Pith. sign in

REVIEW 4 major objections 6 minor 102 references

Optical Flares Detected on a Contact Binary: The First Photometric and Spectroscopic Analysis of a Long-period Low Mass Ratio Contact Binary HAT 307-0007476

T0 review · 4 major / 6 minor · reviewed 2026-08-10 · deepseek-v4-flash

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

Pith's one-line read A contact binary has been shown to host superflares and to remain dynamically stable, with its parameters measured for the first time.

desk verdict A solid first characterization of a long-period low-q contact binary; the superflare claim survives the distance-uncertainty stress test, and the remaining soft spots are minor. read the letter →

arxiv 2501.10613 v1 pith:PIELNTPR submitted 2025-01-18 astro-ph.SR

Ling-Zhi Li , Kai Li , Xiang Gao , Xiao-Dian Chen , Shuai Feng , Dong-Yang Gao , Di-Fu Guo , Xu Chen
show 5 more authors
Xing Gao Guo-You Sun Shahidin Yaqup Chunhai Bai Ali Esamdin
This is my paper · ORCID
classification astro-ph.SR
keywords contactbinarylowmassratiosuperflareorbitalperiodincreasechromosphericactivityWUMa-typetotaleclipseH-alphaemission
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper presents the first photometric and spectroscopic study of HAT 307-0007476, a contact binary with an orbital period of about 0.533 days. The authors argue that the system is a totally eclipsing, low-mass-ratio contact binary ($q \approx 0.114$) with a moderate fill-out factor, and that two optical flares detected in December 2022 reach superflare energies of roughly $3 \times 10^{36}$ erg and $7 \times 10^{35}$ erg. Using LAMOST spectra, they find excess H$\alpha$ emission indicating chromospheric activity, and the $O-C$ diagram shows a long-term period increase that they attribute to mass transfer. They conclude that the binary currently sits in a dynamically stable region according to both the spin-to-orbital angular momentum ratio and the instability parameters.

What carries the argument

The analysis rests on the Wilson-Devinney light-curve code applied to multi-band, multi-telescope photometry, whose q-search method pins the mass ratio because total eclipses with flat-bottom minima make the photometric $q$ reliable when no radial-velocity curve exists. The same models provide the fill-out factor, and the flaring analysis uses a photometric equivalent width integrated against the quiescent model light curve to get flare energies. Stability is judged by comparing $J_{\rm spin}/J_{\rm orb}$ with the one-third Darwin-instability threshold and by comparing current parameters with the instability mass ratio, separation, and period from the Wadhwa criterion.

What would settle it

A radial-velocity orbit that contradicts $q \approx 0.114$, or an independent distance estimate that lowers the system luminosity enough to push the flare energies below the roughly $10^{35}$ erg superflare threshold, would falsify the central claims.

Watch

Extended reading notes

Core claim

HAT 307-0007476 is established as a long-period, low-mass-ratio contact binary in a totally eclipsing configuration; its flat-bottom minima make the photometric mass ratio trustworthy despite the absence of radial velocities. The system shows two flare events in December 2022 with energies above $10^{35}$ erg, placing them at the superflare level, along with H$\alpha$ excess in LAMOST spectra. The $O-C$ diagram reveals a secular period increase of $dP/dt = 2.67(\pm 0.42)\times 10^{-8}$ d/yr, interpreted as mass transfer from the less massive to the more massive component. Stability arguments based on $J_{\rm spin}/J_{\rm orb}$ and on the instability parameters indicate that the binary is currently stable.

Load-bearing premise

The central results assume that the flat-bottom total eclipses make the photometric mass ratio equal to the true mass ratio, since no radial-velocity curve exists to check it.

Editorial extensions

If this is right

  • The system becomes a benchmark for long-period, low-mass-ratio contact binaries, one of the few with both a reliable photometric mass ratio and superflare detections.
  • The measured period increase, if real, constrains the mass-transfer rate and supports transfer from the less massive to the more massive component at about $3\times 10^{-9}\,M_\odot$ per year.
  • The detection of superflares on an A9/F0-type contact binary shows that flare activity is not confined to cool stars and can reach superflare energies in hotter systems.
  • The stability conclusion predicts that the binary will not merge in the near term, so it can be monitored for further flares and period changes.
  • The method chain (total-eclipse q-search plus Gaia distance plus photometric equivalent width) can be applied to other single-lined contact binaries without radial velocities.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the mass-ratio reliability from total eclipses holds generally, many single-lined contact binaries in survey data could have their parameters upgraded, expanding the sample for testing the low-mass-ratio cutoff.
  • The 4-day separation of the two flares and their occurrence at different orbital phases may hint at a persistent active longitude system on the primary; multi-epoch monitoring could test this.
  • The reported period increase could also be partially produced by a light-travel-time effect from a third body or by magnetic activity cycles; radial-velocity monitoring over a few years would discriminate.
  • Because the flare energies scale with the adopted extinction and distance, independent reddening estimates or a direct distance from the eclipsing-binary fit would tighten the superflare classification.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

4 major / 6 minor

Summary. The paper reports the first detailed photometric and spectroscopic study of the contact binary HAT 307-0007476. Multi-band light curves from NEXT, WHOT, XL, and PAT, together with TESS and archival survey photometry, are modeled with the Wilson-Devinney code to derive a low mass ratio q~0.114 and a medium contact factor f~37.1%. Two optical flare events in December 2022 are identified and characterized, with quoted energies of 2.8e36 and 6.8e35 erg, placing them in the superflare regime. LAMOST spectra are used to infer chromospheric activity via H-alpha excess emission. An O-C analysis of 273 eclipse timings yields a secular orbital period increase of dP/dt = 2.67e-8 d/yr, attributed to conservative mass transfer. Stability is assessed through Jspin/Jorb and Wadhwa et al. instability parameters, concluding the system is currently stable.

Significance. If the results hold, the paper adds a rare long-period, low-mass-ratio contact binary with detected superflares to a small sample, and it demonstrates the utility of combining small-telescope multiband photometry with TESS and archival data. The analysis benefits from consistent photometric solutions across several independent surveys, explicit rejection of two TESS artifacts, and a clear absolute-parameter chain from Gaia parallaxes. The main quantitative claims nevertheless depend on a photometric-only mass ratio and on a distance/extinction scale that is not independently cross-checked, so the quoted masses, luminosities, and flare energies carry systematic uncertainties that are not fully reflected in the reported errors.

major comments (4)
  1. [§2.1, Table 6] The paper adopts the literature definition of a flare as a brightening with peak amplitude not less than 0.03 mag, and further states that the detected humps are above at least four times the observational sigma. For Flare2 in the r' band, however, the quoted amplitude is 0.027 mag with an r' photometric error of about 0.007 mag from Table 1, which is below the 0.03 mag threshold and corresponds to only about 3.9 sigma. The authors should either justify retaining Flare2 as a confirmed multi-band flare despite this sub-threshold point, or revise the stated detection criteria.
  2. [§5.1, §5.3] The flare energies are computed as E_flare = L_star x EW with L_star derived from the Gaia DR3 distance D = 1601.6 ± 44.0 pc and an adopted extinction A_V = 0.462 from a single extinction map. No uncertainty is propagated into E_flare, and the quoted distance error is only the formal parallax error, not including extinction systematics or possible photocenter effects in a resolved-binary parallax. Because E scales as D^2 and 10^(0.4 A_V), realistic systematic errors of 20-40% in the absolute scale are plausible. The authors should provide an error budget for E_flare and explicitly state whether the 'superflare' classification is robust to those systematics; the large margin above 1e33 erg suggests it is, but the current presentation overstates the precision of the energies.
  3. [§5.3, Table 6] Table 6 lists per-band amplitudes and durations but only a single equivalent width (91 s for Flare1 and 22 s for Flare2) and a single energy per flare. The text does not explain how the per-band EW measurements are combined, nor whether multiplying a bandpass EW by the bolometric stellar luminosity is an adequate approximation for the flare spectral energy distribution. The authors should specify the band or bands used for the EW integral and discuss any color/bolometric correction applied, particularly since the amplitudes differ by a factor of about two among g', r', and i' for Flare2.
  4. [§4, Eq. (3), Table 5] The quadratic O-C fit that yields dP/dt = 2.67e-8 d/yr is based on 273 eclipse timings from very heterogeneous sources, with dense TESS coverage in 2021, sparse SuperWASP points from 2006-2011, and small numbers of ASAS-SN, ZTF, CSS, and ground-based minima. The paper itself labels the result as preliminary. The authors should demonstrate the robustness of the quadratic term, for example by showing the fit with early SuperWASP and late TESS subsets removed, and by reporting a weighted chi-square or equivalent goodness-of-fit statistic, before using the period increase to derive a mass-transfer rate in Eq. (4).
minor comments (6)
  1. [§5.4, Eq. (7)] Equation (7) contains a typo in the second term of the bracket: it should be q(k2 r2)^2, not q(k1 r1)^2. The numerical results appear to use the correct expression, but the equation as printed is misleading.
  2. [§3.2, Table 2] The H-alpha equivalent widths in Table 2 are quoted without uncertainties, and the statement that the first and fourth spectra show 'clear' emission while the middle two do not is not quantified. Given the low LAMOST resolution, the authors should provide at least approximate errors or a significance criterion for the excess emission.
  3. [§3.1, Table 3] The simultaneous solution gives q = 0.109 ± 0.001 while the adopted TESS solution gives q = 0.114 ± 0.001, and the survey solutions range from 0.096 to 0.110. The paper should clarify why the TESS value is chosen as final and whether the scatter among surveys is included in any systematic error estimate for the mass ratio.
  4. [§5.4] The linear relation k1 = 0.014M + 0.152 (M1 > 1.4 M_sun) is used without stating the units of M or the source range of validity; please specify that M is in solar masses and cite the relevant tabulated data from Landin et al. (2009).
  5. [§3.2] The text contains a broken cross-reference 'From Table??' when discussing the temperature differences between the template stars and the binary components; this should be corrected to refer to a specific table.
  6. [Abstract and §5.3] The abstract states the average duration of the two flares is about 2289 s, but Table 6 gives different durations per band; please clarify whether the quoted value is an average over bands and flares and quote the band-to-band spread.

Circularity Check

0 steps flagged · score 2.0 of 10

No circular derivation chain: the photometric mass ratio, flare energies, O-C period increase, and stability ratios are direct fits or explicit calculations from external inputs; the paper's self-citations are methodological and not load-bearing.

full rationale

Walking the derivation chain, each central quantity is either fitted directly or computed from stated equations with independent inputs. The mass ratio q~0.114 comes from a W-D q-search whose minimum is shown, with the total-eclipse reliability argument resting primarily on external statistical (Pribulla et al. 2003) and numerical (Terrell & Wilson 2005) studies; the same-group citation (Li et al. 2021) merely restates that conclusion and is not the load-bearing evidence. Flare energies use E = L* EW, where L* is the quiescent stellar luminosity from Section 5.1, fixed by Gaia DR3 parallax, GALEXTIN extinction, and the photometric solution fitted to flare-free light curves; the flare EW is measured from the residuals, so the superflare classification is not manufactured by the fit. The O-C period increase dP/dt = 2.67e-8 d/yr is a least-squares quadratic coefficient from 273 eclipse times, a fit rather than a prediction. The Jspin/Jorb and instability-parameter stability conclusion is a direct application of standard formulae (Yang & Qian 2015; Wadhwa et al. 2021) using the same solution. The self-citations (Li et al. 2019, 2020, 2021, 2024a) are methodological or contextual and are not used as the sole justification for any central claim, so there is no circular reduction. The distance/extinction sensitivity is a robustness caveat, not a circularity.

Assumptions & free parameters 7 free parameters · 7 assumptions · 0 invented entities

The central claims rest on standard contact-binary modeling assumptions (Roche geometry, total-eclipse reliability, W-D Mode 3) and on adopted literature values (gyration radii, template stars, extinction, distance). No new physical entities are introduced. The primary free parameters are the W-D photometric elements and the O-C quadratic coefficient.

free parameters (7)
  • Mass ratio q = 0.114 ± 0.001 (TESS solution)
    Fitted by q-search method minimizing mean residual of W-D light-curve fits to NEXT, WHOT, and TESS data.
  • Orbital inclination i = 76.3° ± 0.1°
    Fitted by W-D code in the simultaneous photometric solution.
  • Secondary effective temperature T2 = 6474 ± 6 K
    Fitted by W-D code; primary temperature fixed at 6845 K from the average of LAMOST values.
  • Surface potential Omega1=Omega2 = 1.973 ± 0.002
    Fitted by W-D code; determines the fill-out factor f=37.1%.
  • Primary relative luminosity L1/(L1+L2) in TESS band = 0.887 ± 0.001
    Fitted per band in the W-D solution; TESS-band value listed as representative.
  • Quadratic coefficient of O-C ephemeris = 1.95(±0.42) x 10^-11 d
    Least-squares fit to 273 eclipse times; yields dP/dt = 2.67(±0.42) x 10^-8 d/yr.
  • Gyration radii k1^2, k2^2 = 0.06 (both), later 0.205 for k2 and 0.014M+0.152 for k1
    Adopted from Li & Zhang (2006), Arbutina (2007), and Landin et al. (2009); chosen values, not fitted, but they directly affect the Jspin/Jorb stability estimate.
assumptions (7)
  • domain assumption The system is a totally eclipsing contact binary with flat-bottom minima, so the photometric mass ratio equals the spectroscopic value.
    Section 3.1 relies on Pribulla et al. (2003) and Terrell & Wilson (2005) statistical results; no radial-velocity curve is available to check this directly.
  • domain assumption Both components fill their Roche lobes and the W-D Mode 3 over-contact model applies.
    Section 3.1: the Wilson-Devinney model assumes a contact configuration with both components filling their Roche lobes.
  • domain assumption Gravity darkening and albedo coefficients g1=g2=0.32 and A1=A2=0.5 are appropriate for this system.
    Section 3.1: these values are adopted from von Zeipel (1924) and standard practice; the primary is A9/F0, for which a convective-envelope gravity darkening exponent may be questionable, but this is a common modeling choice.
  • domain assumption The template stars TYC 3128-1088-1 and TYC 1877-1578-1 are inactive and their composite spectrum represents the binary photosphere.
    Section 3.2: spectral subtraction assumes the templates have no activity and match the components' parameters; the text contains a 'Table??' placeholder for the temperature comparison.
  • domain assumption The Gaia DR3 distance and GALEXTIN extinction are correct.
    Section 5.1: absolute parameters and flare energies scale with distance D=1601.6±44.0 pc and AV=0.462, so errors in these external inputs propagate into masses, radii, and flare energies.
  • domain assumption The upward O-C parabola is caused solely by conservative mass transfer from the less massive to the more massive star.
    Section 5.2: Eq. 4 (Kwee 1958) converts dP/dt to dM1/dt; alternative mechanisms (e.g., Applegate, magnetic braking) are not considered.
  • standard math Kepler's third law and blackbody emission are valid for deriving absolute parameters.
    Section 5.1: uses L = 4πσT^4(ar)^2 and M1 + M2 = 0.0134 a^3 / P^2.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Optical Flares Detected on a Contact Binary: The First Photometric and Spectroscopic Analysis of a Long-period Low Mass Ratio Contact Binary HAT 307-0007476." pith.science (2026). https://pith.science/paper/PIELNTPR

@misc{pith2026250110613,
  author       = {Pith},
  title        = {Pith review of: Optical Flares Detected on a Contact Binary: The First Photometric and Spectroscopic Analysis of a Long-period Low Mass Ratio Contact Binary HAT 307-0007476},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/PIELNTPR}},
  note         = {Machine review of arXiv:2501.10613}
}
abstract

This paper presents the photometric and spectroscopic analysis of a long-period totally eclipsing contact binary (HAT 307-0007476) for the first time. This system is a low mass ratio ($q\sim0.114$) and medium contact binary ($f\sim37.1\%$). Two flare events were detected in multiple bands observations in December 2022. The interval between the two flare events is 4 days. The average duration of these two flares is about 2289s. Both the two flares achieve the energy levels of superflares. The excess emission of the H$_\alpha$ line in the LAMOST spectra of this object was analyzed, indicating its chromospheric activity. The $O-C$ diagram showed a long-term orbital period increase, which is due to the mass transfer between the two component stars. We conclude that HAT 307-0007476 is currently in a stable region based on both $J_{spin}/J_{orb}$ and the comparison between the instability parameters and its current values.

Figures

Figures reproduced from arXiv: 2501.10613 by the authors.

Figure 1
Figure 1. Light curves with flares of HAT 307-0007476 on 2022 December 21 (top left), and 25 (top right). The yellow arrows indicate the flare events. All the CCD images were reduced by IRAF1 . The data reduction includes bias and flat corrections, aperture photometry for the target, the comparison and check stars. The differential photometry method was adopted to obtain the light curves. The target’s right ascension is 03ℎ23… view at source ↗
Figure 2
Figure 2. The left panel shows the photometric aperture pixels (the rectangular box) selected using lightkurve, and the right panel shows the selected background skylight pixels (the rectangular box) [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. The raw complete light curves extracted from the FFI of Sectors 42 and the zoomed-in view of two fake flare events. to extract light curves, incorporating the background subtraction process. Finally, the light curve was de-trended by applying a polynomial fit, and then we normalized the flux. The light curves obtained are in a 10-minute cadence. In the raw light curve extracted from the FFI of Sector-42 (see [PITH_… view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: The final adopted light curves extracted from the FFI of Sector-42, 43 and 44. the first panel of [PITH_FULL_IMAGE:figures/full_fig_p005_4.png]
Figure 5
Figure 5. Figure 5: The relationship between mean residual and the mass ratio q. The small diagram in the figure is a zoomed-in view near the optimal solution [PITH_FULL_IMAGE:figures/full_fig_p007_5.png]
Figure 6
Figure 6. Figure 6: The theoretical light curves (continuous lines) with simultaneous solution and observed light curves from WHOT, NEXT, and TESS. MNRAS 000, 1–17 (2025) [PITH_FULL_IMAGE:figures/full_fig_p007_6.png]
Figure 7
Figure 7. Figure 7: Theoretical light curves and observed curves with flare activities for HAT 307-0007476. The solid line indicates the best-fit light curve [PITH_FULL_IMAGE:figures/full_fig_p008_7.png]
Figure 8
Figure 8. Figure 8: Theoretical light curves and observed light curves of HAT 307-0007476. 3.2 Spectroscopic investigation Contact binaries often exhibit magnetic activity such as spots, flares, or plages, which are related to chromosphere activity. Excess emission from the H𝛼 line is one…
Figure 9
Figure 9. Figure 9: The H𝛼 region of low-resolution LAMOST spectra (black line) and synthetic spectra (yellow line) for the HAT 307-0007476 is shown. The continuous blue line in each plot shows the subtracted spectra in the same region. 4 ORBITAL PERIOD INVESTIGATIONS The study of orbital…
Figure 10
Figure 10. Figure 10: The O-C diagram of HAT 307-0007476. The values of O-C are shown at the top of the figure, and the residuals are shown at the bottom of the figure. (𝐵𝐽𝐷)𝑀𝑖𝑛.𝐼 =2459935.15486(±0.00015) + 0.5329393(±0.0000001) × 𝐸. (2) Then the corresponding epoch and O–C values were cal…
Figure 11
Figure 11. Figure 11: Relationships between flare energy and duration (left) or amplitude (right). The red triangles represent flares from this work. The brown dots represent flares from Y23 and the solid lines are linear fits from Y23 [PITH_FULL_IMAGE:figures/full_fig_p014_11.png]

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

102 extracted references · 25 canonical work pages

  1. [1]

    B., et al., 2021, @doi [ ] 10.1093/mnras/stab2248 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.508.1788A 508, 1788

    Am \^o res E. B., et al., 2021, @doi [ ] 10.1093/mnras/stab2248 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.508.1788A 508, 1788

    doi:10.1093/mnras/stab2248 2021

  2. [2]

    Arbutina B., 2007, @doi [ ] 10.1111/j.1365-2966.2007.11723.x , https://ui.adsabs.harvard.edu/abs/2007MNRAS.377.1635A 377, 1635

    arXiv 2007

  3. [3]

    Arbutina B., 2009, @doi [ ] 10.1111/j.1365-2966.2008.14332.x , https://ui.adsabs.harvard.edu/abs/2009MNRAS.394..501A 394, 501

    arXiv 2009

  4. [4]

    C., 1985, @doi [ ] 10.1086/163361 , https://ui.adsabs.harvard.edu/abs/1985ApJ...295..162B 295, 162

    Barden S. C., 1985, @doi [ ] 10.1086/163361 , https://ui.adsabs.harvard.edu/abs/1985ApJ...295..162B 295, 162

    doi:10.1086/163361 1985

  5. [5]

    C., et al., 2019, @doi [ ] 10.1088/1538-3873/aaecbe , https://ui.adsabs.harvard.edu/abs/2019PASP..131a8002B 131, 018002

    Bellm E. C., et al., 2019, @doi [ ] 10.1088/1538-3873/aaecbe , https://ui.adsabs.harvard.edu/abs/2019PASP..131a8002B 131, 018002

    doi:10.1088/1538-3873/aaecbe 2019

  6. [6]

    O., G \"u del M., 2010, @doi [ ] 10.1146/annurev-astro-082708-101757 , https://ui.adsabs.harvard.edu/abs/2010ARA&A..48..241B 48, 241

    Benz A. O., G \"u del M., 2010, @doi [ ] 10.1146/annurev-astro-082708-101757 , https://ui.adsabs.harvard.edu/abs/2010ARA&A..48..241B 48, 241

    doi:10.1146/annurev-astro-082708-101757 2010

  7. [7]

    Boro Saikia S., et al., 2018, @doi [ ] 10.1051/0004-6361/201629518 , https://ui.adsabs.harvard.edu/abs/2018A&A...616A.108B 616, A108

    doi:10.1051/0004-6361/201629518 2018

  8. [8]

    E., Phillip C., Fleming S

    Brasseur C. E., Phillip C., Fleming S. W., Mullally S. E., White R. L., 2019, Astrocut: Tools for creating cutouts of TESS images , Astrophysics Source Code Library, record ascl:1905.007 ( @eprint ascl 1905.007 )

    2019

Show all 102 references
  1. [9]

    W., et al., 2010, @doi [ ] 10.1051/0004-6361/201015655 , https://ui.adsabs.harvard.edu/abs/2010A&A...520L..10B 520, L10

    Butters O. W., et al., 2010, @doi [ ] 10.1051/0004-6361/201015655 , https://ui.adsabs.harvard.edu/abs/2010A&A...520L..10B 520, L10

    2010 doi

  2. [10]

    Candelaresi S., Hillier A., Maehara H., Brandenburg A., Shibata K., 2014, @doi [ ] 10.1088/0004-637X/792/1/67 , https://ui.adsabs.harvard.edu/abs/2014ApJ...792...67C 792, 67

    2014 doi

  3. [11]

    R., Samec R

    Caton D., Gentry D. R., Samec R. G., Chamberlain H., Robb R., Faulkner D. R., Hill R., 2019, @doi [ ] 10.1088/1538-3873/aafb8f , https://ui.adsabs.harvard.edu/abs/2019PASP..131e4203C 131, 054203

    2019 doi

  4. [12]

    W., Byun Y

    Chang S. W., Byun Y. I., Hartman J. D., 2015, @doi [ ] 10.1088/0004-637X/814/1/35 , https://ui.adsabs.harvard.edu/abs/2015ApJ...814...35C 814, 35

    2015 doi

  5. [13]

    Y., et al., 2017, @doi [ ] 10.3847/1538-4357/834/1/92 , https://ui.adsabs.harvard.edu/abs/2017ApJ...834...92C 834, 92

    Chang H. Y., et al., 2017, @doi [ ] 10.3847/1538-4357/834/1/92 , https://ui.adsabs.harvard.edu/abs/2017ApJ...834...92C 834, 92

    2017 doi

  6. [14]

    Y., Lin C

    Chang H. Y., Lin C. L., Ip W. H., Huang L. C., Hou W. C., Yu P. C., Song Y. H., Luo A., 2018, @doi [ ] 10.3847/1538-4357/aae2bc , https://ui.adsabs.harvard.edu/abs/2018ApJ...867...78C 867, 78

    2018 doi

  7. [15]

    Chen X., et al., 2016, @doi [ ] 10.3847/0004-6256/152/5/129 , https://ui.adsabs.harvard.edu/abs/2016AJ....152..129C 152, 129

    2016 doi

  8. [16]

    Colina L., Bohlin R., 1997, @doi [ ] 10.1086/118332 , https://ui.adsabs.harvard.edu/abs/1997AJ....113.1138C 113, 1138

    1997 doi

  9. [17]

    Cui X.-Q., et al., 2012, @doi [Research in Astronomy and Astrophysics] 10.1088/1674-4527/12/9/003 , https://ui.adsabs.harvard.edu/abs/2012RAA....12.1197C 12, 1197

    2012 doi

  10. [18]

    H., 1893, The Observatory, https://ui.adsabs.harvard.edu/abs/1893Obs....16..172D 16, 172

    Darwin G. H., 1893, The Observatory, https://ui.adsabs.harvard.edu/abs/1893Obs....16..172D 16, 172

  11. [19]

    J., et al., 2009, @doi [ ] 10.1088/0004-637X/696/1/870 , https://ui.adsabs.harvard.edu/abs/2009ApJ...696..870D 696, 870

    Drake A. J., et al., 2009, @doi [ ] 10.1088/0004-637X/696/1/870 , https://ui.adsabs.harvard.edu/abs/2009ApJ...696..870D 696, 870

    2009 doi

  12. [20]

    J., et al., 2014, @doi [ ] 10.1088/0067-0049/213/1/9 , https://ui.adsabs.harvard.edu/abs/2014ApJS..213....9D 213, 9

    Drake A. J., et al., 2014, @doi [ ] 10.1088/0067-0049/213/1/9 , https://ui.adsabs.harvard.edu/abs/2014ApJS..213....9D 213, 9

    2014 doi

  13. [21]

    arXiv:2208.00211

    Gaia Collaboration et al., 2022, @doi [arXiv e-prints] 10.48550/arXiv.2208.00211 , https://ui.adsabs.harvard.edu/abs/2022arXiv220800211G p. arXiv:2208.00211

    2022 doi arXiv

  14. [22]

    Gao Q., Xin Y., Liu J.-F., Zhang X.-B., Gao S., 2016, @doi [ ] 10.3847/0067-0049/224/2/37 , https://ui.adsabs.harvard.edu/abs/2016ApJS..224...37G 224, 37

    2016 doi

  15. [23]

    J., Geske M

    Gettel S. J., Geske M. T., McKay T. A., 2006, @doi [ ] 10.1086/498016 , https://ui.adsabs.harvard.edu/abs/2006AJ....131..621G 131, 621

    2006 doi

  16. [24]

    M., Schlafly E., Zucker C., Speagle J

    Green G. M., Schlafly E., Zucker C., Speagle J. S., Finkbeiner D., 2019, @doi [ ] 10.3847/1538-4357/ab5362 , https://ui.adsabs.harvard.edu/abs/2019ApJ...887...93G 887, 93

    2019 doi

  17. [25]

    Guo D.-F., et al., 2022, @doi [ ] 10.1093/mnras/stac2811 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.517.1928G 517, 1928

    2022 doi

  18. [27]

    L., Davenport J

    Hawley S. L., Davenport J. R. A., Kowalski A. F., Wisniewski J. P., Hebb L., Deitrick R., Hilton E. J., 2014, @doi [ ] 10.1088/0004-637X/797/2/121 , https://ui.adsabs.harvard.edu/abs/2014ApJ...797..121H 797, 121

    2014 doi

  19. [28]

    Hu S.-M., Han S.-H., Guo D.-F., Du J.-J., 2014, @doi [Research in Astronomy and Astrophysics] 10.1088/1674-4527/14/6/010 , https://ui.adsabs.harvard.edu/abs/2014RAA....14..719H 14, 719

    2014 doi

  20. [29]

    W., Chen B

    Huang Y., Liu X. W., Chen B. Q., Zhang H. W., Yuan H. B., Xiang M. S., Wang C., Tian Z. J., 2018, @doi [ ] 10.3847/1538-3881/aacda5 , https://ui.adsabs.harvard.edu/abs/2018AJ....156...90H 156, 90

    2018 doi

  21. [30]

    Hut P., 1980, , https://ui.adsabs.harvard.edu/abs/1980A&A....92..167H 92, 167

    1980

  22. [31]

    Jayasinghe T., et al., 2018, @doi [ ] 10.1093/mnras/sty838 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.477.3145J 477, 3145

    2018 doi

  23. [32]

    Jayasinghe T., et al., 2019, @doi [ ] 10.1093/mnras/stz844 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.486.1907J 486, 1907

    2019 doi

  24. [33]

    Jiang D., Han Z., Wang J., Jiang T., Li L., 2010, @doi [ ] 10.1111/j.1365-2966.2010.16615.x , https://ui.adsabs.harvard.edu/abs/2010MNRAS.405.2485J 405, 2485

    2010

  25. [34]

    G., Handler G., De Cat P., 2024, @doi [ ] 10.1093/mnras/stad3467 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.527.4076K 527, 4076

    Kahraman Ali c avu s F., Ali c avu s F., C oban C . G., Handler G., De Cat P., 2024, @doi [ ] 10.1093/mnras/stad3467 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.527.4076K 527, 4076

    2024 doi

  26. [35]

    A., Molnar L

    Kobulnicky H. A., Molnar L. A., Cook E. M., Henderson L. E., 2022, @doi [ ] 10.3847/1538-4365/ac75bd , https://ui.adsabs.harvard.edu/abs/2022ApJS..262...12K 262, 12

    2022 doi

  27. [36]

    S., et al., 2017, @doi [ ] 10.1088/1538-3873/aa80d9 , https://ui.adsabs.harvard.edu/abs/2017PASP..129j4502K 129, 104502

    Kochanek C. S., et al., 2017, @doi [ ] 10.1088/1538-3873/aa80d9 , https://ui.adsabs.harvard.edu/abs/2017PASP..129j4502K 129, 104502

    2017 doi

  28. [37]

    F., Hawley S

    Kowalski A. F., Hawley S. L., Holtzman J. A., Wisniewski J. P., Hilton E. J., 2010, @doi [ ] 10.1088/2041-8205/714/1/L98 , https://ui.adsabs.harvard.edu/abs/2010ApJ...714L..98K 714, L98

    2010 doi

  29. [38]

    K., 1958, , https://ui.adsabs.harvard.edu/abs/1958BAN....14..131K 14, 131

    Kwee K. K., 1958, , https://ui.adsabs.harvard.edu/abs/1958BAN....14..131K 14, 131

    1958

  30. [39]

    K., van Woerden H., 1956, , https://ui.adsabs.harvard.edu/abs/1956BAN....12..327K 12, 327

    Kwee K. K., van Woerden H., 1956, , https://ui.adsabs.harvard.edu/abs/1956BAN....12..327K 12, 327

    1956

  31. [40]

    R., Mendes L

    Landin N. R., Mendes L. T. S., Vaz L. P. R., 2009, @doi [ ] 10.1051/0004-6361:20078403 , https://ui.adsabs.harvard.edu/abs/2009A&A...494..209L 494, 209

    2009 doi

  32. [41]

    C., et al., 2023, @doi [ ] 10.1051/0004-6361/202244156 , https://ui.adsabs.harvard.edu/abs/2023A&A...674A..30L 674, A30

    Lanzafame A. C., et al., 2023, @doi [ ] 10.1051/0004-6361/202244156 , https://ui.adsabs.harvard.edu/abs/2023A&A...674A..30L 674, A30

    2023 doi

  33. [42]

    Li L., Zhang F., 2006, @doi [ ] 10.1111/j.1365-2966.2006.10462.x , https://ui.adsabs.harvard.edu/abs/2006MNRAS.369.2001L 369, 2001

    2006

  34. [43]

    Q., Hu S

    Li K., Xia Q. Q., Hu S. M., Guo D. F., Chen X., 2018, @doi [ ] 10.1088/1538-3873/aac067 , https://ui.adsabs.harvard.edu/abs/2018PASP..130g4201L 130, 074201

    2018 doi

  35. [44]

    Li K., et al., 2019, @doi [Research in Astronomy and Astrophysics] 10.1088/1674-4527/19/10/147 , https://ui.adsabs.harvard.edu/abs/2019RAA....19..147L 19, 147

    2019 doi

  36. [45]

    Li K., Kim C.-H., Xia Q.-Q., Michel R., Hu S.-M., Gao X., Guo D.-F., Chen X., 2020, @doi [ ] 10.3847/1538-3881/ab7cda , https://ui.adsabs.harvard.edu/abs/2020AJ....159..189L 159, 189

    2020 doi

  37. [46]

    Li K., et al., 2021, @doi [ ] 10.3847/1538-3881/abfc53 , https://ui.adsabs.harvard.edu/abs/2021AJ....162...13L 162, 13

    2021 doi

  38. [47]

    Li K., Gao X., Liu X.-Y., Gao X., Li L.-Z., Chen X., Sun G.-Y., 2022, @doi [ ] 10.3847/1538-3881/ac8ff2 , https://ui.adsabs.harvard.edu/abs/2022AJ....164..202L 164, 202

    2022 doi

  39. [48]

    Li L.-Z., Li K., Gao X., Chen X.-D., Gao X., Sun G.-Y., 2024a, @doi [ ] 10.1093/mnras/stad3251 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.527.3982L 527, 3982

    doi

  40. [49]

    Li K., et al., 2024b, @doi [ ] 10.1051/0004-6361/202451947 , https://ui.adsabs.harvard.edu/abs/2024A&A...692L...4L 692, L4

    doi

  41. [50]

    L., Ip W

    Lin C. L., Ip W. H., Hou W. C., Huang L. C., Chang H. Y., 2019, @doi [ ] 10.3847/1538-4357/ab041c , https://ui.adsabs.harvard.edu/abs/2019ApJ...873...97L 873, 97

    2019 doi

  42. [51]

    Liu X.-Y., et al., 2023, @doi [ ] 10.1093/mnras/stad026 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.519.5760L 519, 5760

    2023 doi

  43. [52]

    F., L \'o pez-Garc \' a M

    L \'o pez-Santiago J., Albacete Colombo J. F., L \'o pez-Garc \' a M. A., 2010, @doi [ ] 10.1051/0004-6361/201015306 , https://ui.adsabs.harvard.edu/abs/2010A&A...524A..97L 524, A97

    2010 doi

  44. [53]

    L., et al., 2015, @doi [Research in Astronomy and Astrophysics] 10.1088/1674-4527/15/8/002 , https://ui.adsabs.harvard.edu/abs/2015RAA....15.1095L 15, 1095

    Luo A. L., et al., 2015, @doi [Research in Astronomy and Astrophysics] 10.1088/1674-4527/15/8/002 , https://ui.adsabs.harvard.edu/abs/2015RAA....15.1095L 15, 1095

    2015 doi

  45. [54]

    Maehara H., et al., 2012, @doi [ ] 10.1038/nature11063 , https://ui.adsabs.harvard.edu/abs/2012Natur.485..478M 485, 478

    2012 doi

  46. [55]

    J., et al., 2019, @doi [ ] 10.1088/1538-3873/aae8ac , https://ui.adsabs.harvard.edu/abs/2019PASP..131a8003M 131, 018003

    Masci F. J., et al., 2019, @doi [ ] 10.1088/1538-3873/aae8ac , https://ui.adsabs.harvard.edu/abs/2019PASP..131a8003M 131, 018003

    2019 doi

  47. [56]

    A., Blain M

    Molnar L. A., Blain M. G., Cook E. M., Whitten S. M., Kobulnicky H., 2019, in American Astronomical Society Meeting Abstracts \#233. p. 448.05

    2019

  48. [57]

    F., Le G

    Molnar L., Avery A., Blain M., Henderson L., Lau J. F., Le G. M., 2022, in American Astronomical Society Meeting \#240. p. 308.01

    2022

  49. [58]

    J., De Castro E., Cornide M., Latorre A., Sanz-Forcada J., 2000, @doi [ ] 10.1051/aas:2000359 , https://ui.adsabs.harvard.edu/abs/2000A&AS..146..103M 146, 103

    Montes D., Fern \'a ndez-Figueroa M. J., De Castro E., Cornide M., Latorre A., Sanz-Forcada J., 2000, @doi [ ] 10.1051/aas:2000359 , https://ui.adsabs.harvard.edu/abs/2000A&AS..146..103M 146, 103

    2000 doi

  50. [59]

    G., Hoffmann M., Duerbeck H

    Niarchos P. G., Hoffmann M., Duerbeck H. W., 1997, @doi [ ] 10.1051/aas:1997193 , https://ui.adsabs.harvard.edu/abs/1997A&AS..124..291N 124, 291

    1997 doi

  51. [60]

    W., Hartmann L

    Noyes R. W., Hartmann L. W., Baliunas S. L., Duncan D. K., Vaughan A. H., 1984, @doi [ ] 10.1086/161945 , https://ui.adsabs.harvard.edu/abs/1984ApJ...279..763N 279, 763

    1984 doi

  52. [61]

    J., Stassun K

    Oelkers R. J., Stassun K. G., 2018, @doi [ ] 10.3847/1538-3881/aad68e , https://ui.adsabs.harvard.edu/abs/2018AJ....156..132O 156, 132

    2018 doi

  53. [62]

    \"O zdemir S., Mayer P., Drechsel H., Demircan O., Ak H., 2003, @doi [ ] 10.1051/0004-6361:20030392 , https://ui.adsabs.harvard.edu/abs/2003A&A...403..675O 403, 675

    2003 doi

  54. [63]

    C., De Cat P., Tiwari S

    Panchal A., Joshi Y. C., De Cat P., Tiwari S. N., 2022, @doi [ ] 10.3847/1538-4357/ac45fb , https://ui.adsabs.harvard.edu/abs/2022ApJ...927...12P 927, 12

    2022 doi

  55. [64]

    C., Singh K

    Pandey J. C., Singh K. P., 2012, @doi [ ] 10.1111/j.1365-2966.2011.19776.x , https://ui.adsabs.harvard.edu/abs/2012MNRAS.419.1219P 419, 1219

    2012

  56. [65]

    Parimucha S ., Dubovsk \'y P., Va n ko M., C okina M., 2016, @doi [ ] 10.1007/s10509-016-2892-z , https://ui.adsabs.harvard.edu/abs/2016Ap&SS.361..302P 361, 302

    2016 doi

  57. [66]

    V., Evans A., Banerjee D

    Pavlenko Y. V., Evans A., Banerjee D. P. K., Southworth J., Shahbandeh M., Davis S., 2018, @doi [ ] 10.1051/0004-6361/201832717 , https://ui.adsabs.harvard.edu/abs/2018A&A...615A.120P 615, A120

    2018 doi

  58. [67]

    Pavlovski K., Southworth J., Tkachenko A., Van Reeth T., Tamajo E., 2023, @doi [ ] 10.1051/0004-6361/202244980 , https://ui.adsabs.harvard.edu/abs/2023A&A...671A.139P 671, A139

    2023 doi

  59. [68]

    J., Mamajek E

    Pecaut M. J., Mamajek E. E., 2013, @doi [ ] 10.1088/0067-0049/208/1/9 , https://ui.adsabs.harvard.edu/abs/2013ApJS..208....9P 208, 9

    2013 doi

  60. [69]

    L., et al., 2006, @doi [ ] 10.1086/508556 , https://ui.adsabs.harvard.edu/abs/2006PASP..118.1407P 118, 1407

    Pollacco D. L., et al., 2006, @doi [ ] 10.1086/508556 , https://ui.adsabs.harvard.edu/abs/2006PASP..118.1407P 118, 1407

    2006 doi

  61. [70]

    M., Tremko J., 2003, Contributions of the Astronomical Observatory Skalnate Pleso, https://ui.adsabs.harvard.edu/abs/2003CoSka..33...38P 33, 38

    Pribulla T., Kreiner J. M., Tremko J., 2003, Contributions of the Astronomical Observatory Skalnate Pleso, https://ui.adsabs.harvard.edu/abs/2003CoSka..33...38P 33, 38

    2003

  62. [71]

    B., Yang Y

    Qian S. B., Yang Y. G., Soonthornthum B., Zhu L. Y., He J. J., Yuan J. Z., 2005, @doi [ ] 10.1086/430673 , https://ui.adsabs.harvard.edu/abs/2005AJ....130..224Q 130, 224

    2005 doi

  63. [72]

    B., et al., 2014, @doi [ ] 10.1088/0067-0049/212/1/4 , https://ui.adsabs.harvard.edu/abs/2014ApJS..212....4Q 212, 4

    Qian S. B., et al., 2014, @doi [ ] 10.1088/0067-0049/212/1/4 , https://ui.adsabs.harvard.edu/abs/2014ApJS..212....4Q 212, 4

    2014 doi

  64. [73]

    W., Shapley H., 1948, Harvard College Observatory Announcement Card, https://ui.adsabs.harvard.edu/abs/1948HarAC.960....2R 960, 2

    Recht A. W., Shapley H., 1948, Harvard College Observatory Announcement Card, https://ui.adsabs.harvard.edu/abs/1948HarAC.960....2R 960, 2

    1948

  65. [74]

    R., et al., 2014, in Oschmann Jacobus M

    Ricker G. R., et al., 2014, in Oschmann Jacobus M. J., Clampin M., Fazio G. G., MacEwen H. A., eds, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series Vol. 9143, Space Telescopes and Instrumentation 2014: Optical, Infrared, and Millimeter Wave. p. 9143...

    2014 arXiv

  66. [75]

    R., et al., 2015, @doi [Journal of Astronomical Telescopes, Instruments, and Systems] 10.1117/1.JATIS.1.1.014003 , https://ui.adsabs.harvard.edu/abs/2015JATIS...1a4003R 1, 014003

    Ricker G. R., et al., 2015, @doi [Journal of Astronomical Telescopes, Instruments, and Systems] 10.1117/1.JATIS.1.1.014003 , https://ui.adsabs.harvard.edu/abs/2015JATIS...1a4003R 1, 014003

    2015 doi

  67. [76]

    E., 1989, @doi [ ] 10.1086/167162 , https://ui.adsabs.harvard.edu/abs/1989ApJ...337..927S 337, 927

    Schaefer B. E., 1989, @doi [ ] 10.1086/167162 , https://ui.adsabs.harvard.edu/abs/1989ApJ...337..927S 337, 927

    1989 doi

  68. [77]

    E., King J

    Schaefer B. E., King J. R., Deliyannis C. P., 2000, @doi [ ] 10.1086/308325 , https://ui.adsabs.harvard.edu/abs/2000ApJ...529.1026S 529, 1026

    2000 doi

  69. [78]

    J., et al., 2014, @doi [ ] 10.1088/0004-637X/788/1/48 , https://ui.adsabs.harvard.edu/abs/2014ApJ...788...48S 788, 48

    Shappee B. J., et al., 2014, @doi [ ] 10.1088/0004-637X/788/1/48 , https://ui.adsabs.harvard.edu/abs/2014ApJ...788...48S 788, 48

    2014 doi

  70. [79]

    Shibata K., Yokoyama T., 2002, @doi [ ] 10.1086/342141 , https://ui.adsabs.harvard.edu/abs/2002ApJ...577..422S 577, 422

    2002 doi

  71. [80]

    Shibayama T., et al., 2013, @doi [ ] 10.1088/0067-0049/209/1/5 , https://ui.adsabs.harvard.edu/abs/2013ApJS..209....5S 209, 5

    2013 doi

  72. [81]

    Southworth J., 2020, @doi [The Observatory] 10.48550/arXiv.2012.05559 , https://ui.adsabs.harvard.edu/abs/2020Obs...140..247S 140, 247

    2020 doi arXiv

  73. [82]

    Sun W., Chen X., Deng L., de Grijs R., 2020, @doi [ ] 10.3847/1538-4365/ab7894 , https://ui.adsabs.harvard.edu/abs/2020ApJS..247...50S 247, 50

    2020 doi

  74. [83]

    E., 2005, @doi [ ] 10.1007/s10509-005-4449-4 , https://ui.adsabs.harvard.edu/abs/2005Ap&SS.296..221T 296, 221

    Terrell D., Wilson R. E., 2005, @doi [ ] 10.1007/s10509-005-4449-4 , https://ui.adsabs.harvard.edu/abs/2005Ap&SS.296..221T 296, 221

    2005 doi

  75. [84]

    Torres G., 2010, @doi [ ] 10.1088/0004-6256/140/5/1158 , https://ui.adsabs.harvard.edu/abs/2010AJ....140.1158T 140, 1158

    2010 doi

  76. [85]

    Ueda T., Flock M., Okuzumi S., 2019, @doi [ ] 10.3847/1538-4357/aaf3a1 , https://ui.adsabs.harvard.edu/abs/2019ApJ...871...10U 871, 10

    2019 doi

  77. [86]

    Vilhu O., Caillault J.-P., Heise J., 1988, @doi [ ] 10.1086/166522 , https://ui.adsabs.harvard.edu/abs/1988ApJ...330..922V 330, 922

    1988 doi

  78. [87]

    S., De Horta A., Filipovi \'c M

    Wadhwa S. S., De Horta A., Filipovi \'c M. D., Tothill N. F. H., Arbutina B., Petrovi \'c J., Djura s evi \'c G., 2021, @doi [ ] 10.1093/mnras/staa3637 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.501..229W 501, 229

    2021 doi

  79. [88]

    M., et al., 2011, @doi [ ] 10.1088/0004-6256/141/2/50 , https://ui.adsabs.harvard.edu/abs/2011AJ....141...50W 141, 50

    Walkowicz L. M., et al., 2011, @doi [ ] 10.1088/0004-6256/141/2/50 , https://ui.adsabs.harvard.edu/abs/2011AJ....141...50W 141, 50

    2011 doi

  80. [89]

    E., 1979, @doi [ ] 10.1086/157588 , https://ui.adsabs.harvard.edu/abs/1979ApJ...234.1054W 234, 1054

    Wilson R. E., 1979, @doi [ ] 10.1086/157588 , https://ui.adsabs.harvard.edu/abs/1979ApJ...234.1054W 234, 1054

    1979 doi

  81. [90]

    E., 1990, @doi [ ] 10.1086/168867 , https://ui.adsabs.harvard.edu/abs/1990ApJ...356..613W 356, 613

    Wilson R. E., 1990, @doi [ ] 10.1086/168867 , https://ui.adsabs.harvard.edu/abs/1990ApJ...356..613W 356, 613

    1990 doi

  82. [91]

    E., Devinney E

    Wilson R. E., Devinney E. J., 1971, @doi [ ] 10.1086/150986 , https://ui.adsabs.harvard.edu/abs/1971ApJ...166..605W 166, 605

    1971 doi

  83. [92]

    Wu C.-J., Ip W.-H., Huang L.-C., 2015, @doi [ ] 10.1088/0004-637X/798/2/92 , https://ui.adsabs.harvard.edu/abs/2015ApJ...798...92W 798, 92

    2015 doi

  84. [93]

    Yang Y.-G., Qian S.-B., 2015, @doi [ ] 10.1088/0004-6256/150/3/69 , https://ui.adsabs.harvard.edu/abs/2015AJ....150...69Y 150, 69

    2015 doi

  85. [94]

    L., Misra P., Yang J., Pi Q., 2023, @doi [ ] 10.1051/0004-6361/202142710 , https://ui.adsabs.harvard.edu/abs/2023A&A...669A..15Y 669, A15

    Yang Z., Zhang L., Meng G., Han X. L., Misra P., Yang J., Pi Q., 2023, @doi [ ] 10.1051/0004-6361/202142710 , https://ui.adsabs.harvard.edu/abs/2023A&A...669A..15Y 669, A15

    2023 doi

  86. [95]

    Zhang J., Qian S.-B., Han Z.-T., Wu Y., 2017, @doi [ ] 10.1093/mnras/stw3153 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.466.1118Z 466, 1118

    2017 doi

  87. [96]

    Zhang L.-Y., et al., 2020, @doi [ ] 10.1093/mnras/staa942 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.495.1252Z 495, 1252

    2020 doi

  88. [97]

    Zheng S.-Y., Li K., Xia Q.-Q., 2021, @doi [ ] 10.1093/mnras/stab1829 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.4251Z 506, 4251

    2021 doi

  89. [98]

    Zhou A.-Y., Jiang X.-J., Zhang Y.-P., Wei J.-Y., 2009, @doi [Research in Astronomy and Astrophysics] 10.1088/1674-4527/9/3/010 , https://ui.adsabs.harvard.edu/abs/2009RAA.....9..349Z 9, 349

    2009 doi

  90. [99]

    B., Zhang J., Jiang L

    Zhou X., Qian S. B., Zhang J., Jiang L. Q., Zhang B., Kreiner J., 2016, @doi [ ] 10.3847/0004-637X/817/2/133 , https://ui.adsabs.harvard.edu/abs/2016ApJ...817..133Z 817, 133

    2016 doi

  91. [100]

    C., Reddy B

    da Silva R., Milone A. C., Reddy B. E., 2011, @doi [ ] 10.1051/0004-6361/201015907 , https://ui.adsabs.harvard.edu/abs/2011A&A...526A..71D 526, A71

    2011 doi

  92. [101]

    S melcer L., Wolf M., Ku c \'a kov \'a H., B \' lek F., Dubovsk \'y P., Ho n kov \'a K., Vra s til J., 2017, @doi [ ] 10.1093/mnras/stw3179 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.466.2542S 466, 2542

    2017 doi

  93. [102]

    van Hamme W., 1993, @doi [ ] 10.1086/116788 , https://ui.adsabs.harvard.edu/abs/1993AJ....106.2096V 106, 2096

    1993 doi

  94. [103]

    von Zeipel H., 1924, @doi [ ] 10.1093/mnras/84.9.665 , https://ui.adsabs.harvard.edu/abs/1924MNRAS..84..665V 84, 665

    1924 doi

Pith tools

Reviewed August 10, 2026 · model on record in the stance chip above.