New Astronomy最新文献

{"title":"Effects of expansion-free condition on adiabatic collapse in f(G,T) gravity","authors":"Riaz Ahmed","doi":"10.1016/j.newast.2024.102256","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102256","url":null,"abstract":"<div><p>This study explores the impact of <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>G,T</mi><mo>)</mo></mrow></mrow></math></span> gravity, where <span><math><mi>G</mi></math></span> is the Gauss Bonnet invariant and <span><math><mi>T</mi></math></span> is the trace of the energy–momentum tensor, on the adiabatic anisotropic spherical gravitating source under the expansion-free condition. We coupled the relativistic matter with spherical symmetric structure by applying <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>G,T</mi><mo>)</mo></mrow><mo>=</mo><mi>α</mi><msup><mrow><mi>G</mi></mrow><mrow><mi>n</mi></mrow></msup><mo>+</mo><mi>λ</mi><mi>T</mi></mrow></math></span> Gauss–Bonnet model with a linear trace. To derive the collapse equation, we used the perturbation method on the field equations and the contracted Bianchi identities. The dynamics of instability range is depicted in Newtonian (<span><math><mi>N</mi></math></span>) and post-Newtonian (pN) regimes. Furthermore, instead of using the adiabatic index, we establish the instability range by looking at the density profile and anisotropic pressure configuration. We investigate the analytic solutions that meets the expansion-free condition. Finally, we have successfully achieved the original results obtained by Herrera et al. (2012) in General Relativity by setting <span><math><mrow><mi>α</mi><mo>=</mo><mi>λ</mi><mo>=</mo><mn>0</mn></mrow></math></span> in proposed cosmological model.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"112 ","pages":"Article 102256"},"PeriodicalIF":2.0,"publicationDate":"2024-05-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141291523","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Out-of-plane dynamics: a study within the circular restricted eight-body framework","authors":"M．Javed Idrisi ,&nbsp;M．Shahbaz Ullah ,&nbsp;Worku Tenna ,&nbsp;M．Tauheed Khan ,&nbsp;M．Faisal Khan ,&nbsp;Mustafa Kamal","doi":"10.1016/j.newast.2024.102260","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102260","url":null,"abstract":"<div><p>This manuscript thoroughly explores the dynamics of a test particle around out-of-plane equilibrium points within the circular restricted eight-body problem. This particular scenario features a central primary emitting radiation, and it is a specific case derived from Kalvouridis and Hadjifotinou's analysis of Maxwell's ring problem in 2011. Our investigation uncovers two symmetrical out-of-plane equilibrium points denoted as <em>E</em>_1,2(0, 0, <em>z</em>₀), where <em>z</em>₀ is determined by the equation <em>z</em>₀ = ±<em>a</em> tanυ; υ = arcsin[(‒<em>q</em>/6)^1/3], with <em>q</em> falling within the range (‒6, 0). Here, <em>a</em> denotes the radius of the circular orbit of peripheral primaries around the radiating central primary, and <em>q</em> signifies the radiation factor due to the central primary. Significantly, for a critical radiation factor value, <em>q_c</em> = ‒3/√2, the equilibrium points <em>E</em>_1,2 precisely align along the <em>z</em>-axis on the sphere of radius <em>a</em> and centered at the central primary. Within the intervals of ‒6 &lt; <em>q</em> &lt; <em>q_c</em> and <em>q_c</em> &lt; <em>q</em> &lt; 0, equilibrium points <em>E</em>₁ and <em>E</em>₂ are situated outside and inside the mentioned sphere on the <em>z</em>-axis, respectively. Specifically, for <em>q</em> ≤ <em>q_c</em>, | <em>z</em>₀ | ≤ <em>a</em>, while for <em>q</em> &gt; <em>q_c</em>, | <em>z</em>₀ | &gt; <em>a</em>. The study further explores the linear stability of <em>E</em>_1,2. By analyzing characteristic curves derived from the variational equations of motion for infinitesimal mass around these equilibrium points, particularly for <em>q</em> values of ‒3/4, ‒3/√2, and ‒9√3/4, we observe that these out-of-plane equilibria, <em>E</em>_1,2, demonstrate linear instability. This insight provides a comprehensive understanding of the intricate dynamics in this specific multi-body problem. Finally, the research illustrates periodic orbits surrounding the out-of-plane equilibrium point for specific values of <em>q</em>.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"111 ","pages":"Article 102260"},"PeriodicalIF":2.0,"publicationDate":"2024-05-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141240141","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Fate of charged wormhole structures utilizing Karmarkar approach","authors":"Iffat Fayyaz ,&nbsp;Tayyaba Naz ,&nbsp;Adnan Malik","doi":"10.1016/j.newast.2024.102255","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102255","url":null,"abstract":"<div><p>The purpose of this study is to elaborate on the Morris–Thorne wormhole notion by creating a detailed model of a charged wormhole shape function. The classical embedding theory, which has played a significant role in the general theory of relativity, accomplishes this objective. Here, we assume redshift function along with charge i.e. <span><math><mrow><mi>ψ</mi><mrow><mo>(</mo><mi>r</mi><mo>,</mo><msup><mrow><mi>Q</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>)</mo></mrow><mo>=</mo><mi>L</mi><mi>o</mi><mi>g</mi><mrow><mo>[</mo><mn>1</mn><mo>+</mo><mfrac><mrow><msup><mrow><mi>Q</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow><mrow><msup><mrow><mi>r</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></mfrac><mo>]</mo></mrow></mrow></math></span> and <span><math><mrow><mi>Q</mi><mrow><mo>(</mo><mi>r</mi><mo>)</mo></mrow><mo>=</mo><mi>ξ</mi><msqrt><mrow><mi>r</mi></mrow></msqrt></mrow></math></span>. For this particular choice, the surface redshift function remains positive and finite everywhere even for the larger range of radial coordinate <span><math><mi>r</mi></math></span>. In wormhole geometry, the violation of Null energy condition have a crucial role which leads to the exotic matter. We examined our solutions through energy bounds (Null, Weak and Strong energy bounds) to check their stable state and its viability. Interestingly, in present work we analyze that the presence of electric charge amplify the results and provides the traversable charged wormhole solutions without exotic matter near the throat in the context of general theory of relativity.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"112 ","pages":"Article 102255"},"PeriodicalIF":2.0,"publicationDate":"2024-05-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141239252","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Spectra and equitemporal surfaces of the photosphere of the ultrarelativistic shell as applied to Gamma-ray bursts","authors":"Aksana Kurhuzava","doi":"10.1016/j.newast.2024.102257","DOIUrl":"10.1016/j.newast.2024.102257","url":null,"abstract":"<div><p>We study the radiation of the ultrarelativistic shell in the diffusion approximation, which takes place at the initial stage of a gamma-ray burst. We get the effective temperature, instantaneous and time-integrated spectra for the parabolic distribution of the initial internal energy of the shell. Also we considered the types of the equitemporal surfaces with a different type of the movement of the shell.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"111 ","pages":"Article 102257"},"PeriodicalIF":2.0,"publicationDate":"2024-05-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141138236","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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 comprehensive photometric analysis of the shallow contact binary IR Vir","authors":"M.F. Yıldırım","doi":"10.1016/j.newast.2024.102252","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102252","url":null,"abstract":"<div><p>The light curves (LC(s)) of the shallow contact binary (SCB(s)) IR Vir were retrieved from the TESS, Kepler (K2), ASAS, ASAS-SN, and KWS databases and comprehensively analyzed in this paper. For IR Vir, a q search was conducted to determine the mass ratio, which was found to be <span><math><mrow><mn>0</mn><mo>.</mo><mn>371</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>008</mn></mrow></math></span>. The analysis indicates that IR Vir was a typical A-type W UMa. Since the determination of absolute parameters is crucial for analyzing the evolution of such systems, the masses of the bodies of IR Vir were estimated as <span><math><mrow><msub><mrow><mi>M</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>=</mo><mn>1</mn><mo>.</mo><mn>03</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>10</mn></mrow></math></span> M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, <span><math><mrow><msub><mrow><mi>M</mi></mrow><mrow><mn>2</mn></mrow></msub><mo>=</mo><mn>0</mn><mo>.</mo><mn>38</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>05</mn></mrow></math></span> M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, and the radii as <span><math><mrow><msub><mrow><mi>R</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>=</mo><mn>1</mn><mo>.</mo><mn>16</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>06</mn></mrow></math></span> R<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, <span><math><mrow><msub><mrow><mi>R</mi></mrow><mrow><mn>2</mn></mrow></msub><mo>=</mo><mn>0</mn><mo>.</mo><mn>73</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>04</mn></mrow></math></span> R<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>. In the analysis of the orbital period (OP(s)) for IR Vir, it was found that the OP of IR Vir was increasing, and this value was calculated to be 0.0376 s per year. The OP increase can be explained by the conserved mass exchange between the bodies, and it can be proposed to be from the low mass body to the more one. This value was calculated as <span><math><mrow><mn>2</mn><mo>.</mo><mn>4</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>7</mn></mrow></msup></mrow></math></span> <span><math><msub><mrow><mi>M</mi></mrow><mrow><mo>⊙</mo></mrow></msub></math></span> per year. Furthermore, a sinusoidal change in the OP was also identified, and it was proposed that this could be attributed to the presence of a third body or magnetic activity. Finally, to gain a better understanding of the nature of IR Vir, it was positioned in the logM<span><math><msub><mrow></mrow><mrow><mi>t</mi><mi>o</mi><mi>t</mi></mrow></msub></math></span> <span><math><mo>−</mo></math></span> logJ and HR (Hertzsprung-Russell) diagrams.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"111 ","pages":"Article 102252"},"PeriodicalIF":2.0,"publicationDate":"2024-05-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141090384","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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 photometric study of a total-eclipse contact binary V458 Mon","authors":"Ahmed Waqas Zubairi ,&nbsp;Zhao Ergang ,&nbsp;Jiajia He ,&nbsp;Fuxing Li ,&nbsp;Liying Zhu ,&nbsp;Azizbek Matekov","doi":"10.1016/j.newast.2024.102250","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102250","url":null,"abstract":"<div><p>We present light curve solution of V458 Mon firstly by using the Wilson-Devinney code. The total eclipse and deep minima of the light curves of V458 Mon<!--> <!-->enable us to determine reliable orbital parameters of the binary system. The solution suggests that V458 Mon<!--> <!-->is a low mass ratio binary system with about 0.2 possessing a moderate degree of contact. The long-term period investigation showed that the period of V458 Mon<!--> <!-->is increasing at <span><math><mrow><mi>d</mi><mi>P</mi><mo>/</mo><mi>d</mi><mi>t</mi><mo>=</mo><mo>+</mo><mn>2</mn><mo>.</mo><mn>59</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>7</mn></mrow></msup><mi>d</mi><mi>a</mi><mi>y</mi><mi>s</mi><mo>/</mo><mi>y</mi><mi>r</mi></mrow></math></span>, which could be the reason of mass transfer from the less massive component to more massive primary one, together with a periodic change. The oscillation in orbital period may be due to an unseen tertiary companion with the mass about <span><math><mrow><msub><mrow><mi>M</mi></mrow><mrow><mn>3</mn></mrow></msub><mo>=</mo><mn>1</mn><mo>.</mo><mn>8</mn><msub><mrow><mi>M</mi></mrow><mrow><mo>⊙</mo></mrow></msub></mrow></math></span> . After removing these change, there is still a weak cyclic change maybe due to magnetic activity. With the increase in orbital period of binary, the separation increases and mass ratio decreases which eventually leads V458 Mon<!--> <!-->towards merger.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"111 ","pages":"Article 102250"},"PeriodicalIF":2.0,"publicationDate":"2024-05-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141097814","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Radiation pressure and galactic cosmic rays-driven gravitational instability in rotating and magnetized viscoelastic fluids","authors":"Joginder Singh Dhiman,&nbsp;Mehak Mahajan","doi":"10.1016/j.newast.2024.102251","DOIUrl":"10.1016/j.newast.2024.102251","url":null,"abstract":"<div><p>This paper studies the combined effects of radiation and galactic cosmic ray pressures on the gravitational instability of magnetized and rotating viscoelastic fluids. The dispersion relations are derived using the normal mode analysis and discussed in the hydrodynamic (weakly coupled fluid) and kinetic (strongly coupled fluid) limits. These dispersion relations are analyzed separately for transverse and longitudinal wave propagation modes. Jeans instability criteria are obtained for kinetic and hydrodynamic limits for both modes of wave propagation, and it is found that the critical Jeans wavenumbers in each case are modified due to the presence of viscoelastic effects, radiation and cosmic rays pressures, and Alfvên wave velocity. It is also observed that the radiation pressure, cosmic ray pressure and viscoelastic parameters suppress the growth rate and thus have stabilizing effects on the Jeans instability. However, cosmic ray diffusion has a destabilizing effect on the onset of gravitational instability. The effects of various parameters on the growth rate of instability are calculated numerically and the outcomes are depicted graphically. The results of the present analysis shall be helpful in understanding the impact of cosmic rays and radiative mechanisms on the gravitational collapse in the viscoelastic region of molecular cloud clumps.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"111 ","pages":"Article 102251"},"PeriodicalIF":2.0,"publicationDate":"2024-05-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141026716","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Nonlinearly charged black holes: Shadow and thin-accretion disk","authors":"Akhil Uniyal ,&nbsp;Sayan Chakrabarti ,&nbsp;Reggie C. Pantig ,&nbsp;Ali Övgün","doi":"10.1016/j.newast.2024.102249","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102249","url":null,"abstract":"<div><p>In this paper, we explore the effect of the parameters of non-linear electrodynamics (NLED) and magnetic charges on various aspects of black holes (BH) arising in the particular NLED theory. More precisely, we look into the behavior of photons around the BH and produce shadow by considering a thin accretion disk model. We initially examine the overall behavior of the photon sphere and the corresponding shadow silhouette under the effects of these parameters. Using the EHT data for Sgr. A* and M87*, we provide constraints on the magnetic charge <span><math><msub><mrow><mi>q</mi></mrow><mrow><mi>m</mi></mrow></msub></math></span>. Our results indicate that M87* gives better constraints, and as the value of the NLED coupling parameter <span><math><mi>β</mi></math></span> is increased, the constrained range for <span><math><msub><mrow><mi>q</mi></mrow><mrow><mi>m</mi></mrow></msub></math></span> widens. At lower values of <span><math><msub><mrow><mi>q</mi></mrow><mrow><mi>m</mi></mrow></msub></math></span>, we find that the shadow radius is close to the observed value. Then, we study different other aspects, such as the energy emitted by the accretion disk, the temperature of the disk around the BH, and the nature of light it gives off. We also look at how the black hole shadow appears in different situations. Finally, we investigate how the magnetic charge affects all the above mentioned aspects when we take into account NLED along with gravity. This study helps us understand the complex relationship between magnetic charge and its effect on various aspects related to a BH.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"111 ","pages":"Article 102249"},"PeriodicalIF":2.0,"publicationDate":"2024-05-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140909802","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Does dynamical wormhole evolve from emergent scenario?","authors":"Dhritimalya Roy ,&nbsp;Ayanendu Dutta ,&nbsp;Bikram Ghosh ,&nbsp;Subenoy Chakraborty","doi":"10.1016/j.newast.2024.102248","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102248","url":null,"abstract":"<div><p>In the present work we analyze a dynamical wormhole solution with two fluids system (one isotropic and homogeneous and the other being inhomogeneous and anisotropic in nature) as the matter at the throat. We choose two different forms of Equation of State(EoS) and investigate two solutions of the wormhole geometry. The properties to ensure existence and traversability has been analyzed. Also, the model of the dynamic wormhole has been examined for a possibility of the Emergent Universe(EU) model in cosmological context. Finally, for the dynamical wormholes so obtained, Null Energy Condition(NEC) has been examined near the throat.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"111 ","pages":"Article 102248"},"PeriodicalIF":2.0,"publicationDate":"2024-05-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140894097","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Three-dimensional stellar orbits due to off-centered dark matter halo at the center of the disc galaxies","authors":"Meenu Prajapati,&nbsp;Mamta Gulati","doi":"10.1016/j.newast.2024.102246","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102246","url":null,"abstract":"<div><p>Stellar orbits and the evolution of galaxies are intertwined processes that have long-term implications on each other. This paper studies how stellar orbits at the galaxy’s central region are disturbed by an asymmetric dark matter halo potential. Evidence from the observations and simulations in the Milky Way type galaxy suggests that the center of the dark matter halo could be off-centered by a few parsecs concerning the center of the core. The equations of motion of stars in the core of galaxies are expressed in terms of three-dimensional perturbed potential arising from the offset halo. The central region’s azimuthal variation in the effective potential is obtained and the first-order epicyclic theory is used to solve for the orbits. The magnitude of this perturbation potential grows at small radii and exhibits <span><math><mrow><mi>m</mi><mo>=</mo><mn>1</mn></mrow></math></span> azimuthal fluctuations. In the central region, within 3 kpc radius, even a small halo offset of 300 pc can cause a surprisingly strong spatial and kinematical lopsidedness. A planar orbit, initially assumed to be in disc plane, tends to leave the plane giving rise to non-planar configuration. Furthermore, as long as the halo offset persists, the central region will stay lopsided. The dark matter halo would significantly impact the dynamic development of this region and could help fuel the active galactic nucleus.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"111 ","pages":"Article 102246"},"PeriodicalIF":2.0,"publicationDate":"2024-05-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140894096","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}