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REVIEW 3 major objections 4 minor 293 references

A white dwarf has been caught rotating once every 289 days, the slowest spin ever directly measured for any degenerate star, with accreted metals concentrated at both magnetic poles.

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2026-08-01 06:35 UTC pith:APDZ7LJO

load-bearing objection This paper almost certainly establishes a record-slow white-dwarf rotation period of roughly 289 d, but the quoted ±0.9 d precision is not supported by the data. the 3 major comments →

arxiv 2607.21846 v1 pith:APDZ7LJO submitted 2026-07-23 astro-ph.SR

Magnetically guided accretion and extremely slow rotation in a metal-enriched white dwarf

S. Bagnulo , M.A. Stroet , C.P. Folsom , M.A. Hollands , J.D. Landstreet , G. Ramsay This is my paper
classification astro-ph.SR
keywords white dwarfsmagnetic fieldspolluted white dwarfsDZ white dwarfsrotation periodsaccretionspectropolarimetryWD 1532+129
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This paper reports that the nearby magnetic, metal-polluted white dwarf WD 1532+129 has a rotation period of 288.7 ± 0.9 days — about 16 times longer than the previous direct record for a white dwarf. The discovery comes from combining long-baseline photometry with spectropolarimetric measurements: the star's brightness varies with a 144.35-day period, but because its mean magnetic field reverses sign, the true rotation period must be twice that. The same data show that heavy elements are not spread evenly across the surface but are enhanced near both magnetic poles, making this the third nearby magnetic DZ white dwarf with metal patches tied to magnetic geometry. If correct, the result implies that magnetically guided accretion is common among magnetic metal-enriched white dwarfs and that at least some white dwarfs can preserve extremely slow rotation from their progenitors.

Core claim

WD 1532+129 is a cool, weakly magnetic DZ white dwarf whose longitudinal magnetic field reverses sign as it rotates, proving that both magnetic hemispheres become visible during one rotation. The six photometric light curves, three equivalent-width curves, and the longitudinal-field curve are all consistent with a single rotation period of 288.7 ± 0.9 days, with the dominant photometric period of 144.35 days being exactly half the true period because the brightness pattern repeats twice per rotation. Metal-line strengths peak when either magnetic pole faces the observer, showing that accreted metals are concentrated near both poles, and the star is slightly fainter at pole-on phases, indicat

What carries the argument

The central argument is the period-doubling identity: because the disk-averaged longitudinal field ⟨Bz⟩ reverses sign across the cycle, the star must show both magnetic hemispheres, so the 144.35-day photometric modulation (which repeats twice per rotation) is half the true rotation period. The fit uses a second-order harmonic model for each photometric and equivalent-width series and a sinusoid for ⟨Bz⟩, all phased with P = 288.7 days. The longitudinal field is treated as dominated by the dipolar component, so its sign reversal is a reliable geometric indicator that both poles rotate into view.

Load-bearing premise

The entire 288.7-day rotation period rests on the assumption that the true period is exactly twice the 144.35-day photometric period, which requires that the brightness modulation is stable and strictly periodic across the full multi-year baseline and that the sign reversal of the longitudinal field really does prove both magnetic hemispheres rotate into view with rigid rotation.

What would settle it

Continue monitoring the star's longitudinal field and metal-line equivalent widths for another two or three rotation cycles: if upcoming ⟨Bz⟩ nulls or sign reversals occur at phases inconsistent with P = 288.7 ± 0.9 days, or if the 144-day photometric modulation shifts phase, the period-doubling interpretation fails. High-resolution spectropolarimetry that resolves Zeeman splitting and measures a field modulus inconsistent with a ~100–150 kG dipole would also falsify the proposed geometry.

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

If this is right

  • If the period is real, WD 1532+129 is by far the slowest-rotating white dwarf with a directly measured spin period, exceeding the previous record by a factor of about 16.
  • Metal enhancement at both magnetic poles in a third nearby magnetic DZ white dwarf strengthens the case that magnetic fields guide accreted planetary debris toward polar regions and inhibit its redistribution.
  • The star's extreme slowness is unlikely to be caused by magnetic braking or disk locking during the white-dwarf phase, given the tiny Alfvén radius and corotation radius compared with the accretion geometry.
  • The rotation period likely reflects an unusually slowly rotating progenitor, possibly a magnetic Ap star, combined with substantial angular-momentum loss during post-main-sequence evolution.
  • The observed pole-on flux deficit challenges the usual assumption that magnetic white-dwarf surfaces radiate uniformly, motivating revised atmospheric models.

Where Pith is reading between the lines

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

  • If continued monitoring shows the 144.35-day photometric modulation holding phase over a decade, the 288.7-day period will be confirmed; if the spot pattern evolves or the period drifts, the quoted precision and polar-geometry picture may need revision.
  • The existence of one 289-day rotator suggests there may be a hidden population of very slowly rotating white dwarfs missed by short-cadence surveys like TESS; systematic long-baseline photometric searches could reveal more.
  • A testable extension: high-resolution spectroscopy of the Fe ii lines could resolve Zeeman splitting and directly measure the field modulus, checking the inferred 100–150 kG dipole polar strength and the pole-on geometry.
  • If polar metal enhancement is causally linked to slow rotation, then magnetic DZ white dwarfs with long periods should preferentially show abundance patches, a prediction that can be checked against the fourth known local magnetic DZ, WD 1009−184.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. The paper reports multi-epoch FORS2 spectropolarimetry and archival ZTF, ATLAS, and GOTO photometry of the magnetic DZ white dwarf WD 1532+129. A photometric period of 144.35 d is detected independently in three surveys, with comparison stars showing no similar signal. Because the mean longitudinal field Bz reverses sign, the authors argue that the photometric modulation repeats twice per rotation and adopt a rotation period P = 288.7 ± 0.9 d, which would be by far the longest directly measured rotation period for a white dwarf. Equivalent-width variations phased with Bz are interpreted as metal abundance enhancements near both magnetic poles, making WD 1532+129 the third magnetic DZ white dwarf in the 20 pc volume to show polar metal enhancement. The paper also discusses why such slow rotation is unlikely to arise from disk locking and suggests a slowly rotating magnetic Ap progenitor.

Significance. If the 288.7 d period is correct, the result is significant: it would be an extreme outlier in white-dwarf rotation, with implications for angular-momentum loss during post-main-sequence evolution and for the rotation distribution of magnetic white dwarfs. The paper has clear strengths: the 144.35 d photometric signal is seen in three independent surveys with a low false-alarm probability, the comparison-star check supports its stellar origin, the Bz sign reversal is a physically motivated reason to double the period, and the 2026 observation was obtained as an out-of-sample test of the predicted Bz null and EW minimum. These elements make the qualitative conclusion of a rotation period of order 300 days credible. However, the quantitative period and the detailed polar-geometry interpretation rest on only seven Bz epochs and on several model assumptions, and the current text does not yet demonstrate that the quoted ±0.9 d precision and the ‘both poles’ enhancement are robust.

major comments (3)
  1. [§3, Table 1, Fig. 2] The ‘fully consistent fit’ at P = 288.7 d is strained by the two near-null Bz epochs. At phase ≈0.31 (2019-03-18, Bz = −5.0 ± 1.4 kG) and phase ≈0.28 (2026-04-18, Bz = +1.6 ± 1.1 kG), the two measurements differ by ≈6.6 kG, i.e. ≈3.7σ. A single sinusoid at P = 288.7 d cannot accommodate both without treating one as an outlier or shifting the adopted phase/period. Because these points are separated by ~7.6 rotation cycles and largely pin the absolute phase, this inconsistency directly affects the claimed ±0.9 d precision. I request a robustness analysis: fit Bz alone as a function of period and phase, show a χ² map or confidence interval, and repeat the joint fit after dropping each Bz epoch or allowing a small period offset (including the ISIS point). If the period is formally degenerate or the fit requires an outlier, the quoted uncertainty and the quantitative polar-geometry statements
  2. [§3, App. C] The uncertainty P = 288.7 ± 0.9 d is asserted without a transparent statistical derivation. The text does not provide a periodogram of the combined photometric + EW + Bz fit, a definition of the uncertainty (Monte Carlo? covariance? bootstrap?), or a test of yearly aliases in the sparse FORS2 sampling. Since the photometric period is 144.35 d and the doubling to 288.7 d rests entirely on the Bz sign reversal, the paper should demonstrate that 288.7 d is uniquely preferred over 144.35 d with a non-sinusoidal Bz curve, and over nearby periods consistent with the photometric window function. A small period change of order 1 d shifts the 2026-04-18 phase by ~9° across the 2200-d baseline; the reported ±0.9 d therefore carries real weight and should be justified by an explicit period search.
  3. [§4, Table A.1] The claim that metals are enhanced at both magnetic poles is supported mainly by the 2025 positive-pole EWs (EW1 ≈ 19.2 Å) and the 2019-06-19 negative-pole epoch (EW1 = 17.66 Å). While the negative-pole EW is higher than the equator values (≈16.5 Å), it is ~8% lower than the positive-pole maximum. The paper should quantify whether the two pole enhancements are consistent with a symmetric abundance pattern, or whether the difference reflects spot evolution, unequal polar abundances, or model-dependent limb/brightness effects. In addition, the field-geometry inversion (Bp ≈ 100–150 kG) relies on ‘somewhat arbitrarily’ chosen i = 90°, β = 60°/30° and a centred dipole; this should be stated more prominently as illustrative, and the parameter dependence of the polar-enhancement conclusion should be discussed.
minor comments (4)
  1. [Fig. B.1 caption] Typo: ‘onlt a small change’ should be ‘only a small change’.
  2. [§2.1 / App. B] The acronym ‘FLI’ is used without definition; please spell out ‘fractional lunar illumination’ at first use. Also, the exclusion of the ISIS spectrum from the EW analysis is mentioned only in App. A; add a sentence in §3 when the ISIS Bz point is shown but not fitted.
  3. [§3 / Fig. 2] The best-fit harmonic coefficients for the six light curves and three EW curves are not tabulated. If possible, provide them in an appendix or as a machine-readable table to improve reproducibility.
  4. [Abstract / §5] The abstract says ‘any degenerate star’ while §5 says ‘any white dwarf’. Since the comparison with other degenerate stars (e.g. neutron stars) is not established in the text, please qualify the record claim to white dwarfs throughout, or provide the relevant context.

Circularity Check

0 steps flagged

No significant circularity: the 288.7-d rotation period is derived from independent photometric and spectropolarimetric measurements, not from the conclusions it is used to support.

full rationale

The paper's central claim is a measured rotation period. The photometric period of 144.35 d comes from Lomb-Scargle periodograms of ZTF, ATLAS, and GOTO light curves (Fig. C.1), with comparisons to nearby stars used to exclude systematic survey effects. The doubling to 288.7 d is justified by the observed sign reversal of the mean longitudinal field: because the disk-averaged Bz is dominated by the dipolar component, a sign reversal requires both magnetic hemispheres to be viewed during one rotation, so a two-spot photometric pattern repeats twice per rotation. This is a physical interpretation of independent observables, not a parameter fitted from the quantity it predicts. The subsequent fit of Bz, equivalent widths, and photometry at P=288.7 d uses data that were not used to define the photometric period, providing an independent consistency check. Moreover, Appendix B reports that the model was used to predict a null Bz and EW minimum in 2026 before that epoch was observed, and the 2026-04-18 data confirmed it, which is an out-of-sample test rather than circular reasoning. The authors' prior work (Bagnulo et al. 2024a,b) is cited for the magnetically channelled accretion interpretation and for the existence of polar metal patches in other white dwarfs, but the rotation-period derivation does not depend on those citations. The sparse Bz sampling and the ~3.8-sigma discrepancy between two near-null epochs are statistical robustness concerns, not circularity. No step in the derivation reduces to its own input or to a self-citation chain.

Axiom & Free-Parameter Ledger

8 free parameters · 6 axioms · 0 invented entities

The central claims are observational: a fitted rotation period and a phased abundance pattern. No new physical entities are introduced. The quantitative interpretation carries several hand-chosen inputs (dipole geometry, Mdot, geff, abundance offset) which the authors flag as approximate. The main interpretive load is carried by the authors' own prior mechanism — magnetically channelled accretion with a collisional ionisation cascade (Bagnulo et al. 2024a) — which is ad hoc relative to the available physics (cool DZs emit insufficient UV to ionise the debris). Free fitting coefficients of the harmonic model are listed for completeness; they are standard light-curve modelling, not theory parameters.

free parameters (8)
  • Rotation period P = 288.7 ± 0.9 d
    Best-fitting period of the combined second-order harmonic model applied to six photometric light curves, three EW curves and <Bz> (§3). The central measured quantity; equals 2 × 144.35 d under the double-peaked-pattern assumption.
  • Dominant photometric period = 144.35 d
    Lomb-Scargle peak in the ZTF/ATLAS/GOTO photometry (Fig. C.1); the input from which the rotation period is derived by doubling.
  • Phase zero-point = MJD 59047.566
    Set to the minimum of the ZTF g-band light curve (§3); all phase coherence between photometry, EW and Bz depends on it.
  • Harmonic model coefficients = A_i,B_i,C_i,D_i,E_i per series; A',B',C' for Bz (~48 total)
    Fit coefficients of the second-order harmonic model (§3). The functional form is assumed; the period precision and the 'fully consistent fit' claim are conditional on it.
  • Dipole geometry (i, beta, limb-darkening u) = i=90°, beta=60° (or 30°), u=0.5
    Adopted 'somewhat arbitrarily' in §4 to convert the maximum |<Bz>|~25 kG into a polar field strength Bp ~100-160 kG. Does not affect the period, but underpins the field-strength quotes in the interpretation.
  • Abundance offset = +0.2 dex Fe and Ca
    Illustrative radiative-transfer input (App. B) used to show abundance changes can reproduce the observed EW behaviour; not fitted.
  • Mass accretion rate Mdot = 1e8 g/s
    'Chosen conservatively' (§5) for the Alfvén-radius and disk-locking discussion; smaller than the lowest Swan et al. (2023) estimate.
  • Effective Landé factor = geff = 1.25
    Adopted for all <Bz> measurements (§2.1); the authors note <Bz> values are meaningful only for internal consistency (Landstreet et al. 2014).
axioms (6)
  • domain assumption The disk-averaged longitudinal field <Bz> is dominated by the dipolar field component; higher-order multipoles largely cancel in the disk average.
    Invoked in §4 to justify interpreting the Bz sign reversal as both magnetic poles becoming visible and to justify a sinusoidal Bz model. Standard result (Schwarzschild 1950; Bagnulo et al. 1996).
  • domain assumption WD 1532+129 is a single star.
    Quoted from Toonen et al. (2017) in §3; used to attribute the 289-d periodicity to stellar rotation rather than orbital motion.
  • domain assumption A ~100 kG magnetic field does not by itself suppress convection in cool He-rich WD atmospheres, so convective homogenisation would normally erase metal patches.
    Used in §4 to argue the persistence of polar metal patches is magnetically significant (Cunningham et al. 2021).
  • ad hoc to paper A seed population of ions near the white dwarf can trigger a collisional ionisation cascade, allowing weakly-ionised debris to be channelled along field lines.
    Proposed by the authors in Bagnulo et al. (2024a), cited in §4 to overcome the objection that cool DZ stars emit too little UV to ionise accreting gas. Load-bearing for the 'magnetically guided accretion is common' interpretation; no independent test.
  • domain assumption In non-magnetic cool DZ white dwarfs, accreted metals are vertically mixed through the convection zone and redistributed horizontally on vertical-diffusion timescales.
    Background used in §4 to define why patches are unexpected without magnetism (Koester 2009; Cunningham et al. 2021).
  • domain assumption Post-main-sequence evolution requires substantial angular-momentum loss beyond structural contraction; typical WD rotation periods arise from this evolutionary channel.
    Used in §5 to argue the 289-d period implies an unusually slowly rotating progenitor such as a magnetic Ap star (Spruit 1998; Koester et al. 1998; Hermes et al. 2017).

pith-pipeline@v1.3.0-alltime-deepseek · 14524 in / 36095 out tokens · 356361 ms · 2026-08-01T06:35:29.889295+00:00 · methodology

0 comments
read the original abstract

White dwarfs that show atmospheric metal enrichment offer a direct window into the bulk composition of exoplanetary material and provide some of the most direct constraints on the building blocks of rocky exoplanetary systems. Recent work has suggested that magnetic fields may influence how this material is accreted, potentially channelling debris along field lines and retaining it near magnetic poles rather than allowing it to be redistributed uniformly across the stellar surface. Here we report the discovery of photometric, spectroscopic, and spectropolarimetric variability in the magnetic DZ white dwarf WD1532+129, revealing a rotation period of about 289 days, by far the longest yet directly measured for any degenerate star. The observed period may result from the combined effect of angular-momentum loss during the evolution leading to the white dwarf stage and an unusually slowly rotating progenitor, perhaps a magnetic Ap star. The white dwarf exhibits surface abundance inhomogeneities, with metals concentrated near both magnetic poles, and the observed modulation is consistent with localised metal-rich regions aligned with the magnetic geometry. WD1532+129 is the third of the four known magnetic DZ white dwarfs within 20 pc to show evidence for polar metal enhancement, indicating that magnetically guided inhomogeneities are a common property of magnetic metal-enriched white dwarfs.

Figures

Figures reproduced from arXiv: 2607.21846 by C.P. Folsom, G. Ramsay, J.D. Landstreet, M.A. Hollands, M.A. Stroet, S. Bagnulo.

Figure 1
Figure 1. Figure 1: Intensity I normalised by the continuum Ic, and reduced polarised spectra (Stokes V/I) of WD 1532+129 obtained at four different epochs. The two right panels show an enlarged view of the two left panels. The red lines correspond to a time when the mean longitudinal magnetic field has a positive maximum (∼ 26 kG), and the star is viewed approximately magnetic-pole-on; the black lines correspond to epochs wh… view at source ↗
Figure 2
Figure 2. Figure 2: From top to bottom: WD 1532+129 photometry from ZTF, GOTO, and ATLAS; equivalent width measurements from FORS2 spectra; and mean longitudinal field values, all phased with a rotational period of 288.7 d and a zero-point of MJD 59047.566. Solid curves show the best-fit models, while orange shaded regions mark the 1σ and 3σ confidence intervals. In the bottom panel, the red point with a visible error bar is … view at source ↗

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Reference graph

Works this paper leans on

293 extracted references · 82 canonical work pages

  1. [1]

    , keywords =

    The Magnetic Field and Abundance Distribution Geometry of the Peculiar A Star 53 Camelopardalis. , keywords =. doi:10.1086/166155 , adsurl =

    doi:10.1086/166155

  2. [2]

    Summary of the content and survey properties

    Gaia Data Release 3. Summary of the content and survey properties. , keywords =. doi:10.1051/0004-6361/202243940 , archivePrefix =. 2208.00211 , primaryClass =

    Pith/arXiv arXiv

  3. [3]

    , keywords =

    The Zwicky Transient Facility: System Overview, Performance, and First Results. , keywords =. doi:10.1088/1538-3873/aaecbe , archivePrefix =. 1902.01932 , primaryClass =

    Pith/arXiv arXiv 1902

  4. [4]

    , keywords =

    A First Catalog of Variable Stars Measured by the Asteroid Terrestrial-impact Last Alert System (ATLAS). , keywords =. doi:10.3847/1538-3881/aae47f , archivePrefix =. 1804.02132 , primaryClass =

    Pith/arXiv arXiv

  5. [5]

    , keywords =

    ATLAS: A High-cadence All-sky Survey System. , keywords =. doi:10.1088/1538-3873/aabadf , archivePrefix =. 1802.00879 , primaryClass =

    Pith/arXiv arXiv

  6. [6]

    Ground-based and Airborne Telescopes X , year = 2024, editor =

    The Gravitational-wave Optical Transient Observer (GOTO). Ground-based and Airborne Telescopes X , year = 2024, editor =. doi:10.1117/12.3018305 , archivePrefix =. 2407.17176 , primaryClass =

    Pith/arXiv arXiv 2024

  7. [7]

    arXiv e-prints , keywords =

    The Gravitational-wave Optical Transient Observer (GOTO) data pipeline and workflow for transient discovery. arXiv e-prints , keywords =. doi:10.48550/arXiv.2603.02330 , archivePrefix =. 2603.02330 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2603.02330

  8. [8]

    , keywords =

    Linking the interiors and surfaces of magnetic stars. , keywords =. doi:10.1093/mnras/stad475 , archivePrefix =. 2301.11914 , primaryClass =

    Pith/arXiv arXiv

  9. [9]

    , keywords =

    The frequency of planetary debris around young white dwarfs. , keywords =. doi:10.1051/0004-6361/201423691 , archivePrefix =. 1404.2617 , primaryClass =

    Pith/arXiv arXiv

  10. [10]

    , keywords =

    Metal accretion scars may be common on magnetic, polluted white dwarfs. , keywords =. doi:10.1051/0004-6361/202451215 , archivePrefix =. 2407.17196 , primaryClass =

    Pith/arXiv arXiv

  11. [11]

    , keywords =

    Strong magnetic fields of old white dwarfs are symmetric about the stellar rotation axes. , keywords =. doi:10.1051/0004-6361/202451386 , archivePrefix =. 2411.10270 , primaryClass =

    Pith/arXiv arXiv

  12. [12]

    New diffusion timescales and applications to GD 362 and G 29-38

    Accretion and diffusion in white dwarfs. New diffusion timescales and applications to GD 362 and G 29-38. , keywords =. doi:10.1051/0004-6361/200811468 , archivePrefix =. 0903.1499 , primaryClass =

    Pith/arXiv arXiv

  13. [13]

    Accretion by rotating magnetic neutron stars. III. Accretion torques and period changes in pulsating X-ray sources. , keywords =. doi:10.1086/157498 , adsurl =

    doi:10.1086/157498

  14. [14]

    Protostars and Planets V , year = 2007, editor =

    Magnetospheric Accretion in Classical T Tauri Stars. Protostars and Planets V , year = 2007, editor =. doi:10.48550/arXiv.astro-ph/0603498 , archivePrefix =. astro-ph/0603498 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0603498 2007

  15. [15]

    , keywords =

    Locking of the Rotation of Disk-Accreting Magnetized Stars. , keywords =. doi:10.1086/497000 , archivePrefix =. astro-ph/0510659 , primaryClass =

    Pith/arXiv arXiv

  16. [16]

    , keywords =

    Disk Accretion onto Magnetic T Tauri Stars. , keywords =. doi:10.1086/185972 , adsurl =

    doi:10.1086/185972

  17. [17]

    , keywords =

    Discovery of Magnetically Guided Metal Accretion onto a Polluted White Dwarf. , keywords =. doi:10.3847/2041-8213/ad2619 , archivePrefix =. 2402.16526 , primaryClass =

    Pith/arXiv arXiv 2041

  18. [18]

    , keywords =

    Ohmic Heating of Asteroids around Magnetic Stars. , keywords =. doi:10.3847/1538-4357/ab12e9 , archivePrefix =. 1903.11533 , primaryClass =

    Pith/arXiv arXiv 1903

  19. [19]

    , keywords =

    Induction heating of planetary interiors in white dwarf systems. , keywords =. doi:10.1051/0004-6361/202245225 , adsurl =

    doi:10.1051/0004-6361/202245225

  20. [20]

    Journal of Astronomical Telescopes, Instruments, and Systems , year = 2015, month = jan, volume =

    Transiting Exoplanet Survey Satellite (TESS). Journal of Astronomical Telescopes, Instruments, and Systems , year = 2015, month = jan, volume =. doi:10.1117/1.JATIS.1.1.014003 , adsurl =

    doi:10.1117/1.jatis.1.1.014003 2015

  21. [21]

    , keywords =

    Periodic optical variability and debris accretion in white dwarfs: a test for a causal connection*. , keywords =. doi:10.1093/mnras/sty257 , archivePrefix =. 1711.10488 , primaryClass =

    Pith/arXiv arXiv

  22. [22]

    , keywords =

    Chemical Abundances in the Externally Polluted White Dwarf GD 40: Evidence of a Rocky Extrasolar Minor Planet. , keywords =. doi:10.1088/0004-637X/709/2/950 , archivePrefix =. 0912.1422 , primaryClass =

    Pith/arXiv arXiv

  23. [23]

    , keywords =

    Diffusion time scales in white dwarfs. , keywords =. doi:10.1086/157247 , adsurl =

    doi:10.1086/157247

  24. [24]

    , keywords =

    The chemical evolution of white dwarf atmospheres : diffusion and accretion. , keywords =

  25. [25]

    , keywords =

    Magnetism, X-rays and accretion rates in WD 1145+017 and other polluted white dwarf systems. , keywords =. doi:10.1093/mnras/stx2664 , archivePrefix =. 1709.08206 , primaryClass =

    Pith/arXiv arXiv

  26. [26]

    , keywords =

    Does a Differentiated, Carbonate-rich, Rocky Object Pollute the White Dwarf SDSS J104341.53+085558.2?. , keywords =. doi:10.3847/1538-4357/834/1/1 , archivePrefix =. 1610.08016 , primaryClass =

    Pith/arXiv arXiv

  27. [27]

    , keywords =

    Search for rotation in white dwarfs. , keywords =

  28. [28]

    Science , keywords =

    Evidence for Water in the Rocky Debris of a Disrupted Extrasolar Minor Planet. Science , keywords =. doi:10.1126/science.1239447 , archivePrefix =. 1310.3269 , primaryClass =

    Pith/arXiv arXiv

  29. [29]

    Science , keywords =

    Oxygen fugacities of extrasolar rocks: Evidence for an Earth-like geochemistry of exoplanets. Science , keywords =. doi:10.1126/science.aax3901 , archivePrefix =. 1910.12989 , primaryClass =

    Pith/arXiv arXiv 1910

  30. [30]

    , keywords =

    The Chemical Composition of an Extrasolar Minor Planet. , keywords =. doi:10.1086/522223 , archivePrefix =. 0708.0198 , primaryClass =

    Pith/arXiv arXiv

  31. [32]

    Royal Society Open Science , keywords =

    Post-main-sequence planetary system evolution. Royal Society Open Science , keywords =. doi:10.1098/rsos.150571 , archivePrefix =. 1601.05419 , primaryClass =

    Pith/arXiv arXiv

  32. [33]

    , keywords =

    White dwarf pollution by asteroids from secular resonances. , keywords =. doi:10.1093/mnras/sty1819 , archivePrefix =. 1807.02610 , primaryClass =

    Pith/arXiv arXiv

  33. [34]

    , keywords =

    Eccentric planets and stellar evolution as a cause of polluted white dwarfs. , keywords =. doi:10.1093/mnras/stu097 , archivePrefix =. 1401.5470 , primaryClass =

    Pith/arXiv arXiv

  34. [35]

    , keywords =

    Tidal Disruption of Planetesimals from an Eccentric Debris Disk Following a White Dwarf Natal Kick. , keywords =. doi:10.3847/2041-8213/ad394c , archivePrefix =. 2404.04296 , primaryClass =

    Pith/arXiv arXiv 2041

  35. [36]

    2005", month =

    Period04 User Guide. Communications in Asteroseismology , year = "2005", month = "Jun", volume =. doi:10.1553/cia146s53 , adsurl =

    doi:10.1553/cia146s53 2005

  36. [37]

    Treatise on Geochemistry , year = 2003, month = dec, volume =

    Compositional Model for the Earth's Core. Treatise on Geochemistry , year = 2003, month = dec, volume =. doi:10.1016/B0-08-043751-6/02015-6 , adsurl =

    doi:10.1016/b0-08-043751-6/02015-6 2003

  37. [38]

    Treatise on Geochemistry , year = 2003, month = dec, volume =

    Cosmochemical Estimates of Mantle Composition. Treatise on Geochemistry , year = 2003, month = dec, volume =. doi:10.1016/B0-08-043751-6/02177-0 , adsurl =

    doi:10.1016/b0-08-043751-6/02177-0 2003

  38. [39]

    Treatise on Geochemistry , year = 2003, month = dec, volume =

    Composition of the Continental Crust. Treatise on Geochemistry , year = 2003, month = dec, volume =. doi:10.1016/B0-08-043751-6/03016-4 , adsurl =

    work page doi:10.1016/b0-08-043751-6/03016-4 2003

  39. [40]

    , keywords =

    Diffusion Coefficients in the Envelopes of White Dwarfs. , keywords =. doi:10.3847/1538-4357/ab91ad , archivePrefix =. 2005.05891 , primaryClass =

    Pith/arXiv arXiv 2005

  40. [41]

    , keywords =

    Rotation plays a role in the generation of magnetic fields in single white dwarfs. , keywords =. doi:10.1093/mnras/stae307 , archivePrefix =. 2401.15158 , primaryClass =

    Pith/arXiv arXiv

  41. [42]

    , keywords =

    A Method to Measure the Transverse Magnetic Field and Orient the Rotational Axis of Stars. , keywords =. doi:10.3847/1538-4357/aa8d72 , archivePrefix =. 1704.03376 , primaryClass =

    Pith/arXiv arXiv

  42. [43]

    , keywords =

    A nearby polluted white dwarf with a 6.2 h spin period. , keywords =. doi:10.1093/mnrasl/slae014 , archivePrefix =. 2312.03845 , primaryClass =

    Pith/arXiv arXiv

  43. [44]

    , keywords =

    Inner Edges of Compact Debris Disks around Metal-rich White Dwarfs. , keywords =. doi:10.1088/0004-637X/760/2/123 , archivePrefix =. 1207.7082 , primaryClass =

    Pith/arXiv arXiv

  44. [46]

    , keywords =

    White dwarf spectra and atmosphere models. , keywords =

  45. [47]

    , keywords =

    X-Ray and Infrared Observations of Two Externally Polluted White Dwarfs. , keywords =. doi:10.1088/0004-637X/699/2/1473 , archivePrefix =. 0905.0117 , primaryClass =

    Pith/arXiv arXiv

  46. [48]

    Chondritic compositions and a massive accretion event

    Planetesimals at DZ stars - I. Chondritic compositions and a massive accretion event. , keywords =. doi:10.1093/mnras/stad2867 , archivePrefix =. 2309.06467 , primaryClass =

    Pith/arXiv arXiv

  47. [49]

    The Solar Neighborhood. Xx. Discovery and Characterization of 21 New Nearby White Dwarf Systems. , keywords =. doi:10.1088/0004-6256/136/3/899 , archivePrefix =. 0805.2515 , primaryClass =

    Pith/arXiv arXiv

  48. [50]

    , keywords =

    X-shooter, the new wide band intermediate resolution spectrograph at the ESO Very Large Telescope. , keywords =. doi:10.1051/0004-6361/201117752 , archivePrefix =. 1110.1944 , primaryClass =

    Pith/arXiv arXiv 1944

  49. [51]

    , keywords =

    Numerical Simulations of Gaseous Disks Generated from Collisional Cascades at the Roche Limits of White Dwarf Stars. , keywords =. doi:10.3847/1538-4357/aa9570 , archivePrefix =. 1711.00026 , primaryClass =

    Pith/arXiv arXiv

  50. [52]

    , keywords =

    Circularization of tidal debris around white dwarfs: implications for gas production and dust variability. , keywords =. doi:10.1093/mnras/staa3940 , archivePrefix =. 2012.07854 , primaryClass =

    Pith/arXiv arXiv 2012

  51. [53]

    Shrinking extremely eccentric collisionless rings

    Formation of planetary debris discs around white dwarfs - II. Shrinking extremely eccentric collisionless rings. , keywords =. doi:10.1093/mnras/stv1195 , archivePrefix =. 1505.06204 , primaryClass =

    Pith/arXiv arXiv

  52. [54]

    , keywords =

    The effect of a magnetic field on the dynamics of debris discs around white dwarfs. , keywords =. doi:10.1093/mnras/staa3316 , archivePrefix =. 2009.03444 , primaryClass =

    Pith/arXiv arXiv 2009

  53. [55]

    , keywords =

    Orbital Migration and Circularization of Tidal Debris by Alfv \'e n-wave Drag: Circumstellar Debris and Pollution around White Dwarfs. , keywords =. doi:10.3847/1538-4357/ac00ae , archivePrefix =. 2105.06475 , primaryClass =

    Pith/arXiv arXiv

  54. [56]

    , keywords =

    A road-map to white dwarf pollution: tidal disruption, eccentric grind-down, and dust accretion. , keywords =. doi:10.1093/mnras/stab3009 , archivePrefix =. 2110.07601 , primaryClass =

    Pith/arXiv arXiv

  55. [57]

    Debris disc structure and ejected interstellar asteroids

    Tidal disruption of planetary bodies by white dwarfs - II. Debris disc structure and ejected interstellar asteroids. , keywords =. doi:10.1093/mnras/staa143 , archivePrefix =. 1911.12184 , primaryClass =

    Pith/arXiv arXiv 1911

  56. [58]

    Nature Astronomy , keywords =

    Rapid formation of exoplanetesimals revealed by white dwarfs. Nature Astronomy , keywords =. doi:10.1038/s41550-022-01815-8 , archivePrefix =. 2211.07244 , primaryClass =

    Pith/arXiv arXiv

  57. [59]

    , keywords =

    Discovery of Beryllium in White Dwarfs Polluted by Planetesimal Accretion. , keywords =. doi:10.3847/1538-4357/abe40b , archivePrefix =. 2102.01834 , primaryClass =

    Pith/arXiv arXiv

  58. [60]

    New Astronomy Reviews , keywords =

    Circumstellar debris and pollution at white dwarf stars. New Astronomy Reviews , keywords =. doi:10.1016/j.newar.2016.03.001 , archivePrefix =. 1604.03092 , primaryClass =

    Pith/arXiv arXiv 2016

  59. [61]

    , keywords =

    Ancient Planetary Systems are Orbiting a Large Fraction of White Dwarf Stars. , keywords =. doi:10.1088/0004-637X/722/1/725 , archivePrefix =. 1007.2252 , primaryClass =

    Pith/arXiv arXiv

  60. [62]

    , keywords =

    I Spy Transits and Pulsations: Empirical Variability in White Dwarfs Using Gaia and the Zwicky Transient Facility. , keywords =. doi:10.3847/1538-4357/abee68 , archivePrefix =. 2012.00035 , primaryClass =

    Pith/arXiv arXiv 2012

  61. [63]

    , keywords =

    Metal Lines in DA White Dwarfs. , keywords =. doi:10.1086/377492 , adsurl =

    doi:10.1086/377492

  62. [64]

    , keywords =

    Solar System Abundances and Condensation Temperatures of the Elements. , keywords =. doi:10.1086/375492 , adsurl =

    doi:10.1086/375492

  63. [65]

    , keywords =

    Interpretation and diversity of exoplanetary material orbiting white dwarfs. , keywords =. doi:10.1093/mnras/stz2337 , archivePrefix =. 1908.08047 , primaryClass =

    Pith/arXiv arXiv 1908

  64. [66]

    , keywords =

    Compositions of Planetary Debris around Dusty White Dwarfs. , keywords =. doi:10.3847/1538-3881/ab4cee , archivePrefix =. 1910.07197 , primaryClass =

    Pith/arXiv arXiv 1910

  65. [67]

    Annual Review of Earth and Planetary Sciences , year = 2014, month = may, volume =

    Extrasolar Cosmochemistry. Annual Review of Earth and Planetary Sciences , year = 2014, month = may, volume =. doi:10.1146/annurev-earth-060313-054740 , adsurl =

    doi:10.1146/annurev-earth-060313-054740 2014

  66. [68]

    , keywords =

    New Chondritic Bodies Identified in Eight Oxygen-bearing White Dwarfs. , keywords =. doi:10.3847/1538-4357/acbd44 , archivePrefix =. 2303.00063 , primaryClass =

    Pith/arXiv arXiv

  67. [69]

    , keywords =

    An Aluminum/Calcium-rich, Iron-poor, White Dwarf Star: Evidence for an Extrasolar Planetary Lithosphere?. , keywords =. doi:10.1088/0004-637X/739/2/101 , archivePrefix =. 1107.2167 , primaryClass =

    Pith/arXiv arXiv

  68. [71]

    , keywords =

    ^ 26 Al in the Early Solar System: Not So Unusual after All. , keywords =. doi:10.1088/2041-8205/775/2/L41 , archivePrefix =. 1308.6325 , primaryClass =

    Pith/arXiv arXiv 2041

  69. [72]

    Application to DQ white dwarfs

    New white dwarf envelope models and diffusion. Application to DQ white dwarfs. , keywords =. doi:10.1051/0004-6361/202037530 , archivePrefix =. 2002.10170 , primaryClass =

    Pith/arXiv arXiv 2002

  70. [73]

    , keywords =

    Multiple Channels for the Onset of Magnetism in Isolated White Dwarfs. , keywords =. doi:10.3847/2041-8213/ac84d3 , archivePrefix =. 2208.02655 , primaryClass =

    Pith/arXiv arXiv 2041

  71. [74]

    , keywords =

    The Gaia mission. , keywords =. doi:10.1051/0004-6361/201629272 , archivePrefix =. 1609.04153 , primaryClass =

    Pith/arXiv arXiv

  72. [75]

    , keywords =

    The influence of the Galactic tidal field on the Oort comet cloud. , keywords =. doi:10.1016/0019-1035(86)90060-6 , adsurl =

    doi:10.1016/0019-1035(86)90060-6

  73. [76]

    Oort cloud Ecology. II. the chronology of the formation of the Oort cloud. , keywords =. doi:10.1051/0004-6361/202040096 , archivePrefix =. 2105.12816 , primaryClass =

    Pith/arXiv arXiv

  74. [77]

    , keywords =

    Time-dependent injection of Oort cloud comets into Earth-crossing orbits. , keywords =. doi:10.1016/0019-1035(87)90161-8 , adsurl =

    work page doi:10.1016/0019-1035(87)90161-8

  75. [78]

    , keywords =

    New stellar encounters discovered in the second Gaia data release. , keywords =. doi:10.1051/0004-6361/201833456 , archivePrefix =. 1805.07581 , primaryClass =

    Pith/arXiv arXiv

  76. [79]

    , year = 1950, month = jan, volume =

    The structure of the cloud of comets surrounding the Solar System and a hypothesis concerning its origin. , year = 1950, month = jan, volume =

    1950

  77. [80]

    , keywords =

    On the accuracy of close stellar approaches determination. , keywords =. doi:10.1093/mnras/stv367 , archivePrefix =. 1502.05518 , primaryClass =

    Pith/arXiv arXiv

  78. [81]

    Simulating observable comets. III. Real stellar perturbers of the Oort cloud and their output. , year = 2006, month = apr, volume =. doi:10.1051/0004-6361:20054284 , adsurl =

    doi:10.1051/0004-6361:20054284 2006

  79. [82]

    , keywords =

    First stars that could significantly perturb comet motion are finally found. , keywords =. doi:10.1093/mnras/stz3127 , archivePrefix =. 1911.01735 , primaryClass =

    Pith/arXiv arXiv 1911

  80. [83]

    , keywords =

    Important stellar perturbers found during the StePPeD database update based on Gaia EDR3 data. , keywords =. doi:10.1051/0004-6361/202243853 , archivePrefix =. 2206.11047 , primaryClass =

    Pith/arXiv arXiv

Showing first 80 references.