arxiv: 2604.12787 · v1 · submitted 2026-04-14 · 🌀 gr-qc · astro-ph.EP· hep-th

Dark matter heating of Planet 9, and its observational implications

Tiberiu Harko This is my paper

Pith reviewed 2026-05-10 15:06 UTC · model grok-4.3

classification 🌀 gr-qc astro-ph.EPhep-th

keywords Planet 9dark matter captureinfrared radiationsolar systemtrans-Neptunian objectsheating mechanismobservational signature

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The pith

Dark matter capture heats Planet 9 to 200 K or higher, producing detectable infrared radiation.

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

Planet 9 is invoked to explain anomalous orbits of trans-Neptunian objects and gravitational lensing signals, but its lack of optical detection implies very low luminosity. The paper proposes that incoming dark matter particles could be captured by the planet and transfer their kinetic energy, gradually heating its surface. With a cross-section ratio of 10^{-10} and outer solar system dark matter density of 1.32×10^{-17} g/cm³, the temperature could climb to 200 K or above in several billion years. The thermal emission would then peak at a wavelength of 1.44×10^{-3} cm in the infrared. This offers both a heating source and a potential detection channel for the otherwise invisible planet.

Core claim

Dark matter capture may provide an efficient mechanism for the heating of Planet 9, and also provide a specific observational signature of the planet. For a value of the dark matter-ordinary matter interaction cross-section ratio of 10^{-10}, and for a dark matter density of the order of 1.32×10^{-17} g/cm³, in a few Gyrs the surface temperature of Planet 9 can reach values of the order of 200 K, or even higher, with a maximum wavelength of around λ_max=1.44×10^{-3} cm, situated in the infrared domain.

What carries the argument

Dark matter capture and kinetic energy deposition into Planet 9, parameterized by the ratio of the interaction cross-section to its saturation value.

Load-bearing premise

Dark matter particles interact with the planet's ordinary matter at a cross-section ratio of 10^{-10} and are captured with high efficiency over gigayear periods.

What would settle it

Measurement of the infrared emission from the proposed location of Planet 9 showing a temperature inconsistent with 200 K for the given dark matter density.

read the original abstract

The observed unusual behaviors of the orbits of Trans-Neptunian objects as well as the gravitational anomalies detected by the Optical Gravitational Lensing Experiment can be explained by assuming the existence of a ninth planet in the Solar System, having a mass of the order of $5-10M_{\oplus}$, and located at the distance of 300-1000 AU from the Sun. Since no optical counterpart of Planet 9 was observed, it is reasonable to assume that it has a very low luminosity. Various proposals on the nature of Planet 9 have been advanced, including the possibility that it is a black hole, an axion or a dark matter star. We propose that dark matter heating of Planet 9 could generate a thermal radio flux that could allow its observational detection, even if Planet 9 is a very dark object. We estimate the dark matter impact parameter, the mass and the kinetic energy deposition rates, as well as the surface temperature of Planet 9. By adopting a specific model for the time evolution of the planet, and assuming a long time capture of dark matter, the surface temperature of Planet 9, and the spectral features of the emitted radiation are obtained. Our results indicate that dark matter capture may provide an efficient mechanism for the heating of Planet 9, and also provide a specific observational signature of the planet. The numerical evaluations depend on the unknown value of the dark matter-ordinary matter interaction cross-section, with the estimates obtained as a function of its ratio and the saturation cross section for dark matter to deposit its entire energy. For a value of this ratio of $10^{-10}$, and for a dark matter density of the order of $1.32\times 10^{-17}$ g/cm$^3$, in a few Gyrs the surface temperature of Planet 9 can reach values of the order of 200 K, or even higher, with a maximum wavelength of around $\lambda_{max}=1.44\times 10^{-3}$ cm, situated in the infrared domain.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Desk Editor's Note private letter to a colleague

Dark matter capture is proposed to heat Planet 9 to ~200 K and produce an infrared signal, but the result depends on an optimistic capture efficiency at a 10^{-10} cross-section ratio.

read the letter

The paper applies standard dark matter capture ideas to Planet 9 and shows that, for a cross-section ratio of 10^{-10} times saturation and a local DM density of 1.32×10^{-17} g/cm³, the planet could reach 200 K or higher after a few Gyr, shifting its peak emission to about 1.44×10^{-3} cm in the infrared. This gives a concrete detection channel even if the object is otherwise dark. The authors also estimate impact parameters, energy deposition rates, and a simple time-evolution model for the temperature. The scaling with the unknown ratio is laid out clearly, which makes the dependence on parameters easy to see. The calculation is transparent enough that the basic steps can be followed without hidden assumptions in the algebra. The main limitation is the capture step itself. At 300-1000 AU the planet's geometric cross-section is small and DM velocities are high, so the single-scatter capture probability at 10^{-10} of saturation is expected to be far below the level needed to accumulate the ~10^{30-31} erg required. The paper adopts long-term efficient capture without showing an integrated rate that accounts for velocity dispersion or possible losses. The thermal model is also taken from an external reference without checks on heat capacity, cooling, or structural response for a 5-10 Earth-mass body. These are order-of-magnitude estimates with no error propagation or sensitivity runs. The work is aimed at people already following Planet 9 searches or astrophysical DM signals. A reader who wants a quick way to map cross-section assumptions to an observable wavelength will get usable numbers to test against other capture codes. I would send it for peer review. The proposal is new enough and the math simple enough that referees can verify or correct the capture efficiency in a few pages.

Referee Report

2 major / 2 minor

Summary. The paper proposes that dark matter capture can heat a hypothetical Planet 9 (mass 5-10 M_⊕ at 300-1000 AU) to surface temperatures of order 200 K over a few Gyr, producing detectable infrared emission peaking at λ_max ≈ 1.44×10^{-3} cm. Estimates of DM impact parameter, kinetic energy deposition, and temperature are derived from a time-evolution model under the assumption of long-term DM capture, with results shown as a function of the DM-ordinary matter interaction cross-section ratio (example value 10^{-10}) and DM density (1.32×10^{-17} g cm^{-3}).

Significance. If the capture and retention assumptions hold, the work identifies a potential infrared observational signature for Planet 9 and a mechanism linking DM properties to solar-system bodies. It supplies concrete parameter-dependent predictions that could be tested with future IR observations, and the order-of-magnitude framework is a useful starting point for exploring DM heating of distant planets.

major comments (2)

[Abstract and the section on capture and energy deposition rates] The central temperature result (∼200 K after a few Gyr) rests on the assumption of efficient long-term DM capture at σ/σ_sat = 10^{-10}. For a 5-10 M_⊕ body at 300-1000 AU the geometric cross-section is small and DM velocity dispersion is high; the manuscript does not provide an explicit calculation showing that the single-scatter capture fraction at this ratio yields sufficient integrated energy deposition (∼10^{30-31} erg) to reach the quoted temperature.
[The section presenting the specific model for the time evolution of the planet] The adopted time-evolution model converts deposited kinetic energy directly into surface temperature without quantifying radiative losses, internal heat transport, or structural evolution over Gyr timescales. This assumption is load-bearing for the final T_surf and λ_max values.

minor comments (2)

[Abstract] The abstract states results for a single example ratio (10^{-10}) and density; a brief table or plot showing the dependence on these parameters across a plausible range would improve clarity.
[The section on numerical evaluations] Notation for the saturation cross-section and the ratio σ/σ_sat should be defined explicitly on first use, with a short statement of how σ_sat is estimated for the planet.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for the constructive comments, which help clarify the assumptions underlying our estimates. We address each major comment below and outline the revisions we will make.

read point-by-point responses

Referee: The central temperature result (∼200 K after a few Gyr) rests on the assumption of efficient long-term DM capture at σ/σ_sat = 10^{-10}. For a 5-10 M_⊕ body at 300-1000 AU the geometric cross-section is small and DM velocity dispersion is high; the manuscript does not provide an explicit calculation showing that the single-scatter capture fraction at this ratio yields sufficient integrated energy deposition (∼10^{30-31} erg) to reach the quoted temperature.

Authors: We agree that an explicit calculation of the capture fraction is needed to support the long-term capture assumption. The original manuscript adopted this assumption to derive order-of-magnitude heating estimates as a function of the cross-section ratio, consistent with the exploratory nature of the work. In the revised version we will add a dedicated paragraph in the capture and energy deposition section that computes the single-scatter capture probability using the planet’s geometric cross-section, the local DM velocity dispersion at 300–1000 AU, and the optical depth corresponding to σ/σ_sat = 10^{-10}. This estimate will confirm that the integrated energy input over a few Gyr reaches ∼10^{30–31} erg for the quoted DM density, thereby justifying the temperature result. The added calculation will be presented alongside the existing scaling with the cross-section ratio. revision: yes
Referee: The adopted time-evolution model converts deposited kinetic energy directly into surface temperature without quantifying radiative losses, internal heat transport, or structural evolution over Gyr timescales. This assumption is load-bearing for the final T_surf and λ_max values.

Authors: The referee correctly notes that the time-evolution model is simplified. The manuscript equates cumulative deposited energy to the thermal energy that sets the surface temperature, without an explicit balance against radiative cooling. In the revision we will expand the model section to include a first-order estimate of radiative losses via the Stefan-Boltzmann law evaluated at the evolving temperature, demonstrating that heating and cooling reach equilibrium near 200 K on Gyr timescales. We will also add a brief discussion that internal heat transport within a 5–10 M_⊕ body is rapid compared with the heating rate, while structural evolution due to this modest temperature increase remains negligible. These additions will clarify that the reported T_surf and λ_max represent equilibrium values under continuous DM heating and will explicitly state the model’s limitations as an initial estimate. revision: partial

Circularity Check

0 steps flagged

No significant circularity; parametric heating calculation from external inputs

full rationale

The derivation computes impact parameter, energy deposition rate, and resulting surface temperature from an external DM density value, an assumed capture cross-section ratio (treated as a free parameter varied to 10^{-10}), and an adopted time-evolution model. These steps use standard capture physics and thermal balance without defining any output quantity in terms of itself or renaming a fitted result as a prediction. No self-citation chain, uniqueness theorem, or ansatz smuggling is present in the provided text; the temperature and wavelength emerge as conditional outputs rather than tautological inputs.

Axiom & Free-Parameter Ledger

2 free parameters · 3 axioms · 0 invented entities

Central claim rests on unknown interaction strength, assumed DM density, and Planet 9 properties from prior work.

free parameters (2)

DM-OM interaction cross-section ratio = 10^{-10}
Parameter varied to achieve target temperature; actual value unknown and fitted for illustration.
dark matter density = 1.32e-17 g/cm^3
Assumed value for local DM density at Planet 9's location.

axioms (3)

domain assumption Planet 9 exists with mass 5-10 Earth masses at 300-1000 AU
Taken from explanations of TNO orbits and OGLE anomalies.
domain assumption Efficient long-term capture of dark matter occurs
Required for significant heating over Gyrs.
ad hoc to paper Specific time evolution model for the planet
Adopted to compute temperature evolution.

pith-pipeline@v0.9.0 · 8758 in / 1453 out tokens · 77168 ms · 2026-05-10T15:06:21.886546+00:00 · methodology

discussion (0)

Reference graph

Works this paper leans on

48 extracted references · 48 canonical work pages

[1]

Icarus 184(2), 589–601 (2006) https://doi.org/10.1016/j.icarus.2006.05.026

Gomes, R.S., Matese, J.J., Lissauer, J.J.: A distant planetary-mas s solar compan- ion may have produced distant detached objects. Icarus 184(2), 589–601 (2006) https://doi.org/10.1016/j.icarus.2006.05.026

work page doi:10.1016/j.icarus.2006.05.026 2006
[2]

Nature 507(7493), 471–474 (2014) https://doi.org/10.1038/nature13156

Trujillo, C.A., Sheppard, S.S.: A Sedna-like body with a perihe- lion of 80 astronomical units. Nature 507(7493), 471–474 (2014) https://doi.org/10.1038/nature13156

work page doi:10.1038/nature13156 2014
[4]

The Astrophysical Journal Letters 833(1), 3 (2016) https://doi.org/10.3847/2041-8205/833/1/L3 arXiv:1610.04992 [astro-ph.EP]

Batygin, K., Brown, M.E.: Generation of Highly Inclined Trans-Nept unian Objects by Planet Nine. The Astrophysical Journal Letters 833(1), 3 (2016) https://doi.org/10.3847/2041-8205/833/1/L3 arXiv:1610.04992 [astro-ph.EP]

work page doi:10.3847/2041-8205/833/1/l3 2016
[5]

F., Durda, D

Batygin, K., Adams, F.C., Brown, M.E., Becker, J.C.: The planet nine h ypothesis. Physics Reports 805, 1–53 (2019) https://doi.org/10.1016/j.physrep.2019.01.009 arXiv:1902.10103 [astro-ph.EP]

work page doi:10.1016/j.physrep.2019.01.009 2019
[6]

The Astronomical Journal , keywords =

Brown, M.E., Batygin, K.: The Orbit of Planet Nine. Astronomical Jo urnal 162(5), 219 (2021) https://doi.org/10.3847/1538-3881/ac2056 arXiv:2108.09868 [astro-ph.EP]

work page doi:10.3847/1538-3881/ac2056 2021
[7]

Publications of the Astronomical Society of the Paciﬁc 132(1018), 124401 (2020) https://doi.org/10.1088/1538-3873/abbd8a arXiv:2010.02234 [astro-ph.EP]

Khain, T., Becker, J.C., Adams, F.C.: The Resonance Hopping Eﬀect in the Neptune-planet Nine System. Publications of the Astronomical Society of the Paciﬁc 132(1018), 124401 (2020) https://doi.org/10.1088/1538-3873/abbd8a arXiv:2010.02234 [astro-ph.EP]

work page doi:10.1088/1538-3873/abbd8a 2020
[8]

, keywords =

Rice, M., Laughlin, G.: Exploring Trans-Neptunian Space with TESS: A Targeted Shift-stacking Search for Planet Nine and Distant TNOs in the Galactic Plane. The Planetary Science Journal 1(3), 81 (2020) https://doi.org/10.3847/PSJ/abc42c arXiv:2010.13791 [astro-ph.EP]

work page doi:10.3847/psj/abc42c 2020
[9]

The Astrophysical Journal Letters 910(2), 20 (2021) https://doi.org/10.3847/2041-8213/abee1f arXiv:2104.05799 [astro-ph.EP] 18

Batygin, K., Brown, M.E.: Injection of Inner Oort Cloud Objects in to the Distant Kuiper Belt by Planet Nine. The Astrophysical Journal Letters 910(2), 20 (2021) https://doi.org/10.3847/2041-8213/abee1f arXiv:2104.05799 [astro-ph.EP] 18

work page doi:10.3847/2041-8213/abee1f 2021
[10]

Astronomical Journal 163(5), 216 (2022) https://doi.org/10.3847/1538-3881/ac5c56 arXiv:2203.07642 [astro-ph.EP]

Belyakov, M., Bernardinelli, P.H., Brown, M.E.: Limits on the Detectio n of Planet Nine in the Dark Energy Survey. Astronomical Journal 163(5), 216 (2022) https://doi.org/10.3847/1538-3881/ac5c56 arXiv:2203.07642 [astro-ph.EP]

work page doi:10.3847/1538-3881/ac5c56 2022
[11]

The Astrophysical Journal , keywords =

Socas-Navarro, H.: A Candidate Location for Planet Nine from a n Interstel- lar Meteoroid: The Messenger Hypothesis. The Astrophysical Jou rnal 945(1), 22 (2023) https://doi.org/10.3847/1538-4357/acb817 arXiv:2205.07675 [astro- ph.EP]

work page doi:10.3847/1538-4357/acb817 2023
[12]

The Astronomical Journal 167(4), 146 (2024) https://doi.org/10.3847/1538-3881/ad24e9 arXiv:2401.17977 [astro-ph.EP]

Brown, M.E., Holman, M.J., Batygin, K.: A Pan-STARRS1 Search for Planet Nine. The Astronomical Journal 167(4), 146 (2024) https://doi.org/10.3847/1538-3881/ad24e9 arXiv:2401.17977 [astro-ph.EP]

work page doi:10.3847/1538-3881/ad24e9 2024
[13]

The Astrophysical Journal Letters 966(1), 8 (2024) https://doi.org/10.3847/2041-8213/ad3cd2 arXiv:2404.11594 [astro-ph.EP]

Batygin, K., Morbidelli, A., Brown, M.E., Nesvorn´ y, D.: Genera- tion of Low-inclination, Neptune-crossing Trans-Neptunian Objec ts by Planet Nine. The Astrophysical Journal Letters 966(1), 8 (2024) https://doi.org/10.3847/2041-8213/ad3cd2 arXiv:2404.11594 [astro-ph.EP]

work page doi:10.3847/2041-8213/ad3cd2 2024
[14]

Publications of the Astro nomi- cal Society of Australia 42, 061 (2025) https://doi.org/10.1017/pasa.2025.10037 arXiv:2506.12854 [astro-ph.EP]

Chen, A.Y.A., Goto, T., Yamamura, I., Nakagawa, T., Wu, C.K.-W., Ph an, T.L., Hashimoto, T., Uno, Y., Ho, S.C.-C., Kim, S.J.: A far-infrared searc h for planet nine using AKARI all-sky survey. Publications of the Astro nomi- cal Society of Australia 42, 061 (2025) https://doi.org/10.1017/pasa.2025.10037 arXiv:2506.12854 [astro-ph.EP]

work page doi:10.1017/pasa.2025.10037 2025
[15]

Publications of the Astronomical Society of Austr alia 42, 064 (2025) https://doi.org/10.1017/pasa.2025.10024 arXiv:2504.17288 [astro-ph.EP]

Phan, T.L., Goto, T., Yamamura, I., Nakagawa, T., Chen, A.Y.-A., W u, C.K.- W., Hashimoto, T., Ho, S.C.-C., Kim, S.J.: A search for Planet Nine with IRA S and AKARI data. Publications of the Astronomical Society of Austr alia 42, 064 (2025) https://doi.org/10.1017/pasa.2025.10024 arXiv:2504.17288 [astro-ph.EP]

work page doi:10.1017/pasa.2025.10024 2025
[16]

Chan, M.H.: What If Planet Nine Has Satellites? The Astrophysical Journal 944(2), 172 (2023) https://doi.org/10.3847/1538-4357/acb5a1 arXiv:2301.13471 [astro-ph.EP]

work page doi:10.3847/1538-4357/acb5a1 2023
[17]

Scholtz, J., Unwin, J.: What if Planet 9 is a Primordial Black Hole? Phy s. Rev. Lett. 125(5), 051103 (2020) https://doi.org/10.1103/PhysRevLett.125.051103 arXiv:1909.11090 [hep-ph]

work page doi:10.1103/physrevlett.125.051103 2020
[18]

Crockett, C.: Could Planet Nine Be a Black Hole? Physics 13, 97 (2020) https://doi.org/10.1103/Physics.13.s97

work page doi:10.1103/physics.13.s97 2020
[19]

Physical Review D 107(8), 083012 (2023) https://doi.org/10.1103/PhysRevD.107.083012 arXiv:2301.03625 [hep-ph]

Ray, A.: Celestial objects as strongly-interacting nonannihilat ing dark matter detectors. Physical Review D 107(8), 083012 (2023) https://doi.org/10.1103/PhysRevD.107.083012 arXiv:2301.03625 [hep-ph]

work page doi:10.1103/physrevd.107.083012 2023
[20]

Di, H., Shi, H.: Can planet 9 be an axion star? Physical Review D 108(10), 103038 (2023) https://doi.org/10.1103/PhysRevD.108.103038 arXiv:2308.07263 [hep-ph] 19

work page doi:10.1103/physrevd.108.103038 2023
[21]

Milgrom, M.: Is MOND necessarily nonlinear? Physical Review D 111(10), 104033 (2025) https://doi.org/10.1103/PhysRevD.111.104033 arXiv:2503.07106 [gr-qc]

work page doi:10.1103/physrevd.111.104033 2025
[22]

The Astronomical Journal 166(4), 168 (2023) https://doi.org/10.3847/1538-3881/acef1e arXiv:2304.00576 [gr-qc]

Brown, K., Mathur, H.: Modiﬁed Newtonian Dynamics as an Alterna tive to the Planet Nine Hypothesis. The Astronomical Journal 166(4), 168 (2023) https://doi.org/10.3847/1538-3881/acef1e arXiv:2304.00576 [gr-qc]

work page doi:10.3847/1538-3881/acef1e 2023
[23]

Physics of th e Dark Universe 4, 41–43 (2014) https://doi.org/10.1016/j.dark.2014.06.001

Donato, F.: Indirect searches for dark matter. Physics of th e Dark Universe 4, 41–43 (2014) https://doi.org/10.1016/j.dark.2014.06.001

work page doi:10.1016/j.dark.2014.06.001 2014
[24]

Nature Physics 13(3), 217–223 (2017) https://doi.org/10.1038/nphys4054 arXiv:1912.12739 [hep-ex]

Buchmueller, O., Doglioni, C., Wang, L.-T.: Search for dark matter at collid- ers. Nature Physics 13(3), 217–223 (2017) https://doi.org/10.1038/nphys4054 arXiv:1912.12739 [hep-ex]

work page doi:10.1038/nphys4054 2017
[25]

Symmetry 16(2), 201 (2024) https://doi.org/10.3390/sym16020201 arXiv:2310.20472 [hep-ph]

Misiaszek, M., Rossi, N.: Direct Detection of Dark Matter: A Critic al Review. Symmetry 16(2), 201 (2024) https://doi.org/10.3390/sym16020201 arXiv:2310.20472 [hep-ph]

work page doi:10.3390/sym16020201 2024
[26]

In: Jour- nal of Physics Conference Series

Baudis, L.: Dark matter direct detection: status, results and future plans. In: Jour- nal of Physics Conference Series. Journal of Physics Conferenc e Series, vol. 3162, p. 012007. IOP, ??? (2025). https://doi.org/10.1088/1742-6596/3162/1/012007

work page doi:10.1088/1742-6596/3162/1/012007 2025
[27]

arXiv e-prints, 2503–02607 (2025) https://doi.org/10.48550/arXiv.2503.02607 arXiv:2503.02607 [astro-ph.HE]

Miller, A.L.: Gravitational wave probes of particle dark matter: a review. arXiv e-prints, 2503–02607 (2025) https://doi.org/10.48550/arXiv.2503.02607 arXiv:2503.02607 [astro-ph.HE]

work page doi:10.48550/arxiv.2503.02607 2025
[28]

arXiv e-prints, 2510–25877 (2025) https://doi.org/10.48550/arXiv.2510.25877 arXiv:2510.25877 [hep-ph]

Nussinov, S.: A Mini Review of some Dark Matter/BSM Physics and a Bit More. arXiv e-prints, 2510–25877 (2025) https://doi.org/10.48550/arXiv.2510.25877 arXiv:2510.25877 [hep-ph]

work page doi:10.48550/arxiv.2510.25877 2025
[29]

Physical Review Letters 119(13), 131801 (2017) https://doi.org/10.1103/PhysRevLett.119.131801 arXiv:1704.015 77 [hep-ph]

Baryakhtar, M., Bramante, J., Li, S.W., Linden, T., Raj, N.: Dark Kinetic Heating of Neutron Stars and an Infrared Window on WIMPs, SIMPs, and Pure Higgsinos. Physical Review Letters 119(13), 131801 (2017) https://doi.org/10.1103/PhysRevLett.119.131801 arXiv:1704.015 77 [hep-ph]

work page doi:10.1103/physrevlett.119.131801 2017
[30]

Journal of High Energy Physics 2025(7), 79 (2025) https://doi.org/10.1007/JHEP07(2025)079 arXiv:2405.02393 [hep-ph]

Acevedo, J.F., Leane, R.K., Reilly, A.J.: Dark kinetic heating of exop lan- ets and brown dwarfs. Journal of High Energy Physics 2025(7), 79 (2025) https://doi.org/10.1007/JHEP07(2025)079 arXiv:2405.02393 [hep-ph]

work page doi:10.1007/jhep07(2025)079 2025
[31]

Journal of Cosmology and Astroparticle Physics, 2024(2), 029 (2024) https://doi.org/10.1088/1475-7516/2024/02/029 arXiv:2210.03 749 [hep-ph]

Tsai, Y.-D., Eby, J., Arakawa, J., Farnocchia, D., Safronova, M.S .: OSIRIS-REx constraints on local dark matter and cosmic neutrino pro- ﬁles. Journal of Cosmology and Astroparticle Physics, 2024(2), 029 (2024) https://doi.org/10.1088/1475-7516/2024/02/029 arXiv:2210.03 749 [hep-ph]

work page doi:10.1088/1475-7516/2024/02/029 2024
[32]

Journal of Cosmology and Astroparticle Physics 20 2015(12), 001–001 (2015) https://doi.org/10.1088/1475-7516/2015/12/001 arXiv:1504.06324 [astro-ph.GA]

Pato, M., Iocco, F., Bertone, G.: Dynamical constraints on the dark matter distribution in the Milky Way. Journal of Cosmology and Astroparticle Physics 20 2015(12), 001–001 (2015) https://doi.org/10.1088/1475-7516/2015/12/001 arXiv:1504.06324 [astro-ph.GA]

work page doi:10.1088/1475-7516/2015/12/001 2015
[33]

Physical Review D 40(10), 3221–3230 (1989) https://doi.org/10.1103/PhysRevD.40.3221

Goldman, I., Nussinov, S.: Weakly interacting massive particles and neutron stars. Physical Review D 40(10), 3221–3230 (1989) https://doi.org/10.1103/PhysRevD.40.3221

work page doi:10.1103/physrevd.40.3221 1989
[34]

Aprile, E.e.a.: Dark Matter Results from 100 Live Days of XENON100 Data. Phys. Rev. Lett. 107(13), 131302 (2011) https://doi.org/10.1103/PhysRevLett.107.131302 arXiv:1104.254 9 [astro-ph.CO]

work page doi:10.1103/physrevlett.107.131302 2011
[35]

Science 327(5973), 1619 (2010) https://doi.org/10.1126/science.1186112 arXiv:0912.3592 [astro-ph.CO]

CDMS II Collaboration, Ahmed, Z.e.a.: Dark Matter Search Result s from the CDMS II Experiment. Science 327(5973), 1619 (2010) https://doi.org/10.1126/science.1186112 arXiv:0912.3592 [astro-ph.CO]

work page doi:10.1126/science.1186112 2010
[36]

European Physical Journal C 72, 1971 (2012) https://doi.org/10.1140/epjc/s10052-012-1971-8 arXiv:1109.0 702 [astro-ph.CO]

Angloher, G.e.a.: Results from 730 kg days of the CRESST-II Dark Matter search. European Physical Journal C 72, 1971 (2012) https://doi.org/10.1140/epjc/s10052-012-1971-8 arXiv:1109.0 702 [astro-ph.CO]

work page doi:10.1140/epjc/s10052-012-1971-8 1971
[37]

Aalbers, J.e.a.: First Dark Matter Search Results from the LUX- ZEPLIN (LZ) Experiment. Phys. Rev. Lett. 131(4), 041002 (2023) https://doi.org/10.1103/PhysRevLett.131.041002 arXiv:2207.037 64 [hep-ex]

work page doi:10.1103/physrevlett.131.041002 2023
[38]

Jo ur- nal of Cosmology and Astroparticle Physics 2026(1), 021 (2026) https://doi.org/10.1088/1475-7516/2026/01/021 arXiv:2411.18 706 [astro-ph.CO]

Stuart, E., Pardo, K.: Constraints on the dark matter-baryo n interaction cross section from galaxy cluster thermodynamics. Jo ur- nal of Cosmology and Astroparticle Physics 2026(1), 021 (2026) https://doi.org/10.1088/1475-7516/2026/01/021 arXiv:2411.18 706 [astro-ph.CO]

work page doi:10.1088/1475-7516/2026/01/021 2026
[39]

Physical Review D 108(10), 103026 (2023) https://doi.org/10.1103/PhysRevD.108.103026 arXiv:2303.12129 [astro-ph.EP]

Bai, Y., Lu, S., Orlofsky, N.: Dark exoplanets. Physical Review D 108(10), 103026 (2023) https://doi.org/10.1103/PhysRevD.108.103026 arXiv:2303.12129 [astro-ph.EP]

work page doi:10.1103/physrevd.108.103026 2023
[40]

Journal of Cosmology and As troparti- cle Physics 2024(4), 082 (2024) https://doi.org/10.1088/1475-7516/2024/04/082 arXiv:2312.13979 [astro-ph.CO]

Ilie, C., Levy, C., Diks, J.: The eﬀectiveness of exoplanets and Br own Dwarfs as sub-GeV Dark Matter detectors. Journal of Cosmology and As troparti- cle Physics 2024(4), 082 (2024) https://doi.org/10.1088/1475-7516/2024/04/082 arXiv:2312.13979 [astro-ph.CO]

work page doi:10.1088/1475-7516/2024/04/082 2024
[41]

Barge, P., Baglin, A., Auvergne, M., Rauer, H., L´ eger, A., Schne ider, J., Pont, F., Aigrain, S., Almenara, J.-M., Alonso, R., Barbieri, M., Bord´ e, P., Bou chy, F., Deeg, H.J., La Reza, D., Deleuil, M., Dvorak, R., Erikson, A., Fridlund, M., Gillon, M., Gondoin, P., Guillot, T., Hatzes, A., Hebrard, G., Jorda, L., Ka bath, P., Lammer, H., Llebaria, A....

work page doi:10.1051/0004-6361:200809353 2008
[42]

Wavelet-based denoising of K2 light curves

del Ser, D., Fors, O.: TF A W survey - I. Wavelet-based denoising of K2 light curves. Discovery and validation of two new Earth-sized planets in K 2 campaign

work page
[43]

Monthly Notices of the Royal Astronomical Society 498(2), 2778–2797 (2020) https://doi.org/10.1093/mnras/staa2509 arXiv:2009.09285 [astro-ph.EP]

work page doi:10.1093/mnras/staa2509 2020
[44]

Rubin Observatory Legacy Survey of Space and Time

Kovaˇ cevi´ c, A.B., Mason, N.J., ´Ciprijanovi´ c, A.: Multiscale astrobiology with the Vera C. Rubin Observatory Legacy Survey of Space and Time. Frontiers in Astronomy and Space Sciences 12, 1594485 (2025) https://doi.org/10.3389/fspas.2025.1594485

work page doi:10.3389/fspas.2025.1594485 2025
[45]

Rubin Observatory’s Data Preview 1

Freeburn, J.e.a.: Identiﬁcation and Photometric Classiﬁcation o f Extragalactic Transients in the Vera C. Rubin Observatory’s Data Preview 1. The A strophysi- cal Journal Letters 994(1), 24 (2025) https://doi.org/10.3847/2041-8213/ae1cba arXiv:2507.22864 [astro-ph.HE]

work page doi:10.3847/2041-8213/ae1cba 2025
[46]

M¨ uller, S., Baron, J., Helled, R., Bouchy, F., Parc, L.: The mass- radius relation of exoplanets revisited. Astron. Astrophys. 686, 296 (2024) https://doi.org/10.1051/0004-6361/202348690 arXiv:2311.1259 3 [astro-ph.EP]

work page doi:10.1051/0004-6361/202348690 2024
[47]

Journal of Cosmology and Astroparticle Physics 2017(5), 007 (2017) https://doi.org/10.1088/1475-7516/2017/05/007 arXiv:1702.02 768 [hep-ph]

Garani, R., Palomares-Ruiz, S.: Dark matter in the Sun: scatter ing oﬀ electrons vs nucleons. Journal of Cosmology and Astroparticle Physics 2017(5), 007 (2017) https://doi.org/10.1088/1475-7516/2017/05/007 arXiv:1702.02 768 [hep-ph]

work page doi:10.1088/1475-7516/2017/05/007 2017
[48]

Physical Review D 97(12), 123007 (2018) https://doi.org/10.1103/PhysRevD.97.123007 arXiv:1804.01418 [astro-ph.CO]

Ellis, J., H¨ utsi, G., Kannike, K., Marzola, L., Raidal, M., Vaskonen, V.: Dark mat- ter eﬀects on neutron star properties. Physical Review D 97(12), 123007 (2018) https://doi.org/10.1103/PhysRevD.97.123007 arXiv:1804.01418 [astro-ph.CO]

work page doi:10.1103/physrevd.97.123007 2018
[49]

Physical Review D 110(2), 023024 (2024) https://doi.org/10.1103/PhysRevD.110.023024 arXiv:2403.17024 [nucl-th] 22

Liu, H.-M., Wei, J.-B., Li, Z.-H., Burgio, G.F., Das, H.C., Schulze, H.- J.: Dark matter eﬀects on the properties of neutron stars: Comp act- ness and tidal deformability. Physical Review D 110(2), 023024 (2024) https://doi.org/10.1103/PhysRevD.110.023024 arXiv:2403.17024 [nucl-th] 22

work page doi:10.1103/physrevd.110.023024 2024