X-ray reverberation lags are used to measure the mass of the stellar-mass black hole Cygnus X-1 for the first time.
C., Lohfink A., Kara E., Parker M
9 Pith papers cite this work, alongside 303 external citations. Polarity classification is still indexing.
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The mHz QPO in 1ES 1927+654 has persisted and stabilized at ~2.5 mHz with stable soft lags, no strong harmonic, and repeatable large-amplitude flux patterns, also seen in NuSTAR.
Turbulent electron-ion coronae around accreting black holes self-regulate into a two-temperature state that generates nonthermal ions and X-ray spectra consistent with observations including an MeV tail.
Seyfert galaxy slab coronae show a nearly constant Compton y-parameter of 0.414, implying regulation by slab radiative equilibrium.
Low-luminosity AGN exhibit optical variability structure function slopes that increase with black hole mass from ~0.1 to ~0.3, with amplitude anticorrelated with luminosity, no breaks observed, and variability continuing to rise on 20-year timescales.
MHD-PIC simulations find that the non-thermal particle spectral index alpha steepens as alpha proportional to beta to the power 0.5 in the relativistic regime, due to inertial mass density acting as an energy sink that reduces Alfven velocity.
A Monte Carlo model of a Kerr black hole corona shows that photon collisions create a dense electron-positron pair cloud concentrated near the black hole, yielding X-ray temperatures, Compton parameters, and 4-10% polarization consistent with binary black hole observations.
A population of AGN coronae with magnetization parameters spanning up to σ ~ 10 can reproduce the entire observed diffuse neutrino flux from TeV to PeV energies.
A balloon mission concept with 8192 TES detectors projects 200 eV FWHM resolution at 511 keV and 35-sigma detection of the galactic center 511 keV line to study its shape and substructure.
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The $\beta$-Dependence of Particle Spectra in Relativistic Turbulent Reconnection
MHD-PIC simulations find that the non-thermal particle spectral index alpha steepens as alpha proportional to beta to the power 0.5 in the relativistic regime, due to inertial mass density acting as an energy sink that reduces Alfven velocity.
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Pair-Rich Corona of an Accreting Kerr Black Hole
A Monte Carlo model of a Kerr black hole corona shows that photon collisions create a dense electron-positron pair cloud concentrated near the black hole, yielding X-ray temperatures, Compton parameters, and 4-10% polarization consistent with binary black hole observations.