高能暂现源 · 每日文献综述

We investigate primordial black hole (PBH) formation in a cosmological scenario where curvature perturbations follow purely quadratic non-Gaussianity, <inline-formula><mml:math><mml:mi>ζ</mml:mi><mml:mo>=</mml:mo><mml:mi>A</mml:mi><mml:mo>(</mml:mo><mml:msup><mml:mi>ϕ</mml:mi><mml:mn>2</mml:mn></mml:msup><mml:mo>-</mml:mo><mml:mo>⟨</mml:mo><mml:msup><mml:mi>ϕ</mml:mi><mml:mn>2</mml:mn></mml:msup><mml:mo>⟩</mml:mo><mml:mo>)</mml:mo></mml:math></inline-formula>, arising from tachyonic instability in multicomponent inflationary models. Within an extended Press-Schechter framework based on the compaction function, we derive the probability distribution of the linear compaction function and its asymptotic exponential tail, demonstrating that the PBH abundance is exponentially sensitive not only to the amplitude of perturbations but also to the correlation coefficient <inline-formula><mml:math><mml:mi>ρ</mml:mi></mml:math></inline-formula> between the smoothed field and its radial gradient. We further find that, in this tachyonic amplification scenario, the spectral width of the curvature power spectrum plays a decisive role in avoiding PBH overproduction: broad spectra yield mildly negative <inline-formula><mml:math><mml:mi>ρ</mml:mi></mml:math></inline-formula> and fail to suppress PBH formation, while sufficiently narrow spectra drive <inline-formula><mml:math><mml:mi>ρ</mml:mi><mml:mo>→</mml:mo><mml:mo>-</mml:mo><mml:mn>1</mml:mn></mml:math></inline-formula>, resulting in exponential suppression while maintaining a sizable gravitational-wave signal. Thermal inflation serves as a benchmark for asteroid-mass PBH dark matter and high-frequency scalar-induced gravitational waves potentially detectable by future space-based interferometers, but its typically broad spectra make it challenging to reconcile pulsar timing array observations with PBH constraints.