Astroparticle physics with compact objects

Abstract

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Solar mass black holes from neutron stars and bosonic dark matter

“…where m H = v(2λ H ) 1/2 ≈ 125 GeV. Importantly, the scattering probability f ≡ σ/σ crit < 1 should be large enough to capture the φ-particles inside the neutron star, see the constraints ( 21), (23). Thus, the coupling y is large.…”

“…All its repulsive terms should be suppressed at least by the scale Λ rep in Eqs. (18), (23). The potential may become flatter than quadratic (attractive) inside finite φ intervals, but that should not ruin its renormalizability or destabilize the vacuum.…”

“…Stages (i), (ii), and (iv), i.e. the beginning of the process and its very end, have been extensively discussed in the literature, see the review [23] and [24,25]. We will provide a short summary of these results in the next section.…”