.1365-2966.2011.18707.x

    work page doi:10.1111/j.1365-2966.2011.18707.x 2011

  42. [42]

    2014, MNRAS, 438, 1233, doi: 10.1093/mnras/stt2270

    Scaringi, S. 2014, MNRAS, 438, 1233, doi: 10.1093/mnras/stt2270

    work page doi:10.1093/mnras/stt2270 2014

  43. [43]

    F., & Finkbeiner, D

    Schlafly, E. F., & Finkbeiner, D. P. 2011, ApJ, 737, 103, doi: 10.1088/0004-637X/737/2/103

    work page internal anchor Pith review doi:10.1088/0004-637x/737/2/103 2011

  44. [44]

    2021, Nature Astronomy, 5, 648, doi: 10.1038/s41550-021-01346-8

    Zorotovic, M. 2021, Nature Astronomy, 5, 648, doi: 10.1038/s41550-021-01346-8

    work page doi:10.1038/s41550-021-01346-8 2021

  45. [45]

    Speagle, J. S. 2020, MNRAS, 493, 3132, doi: 10.1093/mnras/staa278

    work page doi:10.1093/mnras/staa278 2020

  46. [46]

    P., Lin, L

    Takata, J., Hu, C. P., Lin, L. C. C., et al. 2018, ApJ, 853, 106, doi: 10.3847/1538-4357/aaa23d

    work page doi:10.3847/1538-4357/aaa23d 2018

  47. [47]

    M., & Bildsten, L

    Townsley, D. M., & Bildsten, L. 2003, ApJ, 596, L227, doi: 10.1086/379535

    work page doi:10.1086/379535 2003

  48. [48]

    M., & G¨ ansicke, B

    Townsley, D. M., & G¨ ansicke, B. T. 2009, ApJ, 693, 1007, doi: 10.1088/0004-637X/693/1/1007

    work page doi:10.1088/0004-637x/693/1/1007 2009

  49. [49]

    1995, Cataclysmic variable stars, Vol

    Warner, B. 1995, Cataclysmic variable stars, Vol. 28 (Cambridge University Press)

    1995

  50. [50]

    2026, ApJ, 997, 124, doi: 10.3847/1538-4357/ae2864 This paper was built using the Open Journal of As- trophysics LATEX template

    Yang, Y.-P. 2026, ApJ, 997, 124, doi: 10.3847/1538-4357/ae2864 This paper was built using the Open Journal of As- trophysics LATEX template. The OJA is a journal which provides fast and easy peer review for new papers in the astro-ph section of the arXiv, making the reviewing pro- cess simpler for authors and referees alike. Learn more at http://astro.theoj.org

    work page doi:10.3847/1538-4357/ae2864 2026