Non-Axisymmetric Pillar Structures due to Embedded Stars in AGN Accretion Discs
Abstract
Gravitationally unstable outer regions of AGN discs may host in situ formation of massive stars whose heating produces localized vertical "pillars" on the disc surface, in the same region that emits the broad lines. Here we investigate the reverberation-mapping signatures that such pillars would produce. We compute velocity-delay maps $Ψ(λ, τ)$, time-evolving emission-line spectra, and continuum reverberation lag spectra for these structures. We model each pillar as a 2D Gaussian perturbation to the disc height under lamp-post irradiation and weight the line response with Cloudy photoionization grids covering the major BLR lines. We show Hα, Mg II, and C IV as representative examples. A single pillar produces a localized hotspot in Ψ and a clear "S-wave" pattern in the time-evolving spectrum that persists, though diluted, for N ∼ 100 pillars. Emission-line fluxes are suppressed in shadows behind the pillars, but when normalized by Hβ (or by the local continuum) the line-to-Hβ ratios move in opposite directions: Mg II/Hβ rises while C IV/Hβ drops. This contrast distinguishes pillars from purely kinematic features that would modulate all lines by similar factors. Across scans of the pillar shape and lamp-post height, the pillar models produce an optical continuum reverberation lag spectrum of the observed magnitude. The once-per-orbit modulation grows with sin i from foreshortening, and at sufficiently high inclination the pillar's body geometrically self-occults its lamp-facing inner slope, adding a sharper near/far contrast. These signatures provide observational diagnostics for detecting in situ star formation in AGN discs through velocity-resolved reverberation mapping campaigns.
Versions
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BibTeX
@misc{huang2026nonaxisymmetric,
title = {{Non-Axisymmetric Pillar Structures due to Embedded Stars in AGN Accretion Discs}},
author = {Jiamu Huang and Douglas N. C. Lin and Keith Horne},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.31751},
eprint = {2610.31751},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.31751},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Non-Axisymmetric Pillar Structures due to Embedded Stars in AGN Accretion Discs
AU - Jiamu Huang
AU - Douglas N. C. Lin
AU - Keith Horne
PY - 2026
DA - 2026/10/22
PB - arXiv
DO - 10.48550/arxiv.2610.31751
UR - https://arxiv.org/abs/2610.31751
AB - Gravitationally unstable outer regions of AGN discs may host in situ formation of massive stars whose heating produces localized vertical "pillars" on the disc surface, in the same region that emits the broad lines. Here we investigate the reverberation-mapping signatures that such pillars would produce. We compute velocity-delay maps $Ψ(λ, τ)$, time-evolving emission-line spectra, and continuum reverberation lag spectra for these structures. We model each pillar as a 2D Gaussian perturbation to the disc height under lamp-post irradiation and weight the line response with Cloudy photoionization grids covering the major BLR lines. We show Hα, Mg II, and C IV as representative examples. A single pillar produces a localized hotspot in Ψ and a clear "S-wave" pattern in the time-evolving spectrum that persists, though diluted, for N ∼ 100 pillars. Emission-line fluxes are suppressed in shadows behind the pillars, but when normalized by Hβ (or by the local continuum) the line-to-Hβ ratios move in opposite directions: Mg II/Hβ rises while C IV/Hβ drops. This contrast distinguishes pillars from purely kinematic features that would modulate all lines by similar factors. Across scans of the pillar shape and lamp-post height, the pillar models produce an optical continuum reverberation lag spectrum of the observed magnitude. The once-per-orbit modulation grows with sin i from foreshortening, and at sufficiently high inclination the pillar's body geometrically self-occults its lamp-facing inner slope, adding a sharper near/far contrast. These signatures provide observational diagnostics for detecting in situ star formation in AGN discs through velocity-resolved reverberation mapping campaigns.
ER -