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Hao Jiao

Publications and source records attributed to Hao Jiao.

13 recordsLinked to original sources
arXiv2026

Estimate of Periodic Orbits of Degenerate Hamiltonians

The Arnold conjecture is a classic and important conjecture in the field of symplectic geometry, which describes the estimation of the number of periodic solutions of the Hamiltonian quantity on any symplectic manifold, which is equivalent to the symplectic version of Morse's theory. In the past development process, Andreas Floer was the first to propose Floer's theory, and solved the situation of non-degenerate Hamiltonian quantities under monotonic symplectic manifolds, and then Kenji Fukaya and Kaoru Ono solved the estimation of non-degenerate Hamiltonian quantities under rational coefficients in 1999. In 2023, Bai-Xu solved the estimation under the integer coefficient, and the non-degenerate version of Arnold's conjecture was completely resolved, but the degenerate version of Arnold conjecture did not progress so smoothly. In this paper, we have compiled some work on the degenerate version of Arnold conjecture, and based on these works, a new proof idea is proposed. By combining the action of quantum cohomology on Floer cohomology, combined with a universal energy estimation of the trajectories of $bar{partial}_H$-holomorphic in the paper, we can prove the degenerate Arnold conjecture in some special cases under the framework of Floer's theory.

math.SG↗
arXiv2026

Constraints on Axion-photon coupling from the Global 21-cm Signal

A radiation field can be excited via parametric resonance when an oscillating axion field couples to the electromagnetic sector through a Chern-Simons interaction. As demonstrated in previous works, this mechanism can generate primordial magnetic fields shortly after recombination and provide sufficient ultraviolet radiation for the formation of direct collapse black holes (DCBHs). In this study, I analyze constraints on the parametric resonance scenario from global 21cm observations. I find that there exist viable regions in the parameter space that satisfy both observational limits and the physical requirements of the magnetic field and DCBH formation scenarios.

astro-ph.CO↗
arXiv2026

Investigating cosmic strings using large-volume hydrodynamical simulations in the context of JWST's massive UV-bright galaxies

Recent observations from the James Webb Space Telescope (JWST) have uncovered an unexpectedly large abundance of massive, UV-bright galaxies at high redshifts, presenting a significant challenge to established galaxy formation models within the standard $Λ$CDM cosmological framework. Cosmic strings, predicted by a wide range of particle physics theories beyond the Standard Model, provide a promising potential explanation for these observations. They may act as additional gravitational seeds in the early universe, enhancing the process of high-redshift structure formation, potentially resulting in a more substantial population of massive, efficiently star-forming galaxies. We numerically investigate this prediction in large-volume hydrodynamical simulations using the moving-mesh code AREPO and the well-tested IllustrisTNG galaxy formation model. We evaluate the simulation results in the context of recent JWST data and find that sufficiently energetic cosmic strings produce UV luminosity and stellar mass functions that are in slightly to substantially better agreement with observations at high redshifts. Moreover, we observe that the halos seeded by cosmic strings exhibit a greater efficiency of star formation and enhanced central concentrations. Interestingly, our findings indicate that the simulations incorporating cosmic strings converge with those from a baseline $Λ$CDM model by redshift $z \sim 6$. This convergence suggests that the modified cosmological framework effectively replicates the successful predictions of the standard $Λ$CDM model at lower redshifts, where observational constraints are significantly stronger. Our results provide compelling evidence that cosmic strings may play a crucial role in explaining the galaxy properties observed by JWST at high redshifts while maintaining consistency with well-established models at later epochs.

astro-ph.CO↗
arXiv2025

Cosmological Magnetic Fields from Ultralight Dark Matter

We propose a mechanism for the generation of magnetic fields on cosmological scales that is operative after recombination. An essential ingredient is an instability (of parametric resonance type) of the electromagnetic field driven by an oscillating pseudo-scalar dark matter field, $ϕ$, that is coupled to the electromagnetic field tensor via a $ϕF \wedge F$ term in the Lagrangian of axion-electrodynamics. We find that magnetic fields larger than the observational lower bounds can be generated soon after recombination on scales of $1 {\rm{Mpc}}$.

hep-ph↗
arXiv2024

N-Body Simulation of Early Structure Formation from Cosmic String Loops

By means of N-body simulations, we study early structure formation in the presence of a scaling distribution of cosmic string loops. Cosmic string loops dominate the high redshift halo mass function while the fluctuations seeded by the standard structure formation scenario dominate structure at low redshifts. In our study, the effects of the cosmic string loops are taken into account by displacing the dark matter particles and their velocities at the initial time of the simulation by amounts determined by the analytical analysis which makes use of the Zeldovich approximation. We find that the resulting halo mass function is to a good approximation given by the sum of the analytically determined cosmic string halo mass function and the halo mass function obtained from the standard $Λ$CDM model.

astro-ph.CO↗
arXiv2023

The nanohertz stochastic gravitational wave background from cosmic string loops and the abundant high redshift massive galaxies

Recently, pulsar timing array (PTA) experiments have provided compelling evidence for the existence of the nanohertz stochastic gravitational wave background (SGWB). In this work, we demonstrated that cosmic string loops generated from cosmic global strings offer a viable explanation for the observed nanohertz SGWB data, requiring a cosmic string tension parameter of $\log(Gμ) \sim -12$ and a loop number density of $\log N \sim 4$. Additionally, we revisited the impact of cosmic string loops on the abundance of massive galaxies at high redshifts. However, our analysis revealed challenges in identifying a consistent parameter space that can concurrently explain both the SGWB data and observations from the James Webb Space Telescope. This indicates the necessity for either extending the existing model employed in this research or acknowledging distinct physical origins for these two phenomena.

astro-ph.HE↗
arXiv2023

Accretion onto Oscillating Cosmic String Loops

Cosmic string loops are non-linear density fluctuations which form in the early universe and could play an important role in explaining many phenomena which are in tension with the standard $Λ$CDM model. Hence, the details of the accretion process onto cosmic string loops should be studied in detail. Most previous works view loops as point masses and ignore the impact of a finite loop size. In this work, we utilize the Zel'dovich approximation to calculate the non-linear mass sourced by a static extended loop with a time-averaged density profile derived from the trajectory of the loop oscillation, and compare the result with what is obtained for a point-mass source. We find that the finite size of a loop mainly affects the evolution of turnaround shells during the early stages of accretion, converging to the point mass result after a critical redshift, $z^{(II)/(III)}_{c}$. For $z>z^{(II)/(III)}_{c}$, the total accreted mass surrounding a loop is suppressed relative to the point mass case and has a growth rate proportional to $(1+z)^{-3/2}$. As an immediate extension, we also qualitatively analyse the accretion onto moving point masses and onto moving extended loops. In addition to the reduction in the nonlinear mass, the loop finite size also changes the shape of the turnaround surface at early stages of accretion.

astro-ph.CO↗
arXiv2023

Early Structure Formation from Cosmic String Loops in Light of Early JWST Observations

Cosmic strings, if they exist, source nonlinear and non-Gaussian perturbations all the way back to the time of equal matter and radiation (and earlier). Here, we compute the mass function of halos seeded by a scaling distribution of cosmic string loops, and we compare the results with the predictions of the standard Gaussian $Λ$CDM model. Assuming a simple linear relation between stellar mass and halo mass, we also compute the stellar mass function. The contribution of cosmic strings dominates at sufficiently high redshifts $z > z_c$ where $z_c$ depends on the mass of the halo and on the mass per unit length $μ$ of the strings and is of the order $z_c \sim 12$ for $Gμ= 10^{-8}$. We find that strings with this value of $Gμ$ can explain the preliminary JWST data on the high redshift stellar mass density. Based on an extreme value statistic, we find that the mass of the heaviest expected string-seeded galaxy for the current JWST sky coverage is compatible with the heaviest detected galaxy. Given the uncertainties in the interpretation of the JWST data, we discuss predictions for higher redshift observations.

astro-ph.CO↗
arXiv2022

Massive black holes at high redshifts from superconducting cosmic strings

The observation of quasars at high redshifts presents a mystery in the theory of black hole formation. In order to source such objects, one often relies on the presence of heavy seeds ($M \approx 10^{4-6} \, M_{\odot}$) in place at early times. Unfortunately, the formation of these heavy seeds are difficult to realize within the standard astrophysical context. Here, we investigate whether superconducting cosmic string loops can source sufficiently strong overdensities in the early universe to address this mystery. We review a set of direct collapse conditions under which a primordial gas cloud will undergo monolithic collapse into a massive black hole (forming with a mass of $M_{BH} \approx 10^5 \, M_{\odot}$ at $z \approx 300$ in our scenario), and systematically show how superconducting cosmic string loops can satisfy such conditions in regions of the $Gμ-I$ parameter space.

astro-ph.CO↗
arXiv2021

Intermediate Mass Black Hole Seeds from Cosmic String Loops

We demonstrate that cosmic string loops may provide a joint resolution of two mysteries surrounding recently observed black holes. For a string tension in an appropriate range, large radius string loops have the potential to provide the nonlinearities in the early universe which seed supermassive black holes. The more numerous smaller radius string loops can then seed intermediate mass black holes, including those with a mass in the region between 65 and 135 solar masses in which standard black hole formation scenarios predict no black holes are able to form, but which have recently been detected by the LIGO/VIRGO collaboration. We find that there could be as many as $10^6$ of intermediate mass black holes per galaxy, providing a tantalizing target for gravitational wave observatories to look for.

astro-ph.CO↗
arXiv2020

Cosmic Rays and Spectral Distortions from Collapsing Textures

We compute the energy spectrum of photons and neutrinos produced by the unwinding of a scaling distribution of cosmic textures, and discuss the implications for the spectrum of high energy cosmic rays, and for CMB spectral distortions. Textures lead to a contribution to the photon flux which scales as $E^3 F(E) \sim E^{3/2}$. Hence, the tightest constraints on the texture model come from the highest energies from which primordial photons can reach us without being scattered by the CMB and other foregrounds. Textures lead to both $μ$ type and $y$ type distortions. While the constraints on the texture model coming from the current COBE bounds are weaker than the bounds from the angular power spectrum of the CMB, future surveys such as PIXIE can lead to stronger bounds. The high energy neutrino flux is constrained by data from the Pierre Auger experiment and yields a bound on the energy scale of textures which is competitive with CMB bounds.

astro-ph.CO↗
arXiv2019

Cosmic Textures and Global Monopoles as Seeds for Super-Massive Black Holes

We compute the number density of nonlinear seed fluctuations which have the right number density to be able to explain the presence of one supermassive black hole per galaxy, as a function of redshift. We find that there is an interesting range of symmetry breaking scales for which the density of seeds is larger that what is predicted in the standard cosmological model with Gaussian primordial fluctuations. Hence, global defects may help in light of the mounting tension between the standard cosmological model and observations of supermassive black hole candidates at high redshifts.

astro-ph.CO↗