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Orbital Dynamics of the Solar Basin
High Energy Physics - Phenomenology · Submitted 28 Aug 2024
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Our main results are that the effective lifetime of a solar basin at Earth's location is $\tau_{\rm eff} = 1.20\pm 0.09 \,\mathrm{Gyr}$, and that there is annual (semi-annual) modulation of the basin density with known phase and amplitude at the fractional level of 6.5% (2.2%).
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The abstract, sentence by sentence
We study the dynamics of the solar basin -- the accumulated population of weakly-interacting particles on bound orbits in the Solar System. We focus on particles starting off on Sun-crossing orbits, corresponding to initial conditions of production inside the Sun, and investigate their evolution over the age of the Solar System. A combination of analytic methods, secular perturbation theory, and direct numerical integration of orbits sheds light on the long- and short-term evolution of a population of test particles orbiting the Sun and perturbed by the planets. Our main results are that the effective lifetime of a solar basin at Earth's location is $\tau_{\rm eff} = 1.20\pm 0.09 \,\mathrm{Gyr}$, and that there is annual (semi-annual) modulation of the basin density with known phase and amplitude at the fractional level of 6.5% (2.2%). These results have important implications for direct detection searches of solar basin particles, and the strong temporal modulation signature yields a robust discovery channel. Our simulations can also be interpreted in the context of gravitational capture of dark matter in the Solar System, with consequences for any dark-matter phenomenon that may occur below the local escape velocity.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We study the dynamics of the solar basin -- the accumulated population of weakly-interacting particles on bound orbits in the Solar System. | contribution 0.84 | 0.65 | 0.02 | asserted 0.81 |
| s1 | We focus on particles starting off on Sun-crossing orbits, corresponding to initial conditions of production inside the Sun, and investigate their evolution over the age of the Solar System. | contribution 0.96 | 0.67 | 0.02 | asserted 0.86 |
| s2 | A combination of analytic methods, secular perturbation theory, and direct numerical integration of orbits sheds light on the long- and short-term evolution of a population of test particles orbiting the Sun and perturbed by the planets. | method 0.99 | 0.83 | 0.02 | asserted 0.91 |
| s3 | Our main results are that the effective lifetime of a solar basin at Earth's location is $\tau_{\rm eff} = 1.20\pm 0.09 \,\mathrm{Gyr}$, and that there is annual (semi-annual) modulation of the basin density with known phase and amplitude at the fractional level of 6.5% (2.2%). | result 1.00 | 0.96 | 0.97 | asserted 1.00 |
| s4 | These results have important implications for direct detection searches of solar basin particles, and the strong temporal modulation signature yields a robust discovery channel. | interpretation 1.00 | 0.48 | 0.10 | asserted 0.98 |
| s5 | Our simulations can also be interpreted in the context of gravitational capture of dark matter in the Solar System, with consequences for any dark-matter phenomenon that may occur below the local escape velocity. | interpretation 1.00 | 0.56 | 0.03 | hedged possibility 0.78 |
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The paper
Original abstract
We study the dynamics of the solar basin -- the accumulated population of weakly-interacting particles on bound orbits in the Solar System. We focus on particles starting off on Sun-crossing orbits, corresponding to initial conditions of production inside the Sun, and investigate their evolution over the age of the Solar System. A combination of analytic methods, secular perturbation theory, and direct numerical integration of orbits sheds light on the long- and short-term evolution of a population of test particles orbiting the Sun and perturbed by the planets. Our main results are that the effective lifetime of a solar basin at Earth's location is $\tau_{\rm eff} = 1.20\pm 0.09 \,\mathrm{Gyr}$, and that there is annual (semi-annual) modulation of the basin density with known phase and amplitude at the fractional level of 6.5% (2.2%). These results have important implications for direct detection searches of solar basin particles, and the strong temporal modulation signature yields a robust discovery channel. Our simulations can also be interpreted in the context of gravitational capture of dark matter in the Solar System, with consequences for any dark-matter phenomenon that may occur below the local escape velocity.
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References
How the literature uses it
1 arXiv paper cite this in 2 sentences
What it cites · 52 sentences without a confident label
Contests 4 papers
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Our results show that previous analyses [ref] , which assumed that large volumes of phase space would remain unmixed over the lifetime of the Solar System (the “hole” proposed in [ref] ), ignored important physical effects.
Dark matter in the solar system I: The distribution function of WIMPs at the Earth from solar capture · Conclusions · contest 0.93
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Our results show that previous analyses [ref] , which assumed that large volumes of phase space would remain unmixed over the lifetime of the Solar System (the “hole” proposed in [ref] ), ignored important physical effects.
Dark matter in the solar system III: The distribution function of WIMPs at the Earth from gravitational capture · Conclusions · contest 0.93
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Our results show that previous analyses [ref] , which assumed that large volumes of phase space would remain unmixed over the lifetime of the Solar System (the “hole” proposed in [ref] ), ignored important physical effects.
WIMP diffusion in the solar system including solar depletion and its effect on Earth capture rates · Conclusions · contest 0.93
Compares with 3 papers
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[ref] , wherein the effective lifetime would equal the full lifetime of the Sun $τ_eff = t_⊙≈4.5 Gyr$ [ref] .[We conservatively take the fiducial age of the Sun to be slightly lower than these currently most precise estimates, because the overall structure of the Solar System is somewhat uncertain shortly after formation (see section [ref]).] This solidifies the solar basin direct detection limits on axions [ref] and dark photons [ref] , with the updated constraints from the latter providing the most stringent DM-independent bound on the kinetic mixing parameter over significant parts of the mass range $10 eV$–$3 keV$.
Stellar Basins of Gravitationally Bound Particles · Executive summary · 0.96
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[ref] , wherein the effective lifetime would equal the full lifetime of the Sun $τ_eff = t_⊙≈4.5 Gyr$ [ref] .[We conservatively take the fiducial age of the Sun to be slightly lower than these currently most precise estimates, because the overall structure of the Solar System is somewhat uncertain shortly after formation (see section [ref]).] This solidifies the solar basin direct detection limits on axions [ref] and dark photons [ref] , with the updated constraints from the latter providing the most stringent DM-independent bound on the kinetic mixing parameter over significant parts of the mass range $10 eV$–$3 keV$.
Dark Photons in the Solar Basin · Executive summary · 0.96
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[ref] , wherein the effective lifetime would equal the full lifetime of the Sun $τ_eff = t_⊙≈4.5 Gyr$ [ref] .[We conservatively take the fiducial age of the Sun to be slightly lower than these currently most precise estimates, because the overall structure of the Solar System is somewhat uncertain shortly after formation (see section [ref]).] This solidifies the solar basin direct detection limits on axions [ref] and dark photons [ref] , with the updated constraints from the latter providing the most stringent DM-independent bound on the kinetic mixing parameter over significant parts of the mass range $10 eV$–$3 keV$.
Solar Models with Helium and Heavy Element Diffusion · Executive summary · 0.96
Cites as background 9 papers
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Axion-like particles with a pseudoscalar coupling to electrons are another quintessential class of BSM particles which could be produced in the Sun and then detected in terrestrial experiments, either through its relativistic flux [ref] or its solar basin [ref] .
Stellar Basins of Gravitationally Bound Particles · Executive summary · 0.93
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Axion-like particles with a pseudoscalar coupling to electrons are another quintessential class of BSM particles which could be produced in the Sun and then detected in terrestrial experiments, either through its relativistic flux [ref] or its solar basin [ref] .
Solar axion flux from the axion-electron coupling · Executive summary · 0.93
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This “secular evolution” has been studied extensively over the centuries; modern studies of secular evolution describe effects on the orbits of planets [ref] , asteroids [ref] , and satellites [ref] .
Constructing the secular architecture of the solar system II: The terrestrial planets · Analytical dynamics · 0.99
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