Journal of High Energy Astrophysics最新文献

{"title":"Soft X-ray observing the cosmic sources by the ESA–CAS satellite SMILE","authors":"Vojtěch Šimon ,&nbsp;René Hudec ,&nbsp;Andrew Read","doi":"10.1016/j.jheap.2024.02.005","DOIUrl":"10.1016/j.jheap.2024.02.005","url":null,"abstract":"<div><p>This paper describes the scientific potential of a Soft X-ray Imager (SXI) onboard the ESA–CAS satellite <em>SMILE</em> for investigating cosmic X-ray sources of various types. We show that this instrument, albeit designed for X-ray imaging of solar wind Charge eXchange of the magnetosheath and the cusps, is also essential for astrophysics because it is able to provide wide-field imaging of the sky in the soft X-ray region. Regarding sufficiently luminous X-ray sources with continuous spectra to be observable by the X-ray monitor MAXI/<em>ISS</em> to assess the object types and their light curves that are expected to be detected by SXI/<em>SMILE</em>, the compact sources accreting matter are promising targets for evaluating the possibilities of SXI. We assumed only the cosmic objects located in the planned fields to be observed by SXI. We used the 2–3<!--> <!-->keV band flux of MAXI/<em>ISS</em> covering at least part of the expected band of the SXI/<em>SMILE</em> telescope. We used the data obtained by MAXI/<em>ISS</em> to assess the object types and their light curves expected to be detected by SXI/<em>SMILE</em>. We show the long-term activity of the examples of X-ray binary types located in this region. We present the typical features of such objects' activity on long timescales (e.g., outbursts and state transitions) and include physical interpretations of these phenomena. Furthermore, we discuss how SXI can contribute to this branch.</p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"41 ","pages":"Pages 97-105"},"PeriodicalIF":3.8,"publicationDate":"2024-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139955768","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":"Investigating stable quark stars in Rastall-Rainbow gravity and their compatibility with gravitational wave observations","authors":"Takol Tangphati ,&nbsp;Dhruba Jyoti Gogoi ,&nbsp;Anirudh Pradhan ,&nbsp;Ayan Banerjee","doi":"10.1016/j.jheap.2024.02.006","DOIUrl":"10.1016/j.jheap.2024.02.006","url":null,"abstract":"<div><p>We present a stable model for quark stars in Rastall-Rainbow (R-R) gravity. The structure of this configuration is obtained by utilizing an interacting quark matter equation of state. The R-R gravity theory is developed as a combination of two distinct theories, namely, the Rastall theory and the gravity's rainbow formalism. Depending on the model parameters (<span><math><mover><mrow><mi>λ</mi></mrow><mrow><mo>¯</mo></mrow></mover><mo>,</mo><mi>η</mi><mo>,</mo><mi>Σ</mi><mo>,</mo><msub><mrow><mi>B</mi></mrow><mrow><mi>eff</mi></mrow></msub></math></span>), the mass-radius relations are numerically computed for modified Tolman-Oppenheimer-Volkoff (TOV) equations with proper boundary conditions. The stability of equilibrium configuration has been checked through the static stability criterion, adiabatic index and the sound velocity. Our calculations predict larger maximum masses for quark stars, and the obtained results are compatible with accepted masses and radii values, including constraints from GW190814 and GW170817 events in all the studied cases.</p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"42 ","pages":"Pages 12-20"},"PeriodicalIF":3.8,"publicationDate":"2024-02-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140016831","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":"Generalized wormhole models within galactic halo region in torsion and matter coupling gravity formalism","authors":"G. Mustafa ,&nbsp;Abdelghani Errehymy ,&nbsp;Faisal Javed ,&nbsp;S.K. Maurya ,&nbsp;Sudan Hansraj ,&nbsp;Sobia Sadiq","doi":"10.1016/j.jheap.2024.02.003","DOIUrl":"10.1016/j.jheap.2024.02.003","url":null,"abstract":"<div><p>In the current analysis, we investigate the possible existence of generalized Wormhole models within the galactic halo region by analyzing specific dark matter models. The observational data is checked in the framework of torsion within minimal matter coupling gravity. By using the variational approach modified versions of the field equations under the anisotropic source of matter are calculated. To discuss the specific necessary characteristics of the embedded wormhole geometry, we have analyzed the energy conditions under the effect of dark matter halos. We consider two embedded wormhole-specific shape functions in terms of the tortoise coordinate for the current study. Further, we compare different wormhole solutions for the different regional ranges depending on the involved parametric values. To check the effect of the dark matter halos, we use the observational data within the signature of the <em>M</em>87 galaxy and the Milky Way galaxy.</p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"42 ","pages":"Pages 1-11"},"PeriodicalIF":3.8,"publicationDate":"2024-02-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139955770","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":"Different behaviors of wavelet results for type-B and type-C QPOs of MAXI J1535-571 based on NICER data","authors":"Xiao Chen,&nbsp;Wei Wang","doi":"10.1016/j.jheap.2024.02.002","DOIUrl":"10.1016/j.jheap.2024.02.002","url":null,"abstract":"<div><p>Wavelet analysis, in addition to power density spectra, is another method to study the quasi-periodic signals in the light curves, but has been rarely used in black hole X-ray transients. We performed wavelet analysis of X-ray timing features and quasi-periodic oscillations (QPOs) based on NICER observations of the black hole candidate MAXI J1535-571 in this paper. Separating the light curves by the confidence level of wavelet results, we find significant differences exist in the PDS, hardness ratio and mean count between light curve segments above and below the confidence level. The S-factor, which is defined as the ratio of the effective oscillation time and the total time, demonstrates distinct values between type-C and type-B QPOs. Based on our results, the S-factor for type-B QPO is very close or equal to 0, no matter the confidence level is set as 95% or 68%, while the S-factor of type-C QPO is significantly higher, especially in the 68% confidence level case. We discuss the implications of the wavelet results on resolving type-B and type-C QPOs in black hole X-ray binaries.</p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"41 ","pages":"Pages 89-96"},"PeriodicalIF":3.8,"publicationDate":"2024-02-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139917797","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":"Reduction of ultra-high energy neutrino flux for spacelike neutrinos from extragalactic sources","authors":"J. Rembieliński ,&nbsp;J. Ciborowski","doi":"10.1016/j.jheap.2024.02.001","DOIUrl":"https://doi.org/10.1016/j.jheap.2024.02.001","url":null,"abstract":"<div><p>Assuming that neutrinos are spacelike (tachyonic) fermions, we calculate width for the kinematically allowed, lepton number conserving, three-body decay <span><math><msub><mrow><mi>ν</mi></mrow><mrow><mi>α</mi></mrow></msub><mo>→</mo><msub><mrow><mi>ν</mi></mrow><mrow><mi>α</mi></mrow></msub><mspace></mspace><msub><mrow><mi>ν</mi></mrow><mrow><mi>β</mi></mrow></msub><msub><mrow><mover><mrow><mi>ν</mi></mrow><mrow><mo>¯</mo></mrow></mover></mrow><mrow><mi>β</mi></mrow></msub></math></span> in the Standard Model. Decays of tachyonic neutrinos over cosmological distances can lead to a reduction of the neutrino flux in the high-energy end of the spectrum. We estimate upper limits on the spacelike neutrino mass based on the PeV-energy cosmological neutrino events observed in the IceCube experiment. These limits are close to those deduced from the measurements of <span><math><msubsup><mrow><mi>m</mi></mrow><mrow><mi>ν</mi></mrow><mrow><mn>2</mn></mrow></msubsup></math></span> in the tritium-decay experiment KATRIN.</p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"41 ","pages":"Pages 81-88"},"PeriodicalIF":3.8,"publicationDate":"2024-02-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S2214404824000065/pdfft?md5=7ed379583f03b783991673e4d61b08ff&pid=1-s2.0-S2214404824000065-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139743191","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The challenge of identifying INTEGRAL sources on the Galactic plane","authors":"Raffaella Landi ,&nbsp;Loredana Bassani ,&nbsp;Gabriele Bruni ,&nbsp;Manuela Molina ,&nbsp;Nicola Masetti ,&nbsp;Angela Malizia ,&nbsp;Mariateresa Fiocchi ,&nbsp;Angela Bazzano ,&nbsp;Pietro Ubertini","doi":"10.1016/j.jheap.2024.01.005","DOIUrl":"10.1016/j.jheap.2024.01.005","url":null,"abstract":"<div><p>(<em>INTEGRAL</em>) has been surveying the sky above 20 keV since its launch in 2002 providing new insights into the nature of the sources that populate our Universe at soft <em>γ</em>-ray energies. The latest IBIS/ISGRI survey lists 929 hard X-ray sources, of which 113 are reported as unidentified, i.e. lacking a lower energy counterpart or simply not studied in other wavebands. To overcome this lack of information, we either browsed the X-ray archives, or, if no data in the X-ray band were available, we requested Target of Opportunity (ToO) observations with the X-ray Telescope (XRT) on-board the Neil Gehrels <em>Swift</em> Observatory. Following this approach, we selected a sample of 10 objects for which X-ray data were key to investigate their nature. We found a single X-ray association for all of the sources, except for IGR J16267−3303, for which two X-ray detections were spotted within the IBIS positional uncertainty. We then browsed multi-waveband archives to search for counterparts to these X-ray detections at other wavelengths and analysed X-ray spectral properties to determine their nature and association with the high-energy emitter. As a result of our analysis, we identified the most likely counterpart for 7 sources, although in some cases its nature/class could not be definitely assessed on the basis of the information collected. Interestingly, SWIFT J2221.6+5952, first reported in the 105-month <em>Swift</em>/Burst Alert Telescope (BAT) survey, is the only source of the sample for which we did not find any counterpart at radio/optical/IR wavebands. Finally, we found that two IBIS source, IGR J17449−3037 and IGR J17596−2315 are positionally associated with a <em>Fermi</em> Large Area Telescope (LAT) object.</p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"41 ","pages":"Pages 67-80"},"PeriodicalIF":3.8,"publicationDate":"2024-01-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139515401","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":"Exact scalar quasibound states solutions of f(R) theory's static spherically symmetric black hole","authors":"David Senjaya","doi":"10.1016/j.jheap.2024.01.004","DOIUrl":"10.1016/j.jheap.2024.01.004","url":null,"abstract":"<div><p>Following the recent developments in black holes' quasibound states exact solutions by <span>Senjaya, 2023b</span>, <span>Senjaya, 2023c</span><span>, in this letter, we present a novel exact solution of quasibound states of a scalar around a static spherically symmetric black hole solution of </span><span><math><mi>f</mi><mo>(</mo><mi>R</mi><mo>)</mo></math></span><span> theory of gravity. We start with the relativistic scalar field wave equation, i.e. the Klein-Gordon equation, isolating the radial equation and finally successfully obtain the exact radial wave solutions in terms of General Heun functions. Having the exact solutions in hand, the energy levels expression is obtained from the radial wave polynomial conditions. In the last part of this letter, the Hawking radiation is investigated via the Damour-Ruffini method and the Hawking temperature is obtained from radiation distribution function.</span></p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"41 ","pages":"Pages 61-66"},"PeriodicalIF":3.8,"publicationDate":"2024-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139470182","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":"Particle correlation in the cosmic ray showers around the spectral knee","authors":"Tadeusz Wibig","doi":"10.1016/j.jheap.2024.01.003","DOIUrl":"10.1016/j.jheap.2024.01.003","url":null,"abstract":"<div><p>In this paper, we answer the question to what extent the particles in showers initiated by particles with energies of 10¹⁴ – 10¹⁷<span> eV observed at the edges of extensive air showers, where average particle densities are low (&lt; a few per m</span>²), are correlated. The particle number multiplicity distributions in the surface detectors of the shower arrays are affected by the existence of such a correlation. They are well described by a negative binomial distribution rather than Poisson. Positive correlations cause the distributions to become broader and, in general, the variance of the observed particle number is larger than is usually assumed in the analysis of the shower registration by the Extensive Air Shower experiments. We show how this increase can alter the results of shower axis localisation algorithms.</p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"41 ","pages":"Pages 54-60"},"PeriodicalIF":3.8,"publicationDate":"2024-01-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139422338","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 BOAT GRB 221009A: A Poynting-flux-dominated narrow jet surrounded by a matter-dominated structured jet wing","authors":"Bing Zhang ,&nbsp;Xiang-Yu Wang ,&nbsp;Jian-He Zheng","doi":"10.1016/j.jheap.2024.01.002","DOIUrl":"10.1016/j.jheap.2024.01.002","url":null,"abstract":"<div><p>We argue that the broad-band observations of the brightest-of-all-time (BOAT) GRB 221009A reveal a physical picture involving two jet components: a narrow (∼0.6 degree half opening angle) pencil-beam jet that has a Poynting-flux-dominated jet composition, and a broader matter-dominated jet with an angular structure. We discuss various observational evidence that supports such a picture. To treat the problem, we develop an analytical structured jet model for both forward and reverse shock emission from the matter dominated structured jet wing during the deceleration phase. We discuss the physical implications of such a two-component jet configuration for this particular burst and for GRBs in general. We argue that in a quasi-universal structured jet scenario, some bright X-ray flares could be similar narrow jets viewed slightly outside the narrow jet cone and that narrow jets may exist in many more GRBs without being detected.</p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"41 ","pages":"Pages 42-53"},"PeriodicalIF":3.8,"publicationDate":"2024-01-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139095466","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":"On the statistical assumption on the distance moduli of Supernovae Ia and its impact on the determination of cosmological parameters","authors":"M.G. Dainotti ,&nbsp;G. Bargiacchi ,&nbsp;M. Bogdan ,&nbsp;S. Capozziello ,&nbsp;S. Nagataki","doi":"10.1016/j.jheap.2024.01.001","DOIUrl":"10.1016/j.jheap.2024.01.001","url":null,"abstract":"<div><p><span>Type Ia Supernovae (SNe Ia) are considered the most reliable </span><em>standard candles</em> and they have played an invaluable role in cosmology since the discovery of the Universe's accelerated expansion. During the last decades, the SNe Ia samples have been improved in number, redshift coverage, calibration methodology, and systematics treatment. These efforts led to the most recent <em>“Pantheon”</em> (2018) and <em>“Pantheon +”</em><span> (2022) releases, which enable to constrain cosmological parameters<span> more precisely than previous samples. In this era of precision cosmology, the community strives to find new ways to reduce uncertainties on cosmological parameters. To this end, we start our investigation even from the likelihood assumption of Gaussianity, implicitly used in this domain. Indeed, the usual practice involves constraining parameters through a Gaussian distance moduli likelihood. This method relies on the implicit assumption that the difference between the distance moduli measured and the ones expected from the cosmological model is Gaussianly distributed. In this work, we test this hypothesis for both the </span></span><em>Pantheon</em> and <em>Pantheon +</em> releases. We find that in both cases this requirement is not fulfilled and the actual underlying distributions are a logistic and a Student's t distribution for the <em>Pantheon</em> and <em>Pantheon +</em> data, respectively. When we apply these new likelihoods fitting a flat ΛCDM model, we significantly reduce the uncertainties on the matter density <span><math><msub><mrow><mi>Ω</mi></mrow><mrow><mi>M</mi></mrow></msub></math></span><span> and the Hubble constant </span><span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span> of <span><math><mo>∼</mo><mn>40</mn><mtext>%</mtext></math></span>. As a result, the Hubble tension is increased at <span><math><mo>&gt;</mo><mn>5</mn><mi>σ</mi></math></span> level. This boosts the SNe Ia power in constraining cosmological parameters, thus representing a huge step forward to shed light on the current debated tensions in cosmology.</p></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"41 ","pages":"Pages 30-41"},"PeriodicalIF":3.8,"publicationDate":"2024-01-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139095500","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}