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A Disintegrating Rocky Planet with Prominent Comet-like Tails Around a Bright Star

T0 review · 3 major / 5 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read BD+05 4868 Ab is a disintegrating rocky planet whose leading and trailing comet-like dust tails imply roughly 1-10 micron grains, a mass-loss rate of about 10 Earth masses per Gyr, and a remaining lifetime of only a few million years.

desk verdict A robust fourth disintegrating planet with a genuinely new dual-tail morphology around the brightest host yet, but the headline dust parameters are model-dependent and should be read as order-of-magnitude estimates. read the letter →

arxiv 2501.05431 v3 pith:NOE2KZME submitted 2025-01-09 astro-ph.EP

Marc Hon , Saul Rappaport , Avi Shporer , Andrew Vanderburg , Karen A. Collins , Cristilyn N. Watkins , Richard P. Schwarz , Khalid Barkaoui
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Samuel W. Yee Joshua N. Winn Alex S. Polanski Emily A. Gilbert David R. Ciardi Jeroen Audenaert William Fong Jack Haviland Katharine Hesse Daniel Muthukrishna Glen Petitpas Ellie Hadjiyska Schmelzer Norio Narita Akihiko Fukui Sara Seager George R. Ricker
This is my paper · ORCID
classification astro-ph.EP
keywords disintegratingplanetcomet-likedusttailsexoplanettransitsgrainsizesmass-lossrateradiationpressureTESSrockycomposition
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

The paper reports the fourth known disintegrating rocky planet, found in satellite photometry around the bright K-dwarf BD+05 4868 A. Its transits are asymmetric, vary in depth from about 0.8% to 2.0%, and last roughly 20 hours, because the planet is shedding dust that forms both a trailing and a leading comet-like tail. Fitting the average transit shape and modeling how dust grains drift under radiation pressure, the authors conclude that the grains are roughly 1-10 microns across, that the planet is losing mass at about 10 Earth masses per Gyr, and that the object — probably lunar-mass — has only a few million years before it disintegrates. Because the host star is bright and the transits are deep, this system is the best target yet for directly studying the mineral composition of a rocky exoplanet's evaporating surface.

What carries the argument

The load-bearing object is the analytic dust-drift relation Phi ≈ N(2 beta - 6 r_H), which connects the angular spread of a dust tail (Phi) to the number of orbits since launch (N), the radiation-pressure parameter (beta), and the planet's Hill-sphere radius (r_H, the radius of the planet's gravitational dominance zone). Because the trailing tail is measured to be about six times longer than the leading tail, this relation yields beta_max ≈ 0.07, and that value, fed through light-scattering cross-sections, fixes the grain size near 1-10 microns. The mass-loss estimate then comes from unrolling the trailing tail into an optically thick dust ribbon of known height, length, and assumed 10-micron depth, divided by a grain lifetime of about 2.5 orbits, with the planet modeled as a 0.02-Earth-mass body losing 10 Earth masses per Gyr. The paper also uses generalized-Gaussian extinction profiles to fit the observed transit shape and numerical grain-orbit simulations to visualize how the two tails form.

What would settle it

A future transit deeper than about 3% would falsify the optically thick dust-ribbon model used for the mass-loss estimate, because the paper's alternative launch scenario in Appendix D predicts a hard ceiling near 2% depth.

Watch

Extended reading notes

Core claim

On the paper's own terms, BD+05 4868 Ab is a disintegrating rocky planet orbiting a 0.70-solar-mass K dwarf every 1.27 days, with the longest orbital period and the deepest, longest transits among the four known objects of this class. The asymmetric light curve requires two dust tails: a trailing tail roughly six times longer than the leading tail, with the time of minimum light occurring only after the planet has nearly crossed the stellar disk. The measured 6:1 tail-length ratio, interpreted through analytic dust-drift equations, fixes the maximum radiation-pressure parameter at beta ≈ 0.07; light-scattering calculations then imply grain sizes of roughly 1-10 microns, and an optically thick dust-ribbon model yields a mass-loss rate of about 10 Earth masses per Gyr and a remaining lifetime of about 2 million years. Radial-velocity limits place the planet's mass below about 6.2 Earth masses, and the host star's brightness plus the planet's roughly 1.2% mean transit depth make this the most promising system for spectroscopic measurements of the dust's mineral content.

Load-bearing premise

The chain of inferences assumes that dust grains detach from the planet's outflowing gas near the edge of its gravitational influence with a speed of 0.4 km/s, are pushed by starlight no harder than beta = 0.07, and that the trailing tail blocks starlight completely in a sheet about 10 microns deep; if any of these assumptions shifts, the inferred grain sizes, mass-loss rate, and remaining lifetime change.

Editorial extensions

If this is right

  • The system becomes a primary target for transmission spectroscopy of a rocky exoplanet's surface: the dust is condensed mineral vapor, and the host is roughly 100-250 times brighter than previously known disintegrating-planet hosts.
  • The presence of both a leading and a trailing tail turns the tail-length ratio into a direct constraint on radiation pressure, so future observations of individual transits can test whether grain properties vary with time.
  • If the inferred short lifetime is typical, surveys like the one that found this object should uncover more disintegrating planets around bright stars, making them a countable population rather than isolated curiosities.
  • Because the transits have persisted for over a decade in ground-based data, the mass-loss process is continuous on human timescales, allowing repeated follow-up.
  • The planet's longer orbital period and lower equilibrium temperature (about 1820 K) relative to the other three disintegrating planets suggest its dust composition and sublimation behavior may differ, which future spectra can test.

Reading between the lines

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

  • Beyond the paper: if the roughly 10-Earth-masses-per-Gyr loss rate holds, the escaping dust samples the planet's crust in real time, so time-series mineral spectroscopy of this one target could map the composition of a rocky planetary surface without landing on it.
  • Beyond the paper: the wide M-dwarf companion, together with the earlier K2-22 system, hints that wide binaries may be overrepresented among disintegrating planets; a systematic census of companions around all such planets could test whether gravitational perturbations drive these planets inward.
  • Beyond the paper: the optically thick dust-ribbon assumption predicts that very deep transits cannot occur; if a future transit deeper than about 3% is seen, the mass-loss estimate would need to be revised, since the paper's own alternative launch scenario predicts a ceiling near 2%.
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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 reports the discovery of BD+05 4868 Ab, a disintegrating rocky planet transiting a bright K dwarf, based on TESS photometry from Sectors 55 and 82, ten years of ASAS-SN photometry, a resolved multi-band LCOGT/MuSCAT3 transit observation, Keck/NIRC2 adaptive-optics imaging, and NEID radial velocities. The authors characterize the host star and its wide M-dwarf companion, fit a generalized-Gaussian dust-extinction profile to the mean and individual TESS transits, simulate dust-grain trajectories under gravity and radiation pressure, and infer a maximum radiation-pressure parameter beta of about 0.07, grain sizes of roughly 1-10 microns, a dust mass-loss rate of about 10 Earth masses per Gyr, and a remaining planetary lifetime of a few Myr. The central discovery claim is that BD+05 4868 Ab is a fourth disintegrating planet, and the first with clearly detected prominent leading and trailing comet-like dust tails.

Significance. If the discovery holds, this is an important system: it is the fourth known disintegrating planet, the first found by TESS, the longest-period example, and by far the brightest host star, making it a uniquely promising target for compositional and dust-tail follow-up. The observational evidence for the discovery is strong and unusually complete for this class: independent detections in two TESS sectors, a decade-long ground-based detection in ASAS-SN, a resolved multi-band LCOGT transit that confirms the primary as the source, AO imaging that rules out blend contamination, and NEID radial velocities that limit the transiting object to a small terrestrial mass. The paper is also careful to report the model-dependence of its dust interpretations, including alternative launch scenarios in Appendix D. The headline physical quantities, however, depend on several explicit modeling assumptions, and those assumptions are load-bearing for the claimed grain sizes and mass-loss rate.

major comments (3)
  1. [Section 6.4, Eq. (13) and Eq. (14)] The mass-loss rate is estimated by modeling the trailing tail as an optically thick ribbon of height H = 2*<delta>*R_star, length L = phi_c * 2*pi*(a/R_star), and depth D = 2*r with an adopted average grain radius r = 5 microns. This makes M_dust and therefore Mdot directly proportional to the assumed optical-depth regime and to the adopted grain radius. If the tail is not optically thick everywhere, the filling factor lowers the dust mass for the same observed depth; if the mean grain radius is not 5 microns, Mdot scales accordingly. The achromaticity test in Section 5.2 is too weak (reported p-values of 0.37 and 0.50) to break this degeneracy. The authors should propagate the optical-depth and grain-radius dependence explicitly and present the mass-loss rate as a range over these assumptions rather than as a single value.
  2. [Section 6.1, Eqs. (4)-(6)] The inference beta_max = 0.07 rests on equating the fitted scale-length ratio xb/xf = 6 with the ratio of angular drift rates Phi_trail/Phi_lead. This mapping assumes that grains decouple from a Parker wind at the Hill sphere with speed v = 0.4 km/s, that the drift rate is well described by the small-beta expansion, and that the observed scale-length ratio is set solely by orbital dynamics. The same observed tail-length ratio can be produced by different decoupling radii or velocities, by a size-dependent sublimation decay, or by optical-depth gradients in the tails, and the authors' own Appendix D shows that a half-orbit-delayed grain-formation scenario changes the tail heights and requires a different optical depth. The resulting beta range, and hence the claimed 1-10 micron grain sizes, is therefore model-dependent and should be presented as such, with a clear statement of which assumptions drive the result.
  3. [Section 6.2 and Appendix D] The nominal Parker-wind launch scenario is acknowledged by the authors to be problematic because high-beta grains need to backflow through the outflowing wind to form the trailing tail. The alternative scenarios in Appendix D produce materially different tail structures: later decoupling gives tail heights up to about 0.02 R_star and requires tau ~ 2, while surface escape-velocity launch reproduces the heights but is inconsistent with a Parker-wind picture. Because these scenarios bracket the geometry used in the mass-loss estimate, the quoted dust mass-loss rate and disintegration timescale of a few Myr should be framed as conditional on the adopted launch scenario. A self-consistent treatment of dust formation and gas-dust coupling, or an explicit scenario-averaged range, is needed before these quantities can be taken as the paper's central result.
minor comments (5)
  1. [Section 6.2.1, after Eq. (9)] In the sentence following Eq. (9), 'as opposed to grains in the trailing with Delta r of only a few percent' should read 'as opposed to grains in the leading tail', since the text is contrasting the wide trailing tail with the narrow leading tail.
  2. [Figure 1 and Section 2] The caption of Figure 1 states that the folded light curve is binned over 6-minute intervals, but the two TESS sectors were taken with 10-minute and 200-second cadences; the caption should state how the 6-minute bins were formed and whether any interpolation was used.
  3. [Abstract and Table 2] The abstract quotes V = 10.16 for the host star while Section 1 and later text quote a TESS magnitude of 9.18; the two quantities should be defined clearly in the text or Table 2 so that the reader can distinguish Johnson V from TESS magnitude.
  4. [Section 6.4, Eq. (13)] The ribbon model in Eq. (13) would benefit from an explicit statement that D = 2*r is an adopted value rather than a fitted or measured quantity, and that the numerical coefficient in the first approximate equality already uses the optically thick limit.
  5. [Appendix B] The description of the two-exponent generalized-Gaussian fit and the single-exponent model is clear, but the main-text statement in Section 5.1 that 'seven free parameters' were fitted could be made easier to verify by giving the limb-darkening treatment and any fixed parameters immediately before that sentence.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: the discovery and the quantitative dust inferences are self-contained forward-inference chains, with model dependence explicitly acknowledged.

full rationale

The central discovery claim is supported by independent TESS, ASAS-SN, LCOGT, AO, and NEID observations, and the disintegrating-planet interpretation is benchmarked against the externally established framework of prior disintegrating-planet work (Kepler-1520b, KOI-2700b, K2-22b) rather than being derived from the present paper's own fitted values. The fitted tail-length ratio xb/xf ≈ 6 from Section 5 is used as an input to Equation 6 to set βmax ≈ 0.07; the inferred grain sizes (1–10 μm) then follow from Mie-theory radiation-pressure calculations. That is a forward chain from an observed shape parameter to a different physical quantity, not a re-derivation of the input. The mass-loss estimate in Section 6.4 uses an explicitly stated optically-thick ribbon assumption (H = 2⟨δ⟩R⋆, D ≈ 2r with adopted r ≈ 5 μm) and a dust lifetime derived from the same model; it is an order-of-magnitude estimate whose assumptions the paper discloses, including the alternative launch scenarios in Appendix D and the acknowledged 'problematic' backflow in Section 6.2.2. The weak achromaticity test (p-values 0.37 and 0.50) is explicitly labeled preliminary. Self-citations to Rappaport et al. (2012, 2014), van Lieshout & Rappaport (2018), and DeVore et al. (2016) supply background and methodology, but they are not the sole load-bearing justification for any central claim. No fitted parameter is renamed as a prediction, and no uniqueness theorem or ansatz is smuggled in via self-citation. The quantitative properties are model-dependent, but model dependence is not circularity.

Assumptions & free parameters 7 free parameters · 6 assumptions · 0 invented entities

The central discovery, a disintegrating planet with comet-like tails, is an observational result that rests on standard photometric and stellar characterization. The derived physical parameters (grain size, mass loss, lifetime) rest on a chain of adopted assumptions: Parker-wind launch velocity, the beta-to-tail-length mapping, the optically thick ribbon approximation, and an e-folding decay chosen to match the data. These are listed above; no new physical entities are introduced.

free parameters (7)
  • Transit model parameters: xp, Ef, Eb, xf, xb, g, b = xp=-0.97, Ef=0.009, Eb=0.0088, xf=0.58, xb=3.6, g=0.85, b=0.05 (Table 3)
    Seven free parameters fitted to the mean TESS transit profile; scale lengths xf and xb set the tail lengths that drive the beta and grain-size inferences.
  • Dust launch velocity v = 0.4 km/s (adopted)
    Chosen from Parker-wind models (gamma=1.3, mu=30 m_H, T=1800 K); controls drift rates (Equation 4) and tail heights (Equation 11); a higher v would double heights.
  • Fiducial planet mass M_p = 0.02 M_Earth
    Used to set the Hill radius r_H and the lifetime estimate (2 Myr); not measured, only bounded by the RV upper limit of 6.2 M_Earth.
  • Grain bulk density rho = 3 g/cm^3
    Assumed for all grains; enters the beta calculation (Equation 12) and the dust mass ribbon estimate (Equation 13).
  • Average grain radius r = 5 microns (adopted)
    Used in the dust mass estimate D about 2r; the inferred range is 1 to 10 microns with a degenerate small-grain alternative.
  • Dust decay e-folding time = 2 planetary orbits
    Adopted in the simulations to match the observed angular extent of the tails; not derived from an independent dust sublimation model.
  • Trailing tail e-folding length phi_c = about 0.1 orbital circumference
    Measured from the average trailing tail profile (Appendix C) and used to derive the dust lifetime T_d of about 2.5 orbits.
assumptions (6)
  • domain assumption Dust grains condense at the Hill sphere and decouple from a thermally driven Parker wind
    Used throughout Section 6.1 and the simulations in Section 6.2; the velocity at the Hill sphere is taken as 0.4 km/s.
  • standard math Grains follow Keplerian orbits under gravity reduced by radiation-pressure parameter beta (Equations 2 to 5)
    Orbital mechanics; requires the approximations v/V much less than 1, beta much less than 1, and r_H much less than 1 for Equation 4.
  • ad hoc to paper The ratio of fitted tail scale lengths (xb/xf about 6) directly maps to a maximum beta of 0.07 via Equation 6
    The analytic mapping assumes the leading tail reaches the maximum drift toward the star (beta to 0) and the trailing tail corresponds to beta_max; other dust size distributions could change the mapping.
  • ad hoc to paper Dust extinction decays with a fixed e-folding time of 2 planetary orbits in the simulations
    Chosen to match the observed angular extent of the tails (Section 6.2); not derived from a physical sublimation model.
  • ad hoc to paper The trailing dust tail can be approximated as an optically thick ribbon of height 2 times average depth times R_star, length phi_c times 2 pi (a/R_star), and depth about 10 microns
    This geometric approximation (Section 6.4) is used to estimate the dust mass and mass-loss rate.
  • domain assumption Mie scattering with assumed refractive indices for iron, quartz, corundum, and fayalite, integrated over a Planck spectrum at Teff, describes radiation pressure on grains
    Used in Equation 12 to convert beta to grain size; grain compositions are not known.

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Cite this review

Pith. "Pith review of A Disintegrating Rocky Planet with Prominent Comet-like Tails Around a Bright Star." pith.science (2026). https://pith.science/paper/NOE2KZME

@misc{pith2026250105431,
  author       = {Pith},
  title        = {Pith review of: A Disintegrating Rocky Planet with Prominent Comet-like Tails Around a Bright Star},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/NOE2KZME}},
  note         = {Machine review of arXiv:2501.05431}
}
abstract

We report the discovery of BD+05$\,$4868$\,$Ab, a transiting exoplanet orbiting a bright ($V=10.16$) K-dwarf (TIC 466376085) with a period of 1.27 days. Observations from NASA's Transiting Exoplanet Survey Satellite (TESS) reveal variable transit depths and asymmetric transit profiles that are characteristic of comet-like tails formed by dusty effluents emanating from a disintegrating planet. Unique to BD+05$\,$4868$\,$Ab is the presence of prominent dust tails in both the trailing and leading directions that contribute to the extinction of starlight from the host star. By fitting the observed transit profile and analytically modeling the drift of dust grains within both dust tails, we infer large grain sizes ($\sim1-10\,\mu$m) and a mass loss rate of $10\,M_{\rm \oplus}\,$Gyr$^{-1}$, suggestive of a lunar-mass object with a disintegration timescale of only several Myr. The host star is probably older than the Sun and is accompanied by an M-dwarf companion at a projected physical separation of 130 AU. The brightness of the host star, combined with the planet's relatively deep transits ($0.8-2.0\%$), presents BD+05$\,$4868$\,$Ab as a prime target for compositional studies of rocky exoplanets and investigations into the nature of catastrophically evaporating planets.

Figures

Figures reproduced from arXiv: 2501.05431 by the authors.

Figure 1
Figure 1. TESS light curve of BD+05 4868 A. (a) Normal￾ized and detrended light curves from Sectors 55 and 82. (b) Phase-folded light curve, repeated for two periods. The light curve is folded at a period of 1.271869 days (∼ 30.5 hrs) and binned over 6-minute intervals (red), showing the average transit profile across 29 transits. (c) Close-up of the transit in the phase-folded light curve. from the wind and drift away from t… view at source ↗
Figure 2
Figure 2. (a-b) Light curves of BD+05 4868 A from the All￾Sky Automated Survey for Supernovae (ASAS-SN) folded at a period of 1.271869 days at the ephemerides determined from TESS data. The ASAS-SN light curves are binned over 75-minute intervals. The shaded bands indicate the formal and binned flux uncertainties added in quadrature. (c) A comparison between the TESS and ASAS-SN phase-folded light curves. exposure times were … view at source ↗
Figure 3
Figure 3. A zoomed-in view of the target, BD+05 4868 A, and its fainter binary companion, BD+05 4868 B, located 3.0′′ to the North-East. This image is taken from one of the rp-band frames obtained with LCO 2.0m/MuSCAT3 on the night of UT 2024 October 17. It shows that the two bi￾nary components were resolved in this observation [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figures from the paper (15 more)
Figure 4
Figure 4. Figure 4: LCO 2.0m/MuSCAT3 light curves of the target, BD+05 4868 A, and its fainter binary companion, BD+05 4868 B, obtained on UT 2024 October 17. (a) The light curves of each of the four bands are shown in the top panels, with the data in small gray points overplotted by binn…
Figure 5
Figure 5. Figure 5: Near-infrared adaptive optics imaging and cor￾responding sensitivity curves for BD+05 4868 A in (a) the narrow band J continuum (Jcont) and in (b) the narrow band K continuum (Kcont). The increased uncertainty at ∆arcsec ∼ 3.0 ′′ is caused by the presence of BD+05 4868…
Figure 6
Figure 6. Figure 6: Spectral energy distribution (SED) of BD+05 4868 AB. The crosses show the observed broadband photometry, with horizontal widths indicating the filter bandwidths. The circles represent the model fluxes in the corresponding bands. Colors denote whether the observa￾tion c…
Figure 7
Figure 7. Figure 7: The fit to the mean transit profile of BD+05 4868 A using the transit model T (ϕ), which convolves the dust extinction profile Y(d) (Eqn. 1) with the stellar disk. (a) Decomposition of Y(d) as a superposition of two Generalized Gaussian distributions representing the t…
Figure 8
Figure 8. Figure 8: Individual transits of BD+05 4868 Ab from the TESS light curve. Transits are numbered based on the cycle count from the first transit at t0,#1 = 2459798.2587 (BJD), taking into account the presence of gaps in the light curve. Transits 1-18 are from TESS Sector 55, whil…
Figure 9
Figure 9. Figure 9: Properties of the single transit observed with LCOGT multi-wavelength photometry. The points are plot￾ted at approximately the central wavelength of the four MuS￾CAT3 bandpasses. (a) A comparison of measured transit depths across the four LCO bandpasses. (b) Integrated…
Figure 10
Figure 10. Figure 10: (a) Distribution of dust grain distances from the planet over time for an impulsive dust ejection event. The colored curves represent different numbers of elapsed orbits since the release. Values of β are drawn from a uni￾form distribution U, while H denotes the Heavi…
Figure 11
Figure 11. Figure 11: 3D simulation of 50,000 dust grains in the co-rotating frame of the orbiting planet, integrated for up to 30 planetary orbits. The host star is shown to scale, while the planet’s size is inflated by a factor of 50 in panels (a) and (c) for visual clarity. (a) A view f…
Figure 12
Figure 12. Figure 12: Trajectories of simulated dust grains as viewed in the x − y plane, with each trajectory colored by the β value of its corresponding grain. The parameters of this sim￾ulation are similar to those presented in [PITH_FULL_IMAGE:figures/full_fig_p014_12.png]
Figure 13
Figure 13. Figure 13: (a) Radiation pressure cross-sections calculated using Mie theory. The cross-sections are normalized by the geometric cross section of the dust grain and are displayed as a function of the grain size (radius) r. Solid curves show cross-sections for illustrative materi…
Figure 14
Figure 14. Figure 14: Simulated contributions to the transit profile. The black, orange, blue, and red curves are the dust extinc￾tion profile, the absorption profile of the transit, the for￾ward scattering peak, and the net observed transit profile. These results were computed using a rep…
Figure 15
Figure 15. Figure 15: Detection limits of the NEID radial velocity (RV) observations in Section 4.1, below which the RV data is insensitive to the presence of a companion to BD+05 4868 A. Shown are curves for three orbital inclination angles (i) of the companion. The spikes at 1 and 2 days…
Figure 16
Figure 16. Figure 16: Corner plot of the posterior distribution to the fit to the mean transit profile of BD+05 4868 A’s TESS light curve. This paper is also based on observations made with the MuSCAT instruments, developed by the Astrobiology Center (ABC) in Japan, the University of Tokyo…
Figure 17
Figure 17. Figure 17: Measured properties from the fitting of individual transits from the TESS light curves in [PITH_FULL_IMAGE:figures/full_fig_p022_17.png]
Figure 18
Figure 18. Figure 18: Same as [PITH_FULL_IMAGE:figures/full_fig_p023_18.png]

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Pith tools

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