Journal of High Energy Astrophysics最新文献

{"title":"The massive black holes, high accretion rates, and non-tilted jet feedback, of jetted AGN triggered by secular processes","authors":"Chandra B. Singh ,&nbsp;David Garofalo","doi":"10.1016/j.jheap.2023.06.001","DOIUrl":"10.1016/j.jheap.2023.06.001","url":null,"abstract":"<div><p>That jetted active galactic nuclei<span><span><span> (AGN) are also hosted in spiral galaxies is now well established. Our understanding of how such objects might fit in the radio loud AGN subclass has been described by Foschini and others over the past decade in that jets in spirals are weaker than those of </span>radio galaxies and </span>quasars because the black holes in spirals tend to be less massive. Recent data, however, may be pointing to a different picture which we describe. Unlike powerful jetted AGN in ellipticals, we illustrate from model perspectives, features of jets in spirals responsible for limiting both their power as well as their effect on their host galaxies. AGN triggered by secular processes fail to generate jet re-orientation, a key ingredient in the jetted AGN feedback mechanism in merger-triggered ellipticals that leads to the red-and-dead radio galaxies at low redshift such as M87. As a result, jetted AGN in spirals tend to live in a separate part of the parameter space compared to radio galaxies and quasars. Because of the absence of jet re-orientation and due to the relatively short-lived jet phases, jetted AGN in spirals are best compared to radio quiet or jetless AGN than any other jetted AGN subclass.</span></p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":null,"pages":null},"PeriodicalIF":3.8,"publicationDate":"2023-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"49495874","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":"Type Ia supernovae induced by primordial black holes from dark first-order phase transition","authors":"Pin-Jung Chen,&nbsp;Po-Yan Tseng","doi":"10.1016/j.jheap.2023.07.002","DOIUrl":"10.1016/j.jheap.2023.07.002","url":null,"abstract":"<div><p><span>A primordial black hole (PBH) with mass </span><span><math><msup><mrow><mn>10</mn></mrow><mrow><mo>−</mo><mn>15</mn></mrow></msup><mo>≤</mo><msub><mrow><mi>M</mi></mrow><mrow><mi>PBH</mi></mrow></msub><mo>/</mo><msub><mrow><mi>M</mi></mrow><mrow><mo>⊙</mo></mrow></msub><mo>≤</mo><msup><mrow><mn>10</mn></mrow><mrow><mo>−</mo><mn>10</mn></mrow></msup></math></span><span> is currently beyond the sensitivity of both microlensing and black hole (BH) evaporation methods. A novel scenario has been proposed: When a PBH with mass </span><span><math><msup><mrow><mn>10</mn></mrow><mrow><mo>−</mo><mn>14</mn></mrow></msup><mo>≤</mo><msub><mrow><mi>M</mi></mrow><mrow><mi>PBH</mi></mrow></msub><mo>/</mo><msub><mrow><mi>M</mi></mrow><mrow><mo>⊙</mo></mrow></msub><mo>≤</mo><msup><mrow><mn>10</mn></mrow><mrow><mo>−</mo><mn>11</mn></mrow></msup></math></span><span><span> transits through a white dwarf (WD) made up of carbon and oxygen, Bondi-Hoyle-Lyttleton (BHL) accretion in a reactive medium creates a shock wave, which generates direct detonation ignition in the WD core and then leads to thermonuclear </span>supernovae (SNe Ia). The aim of this study is to impose constraints on the PBH to dark matter (DM) abundance fraction, </span><span><math><msub><mrow><mi>f</mi></mrow><mrow><mi>PBH</mi></mrow></msub></math></span>, via comparing the SN Ia event rates between PBH hypotheses and observational data. For PBH fraction less than unity, we found the observed event rate prefers PBH mass region, <span><math><mn>7.6</mn><mo>×</mo><msup><mrow><mn>10</mn></mrow><mrow><mo>−</mo><mn>13</mn></mrow></msup><mo>≤</mo><msub><mrow><mi>M</mi></mrow><mrow><mi>PBH</mi></mrow></msub><mo>/</mo><msub><mrow><mi>M</mi></mrow><mrow><mo>⊙</mo></mrow></msub><mo>≤</mo><mn>6.1</mn><mo>×</mo><msup><mrow><mn>10</mn></mrow><mrow><mo>−</mo><mn>12</mn></mrow></msup></math></span>, under the Navarro–Frenk–White (NFW) profile. Meanwhile, the aforementioned PBH mass and abundance can be efficiently produced via a cosmological first-order phase transition (FOPT) in dark sector which associates with <span><math><mi>O</mi><mspace></mspace><mo>(</mo><mtext>MeV</mtext><mo>)</mo></math></span><span> energy scale and thus gives rise to complementary signals of stochastic gravitational waves (GWs) with peak frequencies from </span><span><math><msup><mrow><mn>10</mn></mrow><mrow><mo>−</mo><mn>6</mn></mrow></msup></math></span> Hz to <span><math><msup><mrow><mn>10</mn></mrow><mrow><mo>−</mo><mn>5</mn></mrow></msup></math></span> Hz which can be probed by future μAres GW interferometer.</p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":null,"pages":null},"PeriodicalIF":3.8,"publicationDate":"2023-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"43738781","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":"Entropy as logarithmic term of the central charge and modified Friedmann equation in AdS/CFT correspondence","authors":"M. Bousder ,&nbsp;E. Salmani ,&nbsp;H. Ez-Zahraouy","doi":"10.1016/j.jheap.2023.04.002","DOIUrl":"10.1016/j.jheap.2023.04.002","url":null,"abstract":"<div><p>This paper is about the extended thermodynamics of AdS black holes and its relation to CFT<span> thermodynamics. The logarithmic term of the central charge is interpreted as black hole entropy. We have to obtain a modified Friedmann equation from the Smarr formula. We find that the AdS radius is the critical shadow radius. We obtain the Hawking-Bekenstein formula with logarithmic corrections, which depends on the central charge. The real gas in AdS is a dual of an ideal gas in CFT. This work can be extended to the AdS-Kerr black holes.</span></p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":null,"pages":null},"PeriodicalIF":3.8,"publicationDate":"2023-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"42240837","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":"Gamma rays from nebulae around recurrent novae","authors":"W. Bednarek,&nbsp;J. Sitarek","doi":"10.1016/j.jheap.2023.03.004","DOIUrl":"10.1016/j.jheap.2023.03.004","url":null,"abstract":"<div><p>Novae were discovered to emit transient <em>γ</em> rays during the period of several days to a few weeks after initial explosion, indicating presence of acceleration processes of particles in their expanding shells. In the case of recurrent novae, electrons can be in principle accelerated in the nova shells for the whole recurrence period of nova producing delayed <em>γ</em> ray emission as considered in <span>Bednarek (2022)</span>. Here we extend the ideas presented in this article by considering the fate of electrons which diffuse out of the shells of novae supplying fresh relativistic electrons to the recurrent nova super-remnants during the whole active period of nova (<span><math><mo>≥</mo><msup><mrow><mn>10</mn></mrow><mrow><mn>4</mn></mrow></msup></math></span> yrs). We develop a model for the acceleration of electrons and their escape from the nova shells. The electrons within the recurrent nova super-remnants produce <em>γ</em> rays in the comptonization process of the radiation from the red giant companion and the Cosmic Microwave Background Radiation. As an example, the case of a symbiotic nova RS Oph (with the recurrence period estimated on ∼10-50 yrs) is considered in more detail. Predicted <em>γ</em>-ray emission from the nova super-remnant around RS Oph is discussed in the context of its observability by satellite experiments (i.e. <em>Fermi</em>-LAT) as well as current and future Cherenkov telescopes.</p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":null,"pages":null},"PeriodicalIF":3.8,"publicationDate":"2023-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"43445248","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":"High-energy neutrino fluxes from hard-TeV BL Lacs","authors":"E. Aguilar-Ruiz,&nbsp;N. Fraija,&nbsp;A. Galván-Gámez","doi":"10.1016/j.jheap.2023.02.001","DOIUrl":"10.1016/j.jheap.2023.02.001","url":null,"abstract":"<div><p>Blazars have been pointed out as promising high-energy (HE) neutrinos sources, although the mechanism is still under debate. The blazars with a hard-TeV spectrum, which leptonic models can hardly explain, can be successfully interpreted in the hadronic scenarios. Recently, Aguilar et al. proposed a lepto-hadronic two-zone model to explain the multi-wavelength observations of the six best-known extreme BL Lacs and showed that the hadronic component could mainly interpret very-high-energy (VHE) emission. In this work, we apply this hadronic model to describe the VHE gamma-ray fluxes of 14 extreme BL Lacs and estimate the respective HE neutrino flux from charge-pion decay products. Finally, we compare our result with the diffuse flux observed by the IceCube telescope, showing that the neutrino fluxes from these objects are negligible.</p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":null,"pages":null},"PeriodicalIF":3.8,"publicationDate":"2023-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"47567237","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":"Short Gamma rays bursts from binary black holes merger","authors":"Shad Ali","doi":"10.1016/j.jheap.2023.05.001","DOIUrl":"https://doi.org/10.1016/j.jheap.2023.05.001","url":null,"abstract":"<div><p><span><span><span>In this paper, we introduced a model related to the astronomical events having the co-detection of GW associated with Short Gamma Ray Bursts (SGRBs). Study shows that the existence of magnetized </span>accretion disks<span> is responsible for creating the events of GWs associated with electromagnetic (EM) counterparts from binary BHs mergers. Our model leads from space-time instability to the emission of </span></span>EM radiations<span> as its counterparts. Starting from Maxwell's stress tensor, we found the condition for the growth of instability that is proportional to the </span></span>angular velocity<span><span> and is independent of the magnetic field strength. Considering the event GW150914 with the final product as a Kerr BHs in an equatorial plan, we discussed the motion of particles under an effective potential on circular orbits around it and determined its frequency, redshift factor, and epicyclic frequency. Next, considering the evolution of mass and </span>angular momentum, we calculated the remnant mass, rotational energy, and the magnetic field strength acting along the axis of rotation. The accretion rate and its luminosity are determined by the restoring and shear forces of the magnetic field. The energy extraction efficiency of the flow is determined to be very low. Results show the presence of a weak transient caused by magneto-rotational instability with a strong poloidal magnetic field that causes turbulence in the accretion disk onto black holes.</span></p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":null,"pages":null},"PeriodicalIF":3.8,"publicationDate":"2023-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"50186815","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":"Observationally constrained accelerating cosmological model with higher power of non-metricity and squared trace","authors":"A.S. Agrawal ,&nbsp;B. Mishra ,&nbsp;S.K. Tripathy","doi":"10.1016/j.jheap.2023.04.001","DOIUrl":"10.1016/j.jheap.2023.04.001","url":null,"abstract":"<div><p><span>In this paper, a cosmological model of the Universe is presented in </span><span><math><mi>f</mi><mo>(</mo><mi>Q</mi><mo>,</mo><mi>T</mi><mo>)</mo></math></span> gravity and the parameters are constrained by cosmological data sets. Initially, a generalised form of <span><math><mi>f</mi><mo>(</mo><mi>Q</mi><mo>,</mo><mi>T</mi><mo>)</mo></math></span> model is used as <span><math><mi>f</mi><mo>(</mo><mi>Q</mi><mo>,</mo><mi>T</mi><mo>)</mo><mo>=</mo><mo>−</mo><msub><mrow><mi>λ</mi></mrow><mrow><mn>1</mn></mrow></msub><msup><mrow><mi>Q</mi></mrow><mrow><mi>m</mi></mrow></msup><mo>−</mo><msub><mrow><mi>λ</mi></mrow><mrow><mn>2</mn></mrow></msub><msup><mrow><mi>T</mi></mrow><mrow><mn>2</mn></mrow></msup></math></span>, where <span><math><msub><mrow><mi>λ</mi></mrow><mrow><mn>1</mn></mrow></msub></math></span>, <span><math><msub><mrow><mi>λ</mi></mrow><mrow><mn>2</mn></mrow></msub></math></span> and <em>m</em> are model parameters. With some algebraic manipulation, the Hubble parameter is obtained in terms of redshift. Then, using MCMC analysis, the model parameters are constrained using the most current Hubble and Pantheon⁺<span> data. The model parameters are also verified through the BAO data set. The model shows an early deceleration transitioning to an accelerating phase of the Universe. The </span><span><math><mi>O</mi><mi>m</mi><mo>(</mo><mi>z</mi><mo>)</mo></math></span> diagnostic indicates a positive slope, favouring the model to be in a phantom field dominated phase.</p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":null,"pages":null},"PeriodicalIF":3.8,"publicationDate":"2023-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"47243083","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":"Measurements of spin and orbital parameters in Cen X-3 by Insight-HXMT","authors":"Qi Liu ,&nbsp;Wei Wang","doi":"10.1016/j.jheap.2023.03.002","DOIUrl":"10.1016/j.jheap.2023.03.002","url":null,"abstract":"<div><p><span>We present a detailed temporal analysis for the eclipsing high-mass X-ray binary system Cen X-3 using the Insight-HXMT data in 2018 and 2020. Three consecutive and high statistic observations among data are used for the precise timing analysis. The pulse profiles are revealed to vary with energy and time. The pulse profiles for the 2018 observations showed a double peak in the low energy bands<span> below 10 keV and evolved to a single peak in higher energies without the correlation between pulse fraction and flux, and profiles in low energies changed with time. But the pulse profile for the 2020 observation only showed a broad single-peaked pulse in all energy bands with a positive relation between pulse fraction and flux, which may indicate the transition of the emission patterns from a mixture of a pencil and a fan beam to a dominated pencil-like beam. With performing a binary orbital fitting of spin periods, we obtain an accurate value for the spin period and the orbital parameters. The intrinsic spin period of the neutron star is found to be </span></span><span><math><mn>4.79920</mn><mo>±</mo><mn>0.00006</mn></math></span> s at MJD 58852.697, with the orbital period determined at <span><math><msub><mrow><mi>P</mi></mrow><mrow><mtext>orb</mtext></mrow></msub><mo>=</mo><mn>2.08695634</mn><mo>±</mo><mn>0.00000001</mn></math></span> day, and its decay rate of -(1.7832 ± 0.0001) × 10⁻⁶ yr⁻¹ for the binary.</p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":null,"pages":null},"PeriodicalIF":3.8,"publicationDate":"2023-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"43195798","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":"The reconstruction of constant jerk parameter with f(R,T) gravity","authors":"Anirudh Pradhan ,&nbsp;Gopikant Goswami ,&nbsp;Aroonkumar Beesham","doi":"10.1016/j.jheap.2023.03.001","DOIUrl":"10.1016/j.jheap.2023.03.001","url":null,"abstract":"<div><p>In this work, we have developed an FLRW type model of a universe which displays transition from deceleration in the past to the acceleration at the present. For this, we have considered field equations of f(R,T) gravity and have taken <span><math><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><mi>T</mi><mo>)</mo><mo>=</mo><mi>R</mi><mo>+</mo><mn>2</mn><mi>λ</mi><mi>T</mi></math></span>, <em>λ</em> being an arbitrary constant. We have estimated the <em>λ</em> parameter in such a way that the transition red shift is found similar in the deceleration parameter, pressure and the equation of state parameter <em>ω</em>. The present value of Hubble parameter is estimated on the basis of the three types of observational data set: latest compilation of 46 Hubble data set, SNe Ia 580 data sets of distance modulus and 66 Pantheon data set of apparent magnitude which comprised of 40 SN Ia bined and 26 high redshift data's in the range <span><math><mn>0.014</mn><mo>≤</mo><mi>z</mi><mo>≤</mo><mn>2.26</mn></math></span>. These data are compared with theoretical results through the <span><math><msup><mrow><mi>χ</mi></mrow><mrow><mn>2</mn></mrow></msup></math></span> statistical test. Interestingly, the model satisfies all the three weak, strong and dominant energy conditions. The model fits well with observational findings. We have discussed some of the physical aspects of the model, in particular the age of the universe.</p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":null,"pages":null},"PeriodicalIF":3.8,"publicationDate":"2023-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"46919759","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":"Short Gamma Rays Bursts form binary black holes merger","authors":"Shad Ali","doi":"10.1016/j.jheap.2023.05.001","DOIUrl":"https://doi.org/10.1016/j.jheap.2023.05.001","url":null,"abstract":"","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":null,"pages":null},"PeriodicalIF":3.8,"publicationDate":"2023-05-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"43647956","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}