Razieh Ranjbar, Héctor R. Olivares-Sánchez and Shahram Abbassi
{"title":"Bondi-like Accretion Flow Dynamics: The Role of Gravitational Potential","authors":"Razieh Ranjbar, Héctor R. Olivares-Sánchez and Shahram Abbassi","doi":"10.3847/1538-4357/ae032c","DOIUrl":"https://doi.org/10.3847/1538-4357/ae032c","url":null,"abstract":"The formation of massive black holes and their coevolution with host galaxies are pivotal areas of modern astrophysics. Spherical accretion onto a central point mass serves as a foundational framework in cosmological simulations, semi-analytical models, and observational studies. In this paper, we extend the classical spherical accretion model by incorporating the gravitational potential of host galaxies, including contributions from stellar components and dark matter (DM) halos. Numerical solutions spanning scales from parsecs down to ∼10 rs reveal that the flow structure is highly sensitive to the mass and size of the DM halo. Adding a small amount of angular momentum to the accreting gas demonstrates that such flows resemble spherical Bondi accretion, with mass accretion rates converging toward the Bondi rate. We find that the low angular momentum flow resembles the spherical Bondi flow, and its mass accretion rate approaches the Bondi accretion rate. Remarkably, due to the presence of DM, the mass accretion rate increases by more than ∼100% compared to analogous hydrodynamic solutions without DM. These findings underscore the critical role of stellar and DM gravitational potentials in shaping the dynamics and accretion rates of quasi-spherical flows, providing new insights into astrophysical accretion processes.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"32 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145255711","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"The Frequency-independent Radio Luminosity–Orbital/Rotational Period Relation of RS CVn Stars","authors":"Qichen Huang, 启宸 黄, Biwei Jiang and 碧 沩 姜","doi":"10.3847/1538-4357/ae003c","DOIUrl":"https://doi.org/10.3847/1538-4357/ae003c","url":null,"abstract":"Radio emissions from RS CVn objects exhibit distinct characteristics at low and high frequencies, widely attributed to differing radiation mechanisms. The disparate processes of high-frequency gyrosynchrotron and low-frequency electron cyclotron maser emissions have traditionally suggested an absence of correlation in their radio luminosities. Our study presents a frequency-independent linear correlation between radio luminosity (LR) and orbital/rotational periods (P) in RS CVn binaries. Analyzing the Sydney Radio Star Catalogue data, we derived orbital periods for 42 of 60 RS CVn sources using Transiting Exoplanet Survey Satellite light curves, revealing a strong positive correlation (Pearson correlation coefficient (PCC) = 0.698 and P = 3.95e-7) between and . This correlation remains across frequencies from 144 to 3000 MHz, showing uniform luminosity behavior. By combining light curve analysis with stellar mass–radius–luminosity relationships, we calculated parameters like binary mass, primary/secondary mass, Rossby number, and binary separation for eight RS CVn systems. The results show a notable correlation between radio luminosity and binary mass, primary mass, and separation (PCC = 0.663, 0.663, and 0.719), with separation showing the strongest correlation. This suggests the radio emission may largely originate from the binary components’ interaction, challenging existing models of RS CVn radio emission mechanisms and offering insights into the individual versus collective origins of these emissions.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"87 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145255713","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Surajit Mondal, Bin Chen, Xingyao Chen, Sijie Yu, Dale Gary, Peijin Zhang, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D’Addario, Ivey Davis, Jayce Dowell, Katherine Elder, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O’Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody and Thomas Zentmeyer
{"title":"Possible First Detection of Gyroresonance Emission from a Coronal Mass Ejection in the Middle Corona","authors":"Surajit Mondal, Bin Chen, Xingyao Chen, Sijie Yu, Dale Gary, Peijin Zhang, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D’Addario, Ivey Davis, Jayce Dowell, Katherine Elder, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O’Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody and Thomas Zentmeyer","doi":"10.3847/1538-4357/ae061f","DOIUrl":"https://doi.org/10.3847/1538-4357/ae061f","url":null,"abstract":"Routine measurements of the magnetic field of coronal mass ejections (CMEs) have been a key challenge in solar physics. Making such measurements is important both from a space weather perspective and for understanding the detailed evolution of the CME. In spite of significant efforts and multiple proposed methods, achieving this goal has not been possible to date. Here we report the first possible detection of gyroresonance emission from a CME. Assuming that the emission is happening at the third harmonic, we estimate that the magnetic field strength ranges from 7.9 to 5.6 G between 4.9 and 7.5 R⊙. We also demonstrate that this high magnetic field is not the average magnetic field inside the CME, but most probably is related to small magnetic islands, which are also being observed more frequently with the availability of high-resolution and high-quality white-light images.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"39 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145255602","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Lopsided and Bulging Distribution of Satellites Around Paired Halos. I. Observational Measurements and Comparison with Halo-based Models","authors":"Yanhan Guo, Qinglin Ma and Cheng Li","doi":"10.3847/1538-4357/ae00c3","DOIUrl":"https://doi.org/10.3847/1538-4357/ae00c3","url":null,"abstract":"We investigate the angular distribution of satellite galaxies in and around pairs of galaxy groups in the Sloan Digital Sky Survey (SDSS) and compare the results with the satellite distribution in pairs of dark matter halos by constructing mock catalogs that account for the same selection effects as the observational sample. We find that the angular distribution of satellites in both SDSS and the mock catalog exhibits a pronounced tendency toward lopsidedness, with satellites preferentially located between the two central galaxies. Additionally, there is a significant bulging distribution characterized by a higher concentration of satellites along the line connecting the two centrals compared to those found perpendicular to it. The lopsided and bulging distributions strengthen as pair separation and halo mass increase. The mock catalog successfully reproduces the observational results across all cases considered. We find that the lopsided and bulging distribution of satellites can largely be explained by overlapping two randomly selected halos matched in mass to the actual halo pairs, along with their surrounding satellite distribution, provided that the alignment between the orientations of the halos and the line connecting the halo pairs is taken into account. This suggests that the angular distribution of satellites is a natural consequence of the formation and evolution of large-scale structure in a Λ cold dark matter universe, eliminating the need to introduce other physical origins.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"19 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145255707","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
R. Alfaro, C. Alvarez, A. Andrés, E. Anita-Rangel, M. Araya, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, P. Bangale, E. Belmont-Moreno, A. Bernal, T. Capistrán, A. Carramiñana, F. Carreón, S. Casanova, U. Cotti, E. De la Fuente, D. Depaoli, P. Desiati, N. Di Lalla, R. Diaz Hernandez, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, N. Fraija, S. Fraija, J. A. García-González, F. Garfias, N. Ghosh, A. Gonzalez Muñoz, M. M. González, J. A. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, D. Huang, P. Hüntemeyer, A. Iriarte, S. Kaufmann, D. Kieda, K. Leavitt, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, P. E. Mirón-Enriquez, J. A. Montes, J. A. Morales-Soto, E. Moreno, M. Najafi, A. Nayerhoda, L. Nellen, N. Omodei, M. Osorio, E. Ponce, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rh..
{"title":"HAWC Performance Enhanced by Machine Learning in Gamma-hadron Separation","authors":"R. Alfaro, C. Alvarez, A. Andrés, E. Anita-Rangel, M. Araya, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, P. Bangale, E. Belmont-Moreno, A. Bernal, T. Capistrán, A. Carramiñana, F. Carreón, S. Casanova, U. Cotti, E. De la Fuente, D. Depaoli, P. Desiati, N. Di Lalla, R. Diaz Hernandez, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, N. Fraija, S. Fraija, J. A. García-González, F. Garfias, N. Ghosh, A. Gonzalez Muñoz, M. M. González, J. A. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, D. Huang, P. Hüntemeyer, A. Iriarte, S. Kaufmann, D. Kieda, K. Leavitt, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, P. E. Mirón-Enriquez, J. A. Montes, J. A. Morales-Soto, E. Moreno, M. Najafi, A. Nayerhoda, L. Nellen, N. Omodei, M. Osorio, E. Ponce, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rh..","doi":"10.3847/1538-4357/ae0186","DOIUrl":"https://doi.org/10.3847/1538-4357/ae0186","url":null,"abstract":"Improving gamma-hadron separation is one of the most effective ways to enhance the performance of ground-based gamma-ray observatories. With more than a decade of continuous operation, the High-Altitude Water Cherenkov (HAWC) Observatory has contributed significantly to high-energy astrophysics. To further leverage its rich data set, we introduce a machine learning approach for gamma-hadron separation. A multilayer perceptron shows the best performance, surpassing traditional and other machine learning–based methods. This approach shows a notable improvement in the detector’s sensitivity, supported by results from both simulated and real HAWC data. In particular, it achieves a 19% increase in significance for the Crab Nebula, commonly used as a benchmark. These improvements highlight the potential of machine learning to significantly enhance the performance of HAWC and provide a valuable reference for ground-based observatories, such as the Large High Altitude Air Shower Observatory and the upcoming Southern Wide-field Gamma-ray Observatory.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"121 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145255717","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Magnetohydrodynamic Tests of Galactic Synchrotron Depolarization","authors":"Alan Kogut and David C. Collins","doi":"10.3847/1538-4357/ae0a14","DOIUrl":"https://doi.org/10.3847/1538-4357/ae0a14","url":null,"abstract":"Synchrotron emission from cosmic-ray electrons accelerated in the Galactic magnetic field encodes information on the role of turbulence in the magnetized interstellar medium. Although synchrotron radiation is intrinsically highly polarized, the observed fractional polarization f = P/I is below 5% over most of the sky. Despite this marked depolarization, the remaining signal is highly aligned, with median scatter in polarization angle less than 15° within regions of 20° diameter on the sky. We use magnetohydrodynamic (MHD) simulations to determine the extent to which MHD turbulence can reproduce the observed pattern of substantial depolarization with minimal angular scatter. We evaluate both the synchrotron fractional polarization and polarization angle as projected through a suite of simulations with sonic Mach number and magnetic (Alfvén) Mach number . Simulations with a weakly magnetized plasma and strongly supersonic flow ( with ) match the observed high-latitude sky. The fit improves when the angle between the observer and the seed magnetic field is 15°–30° from perpendicular, in agreement with models of the local inclination angle of the large-scale Galactic magnetic field. Additional improvement occurs if the estimated brightness of the unpolarized Galactic synchrotron emission is reduced, either by subtracting an unpolarized extragalactic component from the observed radio maps or by applying a steeper spectra index when scaling the unpolarized synchrotron intensity from 408 MHz to 30 GHz.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"57 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145255719","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
S. J. Nakoneczny, M. J. Graham, D. Stern, G. Helou, S. G. Djorgovski, E. C. Bellm, T. X. Chen, R. Dekany, A. Drake, A. A. Mahabal, T. A. Prince, R. Riddle, B. Rusholme and N. Sravan
{"title":"QZO: A Catalog of 5 Million Quasars from the Zwicky Transient Facility","authors":"S. J. Nakoneczny, M. J. Graham, D. Stern, G. Helou, S. G. Djorgovski, E. C. Bellm, T. X. Chen, R. Dekany, A. Drake, A. A. Mahabal, T. A. Prince, R. Riddle, B. Rusholme and N. Sravan","doi":"10.3847/1538-4357/adf4e4","DOIUrl":"https://doi.org/10.3847/1538-4357/adf4e4","url":null,"abstract":"Machine learning methods are well established in the classification of quasars (QSOs). However, the advent of light-curve observations adds a great amount of complexity to the problem. Our goal is to use the Zwicky Transient Facility (ZTF) to create a catalog of QSOs. We process the ZTF DR20 light curves with a transformer artificial neural network and combine different surveys with extreme gradient boosting. Based on ZTF g-band and Wide-field Infrared Survey Explorer (WISE) observations, we find 4,849,574 objects classified as QSOs with confidence higher than 90% (QZO). We robustly classify objects fainter than the 5σ signal-to-noise ratio (SNR) limit at g = 20.8 by requiring g < nobs/80 + 20.375. For 33% of QZO objects, with available WISE data, we publish redshifts with estimated error Δz/(1 + z) = 0.14. We find that ZTF classification is superior to the Pan-STARRS static bands, and on par with WISE and Gaia measurements, but the light curves provide the most important features for QSO classification in the ZTF data set. Using ZTF g-band data with at least 100 observational epochs per light curve, we obtain a 97% F1 score for QSOs. We find that with 3 day median cadence, a survey time span of at least 900 days is required to achieve a 90% QSO F1 score. However, one can obtain the same score with a survey time span of 1800 days and the median cadence prolonged to 12 days.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"32 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145255701","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Tidal Heating in Detached Double White Dwarf Binaries","authors":"Lucy O. McNeill and Ryosuke Hirai","doi":"10.3847/1538-4357/ae045f","DOIUrl":"https://doi.org/10.3847/1538-4357/ae045f","url":null,"abstract":"Short-period (P < 1 hr orbits) detached double white dwarf binary (DWDB) components identified with transient surveys (e.g., SDSS, Zwicky Transient Facility, hereafter ZTF) have hot surface temperatures (>10,000 K) and observed radii a factor of 2 larger than completely degenerate white dwarfs. We formulate tidal heating in helium composition, extremely low-mass white dwarf components of detached DWDBs, which reach mass transfer within a Hubble time. We combine a mass–radius relation that varies with surface temperature and the equilibrium tidal friction model of Hut 1981, where the additional orbital energy loss from tidal friction is accounted for by increases in the primary surface temperature, and hence increasing radius. Applying this heating model to the current sample of binaries with ZTF, we predict temperature increases from the present day of up to ∼40% before the onset of mass transfer. We find that helium white dwarfs are generically hot and large at the onset of mass transfer, even for the oldest DWDBs whose components can cool to be degenerate by the present day. In the population of Galactic DWDBs, we find that the onset of mass transfer should occur at orbital periods as long as 1000 s (17 minutes), or binary gravitational-wave frequency of 2 mHz. This is over 3 times longer than periods expected for degenerate white dwarfs (5 minutes). Since mass transferring DWDBs are progenitors for a variety of transients and stellar populations, e.g., RCrB stars, AM CVn binaries, so-called Type .Ia supernova, the finite temperature of donor white dwarfs should be taken into account.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"37 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145255712","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Nayyer Raza, Man Leong Chan, Daryl Haggard, Ashish Mahabal, Jess McIver, Audrey Durand, Alexandre Larouche and Hadi Moazen
{"title":"GWSkyNet-Multi. II. An Updated Machine Learning Model for Rapid Classification of Gravitational-wave Events","authors":"Nayyer Raza, Man Leong Chan, Daryl Haggard, Ashish Mahabal, Jess McIver, Audrey Durand, Alexandre Larouche and Hadi Moazen","doi":"10.3847/1538-4357/adfc58","DOIUrl":"https://doi.org/10.3847/1538-4357/adfc58","url":null,"abstract":"Multimessenger observations of gravitational waves and electromagnetic emission from compact object mergers offer unique insights into the structure of neutron stars, the formation of heavy elements, and the expansion rate of the Universe. With the LIGO–Virgo–KAGRA (LVK) gravitational-wave detectors currently in their fourth observing run (O4), it is an exciting time for detecting these mergers. However, assessing whether to follow up a candidate gravitational-wave event given limited telescope time and resources is challenging; the candidate can be a false alert due to detector glitches, or may not have any detectable electromagnetic counterpart even if it is real. GWSkyNet-Multi is a machine learning model developed to facilitate follow-up decisions by providing real-time classification of candidate events, using localization information released in LVK rapid public alerts. Here we introduce GWSkyNet-Multi II, an updated model targeted toward providing more robust and informative predictions during O4 and beyond. Specifically, the model now provides normalized probability scores and associated uncertainties for each of the four corresponding source categories released by the LVK: glitch, binary black hole, neutron star–black hole, and binary neutron star. Informed by explainability studies of the original model, the updated model architecture is also significantly simplified, including replacing input images with intuitive summary values that are more interpretable. For significant event alerts issued during O4a and O4b, GWSkyNet-Multi II produces a prediction that is consistent with the updated LVK classification for 93% of events. The updated model can be used by the community to help make time-critical follow-up decisions.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"40 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145255702","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"On the Eddington Capture Surface around Spherically Symmetric Compact Objects with Separable Luminosity Distributions","authors":"Noah Monk and Adam Rogers","doi":"10.3847/1538-4357/ae00c7","DOIUrl":"https://doi.org/10.3847/1538-4357/ae00c7","url":null,"abstract":"Radiation exerts pressure, and therefore it is possible for an intensely bright object to balance the gravitational force near a massive compact object. General relativity demonstrates that this balance occurs for super-Eddington luminosities at a finite distance from the center of the mass. These equilibrium positions are referred to as Eddington capture surfaces (ECSs). At the ECSs, particles can collect in a thin shell, balanced between the inward curvature of spacetime and the outward flow of radiation. We adopt spherical symmetry but otherwise leave the metric functions generalized. This approach allows us to study the ECSs under the effect of arbitrary spherically symmetric metrics. We adopt a separable luminosity function that depends on both the radial direction and the angular coordinates over the surface of the star. We demonstrate that the morphology of an ECS varies depending on the angular luminosity distribution and can even split into multiple, separate, disconnected equilibrium surfaces. The ECS phenomenon is closely related to type I photospheric radius expansion X-ray bursts.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"122 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145255709","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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