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Strong magnetic fields of old white dwarfs are symmetric about the stellar rotation axes

T0 review · 3 major / 5 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read Old, strongly magnetic white dwarfs keep their polarisation steady because their fields align with their spin axes.

desk verdict New empirical pattern is solid; the argument against slow rotation is not yet quantitative enough. read the letter →

arxiv 2411.10270 v1 pith:76NHS2G6 submitted 2024-11-15 astro-ph.SR

S. Bagnulo , J.D. Landstreet This is my paper · ORCID
classification astro-ph.SR
keywords whitedwarfsmagneticfieldspolarimetrystellarrotationfieldevolutioncrystallisationdynamodwarfmergerscircularpolarisation
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

Most magnetic white dwarfs show circular polarisation that changes as the star rotates, because the magnetic axis is tilted relative to the spin axis. The paper assembles observations of 74 magnetic white dwarfs and finds a sharp exception: among normal-mass ($M \le 1.0\,M_\odot$) white dwarfs with cooling ages older than about 2 Gyr and fields above about 10 MG, 16 of 17 show constant polarisation. The paper argues that this constancy is not evidence of rotation periods of centuries, because no white dwarf with a measured period between about two weeks and a century is known. It concludes that old, strongly magnetic normal-mass white dwarfs have fields roughly symmetric about the rotation axis, and sketches how magnetic distortion plus energy dissipation could align the magnetic axis with the angular momentum axis.

What carries the argument

The load-bearing tool is time-resolved circular spectropolarimetry: the line-of-sight component of the field, encoded in Stokes $V$, changes only if the magnetic configuration seen by the observer changes with rotation. The paper classifies 74 stars as variable, non-variable, or candidate non-variable, and uses a binomial likelihood to compare the frequency of constant polarisation across age and field-strength bins. The physical proposal for why old strong fields become axisymmetric is an asymmetric-top alignment mechanism: a strong oblique magnetic field distorts the star's shape, shifting the principal axis of maximum inertia away from the spin axis; energy dissipation then drives that principal axis toward the angular momentum axis, aligning the magnetic axis with rotation.

What would settle it

A monitoring programme with cadences and baselines long enough to detect rotation periods between about two weeks and several decades, applied to the old strong-field non-variable stars, would settle it: a substantial detection rate of periodic variation in this gap would mean their constancy had been a selection effect, while a clean null result would confirm the gap is real and the axisymmetry reading stands.

Watch

Extended reading notes

Core claim

The central discovery is an empirical pattern plus a reinterpretation. The pattern: variable polarisation is nearly universal among weakly magnetic white dwarfs of all ages and among young normal-mass white dwarfs even with strong fields, while 16 of the 17 normal-mass stars older than 2 Gyr with $\langle |B| \rangle \ge 10$ MG show constant polarisation. The reinterpretation: such constancy does not mean the star is barely rotating. The paper points to the complete absence of white dwarfs with measured periods longer than about two weeks and argues that a bimodal period distribution peaking at hours-to-days and at centuries is implausible. Instead, the field structure is approximately axisymmetric around the rotation axis, so the observed polarisation does not change as the star spins. For massive white dwarfs the same sample shows both variable and constant strong fields, possibly reflecting two formation channels or very rapid rotation.

Load-bearing premise

The conclusion depends on the absence of measured white dwarf rotation periods between about two weeks and a century being real rather than a selection effect of monitoring baselines too short to find such periods.

Editorial extensions

If this is right

  • The supposed class of century-period magnetic white dwarfs would largely disappear: constant-polarisation stars are normal rotators seen through an axisymmetric field.
  • Any successful theory of magnetic field origin and evolution in white dwarfs must explain why old, strong fields are axisymmetric while weak and young strong fields are oblique.
  • The onset of constancy near a field strength of a few megagauss and near a cooling age of 2 Gyr ties field geometry to the evolutionary state, plausibly the onset of core crystallisation.
  • Massive magnetic white dwarfs split into one group with oblique fields and another with either axisymmetric fields or sub-exposure rotation periods, pointing to at least two formation channels.

Reading between the lines

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

  • If the alignment timescale is long, a larger sample of young strong-field normal-mass white dwarfs should show a broad distribution of obliquities that narrows with cooling age; this is a test the paper's data do not yet perform.
  • The absence of periods between two weeks and a century could partly be a selection effect of short monitoring baselines; quantifying that detectability would sharpen or weaken the central argument.
  • Axisymmetric aligned fields would be expected to suppress rotational modulation of surface brightness and chemistry, so photometric variability statistics of old magnetic white dwarfs could provide an independent check of the geometry claim.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. The paper compiles new and archival spectropolarimetric observations of 74 magnetic white dwarfs and classifies each as polarimetrically variable or non-variable, using explicit criteria based on repeat circular-polarisation measurements. For normal-mass (M ≤ 1 M⊙) white dwarfs, the authors report a striking pattern: among old (cooling age > 2 Gyr) strongly magnetic (⟨|B|⟩ ≥ 10 MG) stars, 16 of 17 show constant polarisation, whereas weak-field stars of all ages and young strong-field stars are mostly variable. They argue that this constancy is not due to extremely slow rotation and interpret it as evidence that the magnetic fields of old strong-field white dwarfs are approximately symmetric about their rotation axes. They discuss possible physical mechanisms, including alignment of the magnetic axis with the rotation axis through magnetic distortion and energy dissipation, as well as a crystallisation dynamo origin, and contrast the behaviour of massive (M > 1 M⊙) white dwarfs.

Significance. If the underlying pattern is confirmed, it is an important empirical constraint on the evolution of magnetic fields in white dwarfs: it would imply that the geometry of the surface field changes systematically with cooling age and field strength, with old strong-field objects evolving toward axisymmetry. The paper brings together a large sample with homogeneous classification criteria, provides new observations of 13 stars, and includes a transparent statistical treatment of the observed fractions (Eq. 1, Table 1). The main strength is the empirical pattern itself, which does not depend on fitted models or circular reasoning. However, the title-level interpretation ('fields are symmetric about the rotation axes') is not yet secured, because the alternative that these stars are extremely slow rotators is not quantitatively excluded; the significance of the paper would remain high if it instead established upper limits on rotation periods and explicitly highlighted the ambiguity.

major comments (3)
  1. [Section 5.1, with reference to Section 3.2] The argument that constant polarisation cannot be due to extremely slow rotation is not quantitatively supported. Section 3.2 concedes that for most stars classified as 'n.v.' the observations span only months to years and that they could be variable on a timescale of decades. For a non-axisymmetric field with a rotation period between roughly one and one hundred years, the polarisation change across such baselines would generally be below the measurement precision, so the absence of detected periods in the two-week-to-century window is an expected selection effect rather than evidence against slow rotation. Section 5.1 states this absence without presenting per-object detectability limits at given polarimetric amplitudes. Please provide for each non-variable star an estimate of the longest rotation period that can be excluded at a chosen amplitude (e.g., the typical amplitude of variable magnetic white dwarfs), or a population-level simulation showing how many slow rotators with periods between two weeks and a century would have been detected in the existing epoch set. Without this, the central claim that the fields are axisymmetric about the rotation axes is not secured.
  2. [Section 4.2 and Table 2] The 16/17 statistic in Section 4.2 and in the Conclusions counts as constant at least two stars, WD 0236–269 and WD 0708–670, which are classified 'n.v.:' from only two epochs; for WD 0236–269 the non-variability is based on a remark in the discovery paper rather than on published measurements (Section 3.2, Appendix B.9). Please demonstrate the robustness of the statistic by reporting the frequency when all 'n.v.:' objects are excluded or reclassified as 'unknown', and provide in Table 2 (or an appendix) the number of epochs and the temporal baseline for each of the 17 old strong-field stars. Although excluding the two two-epoch objects would change 16/17 to 14/15, the point is that the headline statistic should be transparent about the quality of the underlying classifications.
  3. [Section 7] The Conclusions state: 'The lack of evidence for major variations of circular polarisation on any timescale longer than about two weeks suggests that the interpretation of non-variability arising from extremely long rotational periods is incorrect.' This wording overstates the case: for most of the relevant stars the longest baseline is only months to years, so a rotation period of a decade or longer would not be detected. The conclusion should be rephrased to say that no variations are detected over the available baselines and that the slow-rotation hypothesis remains viable unless quantitative period upper limits are derived.
minor comments (5)
  1. [Section 3.2] The statement that for most non-variable stars 'the observations span a time interval of up to a few months or years, [so they] could be variable on a timescale of decades' is an important limitation; it should be repeated in the abstract or conclusions so that the reader is not misled.
  2. [Section 5.2] The provisional ruling against very rapid rotation for constant massive white dwarfs cites 'Hernandez, priv. comm.; Ramsay, priv. comm.' Please replace these private communications with published TESS results or include the relevant light curves as data.
  3. [Section 6.1.1] The proposed alignment mechanism is entirely qualitative. The paper correctly notes that previous Ap-star work did not converge; please add an explicit statement that this is an untested hypothesis, not a consequence of the observations, in the abstract's summary of the mechanism.
  4. [Table 1 and Eq. (2)] For extreme fractions such as 16/17, the quoted binomial standard deviation is asymmetric in reality; a Jeffreys or beta-distribution interval would be more appropriate. This does not change the conclusions.
  5. [Appendix B.55] The comparison between the 1980 and 2019 spectra of WD 1658+440 is affected by a possible wavelength calibration issue and by Hα falling at the chip edge in 2019. This should be stated in the main text, as the classification 'n.v.:' relies on this comparison.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the core claim is an empirical pattern inferred from polarimetric monitoring, with no fitted parameter or self-citation chain forcing the conclusion.

full rationale

The paper's central claim — that 16/17 old (τ > 2 Gyr) normal-mass white dwarfs with B ≥ 10 MG show constant polarisation, interpreted as fields roughly symmetric about the rotation axis — is an observational inference, not a quantity defined in terms of itself. No equation in the paper fits a parameter and then 'predicts' the same parameter; Eq. (1) is a standard Bayesian binomial posterior used to display sampling uncertainty in the observed fractions f = NK/Ntot, and Eq. (2) is the corresponding standard deviation. The alternative explanations (extremely slow rotation, extremely fast rotation) are discussed and rejected with external arguments: the absence of measured periods longer than about 17 d is compared with the continuous period distribution of magnetic Ap/Bp stars, and the fast-rotation alternative is constrained by exposure-time and TESS photometry arguments. The paper's reliance on the authors' earlier work (e.g., Bagnulo & Landstreet 2021, 2022) supplies the age–field correlation and some classifications, but these are independent observational results with stated assumptions; they do not contain the axisymmetry conclusion. The most vulnerable step — excluding very slow rotation from the lack of detected periods between two weeks and a century — is a potential selection-effect weakness, and the authors explicitly concede that 'n.v.' stars observed only over months or years 'are actually variable on a timescale of decades' (Sect. 3.2), but this is an acknowledged limitation of the inference, not a circular reduction of the conclusion to its inputs. No uniqueness theorem from the authors is invoked, and no known result is merely renamed: 'axisymmetric' is a distinct physical hypothesis offered after ruling out alternatives. The analysis is therefore self-contained against external benchmarks as far as circularity is concerned.

Assumptions & free parameters 3 free parameters · 6 assumptions · 0 invented entities

The central claim depends on three analysis thresholds (cooling age 2 Gyr, field strengths 1 and 10 MG) and on assumptions about parameter reliability, orientation, and the interpretation of the period gap. No new physical entities are introduced.

free parameters (3)
  • Cooling age threshold = 2 Gyr
    Divides 'young' and 'old' white dwarfs in the statistical analysis (Table 1, Section 4.4). The central result, 16/17 old strong-field stars non-variable, is defined relative to this boundary.
  • Strong-field threshold = 10 MG
    Defines the 'strong fields' cell in Table 1 (B at least 10 MG). The main claim is stated for fields above this value.
  • Weak-field threshold = 1 MG
    Defines the 'weak fields' cell in Table 1 (B at most 1 MG) for comparison with strong fields.
assumptions (6)
  • domain assumption Stellar parameters (mass, age, temperature, field strength) in Table 2 are reliable as taken from O'Brien et al. (2024), Gentile Fusillo et al. (2021), and Bedard et al. (2020).
    The classification into mass, age, and field bins underpins the entire statistical analysis.
  • domain assumption Constant circular polarisation within measurement uncertainties over the observing baseline implies the magnetic field configuration seen by the observer does not change.
    This is the interpretation rule in Section 3, item 2. It assumes no variability on timescales shorter than the exposure or longer than the baseline.
  • domain assumption The rotation axes of the sample stars are randomly oriented with respect to the line of sight, so the old strong-field stars are not all viewed pole-on.
    A non-axisymmetric field viewed nearly along the rotation axis would also show little variability; the paper invokes this orientation only for WD 1105-340, implying it is rare for the other stars.
  • domain assumption The absence of measured rotation periods between about 2 weeks and a century is real, not a selection effect.
    Section 5.1 uses the period gap to rule out extremely slow rotation; if this assumption fails, non-variability could be due to slow rotation rather than axisymmetry.
  • domain assumption Magnetic braking mechanisms (dipole radiation, ISM coupling, winds) are too weak to spin down magnetic white dwarfs to periods of centuries.
    Section 5.1 argues these mechanisms are weak, supporting the elimination of the slow-rotation hypothesis.
  • ad hoc to paper The physical alignment mechanism of Section 6.1.1 is valid: magnetic distortion of the inertia tensor plus energy dissipation aligns the magnetic axis with the angular momentum axis.
    Proposed as a possible explanation for the observed symmetry. It is not load-bearing for the empirical claim itself, which stands without this mechanism.

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Cite this review

Pith. "Pith review of Strong magnetic fields of old white dwarfs are symmetric about the stellar rotation axes." pith.science (2026). https://pith.science/paper/76NHS2G6

@misc{pith2026241110270,
  author       = {Pith},
  title        = {Pith review of: Strong magnetic fields of old white dwarfs are symmetric about the stellar rotation axes},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/76NHS2G6}},
  note         = {Machine review of arXiv:2411.10270}
}
read the original abstract

Many magnetic white dwarfs exhibit a polarised spectrum that periodically varies as the star rotates because the magnetic field is not symmetric about the rotation axis. In this work, we report the discovery that while weakly magnetic white dwarfs of all ages with M < 1Mo show polarimetric variability with a period between hours and several days, the large majority of magnetic white dwarfs in the same mass range with cooling ages older than 2 Gyr and field strengths > 10 MG show little or no polarimetric variability. This could be interpreted as extremely slow rotation, but a lack of known white dwarfs with measured periods longer than two weeks means that we do not see white dwarfs slowing their rotation. We therefore suggest a different interpretation: old strongly magnetic white dwarfs do not vary because their fields are roughly symmetric about the rotation axes. Symmetry may either be a consequence of field evolution or a physical characteristic intrinsic to the way strong fields are generated in older stars. Specifically, a strong magnetic field could distort the shape of a star, forcing the principal axis of maximum inertia away from the spin axis. Eventually, as a result of energy dissipation, the magnetic axis will align with the angular momentum axis. We also find that the higher-mass strongly magnetised white dwarfs, which are likely the products of the merging of two white dwarfs, may appear as either polarimetrically variable or constant. This may be the symptom of two different formation channels or the consequence of the fact that a dynamo operating during a merger may produce diverse magnetic configurations. Alternatively, the massive white dwarfs with constant polarisation may be rotating with periods much shorter than the typical exposure times of the observations.

Figures

Figures reproduced from arXiv: 2411.10270 by the authors.

Figure 1
Figure 1. Correlations between field strength, magnetic variability, and other stellar parameters. Left panels: Field strength versus effective tempera￾ture and versus cooling age for variable and non-variable stars of [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 3
Figure 3. [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗

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Forward citations

Cited by 2 Pith papers

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Reference graph

Works this paper leans on

156 extracted references · 72 canonical work pages · cited by 2 Pith papers

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all := #1 ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....

  3. [3]

    & Wickramasinghe , D

    Achilleos , N. & Wickramasinghe , D. T. 1989, , 346, 444

    1989

  4. [4]

    T., Liebert , J., Saffer , R

    Achilleos , N., Wickramasinghe , D. T., Liebert , J., Saffer , R. A., & Grauer , A. D. 1992, , 396, 273

    1992

  5. [5]

    Angel , J. R. P. 1978, , 16, 487

    1978

  6. [6]

    Angel , J. R. P., Borra , E. F., & Landstreet , J. D. 1981, , 45, 457

    1981

  7. [7]

    Angel , J. R. P., Hintzen , P., & Landstreet , J. D. 1975, , 196, L27

    1975

  8. [8]

    Angel , J. R. P., Hintzen , P., Strittmatter , P. A., & Martin , P. G. 1974, , 190, L71

    1974

Show all 156 references
  1. [9]

    Angel , J. R. P., Illing , R. M. E., & Landstreet , J. D. 1972 a , , 175, L85

    1972

  2. [10]

    Angel , J. R. P., Illing , R. M. E., & Landstreet , J. D. 1972 b , , 175, L85

    1972

  3. [11]

    Angel , J. R. P. & Landstreet , J. D. 1970, , 162, L61

    1970

  4. [12]

    Angel , J. R. P. & Landstreet , J. D. 1971 a , , 164, L15

    1971

  5. [13]

    Angel , J. R. P. & Landstreet , J. D. 1971 b , , 165, L71

    1971

  6. [14]

    Angel , J. R. P. & Landstreet , J. D. 1972, , 178, L21

    1972

  7. [15]

    Angel , J. R. P. & Landstreet , J. D. 1974, , 191, 457

    1974

  8. [16]

    A., Kolesnikov , S

    Antonyuk , K. A., Kolesnikov , S. V., Pit , N. V., et al. 2016, Astrophysical Bulletin, 71, 475

    2016

  9. [17]

    1998, The Messenger, 94, 1

    Appenzeller , I., Fricke , K., F \"u rtig , W., et al. 1998, The Messenger, 94, 1

    1998

  10. [18]

    2004, , 423, 1081

    Aznar Cuadrado , R., Jordan , S., Napiwotzki , R., et al. 2004, , 423, 1081

    2004

  11. [19]

    D., & Folsom , C

    Bagnulo , S., Farihi , J., Landstreet , J. D., & Folsom , C. P. 2024 a , , 963, L22

    2024

  12. [20]

    & Landstreet , J

    Bagnulo , S. & Landstreet , J. D. 2018, , 618, A113

    2018

  13. [21]

    & Landstreet , J

    Bagnulo , S. & Landstreet , J. D. 2019 a , , 630, A65

    2019

  14. [22]

    & Landstreet , J

    Bagnulo , S. & Landstreet , J. D. 2019 b , , 486, 4655

    2019

  15. [23]

    & Landstreet , J

    Bagnulo , S. & Landstreet , J. D. 2020, , 643, A134

    2020

  16. [24]

    & Landstreet , J

    Bagnulo , S. & Landstreet , J. D. 2021, , 507, 5902

    2021

  17. [25]

    & Landstreet , J

    Bagnulo , S. & Landstreet , J. D. 2022, , 935, L12

    2022

  18. [26]

    D., Farihi , J., et al

    Bagnulo , S., Landstreet , J. D., Farihi , J., et al. 2024 b , , 688, L14

    2024

  19. [27]

    A., Jordan , S., O'Donoghue , D., et al

    Barstow , M. A., Jordan , S., O'Donoghue , D., et al. 1995, , 277, 971

    1995

  20. [28]

    2020, , 901, 93

    B \'e dard , A., Bergeron , P., Brassard , P., & Fontaine , G. 2020, , 901, 93

    2020

  21. [29]

    D., Bagnulo , S., Piirola , V., & Berdyugina , S

    Berdyugin , A., Landstreet , J. D., Bagnulo , S., Piirola , V., & Berdyugina , S. V. 2024, , 690, A10

    2024

  22. [30]

    Berdyugin , A. V. 1995, Astronomy Letters, 21, 695

    1995

  23. [31]

    Berdyugin , A. V. & Piirola , V. 1999, , 352, 619

    1999

  24. [32]

    V., Piirola , V., Bagnulo , S., Landstreet , J

    Berdyugin , A. V., Piirola , V., Bagnulo , S., Landstreet , J. D., & Berdyugina , S. V. 2022, , 657, A105

    2022

  25. [33]

    V., Piirola , V., Bagnulo , S., Landstreet , J

    Berdyugin , A. V., Piirola , V., Bagnulo , S., Landstreet , J. D., & Berdyugina , S. V. 2023, , 670, A2

    2023

  26. [34]

    V., Berdyugin , A

    Berdyugina , S. V., Berdyugin , A. V., & Piirola , V. 2007, , 99, 091101

    2007

  27. [35]

    Bergeron , P., Ruiz , M.-T., & Leggett , S. K. 1992, , 400, 315

    1992

  28. [36]

    & Reinsch , K

    Beuermann , K. & Reinsch , K. 2002, , 381, 487

    2002

  29. [37]

    2021, Galaxies, 9, 110

    Bisikalo , D., Sobolev , A., & Zhilkin , A. 2021, Galaxies, 9, 110

    2021

  30. [38]

    & Ginzburg , S

    Blatman , D. & Ginzburg , S. 2024, , 533, L13

    2024

  31. [39]

    P., Ferrario , L., Tout , C

    Briggs , G. P., Ferrario , L., Tout , C. A., Wickramasinghe , D. T., & Hurley , J. R. 2015, , 447, 1713

    2015

  32. [40]

    S., Burleigh , M

    Brinkworth , C. S., Burleigh , M. R., Lawrie , K., Marsh , T. R., & Knigge , C. 2013, , 773, 47

    2013

  33. [41]

    R., Jordan , S., & Schweizer , W

    Burleigh , M. R., Jordan , S., & Schweizer , W. 1999, , 510, L37

    1999

  34. [42]

    D., Fabrika , S

    Bychkov , V. D., Fabrika , S. N., & Shtol' , V. G. 1991, Pisma v Astronomicheskii Zhurnal, 17, 43

    1991

  35. [43]

    R., Schreiber , M

    Camisassa , M., Fuentes , J. R., Schreiber , M. R., et al. 2024, arXiv e-prints, arXiv:2411.02296

    2024 arXiv

  36. [44]

    E., Raddi , R., Althaus , L

    Camisassa , M. E., Raddi , R., Althaus , L. G., et al. 2022, , 516, L1

    2022

  37. [45]

    2024, arXiv e-prints, arXiv:2406.01807

    Castro-Tapia , M., Zhang , S., & Cumming , A. 2024, arXiv e-prints, arXiv:2406.01807

    2024 arXiv

  38. [46]

    H., Putney , A., & Goodrich , R

    Cohen , M. H., Putney , A., & Goodrich , R. W. 1993, , 405, L67

    1993

  39. [47]

    1988, , 231, 597

    Cropper , M. 1988, , 231, 597

    1988

  40. [48]

    F., Howarth , I

    Donati , J. F., Howarth , I. D., Jardine , M. M., et al. 2006, , 370, 629

    2006

  41. [49]

    & Landstreet , J

    Donati , J.-F. & Landstreet , J. D. 2009, , 47, 333

    2009

  42. [50]

    Downes , R. A. & Margon , B. 1983, , 95, 358

    1983

  43. [51]

    D., et al

    Dufour , P., Bergeron , P., Schmidt , G. D., et al. 2006, , 651, 1112

    2006

  44. [52]

    Efimov , I. S. 1981, Izvestiya Ordena Trudovogo Krasnogo Znameni Krymskoj Astrofizicheskoj Observatorii, 63, 118

    1981

  45. [53]

    Euchner , F., Jordan , S., Beuermann , K., Reinsch , K., & G \"a nsicke , B. T. 2006, , 451, 671

    2006

  46. [54]

    Euchner , F., Reinsch , K., Jordan , S., Beuermann , K., & G \"a nsicke , B. T. 2005, , 442, 651

    2005

  47. [55]

    N., Shtol' , V

    Fabrika , S. N., Shtol' , V. G., Valyavin , G. G., & Bychkov , V. D. 1997, Astronomy Letters, 23, 43

    1997

  48. [56]

    J., et al

    Farihi , J., Fossati , L., Wheatley , P. J., et al. 2018, , 474, 947

    2018

  49. [57]

    2024, , 529, L164

    Farihi , J., Robert , A., & Walters , N. 2024, , 529, L164

    2024

  50. [58]

    Ferrario , L., de Martino , D., & G\" a nsicke, B. T. 2015, , 191, 111

    2015

  51. [59]

    T., Bailey , J

    Ferrario , L., Vennes , S., Wickramasinghe , D. T., Bailey , J. A., & Christian , D. J. 1997, , 292, 205

    1997

  52. [60]

    2020, Advances in Space Research, 66, 1025

    Ferrario , L., Wickramasinghe , D., & Kawka , A. 2020, Advances in Space Research, 66, 1025

    2020

  53. [61]

    & Schramm , S

    Franzon , B. & Schramm , S. 2015, , 92, 083006

    2015

  54. [62]

    1993, in Astronomische Gesellschaft Abstract Series, Vol

    Friedrich , S., \"O streicher , R., & Ruder , H. 1993, in Astronomische Gesellschaft Abstract Series, Vol. 9, Astronomische Gesellschaft Abstract Series, 145

    1993

  55. [63]

    T., Rodr \' guez-Gil , P., Gentile Fusillo , N

    G \"a nsicke , B. T., Rodr \' guez-Gil , P., Gentile Fusillo , N. P., et al. 2020, , 499, 2564

    2020

  56. [64]

    2012, , 749, 25

    Garc \' a-Berro , E., Lor \'e n-Aguilar , P., Aznar-Sigu \'a n , G., et al. 2012, , 749, 25

    2012

  57. [65]

    P., Tremblay , P

    Gentile Fusillo , N. P., Tremblay , P. E., Cukanovaite , E., et al. 2021, , 508, 3877

    2021

  58. [66]

    2022, , 514, 4111

    Ginzburg , S., Fuller , J., Kawka , A., & Caiazzo , I. 2022, , 514, 4111

    2022

  59. [67]

    J., G \"a nsicke , B

    Hermes , J. J., G \"a nsicke , B. T., Kawaler , S. D., et al. 2017, , 232, 23

    2017

  60. [68]

    S., Schreiber , M

    Hernandez , M. S., Schreiber , M. R., Landstreet , J. D., et al. 2024, , 528, 6056

    2024

  61. [69]

    2017, , 836, L28

    Isern , J., Garc \' a-Berro , E., K \"u lebi , B., & Lor \'e n-Aguilar , P. 2017, , 836, L28

    2017

  62. [70]

    2003, in NATO Advanced Study Institute (ASI) Series B, Vol

    Jordan , S. 2003, in NATO Advanced Study Institute (ASI) Series B, Vol. 105, White Dwarfs, 175

    2003

  63. [71]

    & Friedrich , S

    Jordan , S. & Friedrich , S. 2002, , 383, 519

    2002

  64. [72]

    2001, , 376, 614

    Jordan , S., Schmelcher , P., & Becken , W. 2001, , 376, 614

    2001

  65. [73]

    1998, , 336, L33

    Jordan , S., Schmelcher , P., Becken , W., & Schweizer , W. 1998, , 336, L33

    1998

  66. [74]

    Kawaler , S. D. 2015, in Astronomical Society of the Pacific Conference Series, Vol. 493, 19th European Workshop on White Dwarfs, ed. P. Dufour , P. Bergeron , & G. Fontaine , 65

    2015

  67. [75]

    2020, in White Dwarfs as Probes of Fundamental Physics: Tracers of Planetary, Stellar and Galactic Evolution, ed

    Kawka , A. 2020, in White Dwarfs as Probes of Fundamental Physics: Tracers of Planetary, Stellar and Galactic Evolution, ed. M. A. Barstow , S. J. Kleinman , J. L. Provencal , & L. Ferrario , Vol. 357, 60--74

    2020

  68. [76]

    P., Vennes , S., et al

    Kawka , A., Briggs , G. P., Vennes , S., et al. 2017, , 466, 1127

    2017

  69. [77]

    & Vennes , S

    Kawka , A. & Vennes , S. 2012, , 425, 1394

    2012

  70. [78]

    Kawka , A., Vennes , S., & Thorstensen , J. R. 2004, , 127, 1702

    2004

  71. [79]

    C., Coyne , G

    Kemp , J. C., Coyne , G. V., Swedlund , S. J. J. B., & Wolstencroft , R. D. 1974, , 189, L79

    1974

  72. [80]

    C., Swedlund , J

    Kemp , J. C., Swedlund , J. B., Landstreet , J. D., & Angel , J. R. P. 1970, , 161, L77

    1970

  73. [81]

    G., Bergeron , P., & Conly , A

    Kilic , M., Kosakowski , A., Moss , A. G., Bergeron , P., & Conly , A. A. 2021, , 923, L6

    2021

  74. [82]

    2019, , 489, 3648

    Kilic , M., Rolland , B., Bergeron , P., et al. 2019, , 489, 3648

    2019

  75. [83]

    2021, , 29, 1

    Kochukhov , O. 2021, , 29, 1

    2021

  76. [84]

    Koester , D., Dreizler , S., Weidemann , V., & Allard , N. F. 1998, , 338, 612

    1998

  77. [85]

    2009, , 505, 441

    Koester , D., Voss , B., Napiwotzki , R., et al. 2009, , 505, 441

    2009

  78. [86]

    & Landolfi , M., eds

    Landi Degl'Innocenti , E. & Landolfi , M., eds. 2004, Astrophysics and Space Science Library, Vol. 307, Polarization in Spectral Lines

    2004

  79. [87]

    Landstreet , J. D. 1987, , 225, 437

    1987

  80. [88]

    Landstreet , J. D. & Angel , J. R. P. 1971, , 165, L67

    1971

  81. [89]

    Landstreet , J. D. & Angel , J. R. P. 1974, , 190, L25

    1974

  82. [90]

    Landstreet , J. D. & Bagnulo , S. 2019, , 623, A46

    2019

  83. [91]

    Landstreet , J. D. & Bagnulo , S. 2020, , 634, L10

    2020

  84. [92]

    D., Bagnulo , S., Martin , A., & Valyavin , G

    Landstreet , J. D., Bagnulo , S., Martin , A., & Valyavin , G. 2016, , 591, A80

    2016

  85. [93]

    D., Bagnulo , S., Valyavin , G., & Valeev , A

    Landstreet , J. D., Bagnulo , S., Valyavin , G., & Valeev , A. F. 2017, , 607, A92

    2017

  86. [94]

    D., Bagnulo , S., Valyavin , G

    Landstreet , J. D., Bagnulo , S., Valyavin , G. G., et al. 2012, , 545, A30

    2012

  87. [95]

    D., Villaver , E., & Bagnulo , S

    Landstreet , J. D., Villaver , E., & Bagnulo , S. 2023, , 952, 129

    2023

  88. [96]

    A., Burleigh , M

    Lawrie , K. A., Burleigh , M. R., Brinkworth , C. S., et al. 2013, in Astronomical Society of the Pacific Conference Series, Vol. 469, 18th European White Dwarf Workshop., ed. J. Krzesi \'n ski , G. Stachowski , P. Moskalik , & K. Bajan , 429

    2013

  89. [97]

    L., Bagnulo , S., Landolfi , M., & Landi Degl'Innocenti , E

    Leroy , J. L., Bagnulo , S., Landolfi , M., & Landi Degl'Innocenti , E. 1994, , 284, 174

    1994

  90. [98]

    2022, , 610, 43

    Li , G., Deheuvels , S., Ballot , J., & Ligni \`e res , F. 2022, , 610, 43

    2022

  91. [99]

    2023, , 680, A26

    Li , G., Deheuvels , S., Li , T., Ballot , J., & Ligni \`e res , F. 2023, , 680, A26

    2023

  92. [100]

    Liebert , J., Angel , J. R. P., & Landstreet , J. D. 1975, , 202, L139

    1975

  93. [101]

    Liebert , J., Angel , J. R. P., Stockman , H. S., & Beaver , E. A. 1978, , 225, 181

    1978

  94. [102]

    Liebert , J., Angel , J. R. P., Stockman , H. S., Spinrad , H., & Beaver , E. A. 1977, , 214, 457

    1977

  95. [103]

    D., Green , R

    Liebert , J., Schmidt , G. D., Green , R. F., Stockman , H. S., & McGraw , J. T. 1983, , 264, 262

    1983

  96. [104]

    D., Sion , E

    Liebert , J., Schmidt , G. D., Sion , E. M., et al. 1985, , 97, 158

    1985

  97. [105]

    A., Woudt , P

    Macfarlane , S. A., Woudt , P. A., Dufour , P., et al. 2017, , 470, 732

    2017

  98. [106]

    J., G \"a nsicke , B

    Manser , C. J., G \"a nsicke , B. T., Inight , K., et al. 2023, , 521, 4976

    2023

  99. [107]

    & Wickramasinghe , D

    Martin , B. & Wickramasinghe , D. T. 1978, , 183, 533

    1978

  100. [108]

    2008, Contributions of the Astronomical Observatory Skalnate Pleso, 38, 217

    Mathys , G. 2008, Contributions of the Astronomical Observatory Skalnate Pleso, 38, 217

    2008

  101. [109]

    Maxted , P. F. L., Ferrario , L., Marsh , T. R., & Wickramasinghe , D. T. 2000, , 315, L41

    2000

  102. [110]

    McCook , G. P. & Sion , E. M. 1977, A Catalogue of spectroscopically identified white dwarfs

    1977

  103. [111]

    McCook , G. P. & Sion , E. M. 1999, , 121, 1

    1999

  104. [112]

    1999, Stellar magnetism

    Mestel , L. 1999, Stellar magnetism

    1999

  105. [113]

    & Takhar , H

    Mestel , L. & Takhar , H. S. 1972, , 156, 419

    1972

  106. [114]

    Montgomery , M. H. & Dunlap , B. H. 2024, , 961, 197

    2024

  107. [115]

    F., Forveille , T., et al

    Morin , J., Donati , J. F., Forveille , T., et al. 2008 a , , 384, 77

    2008

  108. [116]

    F., Petit , P., et al

    Morin , J., Donati , J. F., Petit , P., et al. 2008 b , , 390, 567

    2008

  109. [117]

    2024, , 527, 10111

    Moss , A., Bergeron , P., Kilic , M., et al. 2024, , 527, 10111

    2024

  110. [118]

    W., Tremblay , P

    O'Brien , M. W., Tremblay , P. E., Gentile Fusillo , N. P., et al. 2023, , 518, 3055

    2023

  111. [119]

    W., Tremblay , P

    O'Brien , M. W., Tremblay , P. E., Klein , B. L., et al. 2024, , 527, 8687

    2024

  112. [120]

    O., Soethe , L

    Oliveira da Rosa , G., Kepler , S. O., Soethe , L. T. T., Romero , A. D., & Bell , K. J. 2024, arXiv e-prints, arXiv:2407.05214

    2024 arXiv

  113. [121]

    & Reiz , A

    Piirola , V. & Reiz , A. 1992, , 259, 143

    1992

  114. [122]

    Preston , G. W. 1971, , 83, 571

    1971

  115. [123]

    1995, , 451, L67

    Putney , A. 1995, , 451, L67

    1995

  116. [124]

    1997, , 112, 527

    Putney , A. 1997, , 112, 527

    1997

  117. [125]

    & Jordan , S

    Putney , A. & Jordan , S. 1995, , 449, 863

    1995

  118. [126]

    S., Hermes , J

    Reding , J. S., Hermes , J. J., Vanderbosch , Z., et al. 2020, , 894, 19

    2020

  119. [127]

    J., & Hopp , U

    Reimers , D., Hagen , H. J., & Hopp , U. 1999, , 343, 157

    1999

  120. [128]

    1996, , 311, 572

    Reimers , D., Jordan , S., Koester , D., et al. 1996, , 311, 572

    1996

  121. [129]

    D., Bergeron , P., & Fegley , B

    Schmidt , G. D., Bergeron , P., & Fegley , B. 1995, , 443, 274

    1995

  122. [130]

    D., Liebert , J., Harris , H

    Schmidt , G. D., Liebert , J., Harris , H. C., Dahn , C. C., & Leggett , S. K. 1999, , 512, 916

    1999

  123. [131]

    Schmidt , G. D. & Norsworthy , J. E. 1991, , 366, 270

    1991

  124. [132]

    Schmidt , G. D. & Smith , P. S. 1994, , 423, L63

    1994

  125. [133]

    Schmidt , G. D. & Smith , P. S. 1995, , 448, 305

    1995

  126. [134]

    D., Vennes , S., Wickramasinghe , D

    Schmidt , G. D., Vennes , S., Wickramasinghe , D. T., & Ferrario , L. 2001, , 328, 203

    2001

  127. [135]

    D., West , S

    Schmidt , G. D., West , S. C., Liebert , J., Green , R. F., & Stockman , H. S. 1986, , 309, 218

    1986

  128. [136]

    R., Belloni , D., G \"a nsicke , B

    Schreiber , M. R., Belloni , D., G \"a nsicke , B. T., Parsons , S. G., & Zorotovic , M. 2021, Nature Astronomy [ [arXiv] 2104.14607 ]

    2021 arXiv

  129. [137]

    2021, , 906, 53

    Schwab , J. 2021, , 906, 53

    2021

  130. [138]

    V., & Bagnulo , S

    Siebenmorgen , R., Voshchinnikov , N. V., & Bagnulo , S. 2014, , 561, A82

    2014

  131. [139]

    M., Liebert , J., Schmidt , G., & Starrfield , S

    Sion , E. M., Liebert , J., Schmidt , G., & Starrfield , S. G. 1984, in Bulletin of the American Astronomical Society, Vol. 16, 725

    1984

  132. [140]

    Spruit , H. C. 1999, , 349, 189

    1999

  133. [141]

    Stibbs , D. W. N. 1950, , 110, 395

    1950

  134. [142]

    B., Wolstencroft , R

    Swedlund , J. B., Wolstencroft , R. D., Michalsky , Jr., J. J., & Kemp , J. C. 1974, , 187, L121

    1974

  135. [143]

    A., Wickramasinghe , D

    Tout , C. A., Wickramasinghe , D. T., Liebert , J., Ferrario , L., & Pringle , J. E. 2008, , 387, 897

    2008

  136. [144]

    2005, , 439, 1099

    Valyavin , G., Bagnulo , S., Monin , D., et al. 2005, , 439, 1099

    2005

  137. [145]

    A., Bagnulo , S., et al

    Valyavin , G., Wade , G. A., Bagnulo , S., et al. 2008, , 683, 466

    2008

  138. [146]

    2018, Contributions of the Astronomical Observatory Skalnate Pleso, 48, 307

    Vennes , S., Kawka , A., Ferrario , L., & Paunzen , E. 2018, Contributions of the Astronomical Observatory Skalnate Pleso, 48, 307

    2018

  139. [147]

    D., Ferrario , L., et al

    Vennes , S., Schmidt , G. D., Ferrario , L., et al. 2003, , 593, 1040

    2003

  140. [148]

    V., Berdyugin , A

    Vornanen , T., Berdyugina , S. V., Berdyugin , A. V., & Piirola , V. 2010, , 720, L52

    2010

  141. [149]

    R., et al

    Walters , N., Farihi , J., Marsh , T. R., et al. 2021, , 503, 3743

    2021

  142. [150]

    1977, , 48, 27

    Wegner , G. 1977, , 48, 27

    1977

  143. [151]

    D., et al

    Wesemael , F., Liebert , J., Schmidt , G. D., et al. 2001, , 554, 1118

    2001

  144. [152]

    West , S. C. 1989 a , , 345, 511

    1989

  145. [153]

    West , S. C. 1989 b , , 345, 511

    1989

  146. [154]

    Wickramasinghe , D. T. & Bessell , M. S. 1976, , 203, L39

    1976

  147. [155]

    Wickramasinghe , D. T. & Cropper , M. 1988, , 235, 1451

    1988

  148. [156]

    2024, , 963, 26

    Zhong , Y., Kashiyama , K., Takasao , S., Shigeyama , T., & Fujisawa , K. 2024, , 963, 26

    2024

Pith tools

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