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REVIEW 4 major objections 3 minor 112 references

Magnetic fields on white dwarfs concentrate accreted metals into narrow polar patches, so standard spectroscopic estimates of metal accretion rates can be orders of magnitude too low.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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2026-08-01 09:29 UTC pith:NZ6H2K2A

load-bearing objection Useful framework, but the paper's magnetic beaming may not get off the ground: nominal ionization fractions give an ambipolar Elsasser number ~0.01, so the gas is not actually coupled to the field. the 4 major comments →

arxiv 2607.20747 v1 pith:NZ6H2K2A submitted 2026-07-22 astro-ph.SR astro-ph.EP

The Effects of Magnetic Accretion on the Spatial Extent of White Dwarf Pollution

Dang Pham , Aster G. Taylor , Tim Cunningham This is my paper
classification astro-ph.SR astro-ph.EP
keywords white dwarf pollutionmagnetic white dwarfsmagnetospheric accretionmetal line variabilityaccretion rate biasdebris diskssurface diffusionWD 2138-332
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 argues that the magnetic fields of white dwarfs channel accreted metals into narrow polar beams, rather than spreading them uniformly over the surface. The metals then spread horizontally only as fast as convection and diffusion allow, while sinking toward the interior on a settling timescale; the ratio of these timescales sets the size of the polluted patch. If the magnetic pole is tilted relative to the spin axis, the patch rotates in and out of view, producing periodic variability in metal lines. The same geometry means that standard spectroscopic estimates of metal accretion rates, which assume a uniform surface distribution, can be too low by up to several orders of magnitude. A patchy-pollution model with a surface covering fraction of about 10% reproduces the observed variability of the magnetic white dwarf WD 2138-332.

Core claim

The paper's central claim is that magnetospheric accretion onto white dwarfs concentrates accreted planetary debris into a small polar region of the photosphere, and that the subsequent horizontal spreading of these metals is controlled by a single ratio, the sinking timescale over the spreading timescale. The model yields a surface covering fraction f_cov ≈ (1/8)(τ_sink/τ_spread) + σ_beam^2/(4R_*^2). For most hydrogen-atmosphere white dwarfs with effective temperatures above about 12,000 K, and for many helium-atmosphere objects, the pollution remains localized; only cool white dwarfs with deep convection zones homogenize. Because observed line strengths are interpreted assuming a uniform s

What carries the argument

The dipole-plus-octupole magnetic field geometry, with the conserved field-line label q mapping disk radius to surface footprint, determines the initial accretion beam area (typically less than 10^-4 of the surface). The atmosphere's response is described by the drift–diffusion equation for metal concentration, whose Green's function is a Gaussian with variance set by the horizontal diffusion coefficient and the sinking timescale; this leads directly to the covering-fraction formula and the projected-area calculation that converts surface patches into line-strength variability and accretion-rate bias.

Load-bearing premise

The gas in the debris disk is ionized enough (by alkali metals or cosmic rays) to couple to the white dwarf's magnetic field near the sublimation radius, and the paper acknowledges that if dust or low abundances suppress ionization, the metals would accrete at the equator instead of being channeled into polar beams.

What would settle it

Measuring the surface metal distribution of a magnetic (B ≳ 1 kG) polluted white dwarf via Doppler or Zeeman mapping and finding it uniform, or measuring an X-ray accretion rate that matches the spectroscopic rate for a strongly magnetic object, would rule out the patch model.

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

If this is right

  • If correct, many polluted magnetic white dwarfs—especially young, hot hydrogen-atmosphere stars and old, strongly magnetic stars—host metal patches covering 10^-4 to 10^-1 of the surface, not the whole star.
  • Spectroscopic accretion rates for such objects are systematically underestimated by factors up to about a thousand; X-ray measurements would not suffer this bias.
  • Periodic variability in metal-line equivalent width is a direct diagnostic of a surface patch and yields the patch area; absence of variability is consistent with aligned spin and field axes, so patchy pollution can hide unnoticed.
  • Different polluting elements have different sinking timescales, so they occupy concentric patches of different sizes and therefore show different variability amplitudes, as observed for calcium and magnesium in WD 2138-332.
  • The mass reservoirs required to supply planetary debris may need to be up to three orders of magnitude more massive than previously thought for some white dwarfs.

Where Pith is reading between the lines

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

  • If the mechanism is general, magnetic stars with circumstellar disks—not only white dwarfs—could show analogous surface-abundance inhomogeneities, though their strong accretion columns would make the patches more directly observable.
  • A direct observational test: measuring the patch radius for multiple elements in one star would provide a handle on the horizontal diffusion coefficient, which is currently taken from non-magnetic simulations, and could calibrate magnetic convection models.
  • The predicted temperature dependence implies that finding a hot, magnetic, polluted white dwarf with a uniform metal distribution would disfavor the model, so targeted surveys of hot magnetic white dwarfs could sharpen or refute it.
  • If the bias is confirmed, the inferred population of white-dwarf accretion rates would shift upward preferentially for magnetic objects, sharpening the distinction between magnetic and non-magnetic polluted white dwarfs and potentially altering the inferred frequency of volatile-rich parent bodies.

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

4 major / 3 minor

Summary. This paper proposes that magnetic fields on white dwarfs channel accretion from a gaseous debris disk onto a narrow polar surface region, and that the subsequent competition between vertical settling and horizontal convective spreading determines whether this patch remains localized or becomes homogeneous. The authors derive the accretion beam area from dipole/octupole field geometry (Sec. 3), compute atmospheric stopping and collision rates (Sec. 4.1–4.2), model convection suppression by magnetic fields (Sec. 4.3), and combine MESA sinking timescales with non-magnetic 3D horizontal diffusion coefficients to estimate surface covering fractions (Sec. 4.4–4.7). They then derive projected-area corrections and mass-accretion-rate biases (Eqs. 31–32), and apply the model to the periodically variable polluted magnetic WD 2138-332, associating its variability with a ~10% surface patch (Sec. 5.3). The main conclusions are that patchy pollution is expected on many magnetic white dwarfs, that rotational variability requires spin–magnetic misalignment, and that inferred accretion rates may be underestimated by up to orders of magnitude.

Significance. If the model survives scrutiny, it is significant: it provides a concrete physical mechanism linking magnetic accretion geometry to the spatial distribution of pollutants on white dwarfs, with a falsifiable prediction that metal-line variability should be tied to the rotation period and to spin/magnetic misalignment. It also offers a potential explanation for the recently observed variable pollution in WD 2138-332 and raises an important systematic bias in accretion-rate estimates. The paper is commendably transparent: the geometric and diffusion derivations are explicit (Appendices A–C), the MESA setups are described in enough detail to reproduce, and the authors are candid about the main caveats (Sec. 6.6). The central idea is novel and timely. However, its strongest claims rest on plasma-coupling and convection-scaling assumptions that are not yet adequately supported.

major comments (4)
  1. [Sec. 2 / Sec. 6.6] The premise that gas couples to the magnetic field near the sublimation radius is not established. The paper quotes x_e ~ 1e-12 (alkali) and ~4e-13 (cosmic rays) and calls these 'sufficient to couple', but no coupling criterion (Elsasser or magnetic Reynolds number) is computed. Using the authors' numbers, n_i ~ 400–1000 cm^-3, ρ_i ~ 2e-20 g/cm^3, with γ ~ 3e13 cm^3/g/s and Ω ~ 8e-5 s^-1, the ambipolar Elsasser number Am = γρ_i/Ω ~ 1e-2 to 1e-3, far below unity. Thus the neutrals, which carry most of the mass, are not locked to the field, and the beaming geometry of Sec. 3 collapses. The paper must either compute Am/Rm (or provide a chemical-network result) and identify a regime where Am>1, or explicitly reframe the model as conditional on that unverified condition.
  2. [Sec. 4.3, Eq. (21)] The magnetic convective velocity v_B is taken from a private communication and has not been derived elsewhere. As written, its dimensions are inconsistent: [(F_conv/L_P)^{2/3}] = M^{2/3} L^{-2/3} T^{-2}, while [(ρ/(ΩB^2 L_P))^{1/3}] = L^{-1} T, giving overall units of M^{2/3} L^{-5/3} T^{-1}, not cm/s. This means Fig. 7 and the statement that B ≳ 100 MG suppresses convection are not quantitatively supported. The authors should supply a correct derivation or reference for the scaling, or present it as an explicit ad hoc assumption with a sensitivity analysis.
  3. [Sec. 5.3, Fig. 10] The 10% polluted-area fraction for WD 2138-332 is effectively inferred from the observed 0.5 dex variability amplitude: Fig. 10 is generated by choosing f so that the model matches the data. Therefore, the agreement is a consistency check, not an independent prediction. The Conclusion's claim that this work 'demonstrates' the variability is explained should be softened, and the paper should compare an independently computed f from the beam-area and f_cov models with the value required by the variability amplitude.
  4. [Sec. 4.5–4.7 and Fig. 8] The entire f_cov calculation uses D_surf from non-magnetic CO5BOLD simulations. Since f_cov = (1/8)τ_sink/τ_spread depends linearly on D_surf, the quantitative predictions (e.g., the magnitude of the accretion-rate bias in Eq. 32) are uncertain. The authors correctly note that magnetic suppression of turbulence would reduce D_surf and thus shrink the patch, which goes in the direction of strengthening their qualitative conclusion. But the paper should still state whether the non-magnetic D_surf is an upper or lower bound and discuss how the derived Mdot biases would change if D_surf is suppressed by even an order of magnitude.
minor comments (3)
  1. [Sec. 4.5] The quantity f_cov is called a covering fraction, but the paper later clarifies that it actually tracks the 1/e gradient of the pollution distribution. Consider renaming it 'gradient parameter' or defining this clearly at first use to avoid confusion for readers.
  2. [Sec. 3.1, Eq. (11)] The text notes that there may be multiple solution branches for θ0 when the octupole component is significant. It would help to give an explicit criterion for selecting the 'outer' versus 'inner' branch, or to add a small figure illustrating the different branches.
  3. [Fig. 7] In the top panel, the legend appears to list '104 G' twice, making it impossible to distinguish which line corresponds to 10^4 G and which to 10^5 G. Please correct the legend.

Circularity Check

0 steps flagged

No significant circularity; the central derivation is self-contained given external inputs, and the 10% patch for WD 2138-332 is an inversion of observed variability rather than an independent prediction.

full rationale

Walking the derivation chain: the magnetic truncation radii (Sec. 2) use standard magnetospheric formulae; the beam geometry (Sec. 3) is an analytic field-line mapping; and the surface covering fraction f_cov (Eqs. 28-29, Appendix C) follows by solving the steady-state drift-diffusion equation. The two inputs to f_cov are tau_sink from MESA (Sec. 4.4) and D_surf from the CO5BOLD simulations of Cunningham et al. (2021). The latter is a co-authored paper, but it is an independent external simulation result used as a tabulated input, with the paper explicitly noting the caveat that it comes from non-magnetic simulations (Sec. 6.6); this is real evidence, not a restatement of the present model. The Mdot bias relation (Eq. 32) is a direct geometric consequence of confining pollution to a projected fraction f_perp, not a self-consistency condition. The only place the model is matched to a specific object is the WD 2138-332 illustration: Sec. 5.3 chooses the f-value whose predicted variability amplitude equals the observed 0.5 dex, and Sec. 6.4 phrases the result as 'consistent with' a 10% patch, explicitly calling for further detections to test the model. This is parameter estimation from data, not a fitted input renamed as a prediction. No equation reduces to its own input, and no load-bearing conclusion rests on an unverified self-citation chain. The ionization-coupling assumption in Sec. 2 is asserted without computing an explicit coupling parameter (e.g., Elsasser or magnetic Reynolds number), but that is an unverified physical assumption or correctness/reliability issue, not circularity.

Axiom & Free-Parameter Ledger

7 free parameters · 7 axioms · 0 invented entities

The central claims rest on standard fluid/magnetospheric physics plus several domain-specific assumptions and one unpublished scaling relation; the authors flag most caveats in Sec. 6.6. No new particles or forces are introduced.

free parameters (7)
  • pollution patch area fraction f for WD 2138-332 = ≈0.1 (10% of surface)
    Set to match the ~0.5 dex observed variability amplitude in Sec 5.3/6.4; not independently predicted.
  • octupole-to-dipole field ratio Γ = varied 0–10
    Model geometry parameter; controls beam width (Fig 5); not constrained by observation in this paper.
  • magnetic pole offset β = 15° or 60° (degenerate)
    Adopted from Bagnulo et al. 2024b degeneracy; affects variability amplitude and phase.
  • viewing angle α = 60° or 15° (degenerate)
    Adopted from Bagnulo et al. 2024b; affects projected covering fraction.
  • rotation period P = 2 hr
    Assumed typical for magnetic white dwarfs (Hernandez et al. 2024); enters τ_conv via Ω.
  • mixing length parameter α_MLT = 0.8 (DA); 1.25 and 0.8 (DB)
    Standard choices from MESA literature; affects τ_sink and hence f_cov.
  • order-unity coefficient in magnetic convective velocity (Eq 21) = unspecified
    Scaling relation from private communication; proportionality constant not given, only used for order-of-magnitude τ_conv.
axioms (7)
  • standard math Steady-state advection-diffusion equation with Green's function solution (Eq C14) and the f_cov formula (Eq C21/C26)
    Standard applied mathematics used without proof in Appendix C.
  • domain assumption Gaseous debris disk ionizes and couples to the magnetic field near the sublimation radius
    Invoked in Sec 2; necessary for magnetospheric accretion to occur. The paper itself flags this as a caveat in Sec 6.6.
  • domain assumption White dwarf magnetic field is a dipole+octupole with negligible higher multipoles (Eq 9)
    Assumed in Sec 3 for computing field-line mapping; higher-order terms near the surface could alter beam sizes.
  • domain assumption Accretion is steady-state and pollutants are trace species
    Used in Sec 4.5 and Appendix C; authors note episodic accretion and non-trace compositions as caveats in Sec 6.6.
  • domain assumption Horizontal diffusion coefficient D_surf from non-magnetic CO5BOLD simulations applies to magnetic white dwarfs to order of magnitude
    Used in Sec 4.5 to compute τ_spread; authors state the coefficient may be suppressed by magnetic fields, which would shrink patches.
  • ad hoc to paper Magnetic convective velocity scaling v_B ~ (F_conv/L_P)^{2/3} (4πρ/(2ΩB^2 L_P))^{1/3} (Eq 21) from private communication (J.R. Fuentes 2025)
    Not published or independently verified; underpins the claim that B ≳ 100 MG suppresses convection (Fig 7).
  • domain assumption MESA 1D models with ML2 convection (Bauer & Bildsten 2019) give valid sinking timescales in both convective and no-convection limits
    Adopted in Sec 4.4; the two limiting cases bracket the unknown magnetic influence on convection.

pith-pipeline@v1.3.0-alltime-deepseek · 31809 in / 18433 out tokens · 154533 ms · 2026-08-01T09:29:32.874750+00:00 · methodology

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read the original abstract

Many white dwarfs are polluted by metals, which are generally understood to be the accreted remnants of a planetary system. Modeling these systems typically assumes that the metal concentration is homogeneous throughout the white dwarf's atmosphere. However, the magnetic fields of a white dwarf may affect the accretion geometry of the white dwarf via magnetospheric accretion. Convection in the white dwarf's photosphere will then transport the metals across the surface, with a structure set by the relative sinking versus spreading timescales. In this work, we construct models for the accretion geometry, subsequent spreading, and observed pollution of magnetic white dwarfs. We show that the magnetic fields will initially concentrate the pollution into a narrow region of the white dwarf's surface. The relative spreading and sinking timescales determine whether the metals become uniformly distributed or remain confined to localized patches. If the magnetic field and spin poles are misaligned, then patchy white dwarfs exhibit periodically variable pollution signatures, which enable constraints on the patch area. We explore this model as a possible explanation for the recent detection of periodically variable pollution signatures in magnetic white dwarfs. Finally, we also demonstrate that the concentration of material due to the magnetic field may lead to systematic underestimates of the mass accretion rate onto these objects.

Figures

Figures reproduced from arXiv: 2607.20747 by Aster G. Taylor, Dang Pham, Tim Cunningham.

Figure 1
Figure 1. Figure 1: The structure of the white dwarf accretion disk. The magnetic truncation radius R g B and the corotation radius Rc are to the right. The disk is not shown to scale. The disk is processed by the Poynting-Robertson (PR) effect from the Roche limit RR. Once the dust reaches the sublimation temperature, at the location Rs, it is coupled to the magnetic field lines and begins to accrete onto a white dwarf with … view at source ↗
Figure 2
Figure 2. Figure 2: A comparison of the various important radii in the white dwarf accretion problem as a function of the stellar rotation rate Ω⋆, magnetic field strength B⋆, mass accretion rate M˙ , and temperature T⋆. The relative location of these radii set the structure of the disk and the magnetic accretion flow. The Roche radius RR sets the outer edge of the debris disk, the corotation radius Rc sets where magnetic cou… view at source ↗
Figure 3
Figure 3. Figure 3: The two-dimensional spatial distribution of the magnetic field lines of the white dwarf. The dipole field is shown in black, while a mixed dipole-octupole field with Γ = 10 is shown as colored lines. The color of the mixed field indicates the q value that a field line corresponds to. Note that the small lobes of field at the equator share q values with the larger field lobes. RX will be concentrated onto t… view at source ↗
Figure 4
Figure 4. Figure 4: The accretion points on a white dwarf, with an angle β = π/6 between the magnetic pole and the spin axis, an inclination I = π/4 between the accretion disk and the spin axis, the octupole-dipole ratio Γ = 1, and a disk trunca￾tion radius at RX = 2R⋆. The spin axis of the white dwarf is straight up, while the blue and red points are the poles of the magnetic field. The blue and red lines show where accreted… view at source ↗
Figure 5
Figure 5. Figure 5: Fraction of the surface polluted by magnetic ac￾cretion as a function of the white dwarf temperature T⋆. The top panel shows the surface pollution fraction for different values of the octupole-dipole field ratio Γ with the inclina￾tion of the disk fixed at I = π/2. The middle panel shows the pollution fraction for variable inclination with Γ = 1. The bottom panel is the same as the middle panel, but the ac… view at source ↗
Figure 6
Figure 6. Figure 6: Diagram illustrating a DA (hydrogen-dominated) white dwarf’s atmospheric structure and dynamics of incoming polluting 40Ca ions. Initially, the incoming particle arrived at the top of the atmosphere with velocity vin, punching through the atmosphere with length Lstop which is a small fraction of the atmospheric pressure scale height. Within the atmosphere, the particle’s motion can be affected by collision… view at source ↗
Figure 7
Figure 7. Figure 7: Top: The maximum convective turnover time to sinking time ratio, τconv/τsink, for a hydrogen-dominated atmosphere white dwarf (abbreviated as DA). The differ￾ent colored curves show this ratio at various magnetic field strengths ranging from B = 104 − 108 G, and the horizon￾tal dashed line shows where the ratio is unity. When the ratio is much less than order unity, then the atmosphere is well-mixed. τconv… view at source ↗
Figure 8
Figure 8. Figure 8: Top left: Sinking timescales of 40Ca on a hydrogen-atmosphere white dwarf (0.6 M⊙, log g = 8, abbreviated as DA) calculated by MESA. Two cases are simulated — full convection with ML2/α = 0.8 and no convection. This latter case represents the limit where the magnetic field significantly affects the base of the convection zone. The α = 0.8 curve corresponds to the fiducial mixing length value used in the ME… view at source ↗
Figure 9
Figure 9. Figure 9: Polluted fraction of the projected visible surface for a given viewing angle and polluted fraction of the total surface. This calculation assumes that β = 0 so that the projected surface is independent of the phase angle of the white dwarf’s rotation. entire surface, but only a projected region. This section calculates the fraction of the projected area of the white dwarf that will be polluted in a given o… view at source ↗
Figure 10
Figure 10. Figure 10: Variability in the projected cover fraction from the rotation of the white dwarf. The viewing angle is set to α = 60◦ and the magnetic field inclination is set to β = 15◦ , matching the model for WD 2138-332. The total polluted area fraction is set to vary from 10−4 –10−1 . strength of the metal lines should vary over the rota￾tion of the star. Here, the observation viewing angle α is defined to be with r… view at source ↗

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Reference graph

Works this paper leans on

112 extracted references · 30 canonical work pages · 3 internal anchors

  1. [1]

    The Astrophysical Journal , author =

    Magnetically. The Astrophysical Journal , author =. 2012 , note =. doi:10.1088/0004-637X/744/1/55 , abstract =

    work page doi:10.1088/0004-637x/744/1/55 2012

  2. [2]

    Progress of Theoretical Physics Supplement , author =

    Chapter 13. Progress of Theoretical Physics Supplement , author =. 1988 , note =. doi:10.1143/PTPS.96.151 , abstract =

    work page doi:10.1143/ptps.96.151 1988

  3. [3]

    , month = jan, year =

    Armitage, Philip J. , month = jan, year =. Astrophysics of planet formation,

  4. [4]

    , month = jun, year =

    Spitzer, Jr., Lyman and Tomasko, Martin G. , month = jun, year =. Heating of. The Astrophysical Journal , publisher =. doi:10.1086/149610 , abstract =

    doi:10.1086/149610

  5. [5]

    Monthly Notices of the Royal Astronomical Society , author =

    The frequency of metal enrichment of cool helium-atmosphere white dwarfs using the. Monthly Notices of the Royal Astronomical Society , author =. 2024 , note =. doi:10.1093/mnrasl/slae026 , abstract =

    work page doi:10.1093/mnrasl/slae026 2024

  6. [6]

    Nature , author =

    Suppression of cooling by strong magnetic fields in white dwarf stars , volume =. Nature , author =. 2014 , note =. doi:10.1038/nature13836 , abstract =

    work page doi:10.1038/nature13836 2014

  7. [7]

    Monthly Notices of the Royal Astronomical Society , author =

    Long-lived planetesimal discs , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2010 , note =. doi:10.1111/j.1365-2966.2009.15739.x , abstract =

    arXiv 2010

  8. [9]

    Monthly Notices of the Royal Astronomical Society , author =

    Horizontal spreading of planetary debris accreted by white dwarfs , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2021 , note =. doi:10.1093/mnras/stab553 , abstract =

    doi:10.1093/mnras/stab553 2021

  9. [10]

    Astronomy and Astrophysics , author =

    White dwarf magnetospheres:. Astronomy and Astrophysics , author =. 2024 , note =. doi:10.1051/0004-6361/202449271 , abstract =

    work page doi:10.1051/0004-6361/202449271 2024

  10. [11]

    2012 , keywords =

    The Astrophysical Journal , author =. 2012 , keywords =. doi:10.1088/0004-637X/745/1/88 , abstract =

    work page doi:10.1088/0004-637x/745/1/88 2012

  11. [12]

    The Astrophysical Journal Letters , author =

    Discovery of. The Astrophysical Journal Letters , author =. 2024 , keywords =. doi:10.3847/2041-8213/ad2619 , abstract =

    doi:10.3847/2041-8213/ad2619 2024

  12. [13]

    The Astrophysical Journal , author =

    Metal. The Astrophysical Journal , author =. 2011 , note =. doi:10.1088/2041-8205/732/1/L3 , abstract =

    work page doi:10.1088/2041-8205/732/1/l3 2011

  13. [14]

    The Astrophysical Journal Supplement Series , author =

    White. The Astrophysical Journal Supplement Series , author =. 2017 , note =. doi:10.3847/1538-4365/aa8bb5 , abstract =

    doi:10.3847/1538-4365/aa8bb5 2017

  14. [15]

    Simultaneous emission from dust and gas in the planetary debris orbiting a white dwarf

    Rogers, Laura K. and Manser, Christopher J. and Bonsor, Amy and Dennihy, Erik and Hodgkin, Simon and Kissler-Patig, Markus and Lai, Samuel and Melis, Carl and Xu, Siyi and Fusillo, Nicola Gentile and Gänsicke, Boris and Swan, Andrew and Toloza, Odette and Veras, Dimitri , month = dec, year =. Simultaneous emission from dust and gas in the planetary debris...

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2412.07647

  15. [16]

    Icarus , author =

    Radiative signatures of circumplanetary disks and envelopes during the late stages of giant planet formation , volume =. Icarus , author =. 2025 , note =. doi:10.1016/j.icarus.2024.116327 , abstract =

    arXiv 2025

  16. [17]

    Icarus , author =

    Formation and structure of circumplanetary disks and envelopes during the late stages of giant planet formation , volume =. Icarus , author =. 2024 , note =. doi:10.1016/j.icarus.2024.116044 , abstract =

    arXiv 2024

  17. [18]

    Characterizing planetary material accreted by cool helium atmosphere white dwarfs using an exponentially decaying disc model

    Characterising planetary material accreted by cool helium atmosphere white dwarfs using an exponentially decaying disc model , url =. arXiv e-prints , author =. 2025 , note =. doi:10.48550/arXiv.2503.05345 , abstract =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2503.05345 2025

  18. [19]

    Accretion

    Hartmann, Lee , month = jan, year =. Accretion

  19. [20]

    Astronomy and Astrophysics , author =

    Black holes in binary systems. Astronomy and Astrophysics , author =. 1973 , note =

    1973

  20. [21]

    The Astrophysical Journal , author =

    Magnetic. The Astrophysical Journal , author =. 2001 , note =. doi:10.1086/321658 , abstract =

    work page doi:10.1086/321658 2001

  21. [22]

    The Astrophysical Journal , author =

    Heating. The Astrophysical Journal , author =. 2004 , note =. doi:10.1086/424509 , abstract =

    work page doi:10.1086/424509 2004

  22. [23]

    The Astrophysical Journal , author =

    X-. The Astrophysical Journal , author =. 1999 , note =. doi:10.1086/307302 , abstract =

    doi:10.1086/307302 1999

  23. [24]

    The Astrophysical Journal , author =

    Ancient. The Astrophysical Journal , author =. 2010 , note =. doi:10.1088/0004-637X/722/1/725 , abstract =

    doi:10.1088/0004-637x/722/1/725 2010

  24. [25]

    The Astrophysical Journal , author =

    A. The Astrophysical Journal , author =. 2003 , note =. doi:10.1086/374036 , abstract =

    doi:10.1086/374036 2003

  25. [26]

    , volume =

    Hydromagnetic flows from accretion disks and the production of radio jets. , volume =. Monthly Notices of the Royal Astronomical Society , author =. 1982 , note =. doi:10.1093/mnras/199.4.883 , abstract =

    doi:10.1093/mnras/199.4.883 1982

  26. [27]

    , volume =

    Disk accretion by magnetic neutron stars. , volume =. The Astrophysical Journal , author =. 1978 , note =. doi:10.1086/182734 , abstract =

    doi:10.1086/182734 1978

  27. [28]

    Klacka, Jozef , month = nov, year =. The. doi:10.48550/arXiv.astro-ph/0211472 , abstract =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0211472

  28. [29]

    Monthly Notices of the Royal Astronomical Society , author =

    A road-map to white dwarf pollution: tidal disruption, eccentric grind-down, and dust accretion , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2022 , pages =. doi:10.1093/mnras/stab3009 , abstract =

    doi:10.1093/mnras/stab3009 2022

  29. [30]

    Annual Review of Astronomy and Astrophysics , author =

    Accretion onto. Annual Review of Astronomy and Astrophysics , author =. 2016 , note =. doi:10.1146/annurev-astro-081915-023347 , abstract =

    doi:10.1146/annurev-astro-081915-023347 2016

  30. [31]

    Astronomy and Astrophysics , author =

    Metal accretion scars may be common on magnetic, polluted white dwarfs , volume =. Astronomy and Astrophysics , author =. 2024 , keywords =. doi:10.1051/0004-6361/202451215 , abstract =

    work page doi:10.1051/0004-6361/202451215 2024

  31. [32]

    Astronomy and Astrophysics , author =

    Strong magnetic fields of old white dwarfs are symmetric about the stellar rotation axes , volume =. Astronomy and Astrophysics , author =. 2024 , keywords =. doi:10.1051/0004-6361/202451386 , abstract =

    work page doi:10.1051/0004-6361/202451386 2024

  32. [33]

    The Astrophysical Journal Supplement Series , author =

    A. The Astrophysical Journal Supplement Series , author =. 1992 , keywords =. doi:10.1086/191728 , abstract =

    work page doi:10.1086/191728 1992

  33. [34]

    Astronomy and Astrophysics , author =

    Accretion and diffusion in white dwarfs. Astronomy and Astrophysics , author =. 2009 , keywords =. doi:10.1051/0004-6361/200811468 , abstract =

    doi:10.1051/0004-6361/200811468 2009

  34. [35]

    The Astrophysical Journal , author =

    Polluted. The Astrophysical Journal , author =. 2019 , keywords =. doi:10.3847/1538-4357/ab0028 , abstract =

    doi:10.3847/1538-4357/ab0028 2019

  35. [36]

    Astronomy and Astrophysics , author =

    Modelling of magnetic fields of. Astronomy and Astrophysics , author =. 1998 , keywords =

    1998

  36. [37]

    Monthly Notices of the Royal Astronomical Society , author =

    Magnetic dynamos in white dwarfs -. Monthly Notices of the Royal Astronomical Society , author =. 2021 , keywords =. doi:10.1093/mnrasl/slab069 , abstract =

    work page doi:10.1093/mnrasl/slab069 2021

  37. [38]

    Huba, Joseph D , year =

  38. [39]

    Reviews in Mineralogy and Geochemistry , author =

    The evolution and delivery of rocky extra-solar materials to white dwarfs , volume =. Reviews in Mineralogy and Geochemistry , author =. 2024 , keywords =. doi:10.2138/rmg.2024.90.05 , number =

    work page doi:10.2138/rmg.2024.90.05 2024

  39. [40]

    Advances in Space Research , author =

    Magnetic fields in isolated and interacting white dwarfs , volume =. Advances in Space Research , author =. 2020 , keywords =. doi:10.1016/j.asr.2019.11.012 , number =

    doi:10.1016/j.asr.2019.11.012 2020

  40. [41]

    The Astrophysical Journal , author =

    Fast radio bursts and interstellar objects , volume =. The Astrophysical Journal , author =. 2024 , keywords =. doi:10.3847/1538-4357/ad932f , abstract =

    work page doi:10.3847/1538-4357/ad932f 2024

  41. [42]

    2008 , pages =

    The Astronomical Journal , author =. 2008 , pages =. doi:10.1088/0004-6256/135/5/1785 , abstract =

    doi:10.1088/0004-6256/135/5/1785 2008

  42. [43]

    The Astrophysical Journal , author =

    Metal. The Astrophysical Journal , author =. 2003 , keywords =. doi:10.1086/377492 , abstract =

    doi:10.1086/377492 2003

  43. [44]

    Monthly Notices of the Royal Astronomical Society , author =

    The unbiased frequency of planetary signatures around single and binary white dwarfs using. Monthly Notices of the Royal Astronomical Society , author =. 2019 , keywords =. doi:10.1093/mnras/stz1050 , abstract =

    doi:10.1093/mnras/stz1050 2019

  44. [45]

    2024 , note =

    Astronomy & Astrophysics , author =. 2024 , note =. doi:10.1051/0004-6361/202450509 , abstract =

    doi:10.1051/0004-6361/202450509 2024

  45. [46]

    The Astrophysical Journal , author =

    Exomoons as. The Astrophysical Journal , author =. 2022 , keywords =. doi:10.3847/1538-4357/ac86d5 , abstract =

    doi:10.3847/1538-4357/ac86d5 2022

  46. [47]

    Astronomy & Astrophysics , author =

    Spectroscopic analysis of. Astronomy & Astrophysics , author =. 2013 , note =. doi:10.1051/0004-6361/201322318 , abstract =

    doi:10.1051/0004-6361/201322318 2013

  47. [48]

    2015 , keywords =

    The Astrophysical Journal , author =. 2015 , keywords =. doi:10.1088/0004-637X/799/2/142 , abstract =

    doi:10.1088/0004-637x/799/2/142 2015

  48. [49]

    Monthly Notices of the Royal Astronomical Society , author =

    Binary star origin of high field magnetic white dwarfs , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2008 , keywords =. doi:10.1111/j.1365-2966.2008.13291.x , abstract =

    arXiv 2008

  49. [50]

    Monthly Notices of the Royal Astronomical Society , author =

    Magnetic fields in white dwarfs and stellar evolution , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2004 , keywords =. doi:10.1111/j.1365-2966.2004.08482.x , abstract =

    arXiv 2004

  50. [51]

    , month = jan, year =

    Shu, Frank H. , month = jan, year =. The

  51. [52]

    The Astrophysical Journal Letters , author =

    Tidal. The Astrophysical Journal Letters , author =. 2024 , keywords =. doi:10.3847/2041-8213/ad394c , abstract =

    doi:10.3847/2041-8213/ad394c 2024

  52. [53]

    The Astrophysical Journal , author =

    On the. The Astrophysical Journal , author =. 1986 , keywords =. doi:10.1086/164005 , abstract =

    doi:10.1086/164005 1986

  53. [54]

    Monthly Notices of the Royal Astronomical Society , author =

    No evidence for a strong decrease of planetesimal accretion in old white dwarfs , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2022 , keywords =. doi:10.1093/mnras/stab3446 , abstract =

    doi:10.1093/mnras/stab3446 2022

  54. [55]

    Monthly Notices of the Royal Astronomical Society , author =

    New insight into the magnetism of degenerate stars from the analysis of a volume-limited sample of white dwarfs , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2021 , keywords =. doi:10.1093/mnras/stab2046 , abstract =

    doi:10.1093/mnras/stab2046 2021

  55. [56]

    Astronomy and Astrophysics , author =

    Convective. Astronomy and Astrophysics , author =. 1971 , pages =

    1971

  56. [57]

    Monthly Notices of the Royal Astronomical Society , author =

    Genesis of magnetic fields in isolated white dwarfs , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2018 , keywords =. doi:10.1093/mnras/sty1150 , abstract =

    doi:10.1093/mnras/sty1150 2018

  57. [58]

    Astronomy & Astrophysics , author =

    Main sequence dynamo magnetic fields emerging in the white dwarf phase , volume =. Astronomy & Astrophysics , author =. 2024 , note =. doi:10.1051/0004-6361/202452539 , abstract =

    doi:10.1051/0004-6361/202452539 2024

  58. [59]

    2016 , keywords =

    The Astrophysical Journal , author =. 2016 , keywords =. doi:10.3847/0004-637X/824/1/14 , abstract =

    doi:10.3847/0004-637x/824/1/14 2016

  59. [60]

    , month = jan, year =

    Chen, Francis F. , month = jan, year =. Introduction to. doi:10.1007/978-3-319-22309-4 , keywords =

    doi:10.1007/978-3-319-22309-4

  60. [61]

    Monthly Notices of the Royal Astronomical Society , author =

    Calibration of the mixing-length theory for structures of helium-dominated atmosphere white dwarfs , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2019 , keywords =. doi:10.1093/mnras/stz2656 , abstract =

    doi:10.1093/mnras/stz2656 2019

  61. [62]

    The Astrophysical Journal , author =

    Are. The Astrophysical Journal , author =. 2002 , keywords =. doi:10.1086/340291 , abstract =

    doi:10.1086/340291 2002

  62. [63]

    Monthly Notices of the Royal Astronomical Society , author =

    Can magnetic fields suppress convection in the atmosphere of cool white dwarfs?. Monthly Notices of the Royal Astronomical Society , author =. 2018 , keywords =. doi:10.1093/mnras/stx2584 , abstract =

    doi:10.1093/mnras/stx2584 2018

  63. [64]

    The Astronomical Journal , author =

    On the. The Astronomical Journal , author =. 2024 , keywords =. doi:10.3847/1538-3881/ad3216 , abstract =

    work page doi:10.3847/1538-3881/ad3216 2024

  64. [65]

    The Astrophysical Journal Letters , author =

    A. The Astrophysical Journal Letters , author =. 2017 , keywords =. doi:10.3847/2041-8213/aa5eae , abstract =

    doi:10.3847/2041-8213/aa5eae 2017

  65. [66]

    Memorie della Societa Astronomica Italiana , author =

    White dwarf spectra and atmosphere models , volume =. Memorie della Societa Astronomica Italiana , author =. 2010 , keywords =

    2010

  66. [67]

    Astronomy & Astrophysics , author =

    New white dwarf envelope models and diffusion -. Astronomy & Astrophysics , author =. 2020 , note =. doi:10.1051/0004-6361/202037530 , abstract =

    doi:10.1051/0004-6361/202037530 2020

  67. [68]

    The Astrophysical Journal , author =

    Magnetic. The Astrophysical Journal , author =. 2025 , keywords =. doi:10.3847/1538-4357/aded8f , abstract =

    doi:10.3847/1538-4357/aded8f 2025

  68. [69]

    Monthly Notices of the Royal Astronomical Society , author =

    Long-term evolution of three-planet systems to the post-main sequence and beyond , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2014 , keywords =. doi:10.1093/mnras/stt1973 , abstract =

    doi:10.1093/mnras/stt1973 2014

  69. [70]

    Monthly Notices of the Royal Astronomical Society , author =

    On the pollution of white dwarfs by exo-. Monthly Notices of the Royal Astronomical Society , author =. 2023 , keywords =. doi:10.1093/mnras/stad2281 , abstract =

    work page doi:10.1093/mnras/stad2281 2023

  70. [71]

    Monthly Notices of the Royal Astronomical Society , author =

    Secular chaos in white dwarf planetary systems: origins of metal pollution and short-period planetary companions , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2022 , keywords =. doi:10.1093/mnras/stac1189 , abstract =

    work page doi:10.1093/mnras/stac1189 2022

  71. [72]

    2013 , keywords =

    The Astrophysical Journal Supplement Series , author =. 2013 , keywords =. doi:10.1088/0067-0049/208/1/4 , abstract =

    doi:10.1088/0067-0049/208/1/4 2013

  72. [73]

    Monthly Notices of the Royal Astronomical Society , author =

    Polluting white dwarfs with. Monthly Notices of the Royal Astronomical Society , author =. 2024 , keywords =. doi:10.1093/mnras/stae986 , abstract =

    work page doi:10.1093/mnras/stae986 2024

  73. [74]

    Astronomy & Astrophysics , author =

    Outer boundary conditions for evolving cool white dwarfs , volume =. Astronomy & Astrophysics , author =. 2012 , note =. doi:10.1051/0004-6361/201219292 , abstract =

    work page doi:10.1051/0004-6361/201219292 2012

  74. [75]

    Monthly Notices of the Royal Astronomical Society , author =

    Simultaneous emission from dust and gas in the planetary debris orbiting a white dwarf , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2025 , keywords =. doi:10.1093/mnrasl/slae117 , abstract =

    doi:10.1093/mnrasl/slae117 2025

  75. [76]

    2015 , keywords =

    The Astrophysical Journal , author =. 2015 , keywords =. doi:10.1088/0004-637X/812/1/19 , abstract =

    doi:10.1088/0004-637x/812/1/19 2015

  76. [77]

    The Astrophysical Journal , author =

    Ionization and. The Astrophysical Journal , author =. 2016 , keywords =. doi:10.3847/1538-4357/833/1/92 , abstract =

    work page doi:10.3847/1538-4357/833/1/92 2016

  77. [78]

    Astronomy and Astrophysics , author =

    Size-dependent charging of dust particles in protoplanetary disks. Astronomy and Astrophysics , author =. 2023 , keywords =. doi:10.1051/0004-6361/202346442 , abstract =

    work page doi:10.1051/0004-6361/202346442 2023

  78. [79]

    Monthly Notices of the Royal Astronomical Society , author =

    The ionization fraction in α models of protoplanetary discs , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2002 , pages =. doi:10.1046/j.1365-8711.2002.04940.x , abstract =

    arXiv 2002

  79. [80]

    Space Science Reviews , author =

    Solar. Space Science Reviews , author =. 2000 , keywords =. doi:10.1023/A:1005293132737 , abstract =

    doi:10.1023/a:1005293132737 2000

  80. [81]

    The Astrophysical Journal Supplement Series , author =

    A study of metal abundance patterns in cool white dwarfs. The Astrophysical Journal Supplement Series , author =. 1993 , keywords =. doi:10.1086/191746 , abstract =

    work page doi:10.1086/191746 1993

Showing first 80 references.