Pith. sign in

REVIEW 5 major objections 4 minor 73 references

Cosmic ray contributions from rapidly rotating stellar mass black holes: Cosmic Ray GeV to EeV proton and anti-proton sources

T0 review · 5 major / 4 minor · reviewed 2026-08-12 · deepseek-v4-flash

Pith's one-line read Radio supernovae and the M87 black hole show one magnetic-field value that ties black-hole spin-down to EeV cosmic rays.

desk verdict A well-anchored empirical claim with an over-reached quantum-gravity conclusion; the anti-proton prediction deserves a referee, the Planck-time 'derivation' doesn't hold. read the letter →

arxiv 2411.11263 v1 pith:CAO2UEJD submitted 2024-11-18 astro-ph.HE

classification astro-ph.HE
keywords cosmicraysblackholespin-downradiosupernovaeanti-protonsEeVPenroseprocessmagneticfieldPlancktime
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper argues that the quantity $(B \times r)$, the magnetic field times distance, is the same for radio supernovae, the M87 black hole, and low-power radio galaxies: $10^{16.0 \pm 0.12}$ Gauss cm, independent of black-hole mass. It interprets this as the signature of a wind from a near-maximally rotating black hole, and uses it to propose that cosmic-ray protons and anti-protons from such winds make up the Galactic EeV proton component with an $E^{-7/3}$ spectrum and an anti-proton fraction approaching one half. The argument culminates in Eq. (12), which claims that the observed $(B \times r)$ forces the Planck time to be the governing time scale of angular momentum transport. If right, this connects black-hole radio observations to cosmic-ray data from GeV to EeV and gives a concrete prediction for the anti-proton content at the highest energies.

What carries the argument

The load-bearing object is the constant $(B \times r) \approx 10^{16}$ G cm inferred from radio observations of radio supernovae, M87, and low-power radio galaxies, treated as a Parker-type wind property with $B_\phi r$ constant. The argument works through a general-relativistic solution for electromagnetic energy and angular momentum fluxes near a Kerr black hole, following the Weber-Davis and Blandford-Znajek prescriptions, which gives a charge density diverging near the horizon, and through detailed-balance equations for proton and anti-proton production and annihilation in the ergo-region. The final identity Eq. (12) connects the observed $(B \times r)$ to the Planck time via the proton mass and three enhancement factors, making the Planck time the rate-governing scale for the Penrose process.

What would settle it

Measure the anti-proton-to-proton ratio of the Galactic cosmic-ray component above a few TeV with a high-energy antimatter detector: if the ratio does not rise toward about one half by EeV energies, or if the EeV component is shown to be nuclei-dominated, the proposed black-hole wind source is ruled out. A measurement of $(B \times r)$ around a near-maximally spinning black hole that deviates from $10^{16}$ G cm would likewise falsify the universality claim.

Watch

Extended reading notes

Core claim

The central claim is that the near environment of any black hole rotating near its maximum rate produces a magnetic wind with $(B \times r) = 10^{16.0 \pm 0.12}$ G cm, and that this same value is seen in radio supernovae from blue and red supergiant stars, in M87's horizon-scale emission, and in the minimum jet powers of low-power radio galaxies. From this, the paper derives that the wind and jet carry a cosmic-ray proton and anti-proton population with a source spectrum $E^{-2}$, steepened by Galactic propagation to $E^{-7/3}$, extending to EeV energies, with collisions in the ergo-region producing roughly equal numbers of protons and anti-protons. Matching the observed angular momentum transport to the particle flux then yields Eq. (12), $(B \times r)^2 = (f_{\mathrm{CR}} f_{\pi'} / f_{\mathrm{ISM}})\, m_p c / \tau_{\mathrm{Pl}}$, so that a near-maximally rotating black hole accepts one proton per log bin of energy, with associated pions, every Planck time.

Load-bearing premise

The numerical coincidence that turns the observed $(B \times r)$ into the Planck time rests on assumed enhancement factors $f_{\mathrm{ISM}}=4$, $f_{\mathrm{CR}}=10^{1.2}$, and $f_{\pi'}=10^{1.5}$, especially the un-derived equality between thermal, non-thermal, and magnetic angular momentum transport.

Editorial extensions

If this is right

  • The Galactic EeV cosmic-ray component previously fitted by Gaisser et al. as "Pop 3*" is identified as protons and anti-protons from rapidly rotating stellar-mass black-hole winds, with a straight $E^{-7/3}$ spectrum from TeV to EeV energies.
  • The anti-proton fraction in this component should approach one half, providing a floor for the anti-proton spectrum and a test at the highest observable energies.
  • The spin-down power of a near-maximal black hole is about $10^{42.8}$ erg/s independent of mass, matching the minimum jet powers of low-power radio galaxies.
  • The angular momentum loss time scale is roughly $10^{3.7}$ yr times $M_{\mathrm{BH}}/M_\odot$, so supermassive black holes above about $10^{6.5}\,M_\odot$ keep near-maximal spin longer than the age of the universe.
  • Collisions in the ergo-region destroy heavier nuclei, so this component is purely protons and anti-protons, and neutrinos from pion decay could carry a significant fraction of the black hole's rotational energy.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the Planck-time relation is taken literally, it implies a quantum-gravitational clock regulating classical spin-down; a testable extension would be to measure $(B \times r)$ for black holes with independently determined spins and see whether the value drifts as spin moves away from maximal.
  • The equal proton and anti-proton prediction means existing EeV detectors, which cannot distinguish particles from antiparticles, may already be counting anti-protons; future particle-identification measurements near the ankle could separate this component from nuclei.
  • The numerical coincidence that produces the Planck time depends on the assumed enhancement factors; a direct measurement of angular momentum transport in a magnetized wind around a young stellar black hole would either confirm or remove that coincidence.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

5 major / 4 minor

Summary. The paper argues that Radio Super Novae (RSNe), the EHT observations of M87, and low-power radio galaxies all exhibit the same value of the magnetic-field–radius product, (B × r) = 10^16.0±0.12 G cm, and interprets this as a mass-independent property of the near-horizon magnetosphere of a near-maximally rotating black hole. It constructs a general-relativistic electrodynamics solution with a particular field ansatz, derives energy and angular momentum fluxes and charge densities, and proposes that collisions in the ergo-region produce a proton/anti-proton pair plasma with an E^-2 source spectrum, which is steepened to an observer-frame E^-7/3 cosmic-ray component extending to EeV energies with an anti-proton fraction approaching 1/2. The paper further claims that the observed (B × r) value implies the Planck time as the governing time scale, expressed in Eq. (12). The observational compilation and the falsifiable cosmic-ray predictions are presented as the main results.

Significance. If the claims were established, the paper would unify disparate observations—RSNe, EHT M87, and radio-galaxy jet powers—and would make distinctive, testable predictions: a Galactic EeV proton/anti-proton component with a nearly equal anti-proton fraction, a floor to the anti-proton spectrum from GeV to EeV, and a neutrino luminosity tied to pion production. The compilation of (B × r) values across source classes is a useful service, and the anti-proton prediction is genuinely falsifiable. However, the central theoretical steps are not derived from first principles: the GR field ansatz in §6.2 is posited, the anti-proton balance in §6.8 rests on unquantified accretion assumptions, and the Planck-time relation in Eq. (12) is an algebraic rearrangement of the observed quantity with the numerical content carried by three order-of-magnitude factors that the text itself describes as approximate. The significance of the paper's strongest claim is therefore not supported, even though the cosmic-ray component could survive as a speculative but testable model.

major comments (5)
  1. [§6.9.2, Eq. (12)] The claimed Planck-time relation is not an independent prediction. Equation (12) reads (B × r)^2 = (f_CR f_π'/f_ISM) m_p c / τ_Pl, with f_ISM = 4, f_CR = 10^1.2, and f_π' = 10^1.5 adopted in the text. With all three factors set to unity, the implied time scale is τ = m_p c / (B × r)^2 ≈ 5 × 10^-46 s, about two orders of magnitude shorter than the Planck time; the product f_CR f_π'/f_ISM ≈ 10^2.1 is what moves τ to 10^-43.3 s. Since each factor is an order-of-magnitude estimate—f_ISM is explicitly based on an ISM analogy rather than a derivation, and f_CR is a logarithmic spectral range factor—the match to the Planck time is a numerical coincidence mediated by the adopted factors, not a consequence of the radio data. The text itself acknowledges this by writing that the product of factors 'perhaps by coincidence' approximates the fine-structure inverse. The abstract's statement that the observed numbers 'imply the Planck time' is therefore unsupported.
  2. [§6.2] The general-relativistic magnetic field ansatz is posited, not derived. The text assumes sqrt(g_rr g_θθ) B_φ = constant = B_p0, Br = B0 / sqrt(g_rr g_θθ g_φφ) with B0 ∼ χ M_BH, and then states 'From this it follows that Bp0 ∼ χ^2.' These scalings are chosen so that the resulting energy flux scales as Ė_rad ∼ χ^4 and the angular momentum flux as L̇_rad ∼ χ^3 M_BH, matching the Punsly & Zhang jet-power scaling and Weber–Davis angular momentum transport. No independent derivation from the Kerr metric or from Maxwell's equations is provided, and no comparison with GRMHD simulations is made. Consequently, the claimed mass independence of (B × r) and the associated energy flux are built into the ansatz rather than being predictions of the model.
  3. [§6.8, Eqs. (8)–(10)] The steady-state proton–anti-proton equality n_pbar = n_p is obtained only after explicitly neglecting accretion from outside and into the black hole, yet the equations retain the terms −n_pbar/τ_BH and −n_p/τ_BH + n_p/τ_gal. The subsequent Eq. (9) shows that when accretion terms are included, the asymmetry (n_p − n_pbar)/n_p is controlled by the ratio of the BH accretion rate to the disk accretion rate, and neither τ_BH nor τ_disk is calculated or bounded in the paper. The annihilation terms cancel in the subtraction because they appear symmetrically, so they do not determine the density ratio. The prediction of an anti-proton fraction approaching 1/2 at EeV is therefore an assumption about unquantified accretion and loss terms, not a consequence of the balance equations.
  4. [§6.5 and §6.7] The charged-particle density near the horizon is estimated in two inconsistent ways. Section 6.5 obtains a density of about 10^14 cm^-3 from the charge-density expression, 'ignoring here the factors with some power of Δ'. Section 6.7 instead uses equipartition between magnetic energy density and particle thermal energy, giving n ≃ 10^21.6 cm^-3 at R = 10^6.4 cm for a 10 M⊙ black hole. The two estimates differ by more than seven orders of magnitude, and this discrepancy is not discussed. The discrepancy matters directly because the collision rate and the proton–anti-proton production rate scale as n^2, so the quantitative predictions for anti-proton production and neutrino luminosity depend sensitively on which density is adopted.
  5. [§6.9.1] The E^-7/3 observer-frame spectrum is asserted rather than derived. The text states that the source spectrum is E^-2 and is 'steepened by an ISM Kolmogorov spectrum of magnetic irregularities in the Galactic disk, so 1/3,' but no transport calculation is presented for the diffusion coefficient, energy losses, confinement time, or the resulting spectral index. The paper also assumes that the same E^-2 spectrum drives the electric currents in jets, citing Gopal-Krishna & Biermann (2024), but does not explain how the near-horizon pair plasma is injected into the jet with that spectrum. Since the E^-7/3 prediction is one of the paper's main observable tests, the absence of this calculation weakens the claim.
minor comments (4)
  1. [§6.8] The equation numbering in the text is inconsistent: the displayed balance equations are unnumbered, yet the text refers to 'eq.(3) and eq.(4)' and 'eq.(10) and eq.(11)' for these equations. The numbering should be corrected throughout the section.
  2. [Figure 2 caption] The caption states that in the abscissa 'the unit is the Kerr radius, in contradiction to the text, where r scales to the Kerr radius.' This self-described contradiction should be resolved: either the figure uses a different normalization than the text, or the caption should be corrected.
  3. [§2] The statement that 'just recently the super-massive black hole in M87 experienced a merger with another black hole, with a spin-flip visible in the data' is attributed to Owen et al. (2000), but that reference reports radio observations of M87 at 90 cm and does not appear to contain a merger or spin-flip claim. A direct reference for this assertion is needed.
  4. [§3] The 'green onion model' is invoked without a definition or reference. Since the paper uses this concept to connect the 2π wind to the jet flow, a brief explanation or citation would greatly improve readability.

Circularity Check

3 steps flagged · score 6.0 of 10

Eq. (12)'s Planck-time claim is constructed from observed (B×r) via the assumed factors f_ISM=4, f_CR=10^1.2, f_pi'=10^1.5; with factors at unity the implied time scale is ~100× shorter, and the f-combination is matched to the Rueda–Ruffini relation announced before the derivation.

  1. fitted input called prediction [§6.9.2, 'Frequency of the Penrose process', Eq. (12)]
    "Extending the spectrum to EeV energies gives for anE−2 spectrum [Gopal-Krishna & Biermann (2024)] a factor of the natural log of the range, so about fCR = 10 1.2. Considering that pions result energetically 30 times as often from p-p collisions as proton-anti-proton pairs adds another factor of fπ′s = 10 1.5 for a total angular momentum of 10 −4.2 g cm2 s−1. ... What time scale per such step is required to match the observed angular momentum transport? The implied time scale is the Planck time of τP l = 10 −43.3 s [Planck (1900)], which yields here 10 39.1 {erg s}/s."

    The time scale is fixed by the ratio of the assumed per-event particle angular momentum (10^-4.2 g cm^2/s, built from f_CR and f_pi') to the magnetic angular-momentum rate derived from the observed B×r; it is not independently measured. With all factors set to unity, the same observed (B×r) gives tau = m_p c/(B r)^2 ≈ 5×10^-46 s, about 100× shorter than the Planck time. The adopted product f_CR f_pi'/f_ISM ≈ 125 is what moves tau to 10^-43.3 s. Thus Eq. (12) is the observed (B×r) rearranged after inserting the assumed f factors; the Planck-time 'prediction' is an output of those factors, not a consequence of the data alone.

  2. renaming known result [§5.1, question 1 and §6.9.2 (Eq. 12)]
    "It can be written as an energy flow with (B × r)2 c = {¯h c}/e2 {mX c2}/τP l with mX close to the proton or neutron mass, and τP l the Planck time (see, e.g., [Rueda & Ruffini (2021)]). ... The term with the factors fCR, fπ′s, and fISM , perhaps by coincidence, approximately equals {¯h c}/e2."

    The paper announces the target relation, complete with the Planck time and the fine-structure coefficient, before the derivation. When §6.9.2 'derives' Eq. (12), the fudge-factor combination f_CR f_pi'/f_ISM is found to be approximately h-bar c/e^2 — the same coefficient as in the announced Rueda–Ruffini relation. The derivation therefore does not independently produce the Planck time; it reproduces the already-cited relation by normalizing the f factors to match the target coefficient. Extracting tau_Pl from Eq. (12) is equivalent to reading it off the input relation, so the conclusion that the observed numbers 'imply the Planck time' is the known result renamed in terms of Penrose zones and f factors.

1 more flagged steps
  1. self citation load bearing [§6.9.1–§6.9.2 (E^-2 spectrum and f_CR)]
    "We note that all jets carry an electric current, driven by a proton-anti-proton pair plasma with a spectrum of E−2 [Gopal-Krishna & Biermann (2024)] to EeV energies, which we identify here with this CR population ... Extending the spectrum to EeV energies gives for anE−2 spectrum [Gopal-Krishna & Biermann (2024)] a factor of the natural log of the range, so about fCR = 10 1.2."

    f_CR is one of the three factors that set the time scale in Eq. (12); it is derived entirely from the E^-2 spectrum. The only support given for that spectrum is a citation to Gopal-Krishna & Biermann (2024), whose authors include two authors of the present paper. The present text provides no independent derivation or external falsification for E^-2. Consequently the Planck-time result is in part carried by a self-citation chain: the E^-2 spectrum is an assumed input imported from the authors' prior work, and it is load-bearing for the numerical match claimed in Eq. (12).

full rationale

The paper contains genuine empirical content: the constancy of (B×r) across RSNe and M87 is an observational claim, and the anti-proton stationarity argument (n_pbar = n_p) is a model consequence independent of the fitted factors. However, the central quantum-gravity claim — that the observed (B×r) implies the Planck time — is circular in content. Section 5.1 announces the Rueda–Ruffini relation with tau_Pl before the derivation; Section 6.9.2 then sets f_ISM=4, f_CR=10^1.2, f_pi'=10^1.5, notes their combination is approximately h-bar c/e^2, and solves for tau = 10^-43.3 s. With the factors at unity, the same equation gives tau ~5×10^-46 s, roughly 100× shorter than the Planck time, showing that the match is carried by the adopted factors, not by the data. The E^-7/3 population is likewise identified with Gaisser's fitted pop 3* rather than independently predicted, and the E^-2 spectrum behind f_CR rests on a self-citation. These are partial circularities in the strongest claim; the cosmic-ray spectral and anti-proton predictions retain some independent content, so the score is 6 rather than higher.

Assumptions & free parameters 4 free parameters · 5 assumptions · 2 invented entities

The model rests on one observed scaling, the universality of (B × r), plus a sequence of assumed field configurations, spectral shapes, and order-unity enhancement factors. The free parameters f_ISM, f_CR, and f_pi' are not independently measured and carry the numerical content of the Planck-time coincidence. The invented Penrose-zone concept has no distinct observable signature aside from the predicted cosmic-ray and neutrino fluxes.

free parameters (4)
  • f_ISM angular momentum enhancement factor = 4
    Introduced in §6.9.2 as a multiplier to the magnetic-field-only angular momentum transport, based on the assumption that thermal and non-thermal particles each match the magnetic field transport in the ISM; no independent measurement fixes this factor.
  • f_CR spectral range factor = 10^1.2
    Logarithm of the ratio of maximum to minimum energy for an E^-2 spectrum from GeV to EeV; the range endpoints are chosen ad hoc and directly enter the Planck-time computation.
  • f_pi' pion-to-pair ratio = 10^1.5
    Ratio of pion production to proton-anti-proton pair production cross-sections, taken as about 30; adopted in §6.9.2 to weight pions in angular momentum transport.
  • spin-down time-scale factor = 5
    In §4, a 'compromise' factor between unity and ten used to convert the magnetic transport time scale to the black hole mass-loss time scale; it sets the derived luminosity 10^42.8 erg/s.
assumptions (5)
  • domain assumption The observed quantity (B × r) = 10^16.0±0.12 G cm is a universal constant for near-maximally rotating black holes, independent of mass.
    Central empirical input from Radio Supernovae, M87 EHT, and low-power radio galaxies; the paper interprets this universality as a property of the near-horizon region.
  • ad hoc to paper The near-horizon magnetic field follows the ansatz Bθ = 0, √(grr gθθ) Bφ = Bp0 = const, with B0 ∝ χ M_BH and Bp0 ∝ χ^2.
    Posited in §6.2 without deriving from a plasma model; these scalings force the jet-power scaling L_jet ∝ χ^4 used as a check.
  • domain assumption The accelerated particle spectrum at the source is E^-2 and propagates through a Kolmogorov ISM, steepening to E^-7/3 for the observer.
    Assumed in §6.9.2 and §7; the Kolmogorov exponent 1/3 is a standard propagation assumption but is not derived here.
  • ad hoc to paper In steady state, proton and anti-proton densities are equal when accretion is negligible (Eq. 8).
    Derived from a simplified two-species balance that neglects accretion from the disk, annihilation losses, and energy-dependent cross-sections; it yields the half-anti-proton prediction.
  • domain assumption The fundamental-plane scaling carries accretion physics unchanged across all black hole masses.
    Invoked in §2.1 to extend the Radio Supernovae result to M87 and radio galaxies; a scaling relation with significant scatter.
invented entities (2)
  • Inner and outer Penrose zones
    purpose: Conceptual regions in the ergo-region that organize the spin-down and the production and ejection of secondary protons, anti-protons, and pions
    Introduced in §6.9; no direct observable is tied uniquely to the zones themselves, only to the resulting cosmic-ray and neutrino fluxes.
  • Proton/anti-proton pair plasma with E^-2 spectrum driving jet currents and cosmic rays independent evidence
    purpose: Identified as the carrier of electric currents in jets and as the source of the EeV cosmic-ray component (pop 3*)
    Predicts an anti-proton flux at TeV energies and a ~1/2 anti-proton fraction at EeV, testable by AMS and composition analyses; currently unverified.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Cosmic ray contributions from rapidly rotating stellar mass black holes: Cosmic Ray GeV to EeV proton and anti-proton sources." pith.science (2026). https://pith.science/paper/CAO2UEJD

@misc{pith2026241111263,
  author       = {Pith},
  title        = {Pith review of: Cosmic ray contributions from rapidly rotating stellar mass black holes: Cosmic Ray GeV to EeV proton and anti-proton sources},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/CAO2UEJD}},
  note         = {Machine review of arXiv:2411.11263}
}
abstract

In Radio Super Novae (RSNe) a magnetic field of $(B \, \times \, r) \, = \, 10^{16.0 \pm 0.12} \, {\rm Gauss \, \times \, cm}$ is observed; these are the same numbers for Blue Super Giant (BSG) star explosions as for Red Super Giant (RSG) star explosions, despite their very different wind properties. The EHT data for M87 as well for low power radio galaxies all show consistency with just this value of the quantity $(B \, \times \, r )$, key for angular momentum and energy transport, and can be derived from the radio jet data. We interpret this as a property of the near surroundings of a black hole (BH) at near maximal rotation, independent of BH mass. In the commonly used green onion model, in which a $2 \, \pi$ flow changes over to a jet flow we interpret this as a wind emanating from the BH/accretion disk system and its surroundings. Near the BH collisions in the wind can produce a large fraction of anti-protons. In this scenario the cosmic Ray (CR) population from the wind/jet is proposed to be visible as EeV protons and anti-protons in the CR data to EeV energy, with a $E^{-7/3}$ spectrum. This can be connected to a concept of inner and outer Penrose zones in the ergo-region. The observed numbers for the magnetic field imply the Planck time as the governing time scale: A BH rotating near maximum can accept a proton per log bin of energy in an extended spectrum with the associated pions every Planck time.

Figures

Figures reproduced from arXiv: 2411.11263 by the authors.

Figure 1
Figure 1. Internal structure of 60 M⊙ star just before making a black hole of 38 M⊙. Source: Chieffi 2019 priv.comm., [Limongi & Chieffi (2018), Limongi & Chieffi (2020)]. Spin is 1052.27 erg s, a factor of ∼ 100.21 over limit at 38 M⊙; relatively similar excess for other masses. Considering different radii each time the angular momentum is close to the maximum allowed for the mass contained in this radius; that means we have… view at source ↗
Figure 2
Figure 2. Radial component of the angular momentum flux vs the radius at the equator [PITH_FULL_IMAGE:figures/full_fig_p028_2.png] view at source ↗
Figure 3
Figure 3. Radial component of the magnitude of the rate of energy extraction. The [PITH_FULL_IMAGE:figures/full_fig_p029_3.png] view at source ↗
Figures from the paper (2 more)
Figure 4
Figure 4. Figure 4: Radial component of the magnitude of the angular momentum extraction rate [PITH_FULL_IMAGE:figures/full_fig_p030_4.png]
Figure 5
Figure 5. Figure 5: The key elements of the Kerr black hole with rotation parameter [PITH_FULL_IMAGE:figures/full_fig_p049_5.png]

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

73 extracted references · 68 canonical work pages

  1. [1]

    (1998)] Abbott, D.C., Bieging, J.H., & Churchwell, E., Astrophys

    [Abbott et al. (1998)] Abbott, D.C., Bieging, J.H., & Churchwell, E., Astrophys. J. 280, 671 - 678 (1984); Title: The detection of variable, nonthermal radio emission from two O type stars. [Allen & Kronberg (1998)] Allen, M.L., & Kronberg, P.P., (1998). Radio Spectra of Se- lected Compact Sources in the Nucleus of M82. Astrophys. J. 502, 218 -

  2. [6]

    (1963)] Feynman, R.P., Leighton, R.B., Sands, M., The Feynman Lec- tures on Physics (book) (1963)

    [Feynman et al. (1963)] Feynman, R.P., Leighton, R.B., Sands, M., The Feynman Lec- tures on Physics (book) (1963). here p. 42-9. [Frank & Rees (1976)] Frank, J., & Rees, M.J., (1976). Effects of massive black holes on dense stellar systems. Month. Not. Roy. Astr. Soc. 176, 633 -

  3. [13]

    Hydrodynamical Modeling of the Light Curves of Core-collapse Supernovae with HYPERION

    [Limongi & Chieffi (2020)] Limongi, M., & Chieffi, A., (2020). Hydrodynamical Modeling of the Light Curves of Core-collapse Supernovae with HYPERION. I. The Mass Range 13-25 M⊙, the Metallicities -3 ≤ [F e/H] ≤ 0, and the Case of SN 1999em. Astrophys. J. 902,

  4. [14]

    (2022)] Yusef-Zadeh, F., Arendt, R.G., Wardle, M., Heywood, I., Cot- ton, W., & F

    [Yusef-Zadeh et al. (2022)] Yusef-Zadeh, F., Arendt, R.G., Wardle, M., Heywood, I., Cot- ton, W., & F. Camilo, F., ApJL 925, L18 (2022); Statistical Properties of the Population of the Galactic Center Filaments: the Spectral Index and Equipartition Magnetic Field 81

  5. [17]

    (2002)] McDonald, A.R., Muxlow, T.W.B., Wills, K.A., Pedlar, A., & Beswick, R.J., (2002)

    [McDonald et al. (2002)] McDonald, A.R., Muxlow, T.W.B., Wills, K.A., Pedlar, A., & Beswick, R.J., (2002). A parsec-scale study of the 5/15-GHz spectral indices of the compact radio sources in M82. Month. Not. Roy. Astr. Soc. 334 912 - 924 72 [Meli et al., 2008] Meli, A., Becker, J., Quenby, J. J. (2008); Title: On the origin of ultra high energy cosmic r...

  6. [21]

    (2012)] Chini, R., Hoffmeister, V.H., Nasseri, A., Stahl, O., & Zinnecker, H., (2012)

    [Chini et al. (2012)] Chini, R., Hoffmeister, V.H., Nasseri, A., Stahl, O., & Zinnecker, H., (2012). A spectroscopic survey on the multiplicity of high-mass stars. Month. Not. Roy. Astr. Soc. 424, 1925 -

  7. [26]

    The jet power and emission line correlations of radio loud optically selected quasars

    76 [Punsly & Zhang (2011)] Punsly, B., & Zhang, S., (2011). The jet power and emission line correlations of radio loud optically selected quasars. Astrophys. J. Letters 753, L3. [Pozo Nuˆ nez et al. (2019)] Pozo Nuˆ nez, F., Chini, R., Barr Dom ´ ınguez, A., Fein, Ch., Hackstein, M., Pietrzy´ nski, G., et al., (2019). A survey for high-mass eclipsing bina...

  8. [31]

    Particle creation by black holes

    66 [Hawking (1975)] Hawking, S.W., (1975). Particle creation by black holes. Commun. Math. Phys. 43, 199 -

Show all 73 references
  1. [32]

    The Knee: Theory and Experiment

    [Yodh (2006)] Yodh, G.B., (2006). The Knee: Theory and Experiment. J. of Phys.: Conf. Ser. 47, 1 -

  2. [36]

    (2003)] Igumenshchev, I.V., Narayan, R., & Abramowicz, M.A

    [Igumenshchev et al. (2003)] Igumenshchev, I.V., Narayan, R., & Abramowicz, M.A. (2003). Three-dimensional Magnetohydrodynamic Simulations of Radiatively In- efficient Accretion Flows. Astrophys. J. 592, 1042 -

  3. [37]

    (2018)] Davelaar, J., Mo´ scibrodzka, M., Bronzwaer, T., & Falcke, H., (2018)

    [Davelaar et al. (2018)] Davelaar, J., Mo´ scibrodzka, M., Bronzwaer, T., & Falcke, H., (2018). General relativistic magnetohydrodynamical κ-jet models for Sagittarius A∗. Astron. & Astroph. 612, A34. 62 [Davis & Gammie (2020a)] Davis, S.W., & Gammie, C.F. (2020b). Covariant R...

  4. [45]

    Cosmic winds and the Heliosphere

    Title: Cosmic rays: origin and acceleration - what can we learn from radio astronomy [Biermann (1997)] Biermann, P.L.; invited review chapter in “Cosmic winds and the Heliosphere”, Eds. J. R. Jokipii et al., Univ. of Arizona press, Tucson, Arizona, USA, 1997, p. 887 - 957; ast...

  5. [47]

    (2010)] Diehl, R., Lang, M.G., Martin, P., Ohlendorf, H., Preibisch, Th., Voss, R., et al., (2010)

    [Diehl et al. (2010)] Diehl, R., Lang, M.G., Martin, P., Ohlendorf, H., Preibisch, Th., Voss, R., et al., (2010). Radioactive 26Al from the Scorpius-Centaurus association. Astron. & Astroph. 522, A51. [Diehl et al. (2011)] Diehl, R., Hartmann, D.H., & Prantzos, N., Eds., (2011...

  6. [48]

    The Explosion of a Rotating Star As a Supernova Mechanism

    [Bisnovatyi-Kogan (1970)] Bisnovatyi-Kogan, G.S., (1970); (1971). The Explosion of a Rotating Star As a Supernova Mechanism. Astron. Zh. 47, 813; transl. Sov. Astron. 14,

  7. [49]

    (2022)] Lucchini, M., Ceccobello, C., Markoff, S., Kini, Y., Chhotray, A., Connors, R.M.T., et al., Month

    71 [Luccini et al. (2022)] Lucchini, M., Ceccobello, C., Markoff, S., Kini, Y., Chhotray, A., Connors, R.M.T., et al., Month. Not. Roy. Astr. Soc. 517, 5853 - 5881 (2022); Title: Bhjet: a public multizone, steady state jet + thermal corona spectral model [Lucek & Bell (2000)] ...

  8. [51]

    (2016)] Mo´ scibrodzka, M., Falcke, H., & Noble, S., (2016)

    73 [Mo´ scibrodzka et al. (2016)] Mo´ scibrodzka, M., Falcke, H., & Noble, S., (2016). Scale- invariant radio jets and varying black hole spin. Astron. & Astroph. 596, A13. [Moskalenko & Seo (2019)] Moskalenko, I.V., & Seo, E.-S., (2019). Advances in cosmic- ray astrophysics a...

  9. [55]

    (2002)] Woosley, S.E., Heger, A

    [Woosley et al. (2002)] Woosley, S.E., Heger, A. & Weaver, T.A., Rev. Mod. Phys. 74, 1015 - 1071 (2002); Title: The evolution and explosion of massive stars [Yodh (1992)] Yodh, G.B., (1992). Ultra-High-Energy Astronomy and Cosmic Rays, Ann. New York Acad. Sci. 655, 160 -

  10. [63]

    Cosmic ray antiprotons at high energies

    [Winkler (2017)] Winkler, M.W., (2017). Cosmic ray antiprotons at high energies. J. of Cosmol. and Astrop. Phys. 02,

  11. [69]

    (2021a)] Wong, G.N., Du, Y., Prather, B.S., & Gammie, C.F

    [Wong et al. (2021a)] Wong, G.N., Du, Y., Prather, B.S., & Gammie, C.F. (2021). The Jet-disk Boundary Layer in Black Hole Accretion. Astrophys. J. 914,

  12. [75]

    (2004), Month

    [Komissarov (2004)] Komissarov, S.S. (2004), Month. Not. Roy. Astr. Soc. 350, 427 - 448; Title: Electrodynamics of black hole magnetospheres [Kronberg et al. (1985)] Kronberg, P.P., Biermann, P.L., & Schwab, F.R., (1985). The nucleus of M82 at radio and X-ray bands: Discovery ...

  13. [77]

    On the Gravitational Field of a Mass Point According to Einstein’s Theory

    [Schwarzschild (1916)] Schwarzschild, K., (1916). On the Gravitational Field of a Mass Point According to Einstein’s Theory. Sitz. Ber. Preuß. Akad. Wiss. 189 - 196 [Shaymatov et al. (2015)] Shaymatov, S., Patil, M., Ahmedov, B., ˆJoshi, P.S., (2015). Destroying a near-extrema...

  14. [86]

    (2016)] Thoudam, S., Rachen, J.P., van Vliet, A., Achterberg, A., S

    79 [Thoudam et al. (2016)] Thoudam, S., Rachen, J.P., van Vliet, A., Achterberg, A., S. Buitink, S., Falcke, H., et al., (2016). Cosmic-ray energy spectrum and composition up to the ankle: the case for a second Galactic component. Astron. & Astroph. 595, A33. [Van Dyk (2017)] ...

  15. [94]

    (2006)] Diehl, R., Halloin, H., Kretschmer, K., Lichti, G.G., Sch¨ onfelder, V., Strong, A.W., et al., (2006)

    [Diehl et al. (2006)] Diehl, R., Halloin, H., Kretschmer, K., Lichti, G.G., Sch¨ onfelder, V., Strong, A.W., et al., (2006). Radioactive 26Al from massive stars in the Galaxy. Nature 439, 45 -

  16. [95]

    (2011)] Liu, Ch., Chen, S., Ding, Ch., & Jing, J., (2011)

    [Liu et al. (2011)] Liu, Ch., Chen, S., Ding, Ch., & Jing, J., (2011). Particle acceleration on the background of the Kerr-Taub-NUT spacetime. Phys. Lett.B 701, 285 -

  17. [98]

    The interaction of Crab-like supernova rem- nants with their surroundings

    [Chevalier (1984)] Chevalier, R.A., (1984). The interaction of Crab-like supernova rem- nants with their surroundings. Astrophys. J. 280, 797 -

  18. [105]

    [Cox (1972)] Cox, D.P., (1972); Title: Cooling evolution of a Supernova remnant

    Acceleration in astrophysics. [Cox (1972)] Cox, D.P., (1972); Title: Cooling evolution of a Supernova remnant. Astro- phys. J. 178, 159 - 168 [Daly (2019)] Daly, R.A., (2019). Black Hole Spin and Accretion Disk Magnetic Field Strength Estimates for More Than 750 Active Galacti...

  19. [106]

    (2015), Observational Constraints on the Progenitors of Core-Collapse Supernovae: The Case for Missing High-Mass Stars, Publ

    [Smartt (2015)] Smartt, St.J. (2015), Observational Constraints on the Progenitors of Core-Collapse Supernovae: The Case for Missing High-Mass Stars, Publ. of the Astron. Soc. of Australia , 32, id.e016. [Soderberg et al. (2010)] Soderberg, A.M., Chakraborti, S., Pignata, G., ...

  20. [122]

    (2019)] Porth, O., Chatterjee, K., Narayan, R., Gammie, Ch.F., Mizuno, Y., Anninos, P., et al., (2019)

    [Porth et al. (2019)] Porth, O., Chatterjee, K., Narayan, R., Gammie, Ch.F., Mizuno, Y., Anninos, P., et al., (2019). The Event Horizon General Relativistic Magnetohy- drodynamic Code Comparison Project. Astrophys. J. Suppl. 243,

  21. [162]

    (2023)] Cho, H., Prather, B.S., Narayan, R., Natarajan, P., Su, K.-Y

    [Cho et al. (2023)] Cho, H., Prather, B.S., Narayan, R., Natarajan, P., Su, K.-Y. , Ri- carte, A., et al., Astrophys. J. Letters 959, id.022 (2023); Title: Bridging Scales in Black Hole Accretion and Feedback: Magnetized Bondi Accretion in 3D GRMHD, DOI 10.3847/2041-8213/ad104...

  22. [170]

    (2013)] Barr Dom ´ ınguez, A., Chini, R., Pozo Nu˜ nez, F., Haas, M., Hackstein, M., Drass, H., et al., (2013)

    [Barr Dom ´ ınguez et al. (2013)] Barr Dom ´ ınguez, A., Chini, R., Pozo Nu˜ nez, F., Haas, M., Hackstein, M., Drass, H., et al., (2013). Eclipsing high-mass binaries. I. Light curves and system parameters for CPD - 51 ¨ ı¿½ 8946, PISMIS 24-1, and HD 319702. Astron. & Astroph....

  23. [179]

    ¨Uber irreversible Strahlungsvorg¨ ange,Annal- Phys

    179 [Planck (1900)] Planck, M., (1900). ¨Uber irreversible Strahlungsvorg¨ ange,Annal- Phys. 306, 69 -

  24. [184]

    Composition near the knee: results from the CACTI experiment [Yodh (2005)] Yodh, G.B., (2005)

    80 [Yodh (2003)] Yodh, G.B., (2003). Composition near the knee: results from the CACTI experiment [Yodh (2005)] Yodh, G.B., (2005). Cosmic rays, particle physics and the high energy frontier. Proc. of the 29th Int. Cosmic Ray Conf. 2005, Ed. B. Sripathi Acharya, et al. TIFR, 10, 13 -

  25. [185]

    (2020)] Telescope-Array Coll., Abbasi, R.U., Abe, M., Abu- Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J.W., et al., (2020)

    [Telescope-Array Coll. (2020)] Telescope-Array Coll., Abbasi, R.U., Abe, M., Abu- Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J.W., et al., (2020). Evidence for a Supergalactic Structure of Magnetic Deflection Multiplets of Ultra- high- energy Cosmic Rays. Astroph...

  26. [200]

    (2003)] Narayan, R., Igumenshchev, I.V., & Abramowicz, M.A

    Pub Date: December 2003 [Narayan et al. (2003)] Narayan, R., Igumenshchev, I.V., & Abramowicz, M.A. (2003). Magnetically Arrested Disk: an Energetically Efficient Accretion Flow. Publ. As- tron.Soc.Japan 55, L69 - L72. 74 [Northrop (1963)] Northrop, T.G., (1963). The adiabatic...

  27. [205]

    (2009)] Ba˜ nados, M., Silk, J., & West, S.M., (2009)

    [Banados et al. (2009)] Ba˜ nados, M., Silk, J., & West, S.M., (2009). Kerr Black Holes as Particle Accelerators to Arbitrarily High Energy. Phys. Rev. Letters 103, 111102. [Banados et al. (2011)] Ba˜ nados, M., Hassanain, B., Silk, J., & West, St.M., (2011). Emergent flux fro...

  28. [220]

    (2003)] Heger, A., Fryer, C.L., Woosley, S.E., Langer, N., & Hartmann, D.H., Astrophys

    [Heger et al. (2003)] Heger, A., Fryer, C.L., Woosley, S.E., Langer, N., & Hartmann, D.H., Astrophys. J. 591, 288 - 300 (2003); Title: How massive stars end their life [Hills (1975)] Hills, J.G., (1975). Possible power source of Seyfert galaxies and QSOs. Nature 254, 295 -

  29. [227]

    Vela X and the evolution of plerions

    [Weiler & Panagia (1980)] Weiler, K.W., & Panagia, N., (1980). Vela X and the evolution of plerions. Astron. & Astroph. 90, 269 -

  30. [228]

    Radio continuum studies of the evolved starburst in M82

    [Allen (1999)] Allen, M.L., (1999). Radio continuum studies of the evolved starburst in M82. PhD thesis U. of Toronto, Canada. [Allen et al. (2024)] Allen, M.L., Biermann, P.L., Chieffi, A., Frekers, D., Gergely, L. ´A., Harms, B., et al., Astropart. Phys. 161, 102976 (2024). ...

  31. [232]

    (2021)] Bambhaniya, P., Solanki, D.N., Dey, D., et al., (2021)

    [Bambhaniya et al. (2021)] Bambhaniya, P., Solanki, D.N., Dey, D., et al., (2021). Pre- cession of timelike bound orbits in Kerr spacetime. Eur. Phys. Journ. C 81,

  32. [238]

    The structure of star clusters

    [King (1966)] King, I.R., (1966). The structure of star clusters. III. Some simple dynam- ical models. Astron. J. 71, 64 -

  33. [290]

    [Lovelace (1976)] Lovelace, R.V.E. (1976). Dynamo model of double radio sources. Nature 262, 649 -

  34. [298]

    The London moment: what a rotating super- conductor reveals about superconductivity

    [Hirsch (2014)] Hirsch, J.E., (2014). The London moment: what a rotating super- conductor reveals about superconductivity. Phys. Scripta 89, 015806 (2014); arXiv/1310.3834. [Hirsch (2019)] Hirsch, J.E., (2019). Defying inertia: how rotating superconductors gen- erate magnetic ...

  35. [300]

    The quantum emission of an alive black hole

    [Rueda & Ruffini (2021)] Rueda, J.A., & Ruffini, R., (2021). The quantum emission of an alive black hole. Int. J. of Mod. Phys. D 30, 2141003. [Rueda et al. (2022)] Rueda, J.A., Ruffini, R., & Kerr, R.P., (2022). Gravitomagnetic interaction of a Kerr black hole with a magnetic...

  36. [327]

    (2017)] Tabatabaei, F

    [Tabatabaei et al. (2017)] Tabatabaei, F. S., Schinnerer, E., Krause, M., Dumas, G., Meidt, S., Damas-Segovia, A., et al. (2017), The Radio Spectral Energy Distri- bution and Star-formation Rate Calibration in Galaxies, Astrophys. J. 836, id

  37. [340]

    Electromagnetic extraction of energy from Kerr black holes

    [Blandford & Znajek (1977)] Blandford, R.D., & Znajek, R.L., (1977). Electromagnetic extraction of energy from Kerr black holes. Month. Not. Roy. Astr. Soc. 179, 433 -

  38. [370]

    (1973)] Bardeen, J.M., Carter, B., & Hawking, S.W., (1973)

    58 [Bardeen et al. (1973)] Bardeen, J.M., Carter, B., & Hawking, S.W., (1973). The four laws of black hole mechanics. Commun. Math. Phys. 31, 161 -

  39. [382]

    (2000)] Kronberg, P.P., Sramek, R.A., Birk, G.T., Dufton, Q.W., Clarke, T.W., & Allen, M.L., (2000)

    69 [Kronberg et al. (2000)] Kronberg, P.P., Sramek, R.A., Birk, G.T., Dufton, Q.W., Clarke, T.W., & Allen, M.L., (2000). Search for Flux Density Variations in 24 Compact Radio Sources on M82. Astrophys. J. 535, 706 -

  40. [456]

    (1991)] Breitschwerdt, D., McKenzie, J.F., & Voelk, H.J

    [Breitschwerdt et al. (1991)] Breitschwerdt, D., McKenzie, J.F., & Voelk, H.J. (1991). Galactic winds. I. Cosmic ray and wave-driven winds from the galaxy. Astron. & Astroph. 245, 79 -

  41. [595]

    (2020)] Humphreys, R.M., Helmel, G., Jones, T.J., & Gordon, M.S

    [Humphreys et al. (2020)] Humphreys, R.M., Helmel, G., Jones, T.J., & Gordon, M.S. (2020), Exploring the Mass-loss Histories of the Red Supergiants, Astron. J. 160, id.145. [Hwang et al. (2004)] Hwang, U., Laming, J.M., Badenes, C., Berendse, F., Blondin, J., Cioffi, D., et al...

  42. [647]

    The spins of compact objects born from helium stars in binary systems

    [Fuller & Lu (2022)] Fuller, J., & Lu, W., (2022). The spins of compact objects born from helium stars in binary systems. Month. Not. Roy. Astr. Soc. 511, 3951 -

  43. [652]

    Magnetorotational Supernovae with Jets

    60 [Bisnovatyi-Kogan & Moiseenko (2008)] Bisnovatyi-Kogan, G.S., & Moiseenko, S.G., (2008). Magnetorotational Supernovae with Jets. Chin. J. of Astr. & Astroph. Suppl. 8, 330 -

  44. [676]

    (2010)] Patil, M., Joshi, P.S., & Malafarina, D., (2010)

    [Patil et al. (2010)] Patil, M., Joshi, P.S., & Malafarina, D., (2010). Naked singular- ities as particle accelerators. II. Phys. Rev. D 83 , 104049, DOI 10.1103/Phys- RevD.82.104049 and 10.48550/arXiv.1011.5550 [Patil & Joshi (2011a)] Patil, M., & Joshi, P.S., (2011a). Kerr n...

  45. [702]

    (2015)] Markoff, S., Nowak, M.A., Gallo, E., Hynes, R., Wilms, J., Plotkin, R.M., et al

    [Markoff et al. (2015)] Markoff, S., Nowak, M.A., Gallo, E., Hynes, R., Wilms, J., Plotkin, R.M., et al. (2015). As Above, So Below: Exploiting Mass Scaling in Black Hole Accretion to Break Degeneracies in Spectral Interpretation. Astrophys. J. Let- ters 812, L25 [Martin et al...

  46. [707]

    Extragalactic magnetic fields

    [Kronberg (1994)] Kronberg, P.P., (1994). Extragalactic magnetic fields. Rep. Pro.Phys. 57 , 325 -

  47. [711]

    (2011)] Kronberg, P.P., Lovelace, R.V.E., Lapenta, G., & Colgate, S.A

    [Kronberg et al. (2011)] Kronberg, P.P., Lovelace, R.V.E., Lapenta, G., & Colgate, S.A. (2011). Measurement of the Electric Current in a kpc-scale Jet.Astrophys. J. Letters 741, L15. [Kronberg (2016)] Kronberg, P.P., (2016). Cosmic Magnetic Fields, Cambridge U. Press (283 page...

  48. [758]

    ´A., & Biermann, P.L

    [Gergely & Biermann (2009)] Gergely L. ´A., & Biermann, P.L. (2009). Supermassive black hole mergers, Astrophys. J. 697, 1621 - 1633 (2009); arXiv:0704.1968 65 [Goldreich & Julian (1969)] Goldreich, P., & Julian, W.H. (1969). Pulsar Electrodynam- ics. Astrophys. J. 157, 869 -

  49. [786]

    (2019a)] The Event Horizon Telescope Coll., Akiyama, K., Alberdi, A., Alef, W., Asada, K., Azulay, R., Baczko, A.-K., et al., (2019a)

    63 [EHT-Coll. (2019a)] The Event Horizon Telescope Coll., Akiyama, K., Alberdi, A., Alef, W., Asada, K., Azulay, R., Baczko, A.-K., et al., (2019a). First M87 Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole. Astrophys. J. Letters 875, L1. [EHT-Col...

  50. [801]

    Pre-supernova Evolution of Rotating Solar Metallicity Stars in the Mass Range 13-120M⊙ and their Explosive Yields

    [Chieffi & Limongi (2013)] Chieffi, A., & Limongi, M., (2013). Pre-supernova Evolution of Rotating Solar Metallicity Stars in the Mass Range 13-120M⊙ and their Explosive Yields. Astrophys. J. 764,

  51. [812]

    [Diehl (2013)] Diehl, R., (2013)

    Berlin: Springer. [Diehl (2013)] Diehl, R., (2013). Nuclear astrophysics lessons from INTEGRAL. Rep. Pro.Phys. 76, id. 026301. [Diehl (2017)] Diehl, R., (2017). Gamma-ray line measurements from supernova ex- plosions. in Proc. IAU Symposium 331 ”SN1987A 30 years after”, La Reu...

  52. [880]

    (2003)] Gopal-Krishna, Biermann, P.L., & Wiita, P.J., Astrophys

    [Gopal-Krishna et al. (2003)] Gopal-Krishna, Biermann, P.L., & Wiita, P.J., Astrophys. J. Letters 594, L103 - L106 (2003); Title: The Origin of X-shaped Radio Galaxies: Clues from the Z-symmetric Secondary Lobes [Gopal-Krishna et al. (2012)] Gopal-Krishna, Biermann, P.L., Gerg...

  53. [903]

    Toward the event horizon - the supermassive black hole in the Galactic Center

    [Falcke & Markoff (2013)] Falcke, H., & Markoff, S., (2013). Toward the event horizon - the supermassive black hole in the Galactic Center. Class. Quantum Grav. 30, 244003. [Fermi (1949)] Fermi, E., (1949). On the Origin of the Cosmic Radiation. Phys. Rev. 75, 1169 -

  54. [1056]

    High-energy astrophysics: A rare Galactic anti- matter source? Nature Astron

    [Prantzos (2017)] Prantzos, N., (2017). High-energy astrophysics: A rare Galactic anti- matter source? Nature Astron. 1, 0149 [Rachen et al. (1993)] Rachen, J.P., Stanev, T., & Biermann, P.L., Astron. & Astroph. 273, 377 (1993), astro-ph/9302005. Title: Extragalactic ultra hig...

  55. [1059]

    (2023)] Jaroschewski, I., Becker Tjus, J., Biermann, P

    [Jaroschewski et al. (2023)] Jaroschewski, I., Becker Tjus, J., Biermann, P. L. (2023), Extragalactic neutrino emission induced by Supermassive and Stellar Mass Black Hole mergers, , Month. Not. Roy. Astr. Soc. 518, 6158 - 6182, arXiv:2210.11337, DOI 10.1093/mnras/stac3402 and...

  56. [1076]

    (2006)] Merloni, A., K¨ ording, E., Heinz, S., Markoff, S., Di Matteo, T., & Falcke, H., (2006)

    [Merloni et al. (2006)] Merloni, A., K¨ ording, E., Heinz, S., Markoff, S., Di Matteo, T., & Falcke, H., (2006). Why the fundamental plane of black hole activity is not simply a distance driven artifact. New Astron. 11 567 - 576 [Mirabel et al. (2011)] Mirabel, I.F., Dijkstra,...

  57. [1174]

    Galactic Magnetic Fields and the Origin of Cosmic Radiation

    [Fermi (1954)] Fermi, E., (1954). Galactic Magnetic Fields and the Origin of Cosmic Radiation. Astrophys. J. 119, 1 -

  58. [1801]

    (2015)] Patil, M., Joshi, P.S., Nakao, K., et al., (2015)

    [Patil et al. (2015)] Patil, M., Joshi, P.S., Nakao, K., et al., (2015). Timescale for trans- Planckian collisions in Kerr spacetime. Europhys. Lett. 110, 30004. [Patil et al. (2016)] Patil, M., Harada, T., Nakao, K., Joshi, P.S., & Kimura, M., (2016). Infinite efficiency of t...

  59. [1929]

    (2013a)] Chini, R., Barr, A., Buda, L.S., Dembsky, T., Drass, H., Nasseri, A

    [Chini et al. (2013a)] Chini, R., Barr, A., Buda, L.S., Dembsky, T., Drass, H., Nasseri, A. , et al., (2013a). The Multiplicity of High-mass Stars. Centr. Eur. Astrophys. Bull. 37, 295 - 310, DOI 10.48550/arXiv.1306.1811 61 [Chini et al. (2013b)] Chini, R., Nasseri, A., Dembsk...

  60. [2012]

    Key problems in black hole physics today

    68 [Joshi (2011)] Joshi, P.S., (2011). Key problems in black hole physics today. Fluid Flows To Black Holes: A Tribute to S. Chandrasekhar on His Birth Centenary. Edited by D.J. Saikia and Virginia Trimble. World Scientific. [Joshi (2014)] Joshi, P.S., (2014). Spacetime Singul...

  61. [2017]

    [Drake et al

    IAU Conf 331 Proc., Cambridge, UK, 157 - 163 (2017); eprint arXiv:1704.05937. [Drake et al. (1987)] Drake, St.A., Abbott, D.C., Bastian, T. S., Bieging, J.H., Church- well, E., Dulk, G., et al., Astrophys. J. 322, 902 - 908 (1987); Title: The Discovery of Nonthermal Radio Emis...

  62. [2346]

    Invited, Rapporteur and Highlight papers

    [Bell & Lucek (2001)] Bell, A.R., & Lucek, S.G., Month. Not. Roy. Astr. Soc. 321, 433 - 438 (2001); Title: Cosmic ray acceleration to very high energy through the non- linear amplification by cosmic rays of the seed magnetic field [Biermann (1993)] Biermann, P.L., Astron. & As...

  63. [2417]

    (1994)] Muxlow, T.W.B., Pedlar, A., Wilkinson, P.N., Axon, D

    [Muxlow et al. (1994)] Muxlow, T.W.B., Pedlar, A., Wilkinson, P.N., Axon, D. J., Sanders, E. M., & de Bruyn, A.G., Month. Not. Roy. Astr. Soc. 266, 455 - 467 (1994); Title: The structure of young supernova remnants in M82 [Muxlow et al. (2005)] Muxlow, T.W.B., Pedlar, A., Besw...

  64. [3964]

    (2013)] Gaisser, T.K., Stanev, T., & Tilav, S., (2013)

    [Gaisser et al. (2013)] Gaisser, T.K., Stanev, T., & Tilav, S., (2013). Cosmic ray energy spectrum from measurements of air showers. Invited review, Front. Phys. 8, 748 -

  65. [5173]

    (2011)] Prantzos, N., Boehm, C., Bykov, A.M., Diehl, R., Ferri` ere, K., Guessoum, N., et al., (2011)

    [Prantzos et al. (2011)] Prantzos, N., Boehm, C., Bykov, A.M., Diehl, R., Ferri` ere, K., Guessoum, N., et al., (2011). The 511 keV emission from positron annihilation in the Galaxy. Rev. Mod. Phys. 83, 1001 -

Pith tools

Reviewed August 12, 2026 · model on record in the stance chip above.