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First monitoring campaign of a Main-sequence Radio Pulse emitter: the case of CU Vir

T0 review · 3 major / 6 minor · reviewed 2026-08-15 · deepseek-v4-flash

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Pith's one-line read A 36-epoch radio monitoring campaign of the magnetic star CU Vir shows that its two periodic pulses have frequency-dependent variability that differs by pulse type, establishing that electron cyclotron maser emission from Main-sequence…

desk verdict First dense monitoring campaign of an MRP, with a likely real but imperfectly controlled leading-vs-trailing variability difference; deserves peer review with a request for epoch-set controls and data release. read the letter →

arxiv 2608.00968 v1 pith:2ZBW2HGI submitted 2026-08-02 astro-ph.SR

Barnali Das , Hayley Bignall , Andrew Zic , Poonam Chandra , Joshua Pritchard , John Morgan , Ankita Ghosh , Bhaswati Bhattacharyya
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George Hobbs
This is my paper · ORCID
classification astro-ph.SR
keywords electroncyclotronmaseremissionCUVirmagnetichotstarsradiopulsemonitoringvariabilityindexcoherentstellarrotationperiodcentrifugalbreakout
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper reports the first dedicated monitoring campaign of a Main-sequence Radio Pulse emitter (MRP), observing CU Vir at 36 epochs across 1–3 GHz to see how its rotation-locked radio pulses change over time. The central claim is that the two nearly 100% circularly polarized pulses emitted each rotation cycle behave differently: the 'leading' pulse is more variable at every frequency, with a debiased variability index falling from about 0.60 at 1.5 GHz to 0.45 at 2.3 GHz, while the 'trailing' pulse's index rises from about 0.25 at 1.8 GHz to 0.40 at 2.7 GHz. The campaign also discovers that pulse arrival phases jitter by up to 0.014 rotation cycle (about 10 minutes) and that the pulses drift systematically later in phase, which lets the authors refine CU Vir's rotation period to 0.5206882 days. If these results hold, the variability of coherent magnetospheric radio emission is structured, pulse-type dependent, and measurable with a modest number of pulses: the paper estimates that about 30 pulses suffice to build a stable average profile. A sympathetic reader would care because MRP temporal properties have been nearly unexplored, and monitorable variability would turn electron cyclotron maser emission into a dynamical probe of stellar magnetospheres rather than a one-epoch snapshot.

What carries the argument

The central object is the debiased variability index $V_{\rm rms}^{\rm debiased} = \frac{1}{\langle S\rangle}\sqrt{\sigma_{\rm signal}^{2} - \sigma_{\rm noise}^{2}}$, computed per 128 MHz sub-band from peak Stokes V flux densities over a common set of epochs; it converts epoch-to-epoch scatter into a frequency-resolved measure of pulse instability. A companion simulation uses spectra of the form $S(\nu,t)=\nu^{\alpha}\left(S_0+S_1\sin\tilde{t}\right)\exp(-\delta(\nu,t))$, with $\delta$ drawn from a Gaussian whose width depends on frequency, to show how a stable underlying spectral shape can survive strong frequency-dependent variability. The analysis also leans on a correlation between fluence and peak flux density, which lets peak flux stand in for pulse energy, and on cross-correlation alignment of pulses across epochs, which is necessary because of the newly discovered phase jitter.

What would settle it

Recompute the debiased variability indices from all 36 epochs after relaxing the phase-window filter, or restrict the comparison to epochs where both pulses are fully covered at identical frequencies; if the leading-pulse excess vanishes, the claimed pulse-type difference is an artifact of epoch selection. A second test is to run the same monitoring on an MRP with a near-axisymmetric magnetic field: the centrifugal-breakout explanation predicts a much smaller leading-versus-trailing variability gap for such a star.

Watch

Extended reading notes

Core claim

The paper's central discovery is that the two radio pulses of CU Vir, both produced in the same magnetic hemisphere, have statistically distinct, frequency-dependent variability. Using the debiased variability index computed from peak circularly polarized (Stokes V) flux densities on a common set of 12 epochs, the authors find that the leading pulse is more variable throughout the entire 1–3 GHz band: its variability index decreases from about 0.60 at 1.5 GHz to 0.45 at 2.3 GHz, whereas the trailing pulse's index increases from about 0.25 at 1.8 GHz to 0.40 at 2.7 GHz. They argue that this pattern cannot be produced by interstellar scintillation or by random emission-site instability alone, because neither would single out one pulse. Instead, they propose that centrifugal breakout events around the magnetic equator cause correlated fluctuations across frequencies, while an additional frequency-dependent instability, stronger for the leading pulse, shapes the observed trends. Supporting results are the discovery of arrival-phase jitter up to 0.014 rotation cycle, a refined rotation period of 0.5206882 days indicating a spin-up between 2008 and 2024, and an estimate that roughly 30 pulses are needed to extract a global pulse profile.

Load-bearing premise

The load-bearing premise is that the 12 epochs used for the time-averaged spectra and variability indices represent the full 36-epoch campaign; many epochs were dropped because the adopted ephemeris placed the pulse peak outside the observing window, and if those excluded epochs had systematically different pulse amplitudes or shapes, the measured leading-versus-trailing difference could be an artifact of which epochs survived the filter.

Editorial extensions

If this is right

  • The long-known intermittency of CU Vir's leading pulse at 13 cm is not an on/off switch in the emission but a broadband suppression: a lower break frequency plus higher variability makes that pulse fall below sensitivity at 2.5 GHz more often than the trailing pulse does.
  • Pulse timing of MRPs must now budget for arrival-phase jitter of order 0.014 rotation cycle, and a constant rotation period of 0.5206882 days aligns both the 2019 and 2024 observations without evidence of period evolution between them.
  • A stable global pulse profile for either pulse can be built from about 30 pulses, meaning that dedicated monitoring campaigns of MRPs are feasible with less than 100 hours of telescope time per star.
  • Characteristic spectral shapes, such as a broken power law with break frequency near 2 GHz for the leading pulse and near 2.4 GHz for the trailing pulse, remain recoverable from modest sample sizes even when variability is strong and frequency-dependent.
  • The frequency trend of the variability index can diagnose the spatial structure of emission sites: the trailing pulse's rising index toward higher frequencies is consistent with fewer, smaller emission sites closer to the magnetic poles, where local fluctuations average out less.

Reading between the lines

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

  • If the leading-versus-trailing asymmetry is caused by the oblique magnetosphere's azimuthally asymmetric plasma distribution, then MRPs with nearly axisymmetric fields should show a smaller variability gap between their two pulses; a multi-star monitoring comparison would test this directly.
  • The paper's estimate that about 30 pulses suffice is, by its own caveats, a lower bound: at frequencies where the variability index is higher, more pulses will be needed to reach the same profile stability.
  • A longer campaign reaching sub-GHz frequencies could resolve the giant-pulse question: with only two sub-GHz epochs, the paper cannot tell whether the 2019 giant pulse was a rare event or a sign of intrinsically wider flux-density ranges at low frequencies.
  • Because phase jitter and flux-density variability are measured from the same lightcurves, a within-pulse multi-frequency correlation analysis could separate geometric beaming shifts from intensity changes at the emission site.
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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 / 6 minor

Summary. The paper reports the first dedicated multi-epoch radio monitoring of a Main-sequence Radio Pulse emitter, CU Vir, using ATCA at 36 epochs over 1–3 GHz. The central claim is that the debiased variability index of the leading pulse is significantly higher than that of the trailing pulse throughout the observed band, with opposite frequency trends (leading decreasing from ~0.60 at 1.5 GHz to ~0.45 at 2.3 GHz; trailing increasing from ~0.25 at 1.8 GHz to ~0.40 at 2.7 GHz). Supporting results include pulse arrival-phase jitter up to 0.014 rotation cycle, a refined rotation period of 0.5206882 days, a re-interpretation of the historically intermittent 13 cm leading pulse as a broadband phenomenon, and an estimate that ~30 pulses suffice to construct a global pulse template. The analysis uses a common-epoch constraint within each pulse across frequencies, debiased variability indices with Monte Carlo uncertainties, and a constant-sky-model calibration strategy.

Significance. If the variability-index result is robust, this is the first quantitative, epoch-resolved characterization of pulse-to-pulse variability for an MRP, and it would demonstrate that pulses originating from the same magnetic hemisphere can exhibit statistically different temporal fluctuation properties. This would provide new observational constraints on ECME stability, centrifugal breakout events, and the utility of MRPs as magnetospheric probes. The dataset itself is valuable: 36 epochs over 1–3 GHz is unprecedented for this class. The paper is careful in several respects: it applies a common epoch set across frequencies for each pulse, computes debiased variability indices with Monte Carlo uncertainties, cross-checks against historical VLA spectra, and explicitly lists caveats in the global-template estimate (§5.2). The simulation in §4.3 is clearly labeled as illustrative rather than a quantitative fit. These strengths make the paper a useful contribution if the central comparison can be placed on firmer statistical footing.

major comments (3)
  1. [§4.2 / Figure 6 / Table A1] The headline comparison of debiased variability indices for the leading and trailing pulses is made on two disjoint, seasonally clustered sets of 12 epochs each. The common-epoch constraint is applied within each pulse across frequencies, but not across pulse types: Table A1 shows leading-pulse epochs cluster in April, June, and August–September, while trailing-pulse epochs cluster in April–May, July, and September. Any epoch-dependent systematic—unmodeled calibration gain errors, ionospheric effects, or interstellar scintillation on timescales of days to weeks—will contribute differently to the two second-moment statistics. The dismissal in §5 that scintillation 'should not distinguish between the leading and trailing pulses' assumes the two epoch ensembles are statistically identical, which is not demonstrated and is doubtful given the seasonal separation. Please quantify this risk: either compute the variability indices using a matched set of epochs (e.g., only epochs in the overlapping months, if sufficient) or demonstrate that the off-pulse noise, calibrator gain stability, and scintillation statistics are consistent between the two epoch sets.
  2. [§4.2 / Abstract] The abstract states that the paper finds 'significant differences in the variability indices exhibited by the two pulses as a function of frequencies,' but no formal statistical test of the difference is reported. The Monte Carlo error bars in Figure 6 are a good start, but the paper never states the numerical difference and its uncertainty at any common frequency, nor provides a p-value or a permutation test that respects the disjoint epoch structure. Since the leading and trailing indices are measured from different epochs and partly different frequency ranges, a simple error-bar comparison may be misleading. Please report, at each frequency bin where both pulses are measured (1.8–2.3 GHz), the difference ΔV = V_leading − V_trailing with its uncertainty, and perform a test that accounts for the epoch sampling (e.g., a bootstrap or permutation test).
  3. [§4.1.2 / §4.2 (selection step)] The variability indices and average spectra are computed only from epochs in which the pulse peak fell inside the observing window (after visually identifying the covered frequencies in §4.2 step 1). This selection is not independent of the scientific variables: the adopted ephemeris is known to be inaccurate (§4), and the pulses systematically shift to later phases during the campaign (§4.1.1). Thus the 12 surviving epochs for each pulse are the result of an observational filter tied to the same phase drift that is a target of the analysis. If the excluded partial-coverage sessions had systematically different peak flux densities or pulse shapes, the measured variability difference could be an artifact of which sessions survived. Please show that the peak flux densities of the excluded epochs are statistically consistent with those of the included ones (e.g., by including partially covered epochs with an appropriate treatment of the missing frequencies), or discuss explicitly the direction and magnitude of the potential selection bias.
minor comments (6)
  1. [Abstract / §4.2] The phrase 'throughout our observing band' overstates the frequency overlap: the leading pulse is measured over 1.3–2.3 GHz and the trailing pulse over 1.8–2.7 GHz, so the direct comparison covers only the 1.8–2.3 GHz range. Please rephrase to 'at all common frequencies' or similar.
  2. [§4.1.1 / Figure 2] The phase-jitter claim of 0.014 rotation cycle is based on a visual comparison of falling edges at a small number of epochs. A quantitative estimate of the jitter distribution (e.g., the rms of arrival-time residuals after removing the linear drift shown in Figure 9) would strengthen this discovery claim. Also, the text says the right panel shows 'three consecutive days,' but Table A1 lists 2024-08-30, 08-31, 09-01, and 09-02 as consecutive; please specify the exact epochs shown.
  3. [§4.1.2 / Figure 3] The fluence–peak-flux-density slopes are reported as 1.44±0.05 for the leading pulse and 1.12±0.08 for the trailing pulse and are called 'near identical.' These values differ by about 3σ; please discuss whether this difference is physically meaningful or a statistical fluctuation.
  4. [§4.3] The simulation is explicitly not a fit, and the text would be more accurate if it said the model 'illustrates' rather than 'demonstrates' how the frequency dependence of the variability index could constrain instability mechanisms. As written, 'demonstrates' overstates the evidential weight of a model with chosen functional forms and free constants.
  5. [Table 1] The reduced χ² values of 3.0 (ATCA leading) and 6.5 (ATCA trailing) indicate that the broken power-law model formally does not describe the average spectra within the quoted uncertainties. This is relevant for the derived break frequencies used in §5.1 and for the claim of a 'characteristic spectral shape.' Please comment on the fit quality and consider whether underestimated errors or a different model form are needed.
  6. [§3] The paper states that the flux/bandpass calibrator 1934–638 was used at all but four epochs, where 0823–500 was used instead, but it never identifies which four epochs. Since the variability analysis may be sensitive to a change in the absolute flux scale, please list those epochs (or state that none of them fall in the 12-epoch subsets used for the variability indices).

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the central variability result is an empirical measurement from new observations, and the illustrative simulation and timing fits are not presented as predictions derived from their own outputs.

full rationale

The paper's central claims are empirical measurements from a new 36-epoch ATCA campaign. The debiased variability index (Eq. 3) is computed directly from measured peak flux densities, and the leading-versus-trailing comparison is not derived from any assumed spectral shape or from the simulation. The rotation period in Section 5.3 is obtained by a standard timing fit: the slope of arrival phase versus epoch is minimized by varying the period, and the quoted value 0.5206882 days is presented as a fitted result with uncertainties, not as a prediction independent of the arrival-phase data. Showing flat residuals after applying the fitted period is self-consistent, but it is not circular because the paper does not claim this flatness as an independent test. The Section 4.3 simulation is explicitly illustrative: the text states 'we do not attempt to reproduce the observed spectral properties quantitatively,' and the simulated spectra are generated from arbitrary functional forms rather than fitted to the data. Self-citations (Das & Chandra 2021; Morgan et al. 2026) are used for physical interpretation and background, not as load-bearing evidence for the measured variability difference or the derived period. The epoch-selection and common-epoch-set choices are legitimate data-representativeness concerns, but they are not instances of a result reducing to its own inputs by construction. Therefore no circular step can be exhibited with the required specificity.

Assumptions & free parameters 3 free parameters · 4 assumptions · 0 invented entities

The paper's central measurements rest on standard radio-calibration assumptions and the prior characterization of CU Vir's ECME as approximately 100% circularly polarized. The main fitted physical parameter is the rotation period P0, which is itself an output rather than an external input. The illustrative simulation in §4.3 introduces hand-chosen constants but is not used to fit the data.

free parameters (3)
  • Rotation period P0 = 0.5206882 days
    Determined by varying the period between 0.520662 and 0.52071721 days to minimize the slope of arrival phase versus epoch; used as the refined rotation period for CU Vir in §5.3.
  • Broken power-law fit parameters (A, nu_b, alpha1, alpha2) = ATCA leading: A=8.6, nu_b=1.86 GHz, alpha1=-0.72, alpha2=-2.5; other rows in Table 1
    Fitted to average spectra via Eq. 2 to compare ATCA and VLA spectral shapes; descriptive, not central to variability results.
  • Simulation constants in §4.3 = S0=10 mJy, S1=1.5 mJy, alpha=-1, sigma=0.3(nu/nu0) or 0.7(nu0/nu)
    Hand-chosen inputs for the illustrative simulation; not fitted to data, only used to demonstrate possible variability-index trends.
assumptions (4)
  • domain assumption Stokes V effectively traces the ECME pulses because they are approximately 100% circularly polarized at 1-3 GHz.
    Invoked throughout §4 to justify using Stokes V lightcurves; based on previous observations (Trigilio et al. 2000; Das & Chandra 2021), not re-derived here.
  • domain assumption The rotational phase of pulse emission is stable aside from period evolution and jitter, so arrival-phase trends measure period changes.
    Explicitly assumed in §5.3 ('Assuming that the pulse emitting regions are stable'); if false, the refined rotation period could absorb secular drift of the emission region.
  • domain assumption The 12-epoch common subset used for average spectra and variability indices is representative of the full campaign.
    Needed for the leading/trailing variability comparison in §4.2; partial-coverage epochs were excluded, and representativeness is not demonstrated.
  • ad hoc to paper The toy model in §4.3 (Eq. 6) adequately represents possible correlated plus frequency-dependent variability.
    Chosen to illustrate that variability-index trends can be produced by a frequency-dependent instability; not derived from magnetospheric physics and not quantitatively fitted.

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Cite this review

Pith. "Pith review of First monitoring campaign of a Main-sequence Radio Pulse emitter: the case of CU Vir." pith.science (2026). https://pith.science/paper/2ZBW2HGI

@misc{pith2026260800968,
  author       = {Pith},
  title        = {Pith review of: First monitoring campaign of a Main-sequence Radio Pulse emitter: the case of CU Vir},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/2ZBW2HGI}},
  note         = {Machine review of arXiv:2608.00968}
}
abstract

CU Vir, a magnetic hot star, is the first discovered Main-sequence Radio Pulse emitter (MRP) characterized by its ability to produce periodic radio pulses via electron cyclotron maser emission. Although significant advancements have been made in understanding MRPs, their temporal properties remain mostly unexplored. To overcome this limitation, we conducted a pilot study with the Australia Telescope Compact Array, in which we observed pulses from CU Vir at 36 epochs over $1-3$ GHz. In this frequency range, CU Vir produces two $\approx 100\%$ circularly polarized pulses, called `leading' and `trailing' pulses per rotation period. We find significant differences in the variability indices exhibited by the two pulses as a function of frequencies, with the leading pulse showing higher variability throughout our observing band. This result could be explained in the scenario of centrifugal breakout events in the magnetosphere of an oblique rotator causing correlated fluctuations across frequencies, along with intrinsic instabilities associated with coherent emission. In addition, we discover jittering in the arrival phases of pulses that must be considered in future monitoring campaigns. The pulses also exhibit a systematic shift to later arrival times during the course of our observing campaign, allowing us to refine the rotation period to $0.5206882$ days. Finally, we estimate that $\sim 30$ pulses will be needed to extract global pulse properties for the leading or trailing pulses. This relatively small number strongly motivates more extensive monitoring campaigns of MRPs, both to validate our results, and also to pinpoint the origin of the observed temporal variations.

Figures

Figures reproduced from arXiv: 2608.00968 by the authors.

Figure 1
Figure 1. Dynamic spectra (Stokes V) at four epochs, the time resolution is 1 minute and the spectral resolution is 5 MHz. The epochs in the top panel correspond to the leading pulse and those in the bottom panel correspond to the trailing pulse [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Left and Middle: Comparison of the pulse arrival times for the leading (1.4 GHz) and trailing (2.5 GHz) respectively at two epochs separated by similar timescales. Right: Comparison of the pulse arrival windows for the leading pulse at 1.4 GHz on three consecutive days demonstrating the pulse arrival times ‘jitter’. coverage at the lower half of the band for a number of epochs. In order to maximize the number of epo… view at source ↗
Figure 3
Figure 3. Variation of the fluence (Eq. 1) with peak flux densities at different epochs for the leading (Left) and the trailing (Right) pulses. Note that we have converted the rotational phase bins to time-bins to use a more conventional unit for fluence. This exercise establishes the fact that the peak flux density and the fluence are positively correlated so that one can be used as a proxy for the other. This allows us to u… view at source ↗
Figures from the paper (6 more)
Figure 4
Figure 4. Figure 4: Pulse profiles obtained by stacking lightcurves for the different observing epochs. The Left and the Right panels correspond to the leading and trailing pulses respectively. For the leading pulse profile, 15 pulses were stacked and for the trailing pulse, 13 pulses wer…
Figure 5
Figure 5. Figure 5: Comparison among the peak flux density spec￾tra (Stokes V) observed at different epochs. The top and bottom panels correspond to the leading and trailing pulses respectively. The red shaded regions mark the spectra at individual epochs (the width of the shaded regions …
Figure 6
Figure 6. Figure 6: Epoch to epoch variation of the peak flux density spectra. The debiased variability indices are calculated using Eq. 3 (§4.2). epochs where the pulses at 2.5 GHz were not detected. Thus, the past observations of the disappearance of the leading pulse at 13 cm is actual…
Figure 7
Figure 7. Figure 7: Simulated spectra and the corresponding variability indices. Left panels correspond to a scenario in which the intrinsic instability increases with increasing frequency and the right panels correspond to a scenario in which the instability decreases with increasing fre…
Figure 8
Figure 8. Figure 8: Correlation strength vs the number of pulses averaged for the leading (Left) and the trailing (Right) pulses. For details, see §5.2. The dashed vertical lines mark the knees of the curves (came out to be identical for either distribution) [PITH_FULL_IMAGE:figures/full…
Figure 9
Figure 9. Figure 9: Top: Relative arrival phases calculated using the variable period ephemeris of Z. Mikul´aˇsek et al. (2011) for the pulses observed in our ATCA campaign in 2024, along with that observed by B. Das & P. Chandra (2021) on 2019–06–12 (leftmost data points) with the VLA. F…

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Reference graph

Works this paper leans on

211 extracted references · 24 canonical work pages

  1. [1]

    arXiv e-prints , keywords =

    The Measurement of Polarization in Radio Astronomy. arXiv e-prints , keywords =

  2. [2]

    , keywords =

    Discoveries of Fine Structures and Secondary Pulses in Coherent Radio Emission from a Magnetic Massive Star. , keywords =. doi:10.3847/1538-4357/aded88 , archivePrefix =. 2507.03882 , primaryClass =

    arXiv

  3. [3]

    , keywords =

    The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package. , keywords =. doi:10.3847/1538-4357/ac7c74 , archivePrefix =. 2206.14220 , primaryClass =

    arXiv

  4. [4]

    The effect of interstellar scattering on coherent radio emission from stars: the case of CU Vir. , doi =

  5. [6]

    Science , keywords =

    A massive helium star with a sufficiently strong magnetic field to form a magnetar. Science , keywords =. doi:10.1126/science.ade3293 , archivePrefix =. 2308.08591 , primaryClass =

    arXiv

  6. [7]

    , keywords =

    X-ray emission from Ap-Bp stars: a magnetically confined wind-shock model for IQ Aur. , keywords =

  7. [8]

    High Energy Phenomena in Massive Stars , year = 2010, editor =

    Non-Thermal Radio Emission from Late B and Early A-type Magnetically Peculiar Stars. High Energy Phenomena in Massive Stars , year = 2010, editor =

    2010

  8. [9]

    , keywords =

    A scaling relationship for non-thermal radio emission from ordered magnetospheres: from the top of the main sequence to planets. , keywords =. doi:10.1093/mnras/stab2168 , archivePrefix =. 2107.11995 , primaryClass =

    arXiv

Show all 211 references
  1. [10]

    Magnetic field evolution, mass-loss quenching, and magnetic braking

    The effects of surface fossil magnetic fields on massive star evolution: I. Magnetic field evolution, mass-loss quenching, and magnetic braking. , keywords =. doi:10.1093/mnras/stz772 , archivePrefix =. 1902.09333 , primaryClass =

    1902 arXiv

  2. [11]

    arXiv e-prints , keywords =

    Magnetic Interaction in White Dwarf Binaries as Mechanism for Long-Period Radio Transients. arXiv e-prints , keywords =. doi:10.48550/arXiv.2409.05978 , archivePrefix =. 2409.05978 , primaryClass =

    doi arXiv

  3. [12]

    The crucial influence of rotation on the radio magnetospheres of hot stars

    MOBSTER - VI. The crucial influence of rotation on the radio magnetospheres of hot stars. , keywords =. doi:10.1093/mnras/stac136 , archivePrefix =. 2201.05512 , primaryClass =

    arXiv

  4. [13]

    , keywords =

    Centrifugal breakout reconnection as the electron acceleration mechanism powering the radio magnetospheres of early-type stars. , keywords =. doi:10.1093/mnras/stac341 , archivePrefix =. 2202.05449 , primaryClass =

    arXiv

  5. [14]

    , keywords =

    A Weak Coronal Heating Event Associated with Periodic Particle Acceleration Episodes. , keywords =. doi:10.3847/1538-4357/ab3a94 , archivePrefix =. 1902.10426 , primaryClass =

    1902 arXiv

  6. [15]

    Astronomical Data Analysis Software and Systems XVI , year = 2007, editor =

    CASA Architecture and Applications. Astronomical Data Analysis Software and Systems XVI , year = 2007, editor =

    2007

  7. [16]

    , keywords =

    Outstanding X-ray emission from the stellar radio pulsar CU Virginis. , keywords =. doi:10.1051/0004-6361/201833492 , archivePrefix =. 1808.02367 , primaryClass =

    arXiv

  8. [17]

    , keywords =

    The auroral radio emission of the magnetic B-type star -=OphC. , keywords =. doi:10.1093/mnrasl/slaa157 , archivePrefix =. 2009.02363 , primaryClass =

    2009 arXiv

  9. [18]

    , keywords =

    A Young Radio-emitting Magnetic B Star in the Rho Ophiuchi Cloud. , keywords =. doi:10.1086/166979 , adsurl =

    doi

  10. [19]

    10.1051/0004-6361/201834937

    HST/STIS analysis of the first main sequence pulsar CU Virginis , DOI= "10.1051/0004-6361/201834937", url= "https://doi.org/10.1051/0004-6361/201834937", journal =

    doi

  11. [20]

    , keywords =

    Unravelling the complex magnetosphere of the B star HD 133880 via wideband observation of coherent radio emission. , keywords =. doi:10.1093/mnras/staa2499 , archivePrefix =. 2008.07170 , primaryClass =

    2008 arXiv

  12. [21]

    , keywords =

    VAST: An ASKAP Survey for Variables and Slow Transients. , keywords =. doi:10.1017/pasa.2012.006 , archivePrefix =. 1207.1528 , primaryClass =

    2012 arXiv

  13. [22]

    , keywords =

    A combined multiwavelength VLA/ALMA/Chandra study unveils the complex magnetosphere of the B-type star HR5907. , keywords =. doi:10.1093/mnras/sty244 , archivePrefix =. 1801.08738 , primaryClass =

    arXiv

  14. [23]

    arXiv e-prints , keywords =

    The Sydney Radio Star Catalogue: properties of radio stars at megahertz to gigahertz frequencies. arXiv e-prints , keywords =. doi:10.48550/arXiv.2404.07418 , archivePrefix =. 2404.07418 , primaryClass =

    doi arXiv

  15. [24]

    , keywords =

    Fast Gyrosynchrotron Codes. , keywords =. doi:10.1088/0004-637X/721/2/1127 , adsurl =

    doi

  16. [25]

    , keywords =

    Activity in A-type stars. , keywords =. doi:10.1093/mnras/stt322 , adsurl =

    doi

  17. [26]

    arXiv e-prints , keywords =

    Spots and flares in hot main sequence stars. arXiv e-prints , keywords =

  18. [27]

    , keywords =

    Centrifugal Breakout of Magnetically Confined Line-driven Stellar Winds. , keywords =. doi:10.1086/503382 , archivePrefix =. astro-ph/0601193 , primaryClass =

    arXiv

  19. [28]

    Journal of Geophysical Research (Space Physics) , keywords =

    Loss cone-driven cyclotron maser instability. Journal of Geophysical Research (Space Physics) , keywords =. doi:10.1002/2013JA019298 , adsurl =

    doi

  20. [29]

    , keywords =

    Electron-cyclotron maser emission from white dwarf pairs and white dwarf planetary systems. , keywords =. doi:10.1111/j.1365-2966.2004.07363.x , archivePrefix =. astro-ph/0302583 , primaryClass =

    2004

  21. [30]

    Handbook of Exoplanets , year = 2018, editor =

    Radio Emission from Ultracool Dwarfs. Handbook of Exoplanets , year = 2018, editor =. doi:10.1007/978-3-319-55333-7_171 , adsurl =

    2018 doi

  22. [31]

    , keywords =

    Ultra-wideband, Multiepoch Radio Study of the First Discovered ``Main-sequence Radio Pulse Emitter'' CU Vir. , keywords =. doi:10.3847/1538-4357/ac1075 , archivePrefix =. 2107.00849 , primaryClass =

    arXiv

  23. [33]

    and Haberland, Matt and Reddy, Tyler and Cournapeau, David and Burovski, Evgeni and Peterson, Pearu and Weckesser, Warren and Bright, Jonathan and

    Virtanen, Pauli and Gommers, Ralf and Oliphant, Travis E. and Haberland, Matt and Reddy, Tyler and Cournapeau, David and Burovski, Evgeni and Peterson, Pearu and Weckesser, Warren and Bright, Jonathan and. Nature Methods , year =

  24. [34]

    , keywords =

    Astropy: A community Python package for astronomy. , keywords =. 2013. doi:10.1051/0004-6361/201322068 , archivePrefix =. 1307.6212 , primaryClass =

    2013 arXiv

  25. [35]

    , keywords =

    The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package. , keywords =. doi:10.3847/1538-3881/aabc4f , archivePrefix =. 1801.02634 , primaryClass =

    arXiv

  26. [37]

    , keywords =

    Large-scale magnetic topologies of late M dwarfs*. , keywords =. doi:10.1111/j.1365-2966.2010.17101.x , archivePrefix =. 1005.5552 , primaryClass =

    2010

  27. [38]

    , keywords =

    Discovery of Eight ``Main-sequence Radio Pulse Emitters'' Using the GMRT: Clues to the Onset of Coherent Radio Emission in Hot Magnetic Stars. , keywords =. doi:10.3847/1538-4357/ac2576 , archivePrefix =. 2109.04043 , primaryClass =

    arXiv

  28. [39]

    Observations with moderate dispersion

    Line strengths for southern OB stars-II. Observations with moderate dispersion. , year = 1969, month = jan, volume =. doi:10.1093/mnras/144.1.31 , adsurl =

    1969 doi

  29. [40]

    , keywords =

    A circular polarization survey for radio stars with the Australian SKA Pathfinder. , keywords =. doi:10.1093/mnras/stab299 , archivePrefix =. 2102.01801 , primaryClass =

    arXiv

  30. [41]

    , keywords =

    Testing a scaling relation between coherent radio emission and physical parameters of hot magnetic stars. , keywords =. doi:10.1093/mnras/stac3123 , archivePrefix =. 2210.14746 , primaryClass =

    arXiv

  31. [42]

    , keywords =

    What leads to premature upper cut-off frequencies of auroral radio emission from hot magnetic stars?. , keywords =. doi:10.1093/mnras/stac1894 , archivePrefix =. 2207.00470 , primaryClass =

    arXiv

  32. [43]

    , keywords =

    On the spatial distribution of electron energy loss due to gyro-cooling in hot star magnetospheres. , keywords =. doi:10.1093/mnras/stad2389 , archivePrefix =. 2308.01493 , primaryClass =

    arXiv

  33. [44]

    , keywords =

    Discovery of extraordinary X-ray emission from magnetospheric interaction in the unique binary stellar system ϵ Lupi. , keywords =. doi:10.1093/mnras/stad1276 , archivePrefix =. 2304.12882 , primaryClass =

    arXiv

  34. [45]

    , keywords =

    An `analytic dynamical magnetosphere' formalism for X-ray and optical emission from slowly rotating magnetic massive stars. , keywords =. doi:10.1093/mnras/stw1894 , archivePrefix =. 1607.08568 , primaryClass =

    arXiv

  35. [46]

    , keywords =

    Periodic Radio Emission from the T8 Dwarf WISE J062309.94-045624.6. , keywords =. doi:10.3847/2041-8213/ace188 , archivePrefix =. 2306.15219 , primaryClass =

    arXiv

  36. [48]

    , keywords =

    Unravelling sub-stellar magnetospheres. , keywords =. doi:10.1051/0004-6361/202452094 , archivePrefix =. 2410.18073 , primaryClass =

    arXiv

  37. [49]

    , keywords =

    Confirmation of the Electron Cyclotron Maser Instability as the Dominant Source of Radio Emission from Very Low Mass Stars and Brown Dwarfs. , keywords =. doi:10.1086/590360 , archivePrefix =. 0805.4010 , primaryClass =

    arXiv

  38. [51]

    , keywords =

    A fossil origin for the magnetic field in A stars and white dwarfs. , keywords =. doi:10.1038/nature02934 , archivePrefix =. astro-ph/0502043 , primaryClass =

    arXiv

  39. [52]

    , keywords =

    Auroral Radio Emission from Late L and T Dwarfs: A New Constraint on Dynamo Theory in the Substellar Regime. , keywords =. doi:10.3847/0004-637X/818/1/24 , archivePrefix =. 1511.03661 , primaryClass =

    arXiv

  40. [53]

    , year = 2016, month = sep, volume =

    Accretion onto Pre-Main-Sequence Stars. , year = 2016, month = sep, volume =. doi:10.1146/annurev-astro-081915-023347 , adsurl =

    2016 doi

  41. [54]

    arXiv e-prints , keywords =

    The discovery of a nearby 421 -0.5ex transient with CHIME/FRB/Pulsar. arXiv e-prints , keywords =. doi:10.48550/arXiv.2407.07480 , archivePrefix =. 2407.07480 , primaryClass =

    doi arXiv

  42. [55]

    Nature Astronomy , keywords =

    An emission-state-switching radio transient with a 54-minute period. Nature Astronomy , keywords =. doi:10.1038/s41550-024-02277-w , archivePrefix =. 2407.12266 , primaryClass =

    arXiv

  43. [56]

    arXiv e-prints , keywords =

    A white dwarf binary showing sporadic radio pulses at the orbital period. arXiv e-prints , keywords =. doi:10.48550/arXiv.2408.11536 , archivePrefix =. 2408.11536 , primaryClass =

    doi

  44. [57]

    , keywords =

    Peculiar Spectral Property of Coherent Radio Emission from a Hot Magnetic Star: The Case of an Extreme Oblique Rotator. , keywords =. doi:10.3847/1538-4357/acf929 , archivePrefix =. 2309.06625 , primaryClass =

    arXiv

  45. [58]

    , keywords =

    A 3D Framework to Explore the Propagation Effects in Stars Exhibiting Electron Cyclotron Maser Emission. , keywords =. doi:10.3847/1538-4357/aba8fd , archivePrefix =. 2007.06822 , primaryClass =

    2007 arXiv

  46. [59]

    , keywords =

    Resolved imaging confirms a radiation belt around an ultracool dwarf. , keywords =. doi:10.1038/s41586-023-06138-w , archivePrefix =. 2302.12841 , primaryClass =

    arXiv

  47. [60]

    Finite diffusion effects-an illustrative example

    The magnetic field of a contracting gas cloud-II. Finite diffusion effects-an illustrative example. , year = 1967, month = jan, volume =. doi:10.1093/mnras/137.1.95 , adsurl =

    1967 doi

  48. [61]

    arXiv e-prints , keywords =

    The Polarization Convention of the uGMRT in Band 4. arXiv e-prints , keywords =

  49. [63]

    , keywords =

    A volume-limited survey of mCP stars within 100 pc II: rotational and magnetic properties. , keywords =. doi:10.1093/mnras/sty2895 , adsurl =

    doi

  50. [64]

    , keywords =

    Discovery of new magnetic early-B stars within the MiMeS HARPSpol survey. , keywords =. doi:10.1051/0004-6361/201323286 , archivePrefix =. 1404.5508 , primaryClass =

    arXiv

  51. [65]

    , keywords =

    A magnetic confinement versus rotation classification of massive-star magnetospheres. , keywords =. 2013. doi:10.1093/mnras/sts344 , archivePrefix =. 1211.0282 , primaryClass =

    2013 arXiv

  52. [66]

    , keywords =

    The MiMeS survey of Magnetism in Massive Stars: magnetic analysis of the O-type stars. , keywords =. 2017. doi:10.1093/mnras/stw2743 , archivePrefix =. 1610.07895 , primaryClass =

    2017 arXiv

  53. [68]

    , year = 2020, month = jun, volume =

    Erratum: ``Detection of Coherent Emission from the Bp Star HD 142990 at uGMRT Frequencies'' (2019, ApJ, 877, 123). , year = 2020, month = jun, volume =. doi:10.3847/1538-4357/ab94bb , adsurl =

    2019 doi

  54. [69]

    , keywords =

    Erratum: The fifth main-sequence magnetic B-type star showing coherent radio emission: Is this really a rare phenomenon?. , keywords =. doi:10.1093/mnrasl/slaa077 , adsurl =

    doi

  55. [70]

    , keywords =

    The Discovery of Nonthermal Radio Emission from Magnetic Bp--Ap Stars. , keywords =. doi:10.1086/165784 , adsurl =

    doi

  56. [72]

    Time Variability of the ``Quiet'' Sun Observed with TRACE. II. Physical Parameters, Temperature Evolution, and Energetics of Extreme-Ultraviolet Nanoflares. , keywords =. doi:10.1086/308867 , adsurl =

    doi

  57. [73]

    , keywords =

    X-Ray/Microwave Relation of Different Types of Active Stars. , keywords =. doi:10.1086/186766 , adsurl =

    doi

  58. [74]

    , keywords =

    X-ray/microwave ratio of flares and coronae. , keywords =

  59. [76]

    , keywords =

    Magnetic field topology and chemical abundance distributions of the young, rapidly rotating, chemically peculiar star HR 5624. , keywords =. 2017. doi:10.1051/0004-6361/201730919 , archivePrefix =. 1705.04966 , primaryClass =

    2017 arXiv

  60. [77]

    , keywords =

    Radio Emission from Chemically Peculiar Stars. , keywords =. doi:10.1086/171509 , adsurl =

    doi

  61. [78]

    Radio emission from the stars and the sun

    Rotational Modulation of Radio Emission from the Magnetic BP Star HR 5624. Radio emission from the stars and the sun. Astronomical Society of the Pacific Conference Series, Volume 93; Proceedings of a conference held at the University of Barcelona; Barcelona; Spain; 3-7 July 1...

    1995

  62. [80]

    Breakout or leakage? H emission as a diagnostic of plasma transport in centrifugal magnetospheres

    The magnetic early B-type stars - IV. Breakout or leakage? H emission as a diagnostic of plasma transport in centrifugal magnetospheres. , keywords =. doi:10.1093/mnras/staa3102 , archivePrefix =. 2009.12336 , primaryClass =

    2009 arXiv

  63. [81]

    , keywords =

    Compact non-thermal radio emission from B-peculiar stars. , keywords =. doi:10.1038/334329a0 , adsurl =

    doi

  64. [82]

    , keywords =

    The Flaring Activity of M Dwarfs in the Kepler Field. , keywords =. doi:10.3847/1538-4357/aa8ea2 , adsurl =

    doi

  65. [83]

    , keywords =

    The Kepler Catalog of Stellar Flares. , keywords =. doi:10.3847/0004-637X/829/1/23 , archivePrefix =. 1607.03494 , primaryClass =

    arXiv

  66. [84]

    Characterisation of stellar activity of M dwarfs. I. Long-timescale variability in a large sample and detection of new cycles. , keywords =. doi:10.1051/0004-6361/202244249 , archivePrefix =. 2303.03998 , primaryClass =

    arXiv

  67. [85]

    , keywords =

    Direct VLBI Detection of the Magnetosphere Surrounding the Young Star S1 in rho Ophiuchi. , keywords =. doi:10.1086/170311 , adsurl =

    doi

  68. [86]

    , keywords =

    Magnetospherically driven optical and radio aurorae at the end of the stellar main sequence. , keywords =. doi:10.1038/nature14619 , archivePrefix =. 1507.08739 , primaryClass =

    arXiv

  69. [87]

    , keywords =

    How the breakout-limited mass in B-star centrifugal magnetospheres controls their circumstellar H emission. , keywords =. doi:10.1093/mnras/staa2325 , archivePrefix =. 2009.12359 , primaryClass =

    2009 arXiv

  70. [88]

    , keywords =

    Detection of magnetic field in the B2 star Ophiuchi A with ESO FORS2. , keywords =. doi:10.1051/0004-6361/201732078 , archivePrefix =. 1712.00728 , primaryClass =

    arXiv

  71. [89]

    , keywords =

    Evidence for radio and X-ray auroral emissions from the magnetic B-type star Oph A. , keywords =. doi:10.1093/mnras/staa587 , archivePrefix =. 2002.09251 , primaryClass =

    2002 arXiv

  72. [90]

    , keywords =

    Comparative Analysis of Two Formation Scenarios of Bursty Radio Emission from Ultracool Dwarfs. , keywords =. doi:10.1088/0004-637X/746/1/99 , archivePrefix =. 1111.7019 , primaryClass =

    arXiv

  73. [91]

    , keywords =

    MOST Observations of Ori E: Challenging the Centrifugal Breakout Narrative. , keywords =. doi:10.1088/0004-637X/769/1/33 , archivePrefix =. 1304.2392 , primaryClass =

    arXiv

  74. [92]

    Physics of Magnetic Stars , year = 2019, editor =

    Towards Comprehension of the Variability of the mCP Star CU Virginis. Physics of Magnetic Stars , year = 2019, editor =

    2019

  75. [93]

    , keywords =

    Recurring millimeter flares as evidence for star-star magnetic reconnection events in the DQ Tauri PMS binary system. , keywords =. doi:10.1051/0004-6361/201015197 , archivePrefix =. 1008.0981 , primaryClass =

    arXiv

  76. [94]

    New Windows on Massive Stars , year = 2015, editor =

    The BinaMIcS project: understanding the origin of magnetic fields in massive stars through close binary systems. New Windows on Massive Stars , year = 2015, editor =. doi:10.1017/S1743921314007030 , archivePrefix =. 1409.1094 , primaryClass =

    2015 arXiv

  77. [95]

    , keywords =

    Wideband Dynamic Radio Spectra of Two Ultra-cool Dwarfs. , keywords =. doi:10.1088/0004-637X/802/2/106 , archivePrefix =. 1405.3516 , primaryClass =

    arXiv

  78. [96]

    , keywords =

    The Young Binary DQ Tau: A Hunt for X-ray Emission from Colliding Magnetospheres. , keywords =. doi:10.1088/0004-637X/730/1/6 , archivePrefix =. 1101.4044 , primaryClass =

    arXiv

  79. [97]

    , keywords =

    Discovery of electron cyclotron MASER emission from the magnetic Bp star HD 133880 with the Giant Metrewave Radio Telescope. , keywords =. 2018. doi:10.1093/mnrasl/slx193 , archivePrefix =. 1711.09836 , primaryClass =

    2018 arXiv

  80. [98]

    , keywords =

    The MiMeS survey of magnetism in massive stars: introduction and overview. , keywords =. doi:10.1093/mnras/stv2568 , archivePrefix =. 1511.08425 , primaryClass =

    arXiv

  81. [99]

    , keywords =

    Energetic particle activity in AD Leo: Detection of a solar-like type-IV burst. , keywords =. doi:10.1051/0004-6361/202347924 , archivePrefix =. 2402.00185 , primaryClass =

    arXiv

  82. [101]

    Nature Astronomy , keywords =

    The emission of interpulses by a 6.45-h-period coherent radio transient. Nature Astronomy , keywords =. doi:10.1038/s41550-024-02452-z , archivePrefix =. 2501.09133 , primaryClass =

    arXiv

  83. [102]

    , keywords =

    Deciphering Profile Stability in Millisecond Pulsars: Timescales, Frequency Evolution, and Implications on Emission Mechanisms. , keywords =. doi:10.3847/1538-4357/adff5a , archivePrefix =. 2509.12781 , primaryClass =

  84. [103]

    , keywords =

    Low-frequency pulse-jitter measurement with the uGMRT I: PSR J0437-4715. , keywords =. doi:10.1017/pasa.2024.30 , archivePrefix =. 2312.01875 , primaryClass =

    2024 arXiv

  85. [104]

    , keywords =

    The NANOGrav 12.5 yr Data Set: The Frequency Dependence of Pulse Jitter in Precision Millisecond Pulsars. , keywords =. doi:10.3847/1538-4357/ab01cd , archivePrefix =. 1809.03058 , primaryClass =

    arXiv

  86. [106]

    , keywords =

    An unusual supernova in the error box of the -ray burst of 25 April 1998. , keywords =. doi:10.1038/27150 , archivePrefix =. astro-ph/9806175 , primaryClass =

    1998 arXiv

  87. [107]

    , year = 2022, month = jan, volume =

    A radio transient with unusually slow periodic emission. , year = 2022, month = jan, volume =. doi:10.1038/s41586-021-04272-x , adsurl =

    2022 doi

  88. [108]

    QuartiCal: Fast radio interferometric calibration

  89. [109]

    , keywords =

    Radio variable and transient sources on minute time-scales in the ASKAP pilot surveys. , keywords =. doi:10.1093/mnras/stad1727 , archivePrefix =. 2306.04263 , primaryClass =

    arXiv

  90. [110]

    , keywords =

    Metrewave Galactic Plane with the uGMRT (MeGaPluG) Survey: Lessons from the pilot study. , keywords =. doi:10.1051/0004-6361/202347320 , archivePrefix =. 2308.03746 , primaryClass =

    arXiv

  91. [111]

    arXiv e-prints , keywords =

    uGMRT Band 4 Polarimetry. arXiv e-prints , keywords =. doi:10.48550/arXiv.2305.04420 , archivePrefix =. 2305.04420 , primaryClass =

    doi arXiv

  92. [112]

    arXiv e-prints , keywords =

    A detailed study of the polarisation convention of the Giant Metrewave Radio Telescope. arXiv e-prints , keywords =. doi:10.48550/arXiv.2310.04335 , archivePrefix =. 2310.04335 , primaryClass =

    doi arXiv

  93. [113]

    , keywords =

    Discovery of magnetospheric interactions in the doubly magnetic hot binary ϵ Lupi. , keywords =. doi:10.1093/mnras/stad1756 , archivePrefix =. 2306.05995 , primaryClass =

    arXiv

  94. [114]

    arXiv e-prints , keywords =

    XMM-Newton Perspective of the Unique Magnetic Binary- Lupi. arXiv e-prints , keywords =. doi:10.48550/arXiv.2408.07001 , archivePrefix =. 2408.07001 , primaryClass =

    doi arXiv

  95. [115]

    arXiv e-prints , keywords =

    Coherent radio emission from 'Main-sequence Radio Pulse emitters': a new stellar diagnostic to probe 3D magnetospheric structures. arXiv e-prints , keywords =

  96. [117]

    , keywords =

    Detection of Coherent Emission from the Bp Star HD 142990 at uGMRT Frequencies. , keywords =. 2019. doi:10.3847/1538-4357/ab1b12 , archivePrefix =. 1904.08359 , primaryClass =

    2019 arXiv

  97. [118]

    , keywords =

    The fifth main-sequence magnetic B-type star showing coherent radio emission: Is this really a rare phenomenon?. , keywords =. doi:10.1093/mnrasl/slz137 , archivePrefix =. 1908.09110 , primaryClass =

    1908 arXiv

  98. [119]

    , keywords =

    Periodic radio emission from the helium strong stars HD 37017 and sigma ORI E. , keywords =

  99. [120]

    , keywords =

    The polarization mode of the auroral radio emission from the early-type star HD 142301. , keywords =. 2019. doi:10.1093/mnrasl/sly179 , archivePrefix =. 1809.07504 , primaryClass =

    2019 arXiv

  100. [121]

    , keywords =

    Surprising variations in the rotation of the chemically peculiar stars CU Virginis and V901 Orionis. , keywords =. 2011. doi:10.1051/0004-6361/201117784 , archivePrefix =. 1110.1104 , primaryClass =

    2011 arXiv

  101. [122]

    , keywords =

    Auroral Radio Emission from Stars: The Case of CU Virginis. , keywords =. 2011. doi:10.1088/2041-8205/739/1/L10 , archivePrefix =. 1104.3268 , primaryClass =

    2011 arXiv

  102. [124]

    Multi-frequency VLA observations and 3D-simulations of <ASTROBJ>CU Virginis</ASTROBJ>

    Stellar magnetosphere reconstruction from radio data. Multi-frequency VLA observations and 3D-simulations of <ASTROBJ>CU Virginis</ASTROBJ>. , keywords =. 2006. doi:10.1051/0004-6361:20054511 , archivePrefix =. astro-ph/0610395 , primaryClass =

    2006 arXiv

  103. [125]

    , keywords =

    Extending the radio spectrum of magnetic chemically peculiar stars to the mm range. , keywords =. 2004. doi:10.1051/0004-6361:20040181 , adsurl =

    2004 doi

  104. [126]

    , keywords =

    A three-dimensional model for the radio emission of magnetic chemically peculiar stars. , keywords =. 2004. doi:10.1051/0004-6361:20040060 , archivePrefix =. astro-ph/0402432 , primaryClass =

    2004 arXiv

  105. [127]

    , keywords =

    Coherent radio emission from the magnetic chemically peculiar star CU Virginis. , keywords =. 2000

    2000

  106. [128]

    , keywords =

    3D modelling of stellar auroral radio emission. , keywords =. 2016. doi:10.1093/mnras/stw639 , archivePrefix =. 1603.02423 , primaryClass =

    2016 arXiv

  107. [130]

    , keywords =

    Detection of 610-MHz radio emission from hot magnetic stars. , keywords =. 2015. doi:10.1093/mnras/stv1378 , archivePrefix =. 1505.02139 , primaryClass =

    2015 arXiv

  108. [131]

    , keywords =

    An all-sky survey of circular polarization at 200 MHz. , keywords =. 2018. doi:10.1093/mnras/sty1304 , archivePrefix =. 1805.05482 , primaryClass =

    2018 arXiv

  109. [133]

    , keywords =

    Discovery of X-ray flaring on the magnetic Bp-star Ori E. , keywords =. doi:10.1051/0004-6361:20034300 , archivePrefix =. astro-ph/0402437 , primaryClass =

    arXiv

  110. [134]

    A deep look into the cores of young clusters. I. -Orionis. , keywords =. doi:10.1051/0004-6361:200810267 , archivePrefix =. 0808.3890 , primaryClass =

    arXiv

  111. [135]

    , keywords =

    The magnetic fields of the AP stars. , keywords =. doi:10.1086/190656 , adsurl =

    doi

  112. [136]

    , keywords =

    The Strongest Magnetic Fields on the Coolest Brown Dwarfs. , keywords =. doi:10.3847/1538-4365/aac2d5 , archivePrefix =. 1808.02485 , primaryClass =

    arXiv

  113. [137]

    , keywords =

    X-Ray Emission from Magnetic Massive Stars. , keywords =. doi:10.1088/0067-0049/215/1/10 , archivePrefix =. 1409.1690 , primaryClass =

    arXiv

  114. [138]

    , keywords =

    Discovery of radio emission from the brown dwarf LP944-20. , keywords =. doi:10.48550/arXiv.astro-ph/0102301 , archivePrefix =. astro-ph/0102301 , primaryClass =

    doi arXiv

  115. [139]

    Planetary Radio Emissions III , year = 1992, month = jan, pages =

    Low-frequency auroral radio emission from Jupiter: The hectometric radiation. Planetary Radio Emissions III , year = 1992, month = jan, pages =

    1992

  116. [140]

    , keywords =

    Cluster multispacecraft determination of AKR angular beaming. , keywords =. doi:10.1029/2008GL033377 , archivePrefix =. 0803.0078 , primaryClass =

    arXiv

  117. [141]

    , keywords =

    Radio emission from the sun and stars. , keywords =. doi:10.1146/annurev.aa.23.090185.001125 , adsurl =

  118. [142]

    , year = 1964, month = sep, volume =

    Influence of the Satellite Io on Jupiter's Decametric Emission. , year = 1964, month = sep, volume =. doi:10.1038/2031008a0 , adsurl =

    1964 doi

  119. [143]

    , keywords =

    A Panchromatic View of Brown Dwarf Aurorae. , keywords =. doi:10.3847/1538-4357/aa8596 , archivePrefix =. 1708.02942 , primaryClass =

    arXiv

  120. [144]

    Advances in Space Research , year = 2004, month = jan, volume =

    Radio and plasma waves at the outer planets. Advances in Space Research , year = 2004, month = jan, volume =. doi:10.1016/j.asr.2003.07.055 , adsurl =

    2004 doi

  121. [145]

    arXiv e-prints , keywords =

    Large closed-field corona of WX UMa evidenced from radio observations. arXiv e-prints , keywords =

  122. [146]

    Hint of star exoplanet interaction?

    Probing the magnetosphere of the M8.5 dwarf TVLM 513-46546 by modelling its auroral radio emission. Hint of star exoplanet interaction?. , keywords =. doi:10.1093/mnras/stx995 , archivePrefix =. 1611.00511 , primaryClass =

    arXiv

  123. [147]

    , keywords =

    The detection of variable radio emission from the fast rotating magnetic hot B-star HR 07355 and evidence for its X-ray aurorae. , keywords =. doi:10.1093/mnras/stx267 , archivePrefix =. 1701.07679 , primaryClass =

    arXiv

  124. [148]

    Magnetic Doppler imaging, arbitrary field RRM, and light variability

    Revisiting the rigidly rotating magnetosphere model for Ori E - II. Magnetic Doppler imaging, arbitrary field RRM, and light variability. , keywords =. doi:10.1093/mnras/stv1086 , archivePrefix =. 1505.04839 , primaryClass =

    arXiv

  125. [149]

    , keywords =

    Flares on a Bp Star. , keywords =. doi:10.1088/0004-637X/702/1/759 , adsurl =

    doi

  126. [150]

    , keywords =

    Electron-cyclotron maser emission: Relative growth and damping rates for different modes and harmonics. , keywords =. 1984. doi:10.1029/JA089iA02p00897 , adsurl =

    1984 doi

  127. [151]

    , keywords =

    Comparative study of the loss cone-driven instabilities in the low solar corona. , keywords =. 1984. doi:10.1086/162006 , adsurl =

    1984 doi

  128. [152]

    , keywords =

    Rotational Modulation of the Radio Emission from the M9 Dwarf TVLM 513-46546: Broadband Coherent Emission at the Substellar Boundary?. , keywords =. 2006. doi:10.1086/508678 , archivePrefix =. astro-ph/0608556 , primaryClass =

    2006 arXiv

  129. [153]

    , keywords =

    Periodic Bursts of Coherent Radio Emission from an Ultracool Dwarf. , keywords =. 2007. doi:10.1086/519790 , archivePrefix =. 0705.2054 , primaryClass =

    2007 arXiv

  130. [154]

    , keywords =

    Phenomenology and periodicity of radio emission from the stellar system AU Microscopii. , keywords =. doi:10.1051/0004-6361/202348065 , archivePrefix =. 2312.09071 , primaryClass =

    arXiv

  131. [155]

    , keywords =

    Long-term Behavior of a Type IIP Supernova SN 2004dj in the Radio Bands. , keywords =. doi:10.3847/1538-4357/aad17a , adsurl =

    doi

  132. [156]

    Science , keywords =

    Evidence for a radiation belt around a brown dwarf. Science , keywords =. doi:10.1126/science.adg6635 , adsurl =

    doi

  133. [157]

    Experimental Astronomy , keywords =

    CAPTURE: a continuum imaging pipeline for the uGMRT. Experimental Astronomy , keywords =. doi:10.1007/s10686-020-09677-6 , archivePrefix =. 2010.00196 , primaryClass =

    2010 arXiv

  134. [158]

    , keywords =

    ASKAP detection of periodic and elliptically polarized radio pulses from UV Ceti. , keywords =. doi:10.1093/mnras/stz1684 , archivePrefix =. 1906.06570 , primaryClass =

    1906 arXiv

  135. [159]

    , keywords =

    Fine Structures of Radio Bursts from Flare Star AD Leo with FAST Observations. , keywords =. doi:10.3847/1538-4357/acdb77 , archivePrefix =. 2306.00895 , primaryClass =

    arXiv

  136. [160]

    , keywords =

    Radio Emission from UV Cet: Auroral Emission from a Stellar Magnetosphere. , keywords =. doi:10.3847/1538-4357/ac7d57 , archivePrefix =. 2206.14099 , primaryClass =

    arXiv

  137. [161]

    , keywords =

    An Investigation of Synchrotron Self-absorption and Free-Free Absorption Models in Explanation of the Gigahertz-peaked Spectrum of PKS 1718-649. , keywords =. doi:10.1086/376600 , adsurl =

    doi

  138. [162]

    , keywords =

    Mass loss in main-sequence B stars. , keywords =. doi:10.1051/0004-6361/201321980 , archivePrefix =. 1401.5511 , primaryClass =

    arXiv

  139. [163]

    , keywords =

    Electron scattering emission in the light curves of stars with centrifugal magnetospheres. , keywords =. doi:10.1093/mnras/stac322 , archivePrefix =. 2202.00615 , primaryClass =

    arXiv

  140. [164]

    , keywords =

    Broadband Spectral Modeling of the Extreme Gigahertz-peaked Spectrum Radio Source PKS B0008-421. , keywords =. doi:10.1088/0004-637X/809/2/168 , archivePrefix =. 1507.04819 , primaryClass =

    arXiv

  141. [165]

    , keywords =

    Hunting for exoplanets via magnetic star-planet interactions: geometrical considerations for radio emission. , keywords =. doi:10.1093/mnras/stad2035 , archivePrefix =. 2307.02555 , primaryClass =

    arXiv

  142. [166]

    , keywords =

    V-LoTSS: The circularly polarised LOFAR Two-metre Sky Survey. , keywords =. doi:10.1051/0004-6361/202245567 , archivePrefix =. 2212.09815 , primaryClass =

    arXiv

  143. [167]

    Summary of the contents and survey properties

    Gaia Data Release 2. Summary of the contents and survey properties. , keywords =. doi:10.1051/0004-6361/201833051 , archivePrefix =. 1804.09365 , primaryClass =

    arXiv

  144. [168]

    The rotational evolution and magnetospheric emission of the magnetic early B-type stars

  145. [169]

    , keywords =

    The magnetic early B-type Stars II: stellar atmospheric parameters in the era of Gaia. , keywords =. doi:10.1093/mnras/stz416 , archivePrefix =. 1902.02713 , primaryClass =

    1902 arXiv

  146. [170]

    A main-sequence magnetic, rotational, and magnetospheric biography

    The magnetic early B-type stars - III. A main-sequence magnetic, rotational, and magnetospheric biography. , keywords =. 2019. doi:10.1093/mnras/stz2551 , archivePrefix =. 1909.02530 , primaryClass =

    2019 arXiv

  147. [171]

    , keywords =

    The magnetic early B-type stars I: magnetometry and rotation. , keywords =. 2018. doi:10.1093/mnras/sty103 , archivePrefix =. 1801.02924 , primaryClass =

    2018 arXiv

  148. [173]

    , keywords =

    An update on the rotational period of the magnetic chemically peculiar star CU Virginis. , keywords =. 2013. doi:10.1093/mnras/stt256 , adsurl =

    2013 doi

  149. [174]

    Models at low metallicity

    The effects of surface fossil magnetic fields on massive star evolution: V. Models at low metallicity. , keywords =. doi:10.1093/mnras/stae1855 , archivePrefix =. 2407.20492 , primaryClass =

    arXiv

  150. [175]

    , keywords =

    Magnetic massive stars as progenitors of `heavy' stellar-mass black holes. , keywords =. doi:10.1093/mnras/stw3126 , archivePrefix =. 1611.08964 , primaryClass =

    arXiv

  151. [176]

    , year = 1947, month = jan, volume =

    Zeeman Effect in Stellar Spectra. , year = 1947, month = jan, volume =. doi:10.1086/144887 , adsurl =

    1947 doi

  152. [177]

    , keywords =

    X-rays from magnetically confined wind shocks: effect of cooling-regulated shock retreat. , keywords =. doi:10.1093/mnras/stu769 , archivePrefix =. 1404.5336 , primaryClass =

    arXiv

  153. [178]

    Advances in Space Research , keywords =

    Magnetically confined wind shocks in X-rays - A review. Advances in Space Research , keywords =. doi:10.1016/j.asr.2015.09.025 , archivePrefix =. 1509.06482 , primaryClass =

    2015 arXiv

  154. [179]

    , keywords =

    Stellar mergers as the origin of magnetic massive stars. , keywords =. doi:10.1038/s41586-019-1621-5 , archivePrefix =. 1910.14058 , primaryClass =

    1910 arXiv

  155. [180]

    , keywords =

    3D MHD models of the centrifugal magnetosphere from a massive star with an oblique dipole field. , keywords =. doi:10.1093/mnras/stad345 , archivePrefix =. 2301.11858 , primaryClass =

    arXiv

  156. [181]

    Polarimetry , year = 2015, editor =

    The origin of magnetic fields in hot stars. Polarimetry , year = 2015, editor =. doi:10.1017/S1743921315004524 , archivePrefix =. 1502.00226 , primaryClass =

    2015 arXiv

  157. [183]

    , keywords =

    WSCLEAN: an implementation of a fast, generic wide-field imager for radio astronomy. , keywords =. doi:10.1093/mnras/stu1368 , archivePrefix =. 1407.1943 , primaryClass =

    1943 arXiv

  158. [184]

    , keywords =

    Magnetic field topology of the unique chemically peculiar star CU Virginis. , keywords =. 2014. doi:10.1051/0004-6361/201423472 , archivePrefix =. 1404.2645 , primaryClass =

    2014 arXiv

  159. [186]

    , keywords =

    The accelerating rotation of the magnetic He-weak star HD 142990. , keywords =. 2019. doi:10.1093/mnras/stz1129 , archivePrefix =. 1904.08887 , primaryClass =

    2019 arXiv

  160. [187]

    P., Tollerud , E

    Astropy Collaboration , Robitaille , T. P., Tollerud , E. J., et al. 2013, title Astropy: A community Python package for astronomy , , 558, A33, 10.1051/0004-6361/201322068

    2013 doi

  161. [188]

    M., Sip o cz , B

    Astropy Collaboration , Price-Whelan , A. M., Sip o cz , B. M., et al. 2018, title The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package , , 156, 123, 10.3847/1538-3881/aabc4f

    2018 doi

  162. [189]

    M., Lim , P

    Astropy Collaboration , Price-Whelan , A. M., Lim , P. L., et al. 2022, title The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package , , 935, 167, 10.3847/1538-4357/ac7c74

    2022 doi

  163. [190]

    2021, title Ultra-wideband, Multiepoch Radio Study of the First Discovered ``Main-sequence Radio Pulse Emitter'' CU Vir , , 921, 9, 10.3847/1538-4357/ac1075

    Das , B., & Chandra , P. 2021, title Ultra-wideband, Multiepoch Radio Study of the First Discovered ``Main-sequence Radio Pulse Emitter'' CU Vir , , 921, 9, 10.3847/1538-4357/ac1075

    2021 doi

  164. [191]

    2025 a , title Discoveries of Fine Structures and Secondary Pulses in Coherent Radio Emission from a Magnetic Massive Star , , 989, 163, 10.3847/1538-4357/aded88

    Das , B., Chandra , P., Cotton , W., & Petit , V. 2025 a , title Discoveries of Fine Structures and Secondary Pulses in Coherent Radio Emission from a Magnetic Massive Star , , 989, 163, 10.3847/1538-4357/aded88

    2025 doi

  165. [192]

    2024, title Coherent radio emission from 'Main-sequence Radio Pulse emitters': a new stellar diagnostic to probe 3D magnetospheric structures , arXiv e-prints, arXiv:2408.11242

    Das , B., Chandra , P., & Petit , V. 2024, title Coherent radio emission from 'Main-sequence Radio Pulse emitters': a new stellar diagnostic to probe 3D magnetospheric structures , arXiv e-prints, arXiv:2408.11242. 2408.11242

    2024 arXiv

  166. [193]

    A., Shultz , M

    Das , B., Chandra , P., Wade , G. A., Shultz , M. E., & Sikora , J. 2020 a , title Probing the Magnetospheres of Hot Magnetic Stars Using ECME , in Stellar Magnetism: A Workshop in Honour of the Career and Contributions of John D. Landstreet, ed. G. Wade , E. Alecian , D. Bohl...

    2020 doi arXiv

  167. [194]

    2020 b , title A 3D Framework to Explore the Propagation Effects in Stars Exhibiting Electron Cyclotron Maser Emission , , 900, 156, 10.3847/1538-4357/aba8fd

    Das , B., Mondal , S., & Chandra , P. 2020 b , title A 3D Framework to Explore the Propagation Effects in Stars Exhibiting Electron Cyclotron Maser Emission , , 900, 156, 10.3847/1538-4357/aba8fd

    2020 doi

  168. [195]

    E., et al

    Das , B., Chandra , P., Shultz , M. E., et al. 2022, title Discovery of Eight ``Main-sequence Radio Pulse Emitters'' Using the GMRT: Clues to the Onset of Coherent Radio Emission in Hot Magnetic Stars , , 925, 125, 10.3847/1538-4357/ac2576

    2022 doi

  169. [196]

    E., Pritchard , J., et al

    Das , B., Shultz , M. E., Pritchard , J., et al. 2025 b , title Discovery of Main-sequence Radio Pulse emitters from widefield sky surveys , , 42, e110, 10.1017/pasa.2025.10036

    2025

  170. [197]

    2025, title Deciphering Profile Stability in Millisecond Pulsars: Timescales, Frequency Evolution, and Implications on Emission Mechanisms , , 991, 135, 10.3847/1538-4357/adff5a

    Ghosh , A., Bhattacharyya , B., Sharan , R., et al. 2025, title Deciphering Profile Stability in Millisecond Pulsars: Timescales, Frequency Evolution, and Implications on Emission Mechanisms , , 991, 135, 10.3847/1538-4357/adff5a

    2025 doi

  171. [198]

    2007, title Periodic Bursts of Coherent Radio Emission from an Ultracool Dwarf , , 663, L25, 10.1086/519790

    Hallinan , G., Bourke , S., Lane , C., et al. 2007, title Periodic Bursts of Coherent Radio Emission from an Ultracool Dwarf , , 663, L25, 10.1086/519790

    2007 doi

  172. [199]

    R., Millman, K

    Harris, C. R., Millman, K. J., van der Walt, S. J., et al. 2020, title Array programming with NumPy , Nature, 585, 357, 10.1038/s41586-020-2649-2

    2020 doi

  173. [200]

    D., Vedantham , H

    Kavanagh , R. D., Vedantham , H. K., Rose , K., & Bloot , S. 2024, title Unravelling sub-stellar magnetospheres , , 692, A66, 10.1051/0004-6361/202452094

    2024 doi

  174. [201]

    2014, title Magnetic field topology of the unique chemically peculiar star CU Virginis , , 565, A83, 10.1051/0004-6361/201423472

    Kochukhov , O., L \"u ftinger , T., Neiner , C., Alecian , E., & MiMeS Collaboration . 2014, title Magnetic field topology of the unique chemically peculiar star CU Virginis , , 565, A83, 10.1051/0004-6361/201423472

    2014 doi

  175. [202]

    Lee , Y. W. J., Caleb , M., Murphy , T., et al. 2025, title The emission of interpulses by a 6.45-h-period coherent radio transient , Nature Astronomy, 9, 393, 10.1038/s41550-024-02452-z

    2025 doi

  176. [203]

    S., et al

    Leto , P., Trigilio , C., Buemi , C. S., et al. 2016, title 3D modelling of stellar auroral radio emission , , 459, 1159, 10.1093/mnras/stw639

    2016 doi

  177. [204]

    M., et al

    Leto , P., Trigilio , C., Oskinova , L. M., et al. 2018, title A combined multiwavelength VLA/ALMA/Chandra study unveils the complex magnetosphere of the B-type star HR5907 , , 476, 562, 10.1093/mnras/sty244

    2018 doi

  178. [205]

    A., & Linsky , J

    Lim , J., Drake , S. A., & Linsky , J. L. 1996, Astronomical Society of the Pacific Conference Series, Vol. 93, Rotational Modulation of Radio Emission from the Magnetic BP Star HR 5624 , ed. A. R. Taylor & J. M. Paredes , 324

    1996

  179. [206]

    K., Bray , J

    Lo , K. K., Bray , J. D., Hobbs , G., et al. 2012, title Observations and modelling of pulsed radio emission from CU Virginis , , 421, 3316, 10.1111/j.1365-2966.2012.20555.x

    2012

  180. [207]

    P., Waters , B., Schiebel , D., Young , W., & Golap , K

    McMullin , J. P., Waters , B., Schiebel , D., Young , W., & Golap , K. 2007, title CASA Architecture and Applications , in Astronomical Society of the Pacific Conference Series, Vol. 376, Astronomical Data Analysis Software and Systems XVI, ed. R. A. Shaw , F. Hill , & D. J. B...

    2007

  181. [208]

    B., & Dulk , G

    Melrose , D. B., & Dulk , G. A. 1982, title Electron-cyclotron masers as the source of certain solar and stellar radio bursts. , , 259, 844, 10.1086/160219

    1982 doi

  182. [209]

    W., Jan \' k , J., & Pigulski , A

    Mikul \'a s ek , Z., Krti c ka , J., Henry , G. W., Jan \' k , J., & Pigulski , A. 2019, title Towards Comprehension of the Variability of the mCP Star CU Virginis , in Astronomical Society of the Pacific Conference Series, Vol. 518, Physics of Magnetic Stars, ed. D. O. Kudrya...

    2019 arXiv

  183. [210]

    W., et al

    Mikul \'a s ek , Z., Krti c ka , J., Henry , G. W., et al. 2011, title Surprising variations in the rotation of the chemically peculiar stars CU Virginis and V901 Orionis , , 534, L5, 10.1051/0004-6361/201117784

    2011 doi

  184. [211]

    S., Das , B., & Bignall , H

    Morgan , J. S., Das , B., & Bignall , H. E. 2026, title The effect of interstellar scattering on coherent radio emission from stars: the case of CU Vir , , 1–9, 10.1017/pasa.2026.10197

    2026

  185. [212]

    R., McKinley , B., Hurley-Walker , N., et al

    Offringa , A. R., McKinley , B., Hurley-Walker , N., et al. 2014, title WSCLEAN: an implementation of a fast, generic wide-field imager for radio astronomy , , 444, 606, 10.1093/mnras/stu1368

    2014 doi

  186. [213]

    P., Shultz , M

    Owocki , S. P., Shultz , M. E., ud-Doula , A., et al. 2022, title Centrifugal breakout reconnection as the electron acceleration mechanism powering the radio magnetospheres of early-type stars , , 10.1093/mnras/stac341

    2022 doi

  187. [214]

    P., ud-Doula , A., Sundqvist , J

    Owocki , S. P., ud-Doula , A., Sundqvist , J. O., et al. 2016, title An `analytic dynamical magnetosphere' formalism for X-ray and optical emission from slowly rotating magnetic massive stars , , 462, 3830, 10.1093/mnras/stw1894

    2016 doi

  188. [215]

    P., Wade , G

    Petit , V., Owocki , S. P., Wade , G. A., et al. 2013, title A magnetic confinement versus rotation classification of massive-star magnetospheres , , 429, 398, 10.1093/mnras/sts344

    2013 doi

  189. [216]

    2023, title Unstable Phenomena in Stable Magnetospheres: Searching for Radio Flares from Magnetic OBA Stars Using VCSS , , 958, 152, 10.3847/1538-4357/ad0295

    Polisensky , E., Das , B., Peters , W., et al. 2023, title Unstable Phenomena in Stable Magnetospheres: Searching for Radio Flares from Magnetic OBA Stars Using VCSS , , 958, 152, 10.3847/1538-4357/ad0295

    2023 doi

  190. [217]

    Rathnasree , N., & Rankin , J. M. 1995, title On the Approach to Stability of Pulsar Average Profiles , , 452, 814, 10.1086/176349

    1995 doi

  191. [218]

    2010, title Observations of radio pulses from CU Virginis , , 408, L99, 10.1111/j.1745-3933.2010.00939.x

    Ravi , V., Hobbs , G., Wickramasinghe , D., et al. 2010, title Observations of radio pulses from CU Virginis , , 408, L99, 10.1111/j.1745-3933.2010.00939.x

    2010

  192. [219]

    M., Ricci , R., Ekers , R

    Sadler , E. M., Ricci , R., Ekers , R. D., et al. 2006, title The properties of extragalactic radio sources selected at 20GHz , , 371, 898, 10.1111/j.1365-2966.2006.10729.x

    2006

  193. [220]

    J., Teuben , P

    Sault , R. J., Teuben , P. J., & Wright , M. C. H. 1995, title A Retrospective View of MIRIAD , in Astronomical Society of the Pacific Conference Series, Vol. 77, Astronomical Data Analysis Software and Systems IV, ed. R. A. Shaw , H. E. Payne , & J. J. E. Hayes , 433, 10.4855...

    1995 doi arXiv

  194. [221]

    E., Wade , G

    Shultz , M. E., Wade , G. A., Rivinius , T., et al. 2018, title The magnetic early B-type stars I: magnetometry and rotation , , 475, 5144, 10.1093/mnras/sty103

    2018 doi

  195. [222]

    E., Owocki , S., Rivinius , T., et al

    Shultz , M. E., Owocki , S., Rivinius , T., et al. 2020, title The magnetic early B-type stars - IV. Breakout or leakage? H emission as a diagnostic of plasma transport in centrifugal magnetospheres , , 499, 5379, 10.1093/mnras/staa3102

    2020 doi

  196. [223]

    E., Owocki , S

    Shultz , M. E., Owocki , S. P., ud-Doula , A., et al. 2022, title MOBSTER - VI. The crucial influence of rotation on the radio magnetospheres of hot stars , , 10.1093/mnras/stac136

    2022 doi

  197. [224]

    Townsend , R. H. D., & Owocki , S. P. 2005, title A rigidly rotating magnetosphere model for circumstellar emission from magnetic OB stars , , 357, 251, 10.1111/j.1365-2966.2005.08642.x

    2005

  198. [225]

    Treumann , R. A. 2006, title The electron-cyclotron maser for astrophysical application , , 13, 229, 10.1007/s00159-006-0001-y

    2006 doi

  199. [226]

    2000, title Coherent radio emission from the magnetic chemically peculiar star CU Virginis , , 362, 281

    Trigilio , C., Leto , P., Leone , F., Umana , G., & Buemi , C. 2000, title Coherent radio emission from the magnetic chemically peculiar star CU Virginis , , 362, 281. astro-ph/0007097

    2000 arXiv

  200. [227]

    S., & Leone , F

    Trigilio , C., Leto , P., Umana , G., Buemi , C. S., & Leone , F. 2008, title The radio lighthouse CU Virginis: the spin-down of a single main-sequence star , , 384, 1437, 10.1111/j.1365-2966.2007.12749.x

    2008

  201. [228]

    S., & Leone , F

    Trigilio , C., Leto , P., Umana , G., Buemi , C. S., & Leone , F. 2011, title Auroral Radio Emission from Stars: The Case of CU Virginis , , 739, L10, 10.1088/2041-8205/739/1/L10

    2011 doi

  202. [229]

    P., & Townsend , R

    Ud-Doula , A., Owocki , S. P., & Townsend , R. H. D. 2009, title Dynamical simulations of magnetically channelled line-driven stellar winds - III. Angular momentum loss and rotational spin-down , , 392, 1022, 10.1111/j.1365-2966.2008.14134.x

    2009

  203. [230]

    H., Zhi , Q

    Xu , X., Shang , L. H., Zhi , Q. J., et al. 2021, title A Systematic Study of the Frequency Evolution Behavior of Pulsar Pulse Profiles , , 917, 108, 10.3847/1538-4357/ac0b40

    2021 doi

Pith tools

Reviewed August 15, 2026 · model on record in the stance chip above.