pith. machine review for the scientific record. sign in

arxiv: 2605.12722 · v1 · submitted 2026-05-12 · 🌌 astro-ph.SR · astro-ph.HE

Recognition: 2 theorem links

· Lean Theorem

A New WZ Sagittae-type Dwarf Nova KSP-OT-202104a Near the Period Minimum from the KMTNet Supernova Program

Sang Chul Kim , Youngdae Lee , Dae-Sik Moon , Hong Soo Park , Yuan Qi Ni , Nan Jiang , Hyobin Im
Authors on Pith no claims yet

Pith reviewed 2026-05-14 19:35 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.HE
keywords dwarf novaWZ Sagittaesuperhump periodorbital period minimumAM CVn starscataclysmic variablesKMTNetoutburst
0
0 comments X

The pith

A new WZ Sagittae-type dwarf nova KSP-OT-202104a shows a superhump period of 71.7 minutes, placing it below the orbital period minimum and on a path toward AM CVn stars.

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

The paper reports photometric and spectroscopic observations of KSP-OT-202104a, a dwarf nova that reached outburst amplitudes of about 8 magnitudes and lasted 28.5 days. The authors measure a superhump period of approximately 71.7 minutes and classify the system as WZ Sge-type. Because orbital periods in these objects are typically very close to the superhump period, they conclude that KSP-OT-202104a lies below the period minimum for hydrogen-rich cataclysmic variables and is evolving toward AM Canum Venaticorum stars. The system is presented as a new example of a short-period dwarf nova with low mass-transfer rate.

Core claim

We present photometric and spectroscopic studies of a new WZ Sagittae-type dwarf nova KSP-OT-202104a discovered by the KMTNet Supernova Program. The source exhibits outburst amplitudes of ~8 mag with a duration of ~28.5 days in the V-band. We estimate the superhump period to be P_sh ≈ 71.7 minutes. Since the orbital period in WZ Sge-type DNe is typically very close to the superhump period, we consider that this target would belong to the small sample of DNe below the period minimum and may be evolving toward AM CVn stars. This system therefore adds an example of a short-period dwarf nova with a low mass-transfer rate to the known sample.

What carries the argument

The superhump period of 71.7 minutes together with the established near-equality of superhump and orbital periods in WZ Sge-type dwarf novae, used to infer an orbital period below the hydrogen-rich minimum.

If this is right

  • The system increases the number of known dwarf novae with orbital periods below the hydrogen-rich minimum.
  • It supplies an additional data point supporting the evolutionary channel from WZ Sge-type dwarf novae to helium-rich AM CVn stars.
  • It demonstrates that short-period systems can maintain low mass-transfer rates sufficient to produce large-amplitude outbursts.
  • The measured outburst duration and amplitude provide a benchmark for modeling accretion-disk behavior at extreme short periods.

Where Pith is reading between the lines

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

  • Direct measurement of the orbital period via time-resolved spectroscopy would give an independent check on the superhump-based inference.
  • Discovery of more systems with similar periods could help determine whether objects near the minimum spend a detectable fraction of their lifetime as hydrogen-rich dwarf novae before becoming AM CVn stars.
  • Long-term monitoring of this object could test whether its mass-transfer rate remains low enough to prevent frequent normal outbursts.

Load-bearing premise

The orbital period is assumed to be nearly identical to the observed superhump period, following the usual pattern for WZ Sge-type dwarf novae.

What would settle it

A spectroscopic radial-velocity curve or photometric orbital modulation that yields an orbital period well above the superhump value and above the period minimum would falsify the placement below the minimum.

Figures

Figures reproduced from arXiv: 2605.12722 by Dae-Sik Moon, Hong Soo Park, Hyobin Im, Nan Jiang, Sang Chul Kim, Youngdae Lee, Yuan Qi Ni.

Figure 1
Figure 1. Figure 1: BV I-band light curves of the superoutburst of KSP-OT-202104a with no extinction correction. The cyan dashed vertical line marks the epoch when the Gemini spectrum was taken, and the short green vertical lines at the bottom correspond to the epochs outside the outburst when our V -band observations were made. Labels (a)–(d) denote different phases: (a) quiescent phase prior to the superoutburst in MJD = 58… view at source ↗
Figure 2
Figure 2. Figure 2: Schematic light curve diagram (blue solid curve) of a type D WZ Sge-type DN without rebrightening. Thick grey horizontal line represents the quiescent phase brightness. The beginning points of the four phases—rising, plateau, decline, and tail parts—are marked as 1, 2, 3, and 4, respectively. The short blue dashed line is the extension of the decline part to the quiescent magnitude. ‘Dp’ between points 1 a… view at source ↗
Figure 3
Figure 3. Figure 3: Comparison between the observed V -band light curve of KSP-OT-202104a (without extinction correction) with the best-fit polynomial fittings: blue, black, and green colors are for the observations (filled circles) and fittings (dashed curves) of the rising, plateau, and decline parts, respectively. The inset shows the fitting (red dashed curve) of the near-peak light curve using the equation mpe(d) = Ap(1 −… view at source ↗
Figure 4
Figure 4. Figure 4: V -band images of KSP-OT-202104a. Panel (a) is a quiescent phase image made by stacking 549 60-s exposures obtained during MJD = 58795.27–59298.86 before the superoutburst. Panel (b) is the first detection image at MJD = 59313.40; (c) is a near-peak image of the superoutburst at MJD = 59314.01; and (d) is the last image during the declining part at MJD = 59339.05. The labels (a)–(d) coincide with those in … view at source ↗
Figure 5
Figure 5. Figure 5: (a) Results of PDM analysis and (b) phase-folded profile. In panel (a), the black solid line is median Θ and the shaded area presents 90% confidence range from 1,000 bootstrap resampling. In panel (b), blue, green, and red colors indicate B-, V -, and I-band, respectively. The black dashed curve is a sine curve fitted to the data with the period of 71.7 min [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Color evolution of KSP-OT-202104a: blue, red, and green circles for (B−V ), (V −I), and (B−I) colors without extinction correction. The x-axis represents days from the V -band peak brightness at MJD = 59314.11. The stars with large error bars in the left are colors for the quiescent phase shown for comparison, and the dashed lines show the results of linear fittings of the post-peak color evolution [PITH_… view at source ↗
Figure 7
Figure 7. Figure 7: Gemini spectrum of KSP-OT-202104a obtained by combining blue and red spectra shown after 16˚A smoothing. Extinction is not corrected. The locations of H and He lines often observed in WZ Sge-type DNe are marked by vertical lines: solid, dotted, and dashed lines for H i, He i, and He ii, respectively. They are Hα (6563 ˚A), Hβ (4861 ˚A), Hγ (4340 ˚A), Hδ (4102 ˚A), Hϵ (3970 ˚A), Hζ (3889 ˚A), He i (red), an… view at source ↗
Figure 8
Figure 8. Figure 8: (a) Distribution of orbital periods and mass ratios of short-period DNe: 9 with Porb shorter than the period minimum (large squares and black arrows), 34 WZ Sge-type DNe from T. Kato (2015) (dots with error bars), and 3 period bouncer candidates with Porb greater than the period minimum (large pentagons). For KSP-OT-202104a (red dashed line), we show the superhump period (the orbital period differs from th… view at source ↗
read the original abstract

We present photometric and spectroscopic studies of a new WZ Sagittae (Sge)-type dwarf nova (DN) KSP-OT-202104a discovered by the Korea Microlensing Telescope Network Supernova Program. The source exhibits outburst amplitudes of $\sim 8$ mag with a duration of $\sim 28.5$ days in the $V$-band. It is a type D DN among WZ Sge-types, and we estimate the superhump period to be $P_{\rm sh} \approx 71.7$ minutes ($=0.04978$ days). Its spectrum shows blue continuum as often found in optically-thick accretion disks of DNe during outbursts with hydrogen absorption lines from H$\beta$ to H$\zeta$. Since the orbital period in WZ Sge-type DNe is typically very close to the superhump period, we consider that this target would belong to the small sample of DNe below the period minimum and may be evolving toward AM Canum Venaticorum (AM CVn) stars. This system therefore adds an example of a short-period dwarf nova with a low mass-transfer rate to the known sample.

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 / 0 minor

Summary. The manuscript reports photometric and spectroscopic observations of the newly discovered dwarf nova KSP-OT-202104a from the KMTNet Supernova Program. It exhibits ~8 mag outbursts lasting ~28.5 days, is classified as a type-D WZ Sge system, and yields a superhump period P_sh ≈ 71.7 min (0.04978 d). The spectrum shows a blue continuum with Balmer absorption lines. The authors conclude that the system lies below the period minimum and may be evolving toward AM CVn stars, adding an example of a short-period DN with low mass-transfer rate.

Significance. If the period classification holds, the result enlarges the small sample of hydrogen-rich cataclysmic variables below the ~76 min minimum and supplies an additional anchor point for evolutionary models connecting WZ Sge-type DNe to AM CVn stars. The work also illustrates the utility of wide-field supernova surveys for catching rare, low-amplitude-transfer systems.

major comments (1)
  1. [Abstract] Abstract and discussion of period classification: the claim that KSP-OT-202104a lies below the period minimum rests on the measured superhump period P_sh ≈ 71.7 min together with the statement that 'the orbital period in WZ Sge-type DNe is typically very close to the superhump period.' No independent orbital-period determination (radial-velocity curve, eclipse timing, or quiescent photometry) is reported, and the single spectrum is outburst-only with no phase information. This leaves the precise location relative to the minimum unverified for this specific object and makes the evolutionary inference toward AM CVn stars provisional.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the thorough review and constructive feedback on our manuscript. We agree that the period classification requires careful qualification given the lack of an independent orbital-period measurement, and we have revised the abstract and discussion accordingly to present the conclusion more cautiously while preserving the scientific value of the discovery.

read point-by-point responses

  1. Referee: [Abstract] Abstract and discussion of period classification: the claim that KSP-OT-202104a lies below the period minimum rests on the measured superhump period P_sh ≈ 71.7 min together with the statement that 'the orbital period in WZ Sge-type DNe is typically very close to the superhump period.' No independent orbital-period determination (radial-velocity curve, eclipse timing, or quiescent photometry) is reported, and the single spectrum is outburst-only with no phase information. This leaves the precise location relative to the minimum unverified for this specific object and makes the evolutionary inference toward AM CVn stars provisional.

    Authors: We thank the referee for highlighting this important caveat. It is accurate that our classification relies on the well-established empirical relation for WZ Sge-type systems rather than a direct orbital-period measurement for this object. In the broader literature, the superhump excess in WZ Sge-type dwarf novae is typically small (ε ≈ 0.005–0.02; see Kato et al. 2017 and references therein), so that P_orb lies only ~0.5–1.5 min shorter than the observed P_sh = 71.7 min. Even adopting the upper end of this range yields P_orb ≲ 71.2 min, still well below the ~76 min hydrogen-rich period minimum. We have therefore revised the abstract to state that the system “is likely below the period minimum” and added an explicit paragraph in the discussion that (i) cites the typical superhump excess range, (ii) notes the absence of independent P_orb data, and (iii) qualifies the evolutionary link to AM CVn stars as a plausible interpretation consistent with the small existing sample. These changes make the claim appropriately provisional without altering the core observational results. revision: partial

Circularity Check

0 steps flagged

No circularity; inference applies standard external property of WZ Sge systems to direct measurement

full rationale

The paper measures P_sh directly from photometric data and classifies the object as WZ Sge-type based on outburst amplitude (~8 mag) and duration (~28.5 days). The claim that the system lies below the period minimum follows from applying the literature statement that P_orb is typically close to P_sh in this class; this is an external benchmark, not a quantity fitted or defined inside the paper. No equation or step reduces the result to its own inputs by construction, and no self-citation chain is invoked for the key assumption.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

The abstract relies on established knowledge of cataclysmic variables and the typical closeness of superhump and orbital periods in WZ Sge systems. No new free parameters, axioms, or invented entities are introduced.

pith-pipeline@v0.9.0 · 5546 in / 1155 out tokens · 30723 ms · 2026-05-14T19:35:26.628031+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.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

110 extracted references · 103 canonical work pages · 2 internal anchors

  1. [1]

    R., et al

    Afsariardchi, N., Moon, D.-S., Drout, M. R., et al. 2019, ApJ, 881, 22, doi: 10.3847/1538-4357/ab2be6 Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33, doi: 10.1051/0004-6361/201322068 Astropy Collaboration, Price-Whelan, A. M., Sip˝ ocz, B. M., et al. 2018, AJ, 156, 123, doi: 10.3847/1538-3881/aabc4f

    work page doi:10.3847/1538-4357/ab2be6 2019

  2. [2]

    1996, A&A, 311, 889

    Paradijs, J. 1996, A&A, 311, 889

    1996

  3. [3]

    H., & van Paradijs, J

    Augusteijn, T., van Kerkwijk, M. H., & van Paradijs, J. 1993, A&A, 267, L55

    1993

  4. [4]

    T., Breedt, E., et al

    Aungwerojwit, A., G¨ ansicke, B. T., Breedt, E., et al. 2025, MNRAS, 537, 3078, doi: 10.1093/mnras/staf173

    work page doi:10.1093/mnras/staf173 2025

  5. [5]

    2002, PASJ, 54, L7, doi: 10.1093/pasj/54.1.L7

    Baba, H., Sadakane, K., Norimoto, Y., et al. 2002, PASJ, 54, L7, doi: 10.1093/pasj/54.1.L7

    work page doi:10.1093/pasj/54.1.l7 2002

  6. [6]

    Pontzen and F

    Breedt, E., G¨ ansicke, B. T., Marsh, T. R., et al. 2012, MNRAS, 425, 2548, doi: 10.1111/j.1365-2966.2012.21724.x

    work page doi:10.1111/j.1365-2966.2012.21724.x 2012

  7. [7]

    M., & Mazeh, T

    Brosch, N., Leibowitz, E. M., & Mazeh, T. 1980, ApJL, 236, L29, doi: 10.1086/183192

    work page doi:10.1086/183192 1980

  8. [8]

    Q., et al

    Brown, S., Moon, D.-S., Ni, Y. Q., et al. 2018, ApJ, 860, 21, doi: 10.3847/1538-4357/aabfe2

    work page doi:10.3847/1538-4357/aabfe2 2018

  9. [9]

    K., & Kenyon, S

    Cannizzo, J. K., & Kenyon, S. J. 1987, ApJ, 320, 319, doi: 10.1086/165545

    work page doi:10.1086/165545 1987

  10. [10]

    2026, ApJ, 1001, 103, doi: 10.3847/1538-4357/ae5494

    Chang, E., Moon, D.-S., Sandoval, P., et al. 2026, ApJ, 1001, 103, doi: 10.3847/1538-4357/ae5494

    work page doi:10.3847/1538-4357/ae5494 2026

  11. [11]

    2015, Acta Polytechnica CTU Proceedings, 2, 165, doi: 10.14311/APP.2015.02.0165

    Chochol, D., Shugarov, S., Katysheva, N., et al. 2015, Acta Polytechnica CTU Proceedings, 2, 165, doi: 10.14311/APP.2015.02.0165

    work page doi:10.14311/app.2015.02.0165 2015

  12. [12]

    J., G¨ ansicke, B

    Drake, A. J., G¨ ansicke, B. T., Djorgovski, S. G., et al. 2014, MNRAS, 441, 1186, doi: 10.1093/mnras/stu639 G¨ ansicke, B. T., Dillon, M., Southworth, J., et al. 2009, MNRAS, 397, 2170, doi: 10.1111/j.1365-2966.2009.15126.x

    work page doi:10.1093/mnras/stu639 2014

  13. [13]

    L., Kemper, E., & Suntzeff, N

    Gilliland, R. L., Kemper, E., & Suntzeff, N. 1986, ApJ, 301, 252, doi: 10.1086/163894

    work page doi:10.1086/163894 1986

  14. [14]

    Giovanelli, R., & Haynes, M. P. 2002, ApJL, 571, L107, doi: 10.1086/341368

    work page doi:10.1086/341368 2002

  15. [15]

    Green, G. M. 2018, The Journal of Open Source Software, 3, 695, doi: 10.21105/joss.00695

    work page doi:10.21105/joss.00695 2018

  16. [16]

    , year = 2019, month = dec, volume =

    Finkbeiner, D. 2019, ApJ, 887, 93, doi: 10.3847/1538-4357/ab5362

    work page doi:10.3847/1538-4357/ab5362 2019

  17. [17]

    J., van Roestel, J., & Wong, T

    Green, M. J., van Roestel, J., & Wong, T. L. S. 2025, arXiv e-prints, arXiv:2505.10535, doi: 10.48550/arXiv.2505.10535

    work page doi:10.48550/arxiv.2505.10535 2025

  18. [18]

    J., Marsh, T

    Green, M. J., Marsh, T. R., Steeghs, D. T. H., et al. 2018, MNRAS, 476, 1663, doi: 10.1093/mnras/sty299

    work page doi:10.1093/mnras/sty299 2018

  19. [19]

    J., Marsh, T

    Green, M. J., Marsh, T. R., Carter, P. J., et al. 2020, MNRAS, 496, 1243, doi: 10.1093/mnras/staa1509

    work page doi:10.1093/mnras/staa1509 2020

  20. [20]

    2020, PASJ, 72, 76, doi: 10.1093/pasj/psaa065

    Han, Z., Boonrucksar, S., Qian, S., et al. 2020, PASJ, 72, 76, doi: 10.1093/pasj/psaa065

    work page doi:10.1093/pasj/psaa065 2020

  21. [21]

    R., & Wynn, G

    Harlaftis, E. T., Steeghs, D., Horne, K., Mart´ ın, E., & Magazz´ u, A. 1999, MNRAS, 306, 348, doi: 10.1046/j.1365-8711.1999.02502.x Hern´ andez Santisteban, J. V., Echevarr´ ıa, J., Zharikov, S., et al. 2019, MNRAS, 486, 2631, doi: 10.1093/mnras/stz798

    work page doi:10.1046/j.1365-8711.1999.02502.x 1999

  22. [22]

    V., Robinson, E

    Hessman, F. V., Robinson, E. L., Nather, R. E., & Zhang, E.-H. 1984, ApJ, 286, 747, doi: 10.1086/162651

    work page doi:10.1086/162651 1984

  23. [23]

    1990, PASJ, 42, 135

    Hirose, M., & Osaki, Y. 1990, PASJ, 42, 135

    1990

  24. [24]

    Howarth, I. D. 1981, Information Bulletin on Variable Stars, 1925, 1

    1981

  25. [25]

    B., Nelson, L

    Howell, S. B., Nelson, L. A., & Rappaport, S. 2001, ApJ, 550, 897, doi: 10.1086/319776

    work page doi:10.1086/319776 2001

  26. [26]

    B., Szkody, P., & Cannizzo, J

    Howell, S. B., Szkody, P., & Cannizzo, J. K. 1995, ApJ, 439, 337, doi: 10.1086/175177

    work page doi:10.1086/175177 1995

  27. [27]

    2018, PASJ, 70, 79, doi: 10.1093/pasj/psy074

    Imada, A., Isogai, K., Yanagisawa, K., & Kawai, N. 2018, PASJ, 70, 79, doi: 10.1093/pasj/psy074

    work page doi:10.1093/pasj/psy074 2018

  28. [28]

    2006, PASJ, 58, L23, doi: 10.1093/pasj/58.4.L23

    Imada, A., Kubota, K., Kato, T., et al. 2006, PASJ, 58, L23, doi: 10.1093/pasj/58.4.L23

    work page doi:10.1093/pasj/58.4.l23 2006

  29. [29]

    Q., et al

    Jiang, N., Moon, D.-S., Ni, Y. Q., et al. 2025, ApJ, 989, 53, doi: 10.3847/1538-4357/ade997

    work page doi:10.3847/1538-4357/ade997 2025

  30. [30]

    2015, PASJ, 67, 108, doi: 10.1093/pasj/psv077

    Kato, T. 2015, PASJ, 67, 108, doi: 10.1093/pasj/psv077

    work page doi:10.1093/pasj/psv077 2015

  31. [31]

    2021, PASJ, 73, 1375, doi: 10.1093/pasj/psab080

    Kato, T., & Kojiguchi, N. 2021, PASJ, 73, 1375, doi: 10.1093/pasj/psab080

    work page doi:10.1093/pasj/psab080 2021

  32. [32]

    2013, PASJ, 65, L11, doi: 10.1093/pasj/65.5.L11

    Maehara, H. 2013, PASJ, 65, L11, doi: 10.1093/pasj/65.5.L11

    work page doi:10.1093/pasj/65.5.l11 2013

  33. [33]

    2001, PASJ, 53, 1191, doi: 10.1093/pasj/53.6.1191

    Kato, T., Sekine, Y., & Hirata, R. 2001, PASJ, 53, 1191, doi: 10.1093/pasj/53.6.1191

    work page doi:10.1093/pasj/53.6.1191 2001

  34. [34]

    2009a, PASJ, 61, S395, doi: 10.1093/pasj/61.sp2.S395

    Kato, T., Imada, A., Uemura, M., et al. 2009a, PASJ, 61, S395, doi: 10.1093/pasj/61.sp2.S395

    work page doi:10.1093/pasj/61.sp2.s395

  35. [35]

    P., Maehara, H., et al

    Kato, T., Pavlenko, E. P., Maehara, H., et al. 2009b, PASJ, 61, 601, doi: 10.1093/pasj/61.3.601 WZ Sge-type Dwarf nova : KSP-OT-202104a15

    work page doi:10.1093/pasj/61.3.601

  36. [36]

    A., et al

    Kato, T., Hambsch, F.-J., Dubovsky, P. A., et al. 2015, PASJ, 67, 105, doi: 10.1093/pasj/psv072

    work page doi:10.1093/pasj/psv072 2015

  37. [37]

    2017, PASJ, 69, 75, doi: 10.1093/pasj/psx058

    Kato, T., Isogai, K., Hambsch, F.-J., et al. 2017, PASJ, 69, 75, doi: 10.1093/pasj/psx058

    work page doi:10.1093/pasj/psx058 2017

  38. [38]

    L., Ramsay, G., Kennedy, M., et al

    Killestein, T. L., Ramsay, G., Kennedy, M., et al. 2025, A&A, 699, A8, doi: 10.1051/0004-6361/202553823

    work page doi:10.1051/0004-6361/202553823 2025

  39. [39]

    2016, Journal of Korean Astronomical Society, 49, 37, doi: 10.5303/JKAS.2016.49.1.37

    Kim, S.-L., Lee, C.-U., Park, B.-G., et al. 2016, Journal of Korean Astronomical Society, 49, 37, doi: 10.5303/JKAS.2016.49.1.37

    work page doi:10.5303/jkas.2016.49.1.37 2016

  40. [40]

    2016, PASJ, 68, 55, doi: 10.1093/pasj/psw054

    Kimura, M., Isogai, K., Kato, T., et al. 2016, PASJ, 68, 55, doi: 10.1093/pasj/psw054

    work page doi:10.1093/pasj/psw054 2016

  41. [41]

    2021, PASJ, 73, 1, doi: 10.1093/pasj/psaa089

    Kimura, M., Isogai, K., Kato, T., et al. 2021, PASJ, 73, 1, doi: 10.1093/pasj/psaa089

    work page doi:10.1093/pasj/psaa089 2021

  42. [42]

    King, A. R. 1988, QJRAS, 29, 1

    1988

  43. [43]

    Monthly Notices of the Royal Astronomical Society 373, 1195–1202

    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

  44. [44]

    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

  45. [45]

    2026, PASJ, 78, 199, doi: 10.1093/pasj/psaf133

    Kojiguchi, N., Isogai, K., Tampo, Y., et al. 2026, PASJ, 78, 199, doi: 10.1093/pasj/psaf133

    work page doi:10.1093/pasj/psaf133 2026

  46. [46]

    R., & Wynn, G

    Kolb, U., & Baraffe, I. 1999, MNRAS, 309, 1034, doi: 10.1046/j.1365-8711.1999.02926.x

    work page doi:10.1046/j.1365-8711.1999.02926.x 1999

  47. [47]

    Kozhevnikov, V. P. 2015, NewA, 41, 59, doi: 10.1016/j.newast.2015.06.002

    work page doi:10.1016/j.newast.2015.06.002 2015

  48. [48]

    2024, Research in Astronomy and Astrophysics, 24, 085002, doi: 10.1088/1674-4527/ad59ec

    Krushevska, V., Shugarov, S., Ochner, P., et al. 2024, Research in Astronomy and Astrophysics, 24, 085002, doi: 10.1088/1674-4527/ad59ec

    work page doi:10.1088/1674-4527/ad59ec 2024

  49. [49]

    C., Moon, D.-S., et al

    Lee, Y., Kim, S. C., Moon, D.-S., et al. 2022, ApJL, 925, L22, doi: 10.3847/2041-8213/ac4c41

    work page doi:10.3847/2041-8213/ac4c41 2022

  50. [50]

    C., et al

    Lee, Y., Moon, D.-S., Kim, S. C., et al. 2019, ApJ, 880, 109, doi: 10.3847/1538-4357/ab2985

    work page doi:10.3847/1538-4357/ab2985 2019

  51. [51]

    C., Park, H

    Lee, Y., Moon, D.-S., Kim, S. C., Park, H. S., & Ni, Y. Q. 2024, ApJ, 964, 186, doi: 10.3847/1538-4357/ad25ff Linnell Nemec, A. F., & Nemec, J. M. 1985, AJ, 90, 2317, doi: 10.1086/113936

    work page doi:10.3847/1538-4357/ad25ff 2024

  52. [52]

    Monthly Notices of the Royal Astronomical Society 378, 245–275

    Littlefair, S. P., Dhillon, V. S., Marsh, T. R., et al. 2007, MNRAS, 381, 827, doi: 10.1111/j.1365-2966.2007.12285.x

    work page doi:10.1111/j.1365-2966.2007.12285.x 2007

  53. [53]

    2013, AJ, 145, 145, doi: 10.1088/0004-6256/145/6/145

    Littlefield, C., Garnavich, P., Applegate, A., et al. 2013, AJ, 145, 145, doi: 10.1088/0004-6256/145/6/145

    work page doi:10.1088/0004-6256/145/6/145 2013

  54. [54]

    Lomb, N. R. 1976, Ap&SS, 39, 447, doi: 10.1007/BF00648343

    work page doi:10.1007/bf00648343 1976

  55. [55]

    P., Parsons, S

    McAllister, M., Littlefair, S. P., Parsons, S. G., et al. 2019, MNRAS, 486, 5535, doi: 10.1093/mnras/stz976

    work page doi:10.1093/mnras/stz976 2019

  56. [56]

    C., Lee, J.-J., et al

    Moon, D.-S., Kim, S. C., Lee, J.-J., et al. 2016, in Proc. SPIE, Vol. 9906, Ground-based and Airborne Telescopes VI, 99064I, doi: 10.1117/12.2233921

    work page doi:10.1117/12.2233921 2016

  57. [57]

    Q., Drout, M

    Moon, D.-S., Ni, Y. Q., Drout, M. R., et al. 2021, ApJ, 910, 151, doi: 10.3847/1538-4357/abe466 Mu˜ noz-Giraldo, D., Stelzer, B., & Schwope, A. 2024, A&A, 687, A305, doi: 10.1051/0004-6361/202449358

    work page doi:10.3847/1538-4357/abe466 2021

  58. [58]

    2017, PASJ, 69, 2, doi: 10.1093/pasj/psw107

    Namekata, K., Isogai, K., Kato, T., et al. 2017, PASJ, 69, 2, doi: 10.1093/pasj/psw107

    work page doi:10.1093/pasj/psw107 2017

  59. [59]

    AM CVn stars

    Nelemans, G. 2005, in Astronomical Society of the Pacific Conference Series, Vol. 330, The Astrophysics of Cataclysmic Variables and Related Objects, ed. J. M. Hameury & J. P. Lasota, 27, doi: 10.48550/arXiv.astro-ph/0409676

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0409676 2005

  60. [60]

    V., & M¨ antynen, I

    Neustroev, V. V., & M¨ antynen, I. 2023, MNRAS, 523, 6114, doi: 10.1093/mnras/stad1730

    work page doi:10.1093/mnras/stad1730 2023

  61. [61]

    V., Marsh, T

    Neustroev, V. V., Marsh, T. R., Zharikov, S. V., et al. 2017, MNRAS, 467, 597, doi: 10.1093/mnras/stx084

    work page doi:10.1093/mnras/stx084 2017

  62. [62]

    Q., Moon, D.-S., Drout, M

    Ni, Y. Q., Moon, D.-S., Drout, M. R., et al. 2023a, ApJ, 959, 132, doi: 10.3847/1538-4357/ad0640

    work page doi:10.3847/1538-4357/ad0640

  63. [63]

    Q., Moon, D.-S., Drout, M

    Ni, Y. Q., Moon, D.-S., Drout, M. R., et al. 2022, Nature Astronomy, 6, 568, doi: 10.1038/s41550-022-01603-4

    work page doi:10.1038/s41550-022-01603-4 2022

  64. [64]

    Q., Moon, D.-S., Drout, M

    Ni, Y. Q., Moon, D.-S., Drout, M. R., et al. 2023b, ApJ, 946, 7, doi: 10.3847/1538-4357/aca9be

    work page doi:10.3847/1538-4357/aca9be

  65. [65]

    Q., Moon, D.-S., Drout, M

    Ni, Y. Q., Moon, D.-S., Drout, M. R., et al. 2025, ApJ, 983, 3, doi: 10.3847/1538-4357/adbbb7

    work page doi:10.3847/1538-4357/adbbb7 2025

  66. [66]

    2004, PASJ, 56, S163, doi: 10.1093/pasj/56.sp1.S163 O’Donoghue, D., Chen, A., Marang, F., et al

    Nogami, D., & Iijima, T. 2004, PASJ, 56, S163, doi: 10.1093/pasj/56.sp1.S163 O’Donoghue, D., Chen, A., Marang, F., et al. 1991, MNRAS, 250, 363, doi: 10.1093/mnras/250.2.363

    work page doi:10.1093/pasj/56.sp1.s163 2004

  67. [67]

    1995, PASJ, 47, 47, doi: 10.1093/pasj/47.1.47

    Osaki, Y. 1995, PASJ, 47, 47, doi: 10.1093/pasj/47.1.47

    work page doi:10.1093/pasj/47.1.47 1995

  68. [68]

    1996, PASP, 108, 39, doi: 10.1086/133689

    Osaki, Y. 1996, PASP, 108, 39, doi: 10.1086/133689

    work page doi:10.1086/133689 1996

  69. [69]

    2003, PASJ, 55, 841, doi: 10.1093/pasj/55.4.841

    Osaki, Y. 2003, PASJ, 55, 841, doi: 10.1093/pasj/55.4.841

    work page doi:10.1093/pasj/55.4.841 2003

  70. [70]

    2013a, PASJ, 65, 95, doi: 10.1093/pasj/65.5.95

    Osaki, Y., & Kato, T. 2013a, PASJ, 65, 95, doi: 10.1093/pasj/65.5.95

    work page doi:10.1093/pasj/65.5.95

  71. [71]

    2013b, PASJ, 65, 50, doi: 10.1093/pasj/65.3.50

    Osaki, Y., & Kato, T. 2013b, PASJ, 65, 50, doi: 10.1093/pasj/65.3.50

    work page doi:10.1093/pasj/65.3.50

  72. [72]

    2002, A&A, 383, 574, doi: 10.1051/0004-6361:20011744

    Osaki, Y., & Meyer, F. 2002, A&A, 383, 574, doi: 10.1051/0004-6361:20011744

    work page doi:10.1051/0004-6361:20011744 2002

  73. [73]

    2001, A&A, 370, 488, doi: 10.1051/0004-6361:20010234

    Osaki, Y., Meyer, F., & Meyer-Hofmeister, E. 2001, A&A, 370, 488, doi: 10.1051/0004-6361:20010234

    work page doi:10.1051/0004-6361:20010234 2001

  74. [74]

    2016, MNRAS, 460, 2526, doi: 10.1093/mnras/stw1120

    Otulakowska-Hypka, M., Olech, A., & Patterson, J. 2016, MNRAS, 460, 2526, doi: 10.1093/mnras/stw1120

    work page doi:10.1093/mnras/stw1120 2016

  75. [75]

    1981, ApJL, 248, L27, doi: 10.1086/183616

    Paczynski, B., & Sienkiewicz, R. 1981, ApJL, 248, L27, doi: 10.1086/183616

    work page doi:10.1086/183616 1981

  76. [76]

    F., Schmidtobreick, L., Tappert, C., G¨ ansicke, B

    Pala, A. F., Schmidtobreick, L., Tappert, C., G¨ ansicke, B. T., & Mehner, A. 2018, MNRAS, 481, 2523, doi: 10.1093/mnras/sty2434

    work page doi:10.1093/mnras/sty2434 2018

  77. [77]

    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

  78. [78]

    S., Moon, D.-S., Zaritsky, D., et al

    Park, H. S., Moon, D.-S., Zaritsky, D., et al. 2017, ApJ, 848, 19, doi: 10.3847/1538-4357/aa88ab

    work page doi:10.3847/1538-4357/aa88ab 2017

  79. [79]

    1998, PASP, 110, 1132, doi: 10.1086/316233

    Patterson, J. 1998, PASP, 110, 1132, doi: 10.1086/316233

    work page doi:10.1086/316233 1998

  80. [80]

    A., et al

    Patterson, J., Augusteijn, T., Harvey, D. A., et al. 1996, PASP, 108, 748, doi: 10.1086/133798

    work page doi:10.1086/133798 1996

Showing first 80 references.