REVIEW 3 major objections 5 minor 1 cited by
The accretion disk and neutrino propagation of Barrow-modified Black Hole
T0 review · 3 major / 5 minor · reviewed 2026-08-16 · deepseek-v4-flash
Pith's one-line read A Barrow-modified black hole metric shrinks the ISCO, heats the disk 62.5%, and lifts neutrino energy 8–28 times.
desk verdict The Barrow-disk ISCO formula is new and clean, but the paper's own Table I refutes its headline neutrino enhancement claim. read the letter →
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
The reading
What carries the argument
The load-bearing object is the Barrow-modified metric, Eq. (8): a Schwarzschild-like line element in which the radial coordinate is replaced by $r^{1+\Delta/2}$, with $\Delta\in[0,1]$. This single substitution controls both halves of the paper: it enters the effective potential whose second derivative fixes $r_{\rm ISCO}$, and it changes $g_{tt}$, $g_{rr}$, and $g_{\phi\phi}$ in the null-geodesic equation and in the angular factor $x=\sin\theta_r$ that determines neutrino-pair collision angles. The disk part of the argument then follows the standard Novikov-Thorne flux formula $F(r)$ with the modified metric components. The substitution is the one load-bearing change; no other physical ingredient is altered.
What would settle it
Recompute the ISCO, disk fluxes, and neutrino deposition using an exact black-hole solution whose entropy is Barrow entropy (or an action whose field equations admit it); if the resulting ISCO does not follow the scaling in Eq. (23) or the spectral shape differs, the specific $62.5\%$ and $8$–$28$ enhancements do not survive.
Extended reading notes
Core claim
The central claim is that the substitution $r\to r^{1+\Delta/2}$ in the Schwarzschild metric yields $r_{\rm ISCO}=36^{1/(2+\Delta)}M^{2/(2+\Delta)}$, so the ISCO shrinks monotonically as $\Delta$ grows. Feeding this metric into the Novikov-Thorne thin-disk model gives, at $\Delta=1$, a $22.5\%$ higher peak flux, a $62.5\%$ higher effective temperature, and about a $50\%$ higher differential luminosity in the paper's $M=1$ units. For neutrino pair annihilation, the same metric changes the null-geodesic bending angle, and integrating the local deposition rate gives $\dot{Q}/\dot{Q}_{\rm Newt}$ between $8$ and $28$ for compact sources with $R/M\simeq 3$–$4$ when $\Delta=1$. These are the quantitative relations the paper claims to establish between Barrow's fractal parameter $\Delta$ and accretion-disk emission and neutrino-pair-annihilation energy.
Load-bearing premise
The load-bearing premise is the metric ansatz obtained by replacing $r$ with $r^{1+\Delta/2}$ in Schwarzschild: a prescription imported from Barrow-entropy thermodynamics, not derived from field equations or observations.
Editorial extensions
If this is right
- At $\Delta=1$, the disk inner edge sits near $r\simeq3.3$ rather than $6$ (in $M=1$ units), so the thermal emission peak moves inward and the spectrum is hotter and harder for the same accretion rate.
- Near a source with $R/M\simeq3$–$4$, neutrino-pair annihilation can deposit $8$–$28$ times the Newtonian energy, relaxing the energy budget needed to power short gamma-ray bursts from a Barrow-modified black hole.
- The radiative efficiency $\epsilon=1-2\sqrt{2}/3$ is independent of $\Delta$; the fractal geometry changes where and how the energy is released, not the total energy per accreted mass that escapes to infinity.
- The $\Delta$-dependence gives a direct way to turn future high-precision disk spectra and GRB luminosity estimates into bounds on the fractal parameter.
Reading between the lines
- The paper does not derive the $r\to r^{1+\Delta/2}$ metric from an action or field equations; a natural next step is to construct an exact Barrow-entropy solution and test whether the same ISCO scaling survives, since the numerical enhancements depend on that scaling.
- Because the temperature shift at $\Delta=1$ is a $62.5\%$ change at fixed mass, thermal-state spectra of stellar-mass black holes with well-measured masses and distances could constrain $\Delta$ even before neutrino measurements mature.
- The enhancement in $\dot{Q}/\dot{Q}_{\rm Newt}$ is concentrated near $r/R\sim1$ and falls below the general-relativistic curve at larger radii; this radial structure could be probed in simulations of binary neutron-star merger remnants, which have the relevant $R/M\simeq3$–$4$.
Signed reviews
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. This paper investigates a spherically symmetric black hole spacetime obtained by the replacement r → r^{1+Δ/2} in the Schwarzschild metric, which the authors associate with Barrow's fractal entropy. It derives the ISCO radius r_ISCO = 36^{1/(2+Δ)} M^{2/(2+Δ)}, computes Novikov-Thorne thin-disk flux, temperature, and luminosity profiles for Δ = 0, 0.5, 1, and evaluates the energy deposition rate from νν̄ → e⁺e⁻ pair annihilation near the horizon using the Salmonson-Wilson formalism. The paper's headline results are that Δ = 1 raises the peak disk flux by 22.5%, the effective temperature by 62.5%, the differential luminosity by about 50%, and the neutrino annihilation deposition rate by factors of 8–28 at R/M ≈ 3–4. These claims are presented as the first quantitative link between Barrow's fractal parameter and high-energy astrophysical observables.
Significance. The intended significance is high if the quantitative claims were correct, because they would imply that fractal quantum geometry modifies accretion disk emission and gamma-ray burst energy budgets at an observable level. The paper is transparent in its derivations: the ISCO condition is solved analytically, the disk integrals are written out explicitly, and the neutrino deposition formula follows the standard Salmonson-Wilson framework. The authors also cite the relevant literature on Barrow entropy and pair annihilation. However, the central quantitative claims are invalidated by internal inconsistencies in the manuscript's own tables and equations, and the underlying metric ansatz is imported from previous work without independent justification. At present the paper does not establish its stated conclusions.
major comments (3)
- [§IV, Table I; §V] The abstract and conclusion state that for Δ = 1 the neutrino pair annihilation energy deposition rate is 8 to 28 times higher than the classical Newtonian estimate when R/M ≈ 3–4. Table I, however, lists Qdot for Δ = 1 as 0.78×10^51 erg/s at R/M = 3 and 0.51×10^51 erg/s at R/M = 4, against the Newtonian value 1.50×10^50 erg/s; these ratios are 5.2 and 3.4, respectively. The 8–28 enhancement actually corresponds to the Δ = 0 (Schwarzschild) rows, which give 4.32×10^51 / 1.50×10^50 = 28.8 and 1.10×10^51 / 1.50×10^50 = 7.3. Hence the paper's own data show that fractality (Δ = 1) suppresses the enhancement relative to the general-relativistic (Δ = 0) case, directly contradicting the headline claim.
- [§III, Eqs. (27)–(29), Figs. 4 and 6] The paper claims a 62.5% increase in effective temperature and a 22.5% increase in peak flux for Δ = 1, but these two numbers are not mutually consistent under the blackbody relation T = (F/σ)^{1/4} given in Eq. (29). A 22.5% flux increase implies a temperature increase of only about 5.2%. No separate mechanism is provided to reconcile this discrepancy, so the temperature claim is not supported by the calculation as presented.
- [§II, Eq. (8); §V] The Barrow-modified metric is assumed rather than derived; it is imported from Ref. [12] through the substitution r → r^{1+Δ/2}, with no field equations or quantum-gravity action. Moreover, the same manuscript cites Ref. [22] in the conclusion to state that stability requires Δ ≲ 10^{-3} for solar-mass black holes, which directly contradicts the use of Δ = 1 as the representative 'maximal fractal' case throughout the paper. Even if the internal inconsistencies were fixed, the quantitative predictions for Δ = 1 would be physically unrealistic under the authors' own stability constraint.
minor comments (5)
- [§I, second paragraph] The phrase 'fractal sapcetime' should read 'fractal spacetime'.
- [§IV, Fig. 8 legend] The legend lists 'M = 0.1R, Δ = 0' twice; the second entry should presumably be Δ = 0.5 (or a distinct parameter value) to match the three curves described in the text.
- [§III and §V] The temperature increase is quoted as 62.47% in the body and 62.5% in the conclusion and abstract; these values should be made consistent.
- [§III, Eq. (30)] The efficiency ε is shown to be independent of Δ even though the ISCO shifts; a brief comment explaining why the combination in Eq. (19) evaluated at Eq. (23) yields a constant would help the reader.
- [Abstract and §III] The abstract speaks of a 'spectral radiance' increase of about 50%, while the body reports a differential luminosity increase; these are distinct quantities and the wording should be aligned.
Circularity Check
The claimed Barrow-modified ISCO is a coordinate relabeling of the Schwarzschild ISCO: Eq. (23) is exactly the known 6M ISCO written in the coordinate r = rho^(2/(2+Delta)).
-
renaming known result
[Sec. II, Eqs. (7), (8), (23)]
"The following modifications on r may be produced by comparing Eq.(6) and Eq.(4) [12], r→r1+ ∆/2. (7) It is possible to express the Barrow-modified metric as [12] ds2 = ... (8) ... whose real solution is rISCO = 36 1 2+∆ M 2 2+∆. (23)"
The circular-orbit equations used for the ISCO involve only g_tt and g_phi phi. In Eq. (8) those components are exactly the Schwarzschild ones under rho = r^(1+Delta/2): g_tt = -(1-2M/rho) and g_phi phi = rho^2. The known Schwarzschild ISCO is rho = 6M; substituting rho = r^(1+Delta/2) gives r = (6M)^(2/(2+Delta)) = 36^(1/(2+Delta)) M^(2/(2+Delta)), which is precisely Eq. (23). The paper's own Eq. (22), M(6M - r^(1+Delta/2))(2+Delta)^2 = 0, states this directly. Thus the Delta-dependence of r_ISCO is not a new quantum-gravity prediction but the inverse of the coordinate rescaling inserted in Eq. (7). The claimed inward shift is a labeling artifact of the coordinate r, so the derivation reduces to its input by construction.
-
renaming known result
[Sec. IV, Table I and abstract]
"The energy deposition rate for ∆ = 1 is 8 − 28 times higher than classical estimates when the black hole radius is R/M∼ 3− 4. ... T able I: The rate ˙Q for different values of ∆ and R/M. Newtonian 0 1.50×1050; ∆ = 0 3 4.32×1051, 4 1.10×1051; ∆ = 1 3 0.78×1051, 4 0.51×1051."
The abstract's 8-28x factors are actually the Delta = 0 row of Table I: 4.32e51/1.50e50 = 28.8 and 1.10e51/1.50e50 = 7.3, whereas the Delta = 1 entries give only 5.2x and 3.4x. More fundamentally, R in Eq. (44) is the coordinate radius of metric (8), so for Delta = 1 the range R/M = 3-4 corresponds to the Schwarzschild area radius rho/M = (R/M)^(3/2) = 5.2-8. The 'enhanced' deposition is therefore the standard Schwarzschild result evaluated at larger physical radii and re-expressed in the r-coordinate; the advertised Barrow enhancement is a coordinate relabeling rather than an independent prediction.
full rationale
The central quantitative claim reduces to the coordinate ansatz. The ISCO derivation uses only g_tt and g_phi phi, which, from the replacement r -> r^(1+Delta/2), are exactly the Schwarzschild components in the radial coordinate rho = r^(1+Delta/2). Hence Eq. (23) is just the Schwarzschild ISCO rho = 6M rewritten in r, and the inward shift with Delta is a coordinate artifact. The same relabeling propagates into the neutrino-deposition section: R is the coordinate radius, so the Delta = 1 curves at R/M = 3-4 are Schwarzschild curves at rho/M = 5.2-8. In addition, the paper's own Table I contradicts the abstract: the 8-28x enhancement belongs to Delta = 0, not Delta = 1, whose tabulated ratios are only 5.2x and 3.4x above the Newtonian value. Separately, the disk section is internally inconsistent: with T = (F/sigma)^(1/4), a 22.47% peak flux increase implies about a 5.2% temperature increase, not the claimed 62.47%. These issues do not depend on whether the Barrow metric ansatz itself is externally justified; even if Eq. (8) were accepted, the headline ISCO and enhancement claims are built into the coordinate substitution rather than derived from new physics.
Assumptions & free parameters
free parameters (1)
- Barrow fractal index delta =
Scanned values 0, 0.5, 1
assumptions (3)
- ad hoc to paper The Barrow-modified metric of Eq. (8), with r replaced by r^(1+delta/2), correctly describes a black hole spacetime with fractal horizon.
- domain assumption The Novikov-Thorne thin accretion disk model applies to this metric without modification.
- domain assumption The standard neutrino pair annihilation energy deposition formula of Eq. (35) is valid in this spacetime.
invented entities (1)
-
Barrow fractal-modified black hole spacetime with r -> r^(1+delta/2)
Cite this review
Pith. "Pith review of The accretion disk and neutrino propagation of Barrow-modified Black Hole." pith.science (2026). https://pith.science/paper/R4J5TXJR
@misc{pith2026250415892,
author = {Pith},
title = {Pith review of: The accretion disk and neutrino propagation of Barrow-modified Black Hole},
year = {2026},
howpublished = {\url{https://pith.science/paper/R4J5TXJR}},
note = {Machine review of arXiv:2504.15892}
}
abstract
This paper attempts to clarify the deep consequences of Barrow fractal black hole spacetime configurations caused by quantum gravity on neutrino pair annihilation and accretion disk dynamics. We systematically derive the analytical expression for the innermost stable circular orbit (ISCO) radius ($r_{\text{ISCO}}\propto M^{2/(2+\Delta)}$) by building a Barrow-modified static spherically symmetric metric ($r\rightarrow r^{1+\Delta/2}$), and we find that increasing $\Delta$ significantly shifts the ISCO inward. We numerically solve the radiation flux, effective temperature, and differential luminosity distribution under the modified metric based on the Novikov-Thorne relativistic thin accretion disk model. For $\Delta=1$, the results show that the temperature increases by $62.5\%$, the peak disk radiation flux increases by $22.5\%$, and the spectral radiance increases by around $50\%$. Fractal horizons enhance neutrino trajectory bending effects, according to further study of neutrino pair annihilation ($\nu\bar{\nu}\rightarrow e^+e^-$) energy deposition processes using local Lorentz transformations and null geodesic equations. The energy deposition rate for $\Delta=1$ is $8-28$ times higher than classical estimates when the black hole radius is $R/M\sim3-4$. This work provides important theoretical insights into the influence of quantum spacetime geometry on high-energy astrophysical phenomena in extreme gravitational fields by establishing, for the first time, quantitative relationships between the Barrow parameter $\Delta$ and neutrino pair annihilation energy and accretion disk radiative efficiency.
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Forward citations
Cited by 1 Pith paper
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Reference graph
Works this paper leans on
-
[12]
The area of a rough black hole
John D Barrow. The area of a rough black hole. Physics Letters B, 808:135643, 2020
work page 2020
-
[22]
Sign switching dark energy from a running barrow entropy
Sofia Di Gennaro and Yen Chin Ong. Sign switching dark energy from a running barrow entropy. Universe, 8(10):541, 2022
work page 2022
-
[1]
The mathematical theory of black holes , volume 69
Subrahmanyan Chandrasekhar. The mathematical theory of black holes , volume 69. Oxford university press, 1998
work page 1998
-
[2]
(7) It is possible to express the Barrow-modified metric as [12] ds2 =gµνdxµdxν =− 1− 2M r1+ ∆ 2 dt2 + 1− 2M r1+ ∆ 2 −1 1 + ∆ 2 r∆dr2 +r2+∆ dθ2 + sin2θdφ2 , (8) with ∆ = 0, this leads to the classical case corresponding to the simplest horizon structure. At the most complex, ∆ = 1, it acts as though it had one more geometric di- mension even though it is ...
-
[3]
Gravitation and cosmology: principles and applications of the general theory of relativity
Steven Weinberg. Gravitation and cosmology: principles and applications of the general theory of relativity . John Wiley & Sons, 2013
work page 2013
-
[4]
Thermodynamics of black holes in anti-de sitter space
Stephen W Hawking and Don N Page. Thermodynamics of black holes in anti-de sitter space. Communications in Mathematical Physics, 87:577–588, 1983
work page 1983
-
[5]
Anti-de sitter space, thermal phase tran- sition, and confinement in gauge theories
Edward Witten. Anti-de sitter space, thermal phase tran- sition, and confinement in gauge theories. arXiv preprint hep-th/9803131, 1998
arXiv 1998
-
[6]
Holography, thermodynamics, and fluctuations of charged ads black holes
Andrew Chamblin, Roberto Emparan, Clifford V John- son, and Robert C Myers. Holography, thermodynamics, and fluctuations of charged ads black holes. Physical Re- view D , 60(10):104026, 1999
work page 1999
Show all 67 references
-
[7]
Black holes and entropy
Jacob D Bekenstein. Black holes and entropy. Physical Review D, 7(8):2333, 1973
1973
-
[8]
Aspects of holo- graphic entanglement entropy
Shinsei Ryu and Tadashi Takayanagi. Aspects of holo- graphic entanglement entropy. Journal of High Energy Physics, 2006(08):045, 2006
2006
-
[9]
Properties and astrophysical implica- tions of the 150 m⊙ binary black hole merger gw190521
Richard Abbott, TD Abbott, S Abraham, F Acernese, K Ackley, C Adams, RX Adhikari, VB Adya, C Affeldt, M Agathos, et al. Properties and astrophysical implica- tions of the 150 m⊙ binary black hole merger gw190521. The Astrophysical Journal Letters , 900(1):L13, 2020
2020
-
[10]
Electronic structure of plastocyanin: excited state spectral features
Andrew A Gewirth and Edward I Solomon. Electronic structure of plastocyanin: excited state spectral features. Journal of the American Chemical Society , 110(12):3811– 3819, 1988
1988
-
[11]
Magnetars in the metagalaxy: an origin for ultra-high-energy cosmic rays in the nearby universe
Jonathan Arons. Magnetars in the metagalaxy: an origin for ultra-high-energy cosmic rays in the nearby universe. The Astrophysical Journal , 589(2):871, 2003
2003
-
[13]
Barrow-type structure and thermodynamics of black holes
Athanasios Petridis and Asmaa G Shalaby. Barrow-type structure and thermodynamics of black holes. Physics Letters B, 836:137616, 2023
2023
-
[14]
Barrow en- tropies in black hole thermodynamics
Salvatore Capozziello and Mehdi Shokri. Barrow en- tropies in black hole thermodynamics. The European Physical Journal C , 85(2):200, 2025
2025
-
[15]
Barrow black holes and the minimal length
Li-Hua Wang and Meng-Sen Ma. Barrow black holes and the minimal length. Physics Letters B , 831:137181, 2022
2022
-
[16]
Barrow fractal entropy and the black hole quasinormal modes
Everton MC Abreu and Jorge Ananias Neto. Barrow fractal entropy and the black hole quasinormal modes. Physics Letters B , 807:135602, 2020
2020
-
[17]
Cosmology intertwined: A re- view of the particle physics, astrophysics, and cosmology associated with the cosmological tensions and anomalies
Elcio Abdalla, Guillermo Franco Abell´ an, Amin Aboubrahim, Adriano Agnello, ¨Ozg¨ ur Akarsu, Yashar Akrami, George Alestas, Daniel Aloni, Luca Amendola, Luis A Anchordoqui, et al. Cosmology intertwined: A re- view of the particle physics, astrophysics, and cosmology associate...
2022
-
[18]
Early and late universe holographic cosmology from a new generalized entropy
Shin’ichi Nojiri, Sergei D Odintsov, and Tanmoy Paul. Early and late universe holographic cosmology from a new generalized entropy. Physics Letters B , 831:137189, 2022
2022
-
[19]
Barrow holographic dark energy
Emmanuel N Saridakis. Barrow holographic dark energy. Physical Review D , 102(12):123525, 2020
2020
-
[20]
Kaniadakis holo- graphic dark energy and cosmology
Niki Drepanou, Andreas Lymperis, Emmanuel N Sari- dakis, and Kuralay Yesmakhanova. Kaniadakis holo- graphic dark energy and cosmology. The European Phys- ical Journal C , 82(5):449, 2022
2022
-
[21]
Gen- eralized entropy implies varying-g: Horizon area depen- dent field equations and black hole-cosmology coupling
Hengxin L¨ u, Sofia Di Gennaro, and Yen Chin Ong. Gen- eralized entropy implies varying-g: Horizon area depen- dent field equations and black hole-cosmology coupling. Annals of Physics , 474:169914, 2025
2025
-
[23]
Upper bound of barrow entropy index from black hole fragmentation
Jiayi Xia and Yen Chin Ong. Upper bound of barrow entropy index from black hole fragmentation. Universe, 10(4):177, 2024
2024
-
[24]
How bar- row entropy modifies gravity: with comments on tsallis entropy
Sofia Di Gennaro, Hao Xu, and Yen Chin Ong. How bar- row entropy modifies gravity: with comments on tsallis entropy. The European Physical Journal C , 82(11):1066, 2022
2022
-
[25]
Observational constraints on barrow holographic dark energy
Fotios K Anagnostopoulos, Spyros Basilakos, and Em- manuel N Saridakis. Observational constraints on barrow holographic dark energy. The European Physical Journal C, 80(9):826, 2020
2020
-
[26]
General- ized entropies and corresponding holographic dark energy models
H Moradpour, AH Ziaie, and M Kord Zangeneh. General- ized entropies and corresponding holographic dark energy models. The European Physical Journal C , 80(8):732, 2020
2020
-
[27]
Barrow holographic dark energy in a nonflat universe
Priyanka Adhikary, Sudipta Das, Spyros Basilakos, and Emmanuel N Saridakis. Barrow holographic dark energy in a nonflat universe. Physical Review D, 104(12):123519, 2021
2021
-
[28]
Accretion disk around a schwarzschild black hole in asymptotic safety
Fabi´ an H Zuluaga and Luis A S´ anchez. Accretion disk around a schwarzschild black hole in asymptotic safety. The European Physical Journal C , 81:1–9, 2021
2021
-
[29]
Disk-accretion onto a black hole
Don N Page and Kip S Thorne. Disk-accretion onto a black hole. time-averaged structure of accretion disk. Astrophysical Journal, Vol. 191, pp. 499-506 (1974) , 191:499–506, 1974
1974
-
[30]
Neutrino trapping and accretion models for gamma-ray bursts
Tiziana Di Matteo, Rosalba Perna, and Ramesh Narayan. Neutrino trapping and accretion models for gamma-ray bursts. The Astrophysical Journal , 579(2):706, 2002
2002
-
[31]
Accretion and outflow from a magnetized, neutrino cooled torus around the gamma-ray burst cen- tral engine
Agnieszka Janiuk, Patryk Mioduszewski, and Monika Moscibrodzka. Accretion and outflow from a magnetized, neutrino cooled torus around the gamma-ray burst cen- tral engine. The Astrophysical Journal , 776(2):105, 2013
2013
-
[32]
Neutrino-cooled accretion disk and its stability
Norita Kawanaka and Shin Mineshige. Neutrino-cooled accretion disk and its stability. The Astrophysical Jour- nal, 662(2):1156, 2007. 8
2007
-
[33]
General relativis- tic augmentation of neutrino pair annihilation energy de- position near neutron stars
Jay D Salmonson and James R Wilson. General relativis- tic augmentation of neutrino pair annihilation energy de- position near neutron stars. The Astrophysical Journal , 517(2):859, 1999
1999
-
[34]
Neutrino pair annihilation in the gravitation of gamma-ray burst sources
Katsuaki Asano and Takeshi Fukuyama. Neutrino pair annihilation in the gravitation of gamma-ray burst sources. The Astrophysical Journal , 531(2):949, 2000
2000
-
[35]
Relativistic ef- fects on neutrino pair annihilation above a kerr black hole with the accretion disk
Katsuaki Asano and Takeshi Fukuyama. Relativistic ef- fects on neutrino pair annihilation above a kerr black hole with the accretion disk. The Astrophysical Journal , 546(2):1019, 2001
2001
-
[36]
Off-axis neutrino scattering in gamma-ray burst central engines
Warner A Miller, Nathan D George, Arkady Kheyfets, and John M McGhee. Off-axis neutrino scattering in gamma-ray burst central engines. The Astrophysical Journal, 583(2):833, 2003
2003
-
[37]
Neu- trino pair annihilation near accreting, stellar-mass black holes
Reiner Birkl, MA Aloy, H-Th Janka, and E M¨ uller. Neu- trino pair annihilation near accreting, stellar-mass black holes. Astronomy & Astrophysics , 463(1):51–67, 2007
2007
-
[38]
Effects of modified theories of gravity on neutrino pair annihi- lation energy deposition near neutron stars
Gaetano Lambiase and Leonardo Mastrototaro. Effects of modified theories of gravity on neutrino pair annihi- lation energy deposition near neutron stars. The Astro- physical Journal, 904(1):19, 2020
2020
-
[39]
Energy deposi- tion due to neutrino pair annihilation near rotating neu- tron stars
AR Prasanna and Srubabati Goswami. Energy deposi- tion due to neutrino pair annihilation near rotating neu- tron stars. Physics Letters B , 526(1-2):27–33, 2002
2002
-
[40]
Neutrino pair anni- hilation (ν¯ν−→e−e+) in the presence of quintessence surrounding a black hole
G Lambiase and L Mastrototaro. Neutrino pair anni- hilation (ν¯ν−→e−e+) in the presence of quintessence surrounding a black hole. The European Physical Jour- nal C , 81(10):1–11, 2021
2021
-
[41]
The neutrino pair an- nihilation around a massive source with an f (r) global monopole
Yuxuan Shi and Hongbo Cheng. The neutrino pair an- nihilation around a massive source with an f (r) global monopole. Europhysics Letters, 140(4):49001, 2022
2022
-
[42]
The gamma-ray burst arising from neutrino pair annihilation in the static and spherically symmetric black-hole-like wormholes
Yuxuan Shi and Hongbo Cheng. The gamma-ray burst arising from neutrino pair annihilation in the static and spherically symmetric black-hole-like wormholes. Journal of Cosmology and Astroparticle Physics , 2023(10):062, 2023
2023
-
[43]
The shadow and gamma-ray bursts of a schwarzschild black hole in asymp- totic safety
Yuxuan Shi and Hongbo Cheng. The shadow and gamma-ray bursts of a schwarzschild black hole in asymp- totic safety. Communications in Theoretical Physics , 77(2):025401, 2024
2024
-
[44]
On a continuous curve without tangents constructive from elementary geometry
Helge Von Koch. On a continuous curve without tangents constructive from elementary geometry. In Classics on fractals, pages 24–45. CRC Press, 2019
2019
-
[45]
Allgemeine R¨ aume und Cartesische R¨ aume”
Karl Menger and LEJ Brouwer. Allgemeine R¨ aume und Cartesische R¨ aume”. Zweite Mitteilung:”Ueber um- fassendste ndimensionale Mengen . Springer, 2002
2002
-
[46]
A curve of which every point is a ramifica- tion point
W Sierpinski. A curve of which every point is a ramifica- tion point. COMPTES RENDUS HEBDOMADAIRES DES SEANCES DE L ACADEMIE DES SCIENCES , 160:302–305, 1915
1915
-
[47]
Thin accretion disc luminosity and its image around rotating black holes in perfect fluid dark matter
Malihe Heydari-Fard, Sara Ghassemi Honarvar, and Mo- haddese Heydari-Fard. Thin accretion disc luminosity and its image around rotating black holes in perfect fluid dark matter. Monthly Notices of the Royal Astronomical Society, 521(1):708–716, 2023
2023
-
[48]
Black holes: a laboratory for testing strong gravity, volume 10
Cosimo Bambi. Black holes: a laboratory for testing strong gravity, volume 10. Springer, 2017
2017
-
[49]
Testing hoˇ rava-lifshitz gravity using thin accretion disk properties
Tiberiu Harko, Zolt´ an Kov´ acs, and Francisco SN Lobo. Testing hoˇ rava-lifshitz gravity using thin accretion disk properties. Physical Review D , 80(4):044021, 2009
2009
-
[50]
Black holes, edited by c
ID Novikov and KS Thorne. Black holes, edited by c. dewitt and bs dewitt, 1973
1973
-
[51]
Black holes in binary systems: Observational appearances
NI Shakura and RA Sunyaev. Black holes in binary systems: Observational appearances. In Symposium- International Astronomical Union , volume 55, pages 155–164. Cambridge University Press, 1973
1973
-
[52]
Disk-accretion onto a black hole
Kip S Thorne. Disk-accretion onto a black hole. ii. evo- lution of the hole. Astrophysical Journal, Vol. 191, pp. 507-520 (1974) , 191:507–520, 1974
1974
-
[53]
Distinguishing black holes from naked singu- larities through their accretion disc properties
Pankaj S Joshi, Daniele Malafarina, and Ramesh Narayan. Distinguishing black holes from naked singu- larities through their accretion disc properties. Classical and Quantum Gravity , 31(1):015002, 2013
2013
-
[54]
A code to compute the emission of thin accretion disks in non-kerr spacetimes and test the na- ture of black hole candidates
Cosimo Bambi. A code to compute the emission of thin accretion disks in non-kerr spacetimes and test the na- ture of black hole candidates. The Astrophysical Journal, 761(2):174, 2012
2012
-
[55]
Einstein maxwell scalar black hole: Thermodynamic properties with logarithmic barrow entropy
Ritabrata Biswas and Satyajit Pal. Einstein maxwell scalar black hole: Thermodynamic properties with logarithmic barrow entropy. arXiv preprint arXiv:2505.17172, 2025
2025 arXiv
-
[56]
Hy- peraccreting black holes and gamma-ray bursts
Robert Popham, Stan E Woosley, and Chris Fryer. Hy- peraccreting black holes and gamma-ray bursts. The As- trophysical Journal, 518(1):356, 1999
1999
-
[57]
Spontaneous lorentz symmetry breaking effects on grbs jets arising from neutrino pair annihila- tion process near a black hole
Mohsen Khodadi, Gaetano Lambiase, and Leonardo Mastrototaro. Spontaneous lorentz symmetry breaking effects on grbs jets arising from neutrino pair annihila- tion process near a black hole. The European Physical Journal C , 83(3):239, 2023
2023
-
[58]
Neutrino heat- ing near hyper-accreting black holes
Ivan Zalamea and Andrei M Beloborodov. Neutrino heat- ing near hyper-accreting black holes. Monthly Notices of the Royal Astronomical Society , 410(4):2302–2308, 2011
2011
-
[59]
Shadows and rings of the kehagias-sfetsos black hole surrounded by thin disk ac- cretion
Guo-Ping Li and Ke-Jian He. Shadows and rings of the kehagias-sfetsos black hole surrounded by thin disk ac- cretion. Journal of Cosmology and Astroparticle Physics , 2021(06):037, 2021
2021
-
[60]
Gamma-ray bursts via the neutrino emission from heatedneutron stars
Jay D Salmonson, James R Wilson, and Grant J Math- ews. Gamma-ray bursts via the neutrino emission from heatedneutron stars. The Astrophysical Journal , 553(2):471, 2001
2001
-
[61]
Neutrino annihi- lation between binary neutron stars
Jay D Salmonson and James R Wilson. Neutrino annihi- lation between binary neutron stars. The Astrophysical Journal, 561(2):950, 2001
2001
-
[62]
A model of short gamma-ray bursts: heated neutron stars in close binary systems
Jay D Salmonson and James R Wilson. A model of short gamma-ray bursts: heated neutron stars in close binary systems. The Astrophysical Journal , 578(1):310, 2002
2002
-
[63]
First m87 event horizon telescope results
Kazunori Akiyama, Antxon Alberdi, Walter Alef, Keiichi Asada, Rebecca Azulay, Anne-Kathrin Baczko, David Ball, Mislav Balokovi´ c, John Barrett, Dan Bintley, et al. First m87 event horizon telescope results. iii. data pro- cessing and calibration. The Astrophysical Journal Let...
2019
-
[64]
First m87 event horizon telescope results
Kazunori Akiyama, Antxon Alberdi, Walter Alef, Keiichi Asada, Rebecca Azulay, Anne-Kathrin Baczko, David Ball, Mislav Balokovi´ c, John Barrett, Dan Bintley, et al. First m87 event horizon telescope results. iv. imaging the central supermassive black hole. The Astrophysical Jo...
2019
-
[65]
First m87 event horizon telescope results
Kazunori Akiyama, Antxon Alberdi, Walter Alef, Keiichi Asada, Rebecca Azulay, Anne-Kathrin Baczko, David Ball, Mislav Balokovi´ c, John Barrett, Dan Bintley, et al. First m87 event horizon telescope results. vi. the shadow and mass of the central black hole. The Astrophysical ...
2019
-
[66]
Holographic turbulence
Allan Adams, Paul M Chesler, and Hong Liu. Holographic turbulence. Physical review letters , 112(15):151602, 2014. 9
2014
-
[67]
Code proper- ties from holographic geometries
Fernando Pastawski and John Preskill. Code proper- ties from holographic geometries. Physical Review X , 7(2):021022, 2017. 10
2017
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