Physics of the Dark Universe最新文献

{"title":"Neutron star collapse from accretion: A probe of massive dark matter particles","authors":"Ning Liu,&nbsp;Arvind Kumar Mishra","doi":"10.1016/j.dark.2024.101740","DOIUrl":"10.1016/j.dark.2024.101740","url":null,"abstract":"<div><div>We explore the multi-scatter capturing of the massive dark matter (DM) particle inside the neutron star via a momentum-dependent dark matter-nucleon scattering cross-section. We find that the capturing enhanced for the positive velocity and momentum transfer dependent DM-nucleon scattering in comparison with the constant cross-section case. Further, a large capture of the DM particles can be thermalized and lead to black hole formation and, therefore, destroy the neutron star. Using the observation of the old neutron star in the DM-dominated region, we obtain strong constraints on massive DM parameters.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"47 ","pages":"Article 101740"},"PeriodicalIF":5.0,"publicationDate":"2024-11-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142697704","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Astrophysical implications of Weyl geometric black holes: Shadows and strong gravitational lensing","authors":"Niyaz Uddin Molla ,&nbsp;Himanshu Chaudhary ,&nbsp;Farruh Atamurotov ,&nbsp;G. Mustafa ,&nbsp;Tiberiu Harko ,&nbsp;Ujjal Debnath","doi":"10.1016/j.dark.2024.101735","DOIUrl":"10.1016/j.dark.2024.101735","url":null,"abstract":"<div><div>We consider the astrophysical properties of an exact black hole solution obtained in Weyl geometric gravity theory from the simplest conformally invariant action, constructed from the square of the Weyl scalar and the strength of the Weyl vector only. The action is linearized in the Weyl scalar by introducing an auxiliary scalar field. In static spherical symmetry, this theory admits an exact black hole solution, which generalizes the standard Schwarzschild solution through the presence of two new terms in the metric, having a linear and a quadratic dependence on the radial coordinate. To test the astrophysical validity properties of the solution, we perform a detailed analysis of its lensing properties in the strong field regimes. In particular, we consider the shadow of the Weyl geometric black hole, and we obtain a first set of constraints on the solution parameters by using the observational data from the shadows of the M87* and Sgr A* supermassive black holes. As a second possibility of observationally testing the Weyl geometric black hole and constraining its free parameters, we consider the strong lensing in this geometry. We investigate in detail the basic strong lensing observables, including the angular position of the images, the angular separation, the relative magnification, the radii of the Einstein ring, and the relativistic time delay. For all these quantities, a comparison with the predictions of the standard Schwarzschild black hole solution is performed by using realistic astrophysical data. The obtained results may lead to the possibility of testing Weyl geometry, Weyl geometric gravity, and their effects at galactic and extragalactic levels by using the observational properties of the black hole solutions of the theory.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"47 ","pages":"Article 101735"},"PeriodicalIF":5.0,"publicationDate":"2024-11-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142697702","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Study of cosmological dark energy models under f(Q) gravity","authors":"Vipin Chandra Dubey ,&nbsp;Umesh Kumar Sharma ,&nbsp;Saibal Ray ,&nbsp;Aritra Sanyal","doi":"10.1016/j.dark.2024.101736","DOIUrl":"10.1016/j.dark.2024.101736","url":null,"abstract":"<div><div>In the present study, we focus on the gravitational sector as the primary driver of dark energy evolution, as opposed to the matter source. We explore a modified version of symmetric teleparallel gravity known as <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> gravity, which introduces the non-metricity component <span><math><mi>Q</mi></math></span> to govern gravitational interactions. Our investigation centers on the <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> model, specifically the form <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow><mo>=</mo><mi>α</mi><mi>Q</mi><mo>+</mo><mi>β</mi><msup><mrow><mi>Q</mi></mrow><mrow><mi>n</mi></mrow></msup></mrow></math></span>, incorporating both linear as well as nonlinear representations of the nonmetricity scalar. The parameters <span><math><mi>n</mi></math></span>, <span><math><mi>α</mi></math></span>, and <span><math><mi>β</mi></math></span> are free in this model. In the purpose of examining the behavior of the model, we adopt initial conditions based on <span><math><mi>Λ</mi></math></span>CDM observational Planck 2018 data, specifically <span><math><mrow><msubsup><mrow><mi>Ω</mi></mrow><mrow><mi>D</mi></mrow><mrow><mn>0</mn></mrow></msubsup><mo>=</mo><mn>0</mn><mo>.</mo><mn>73</mn></mrow></math></span> and <span><math><mrow><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>=</mo><mn>67</mn><mo>.</mo><mn>9</mn></mrow></math></span>, for various values of <span><math><mi>n</mi></math></span>. The statefinder pairs (<span><math><mrow><mi>r</mi><mo>,</mo><mspace></mspace><mi>s</mi></mrow></math></span>), (<span><math><mrow><mi>r</mi><mo>,</mo><mspace></mspace><mi>q</mi></mrow></math></span>), (<span><math><mrow><msub><mrow><mi>ω</mi></mrow><mrow><mi>D</mi><mi>E</mi></mrow></msub><mo>,</mo><mspace></mspace><msubsup><mrow><mi>ω</mi></mrow><mrow><mi>D</mi><mi>E</mi></mrow><mrow><msup><mrow></mrow><mrow><mo>′</mo></mrow></msup></mrow></msubsup></mrow></math></span>) pair, <span><math><mrow><mi>O</mi><mi>m</mi><mrow><mo>(</mo><mi>z</mi><mo>)</mo></mrow></mrow></math></span> diagnostic planes and some other tools we have employed. Our findings demonstrate that the model exhibits both Chaplygin gas and quintessence behaviors in the (<span><math><mrow><mi>r</mi><mo>,</mo><mspace></mspace><mi>q</mi></mrow></math></span>) and (<span><math><mrow><mi>r</mi><mo>,</mo><mspace></mspace><mi>s</mi></mrow></math></span>) pair planes across different values of <span><math><mi>n</mi></math></span>. Additionally, we employ <span><math><mrow><mi>O</mi><mi>m</mi><mrow><mo>(</mo><mi>z</mi><mo>)</mo></mrow></mrow></math></span> diagnostic analysis to distinguish our model from other DE models.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"47 ","pages":"Article 101736"},"PeriodicalIF":5.0,"publicationDate":"2024-11-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142697699","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Shadows and quasinormal modes of rotating black holes in Horndeski theory: Parameter constraints using EHT observations of M87* and Sgr A*","authors":"Muhammad Zahid ,&nbsp;Odil Yunusov ,&nbsp;Chao Shen ,&nbsp;Javlon Rayimbaev ,&nbsp;Sokhibjan Muminov","doi":"10.1016/j.dark.2024.101734","DOIUrl":"10.1016/j.dark.2024.101734","url":null,"abstract":"<div><div>One way to test the presence of scalar &amp; vector fields in the spacetime of black holes is to get constraints on the fields and black hole parameters using astrophysical observations such as black hole shadow, quasiperiodic oscillations, etc. In this work, we aimed to investigate spacetime properties around black holes in Horndeski gravity. First, we obtain a rotating black hole solution using the Newman–Janis Algorithm (NJA), and we study the event horizon, statistic limits, and ergoregion of the black hole spacetime. In addition, we calculate the effective gravitational mass of the black hole. We derive equations for null geodesics and show the combined effects of the black hole spin and Horndeski gravity parameter on the shadow shape of the black hole and its radius distortion. We find that black hole spin and Horndeski parameters cause an increase in the values of shadow radius and its deformation. Next, we obtain constraints for the upper and lower values for black hole spin and Horndeski parameters using event horizon telescope (EHT) data from Sgr A* and M87*shadow sizes. Finally, we investigated the shadow radius, equatorial, and polar quasinormal modes using the geometric-optic relationship between the parameters of the quasinormal mode and the conserved values along the geodesics in the spacetime of the rotating Horndeski black hole.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"47 ","pages":"Article 101734"},"PeriodicalIF":5.0,"publicationDate":"2024-11-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142697639","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A supersymmetric suspicion from accelerating black hole shadows","authors":"L. Chakhchi ,&nbsp;H. El Moumni ,&nbsp;K. Masmar","doi":"10.1016/j.dark.2024.101731","DOIUrl":"10.1016/j.dark.2024.101731","url":null,"abstract":"<div><div>In light of the Event Horizon Telescope (EHT) images of the supermassive black holes <span><math><msup><mrow><mtext>Sgr A</mtext></mrow><mrow><mo>⋆</mo></mrow></msup></math></span> and <span><math><msup><mrow><mtext>M87</mtext></mrow><mrow><mo>⋆</mo></mrow></msup></math></span>, we explore a potential supersymmetry suspicion within the observational data. Specifically, we investigate the shadow of a supersymmetric accelerating black hole and compare our findings with observed quantities such as the angular diameter <span><math><mi>D</mi></math></span> and the fractional deviation <span><math><mi>δ</mi></math></span>. Our analysis reveals a significant alignment between the calculated quantities and the EHT collaboration measurements. This alignment suggests that the features of the black hole shadows observed by the EHT exhibit characteristics consistent with the supersymmetry framework.</div><div>Our results provide compelling evidence for supersymmetry from a gravitational perspective, which remains absent from the particle physics viewpoint till now.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"47 ","pages":"Article 101731"},"PeriodicalIF":5.0,"publicationDate":"2024-11-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142697700","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Cosmological inflation in the modified gravity model f(Q,C)","authors":"S. Davood Sadatian ,&nbsp;S. Mohamad Reza Hosseini","doi":"10.1016/j.dark.2024.101737","DOIUrl":"10.1016/j.dark.2024.101737","url":null,"abstract":"<div><div>Slow-roll parameters play a crucial role in characterizing the behavior of the inflation field during inflation. This paper provide an overview of the topic and highlight various aspects of the connection between cosmological inflation and slow-roll parameters. We also discussed the implications of perturbation growth in modified cosmology, numerical simulations of inflationary dynamics, and the study of inflation in the context of non-metric gravity <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>,</mo><mi>C</mi><mo>)</mo></mrow></mrow></math></span>. The choice of <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>,</mo><mi>C</mi><mo>)</mo></mrow></mrow></math></span> as the background gravitational theory is motivated by its ability to incorporate non-metricity, its potential to address conceptual difficulties in quantizing gravity and its relevance to cosmology and late-time acceleration of the universe. Additionally, we mention the importance of accurately estimating cosmological parameters from observational data. Overall, we studied the relationship between cosmological inflation and slow-roll parameters, contributing to our understanding of the dynamics and implications of inflation in the early universe according to the modified gravity model <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>,</mo><mi>C</mi><mo>)</mo></mrow></mrow></math></span>.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"47 ","pages":"Article 101737"},"PeriodicalIF":5.0,"publicationDate":"2024-11-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142697640","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Inflationary dynamics of Mutated Hilltop inflation in Einstein–Gauss–Bonnet Gravity under new slow-roll approximations with generalized reheating","authors":"Yogesh ,&nbsp;Mehnaz Zahoor ,&nbsp;Kashif Ali Wani ,&nbsp;Imtiyaz Ahmad Bhat","doi":"10.1016/j.dark.2024.101732","DOIUrl":"10.1016/j.dark.2024.101732","url":null,"abstract":"<div><div>The advancement in the observational cosmology of the early universe such as Cosmic Microwave Background (CMB) observations, puts severe constraints on the inflationary models. Many inflationary models have been ruled out by CMB, nevertheless the models ruled out in standard cold inflationary scenarios can be resurrected in modified gravity models. In this regard we examine the dynamics of inflation within the framework of Einstein–Gauss–Bonnet (EGB) Gravity using the new slow-roll approximation methods proposed in Pozdeeva et al. (2024). We consider the Mutated Hilltop inflation model (Pal et al., 2010; Pinhero and Pal, 2019) due to its origin from super-gravity, a naturally perfect choice to study the impact of EGB on inflationary observables such as tensor-to-scalar ratio (<span><math><mi>r</mi></math></span>) and scalar spectral index (<span><math><msub><mrow><mi>n</mi></mrow><mrow><mi>s</mi></mrow></msub></math></span>). The period of reheating following the inflationary phase is also examined, and for the <em>Planck’18</em> permitted values of <span><math><msub><mrow><mi>n</mi></mrow><mrow><mi>s</mi></mrow></msub></math></span>, constraints on the reheating temperature (<span><math><msub><mrow><mi>T</mi></mrow><mrow><mi>r</mi><mi>e</mi></mrow></msub></math></span>) are computed for various equations of states during reheating (<span><math><msub><mrow><mi>ω</mi></mrow><mrow><mi>r</mi><mi>e</mi></mrow></msub></math></span>).</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"47 ","pages":"Article 101732"},"PeriodicalIF":5.0,"publicationDate":"2024-11-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142697701","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Barrow Interacting holographic dark energy cosmology with Hubble horizon as IR cutoff: A model can Alleviating the Hubble and S8 Tension","authors":"Muhammad Yarahmadi","doi":"10.1016/j.dark.2024.101733","DOIUrl":"10.1016/j.dark.2024.101733","url":null,"abstract":"<div><div>In this study, we perform a comprehensive analysis of the Hubble constant (<span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span>) and matter clustering (<span><math><msub><mrow><mi>S</mi></mrow><mrow><mn>8</mn></mrow></msub></math></span>) tensions within the framework of non-interacting and interacting Barrow Holographic Dark Energy (BHDE) models. Utilizing a combination of observational datasets, including the Cosmic Microwave Background (CMB), Baryon Acoustic Oscillations (BAO), cosmic chronometers (CC), Pantheon, and lensing data, we assess the degree of tension relative to the Planck 2018 results and recent measurements such as the Riess et al. 2022 (R22) value for <span><math><mrow><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>=</mo><mn>73</mn><mo>.</mo><mn>04</mn><mo>±</mo><mn>1</mn><mo>.</mo><mn>04</mn><mspace></mspace><msup><mrow><mtext>km s</mtext></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup><msup><mrow><mtext>Mpc</mtext></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></math></span> in 68% C.L and KiDS-1000 and DES-Y3 for <span><math><msub><mrow><mi>S</mi></mrow><mrow><mn>8</mn></mrow></msub></math></span>. Our findings show that both BHDE models mitigate the <span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span> and <span><math><msub><mrow><mi>S</mi></mrow><mrow><mn>8</mn></mrow></msub></math></span> tensions compared to the standard <span><math><mi>Λ</mi></math></span> Cold Dark Matter (<span><math><mi>Λ</mi></math></span>CDM) model. The non-interacting BHDE model achieves a moderate reduction in the <span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span> tension, while the interacting BHDE model offers a better fit for both parameters, suggesting it is more effective in addressing the tensions. Additionally, the quantum-gravitational deformation parameter <span><math><mi>Δ</mi></math></span>, constrained using the CMB+All dataset, indicates significant quantum effects in both models. The interacting scenario provides tighter constraints on <span><math><mi>Δ</mi></math></span> and total neutrino mass <span><math><mrow><mo>∑</mo><msub><mrow><mi>m</mi></mrow><mrow><mi>ν</mi></mrow></msub></mrow></math></span>, offering a more precise representation of these effects. This study highlights the potential of BHDE models as viable alternatives to the <span><math><mi>Λ</mi></math></span>CDM framework for resolving cosmological tensions.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"47 ","pages":"Article 101733"},"PeriodicalIF":5.0,"publicationDate":"2024-11-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142698600","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Particle motion and thermal fluctuations of charged AdS black holes surrounded by exotic fluid with modified Chaplygin equation of state","authors":"Faisal Javed ,&nbsp;Arfa Waseem ,&nbsp;G. Mustafa ,&nbsp;Ghulam Fatima ,&nbsp;Shalan Alkarni","doi":"10.1016/j.dark.2024.101723","DOIUrl":"10.1016/j.dark.2024.101723","url":null,"abstract":"<div><div>This study explores the intricate relationships between thermodynamic properties and particle dynamics of charged AdS black holes, emphasizing the impacts of charge <span><math><mi>Q</mi></math></span> and higher-order corrections, particularly the parameter <span><math><mi>β</mi></math></span>, which is a modified Chaplygin gas parameter. Our analysis of entropy reveals that smaller black holes exhibit decreasing entropy variations with increased <span><math><mi>β</mi></math></span>, while larger black holes display a complex behavior characterized by initial entropy increases followed by decreases as the horizon radius expands. The Helmholtz free energy analysis suggests that higher-order corrections significantly modify energy behavior, indicating potential phase transitions influenced by gravitational forces, with increasing <span><math><mi>β</mi></math></span> values counteracting instability linked to larger charges. Internal energy assessments show an evolving stability of black holes, transitioning from negative to positive values as entropy increases, while also highlighting the destabilizing effects of electric charge. The specific heat analysis illustrates a complex thermal stability regime, where a rise in specific heat with increasing <span><math><mi>Q</mi></math></span> correlates with greater stability. However, critical points of instability arise with higher <span><math><mi>B</mi></math></span> values, where <span><math><mi>B</mi></math></span> is the BH model parameter. Moreover, the trajectories of particles around non-rotating charged black holes reveal that lower parameters result in unbounded motion. In contrast, higher parameters tend to restrict particles closer to the event horizon. Collectively, these findings underscore the complex interplay among charge, higher-order corrections, and stability in black hole thermodynamics, shedding light on the fundamental mechanisms governing black hole behavior and paving the way for future explorations using advanced models and simulations.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"47 ","pages":"Article 101723"},"PeriodicalIF":5.0,"publicationDate":"2024-11-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142697705","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"What is the amount of baryonic dark matter in galaxies?","authors":"Václav Vavryčuk","doi":"10.1016/j.dark.2024.101730","DOIUrl":"10.1016/j.dark.2024.101730","url":null,"abstract":"<div><div>In this paper, we re-evaluate the estimates of dust mass in galaxies and demonstrate that current dust models are incomplete and based on a priori assumptions. These models suffer from a circularity problem and account for only a small portion of dust, specifically submicron-sized grains. They overlook larger dust particles and other macroscopic bodies, despite observational evidence supporting their existence. This evidence includes the observed (sub)millimetre excess in dust emission spectra and the power-law size distribution with a differential size index <span><math><mrow><mi>γ</mi><mo>≈</mo><mn>3</mn><mo>.</mo><mn>5</mn><mo>−</mo><mn>4</mn><mo>.</mo><mn>0</mn></mrow></math></span>, which has been measured for large particles and compact bodies across diverse environments. Examples of these large particles include large dust grains and meteoroids detected by satellites, near-Earth objects colliding with Earth, fragments in the Main Asteroid Belt and the Kuiper Belt, interstellar ’Oumuamua-like objects, and exoplanets. As a result, dust-type baryonic dark matter may be more abundant throughout the galaxy by one order of magnitude or even more than previously assumed, with a significant portion of its mass concentrated in large compact bodies. Additionally, black holes may contribute significantly to the total mass of baryonic dark matter. Consequently, current galaxy models do not provide reliable estimates of baryonic mass in galaxies. Clearly, a substantially larger amount of baryonic dark matter in galaxies would have major implications for theories of galaxy dynamics and evolution.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"47 ","pages":"Article 101730"},"PeriodicalIF":5.0,"publicationDate":"2024-11-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142697706","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}