Astroparticle Physics最新文献

{"title":"Glitching pulsars as gravitational wave sources","authors":"B. Haskell ,&nbsp;D.I. Jones","doi":"10.1016/j.astropartphys.2023.102921","DOIUrl":"10.1016/j.astropartphys.2023.102921","url":null,"abstract":"<div><p><span>Spinning neutron stars, when observed as pulsars, are seen to undergo occasional spin-up events known as glitches. Despite several decades of study, the physical mechanisms responsible for glitches are still not well understood, but probably involve an interplay between the star’s outer elastic crust, and the </span>superfluid<span> and superconducting core that lies within. Glitches will be accompanied by some level of gravitational wave emission. In this article, we review proposed models that link gravitational wave emission to glitches, exploring both short duration burst-like emission, and longer-lived signals. We illustrate how detections (and in some cases, non-detections) of gravitational signals probe both the glitch mechanism, and, by extension, the behaviour of matter at high densities.</span></p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"157 ","pages":"Article 102921"},"PeriodicalIF":3.5,"publicationDate":"2023-12-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139051874","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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":"Thermodynamic topology and photon spheres in the hyperscaling violating black holes","authors":"Jafar Sadeghi ,&nbsp;Mohammad Ali S. Afshar ,&nbsp;Saeed Noori Gashti ,&nbsp;Mohammad Reza Alipour","doi":"10.1016/j.astropartphys.2023.102920","DOIUrl":"10.1016/j.astropartphys.2023.102920","url":null,"abstract":"&lt;div&gt;&lt;p&gt;&lt;span&gt;It was shown that a standard ring of light can be imagined outside the event horizon for stationary rotating four-dimensional black holes with axial symmetry using the topological method (Cunha, 2020; Wei and Shao-Wen, 2020). Based on this concept, in this paper, we investigate the topological charge and the conditions of existence of the photon sphere (PS) for a hyperscaling violation (HSV) black hole with various values of the parameters of this model. Then, after carrying out a detailed analysis, we show the conventional topological classes viz &lt;/span&gt;&lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;Q&lt;/mi&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mo&gt;−&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; for the mentioned black hole and &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;Q&lt;/mi&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;&lt;span&gt; for the naked singularities. &lt;/span&gt;&lt;em&gt;Also, we propose a new topological class for naked singularities (&lt;/em&gt;&lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;Q&lt;/mi&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mo&gt;+&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;&lt;em&gt;) with respect to&lt;/em&gt; &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;z&lt;/mi&gt;&lt;mo&gt;≥&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;&lt;em&gt;. We also determined that&lt;/em&gt; &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;z&lt;/mi&gt;&lt;mo&gt;≥&lt;/mo&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;&lt;em&gt;, it either shows a naked singularity form with total topological charge&lt;/em&gt; &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mo&gt;+&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; &lt;em&gt;or has no solution. Therefore, we have the black hole solution only in&lt;/em&gt; &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;mo&gt;≤&lt;/mo&gt;&lt;mi&gt;z&lt;/mi&gt;&lt;mo&gt;&lt;&lt;/mo&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;. Then, we will use two different methods, namely the temperature (Duan’s topological current &lt;span&gt;&lt;math&gt;&lt;mi&gt;Φ&lt;/mi&gt;&lt;/math&gt;&lt;/span&gt;-mapping theory) and the generalized Helmholtz free energy method, to study the topological classes of our black hole. By considering the black hole mentioned, we discuss the critical and zero points (topological charges and topological numbers) for different parameters of hyperscaling violating black holes, such as (&lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;z&lt;/mi&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mover&gt;&lt;mrow&gt;&lt;mi&gt;θ&lt;/mi&gt;&lt;/mrow&gt;&lt;mo&gt;¯&lt;/mo&gt;&lt;/mover&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;&lt;span&gt;) and other free parameters, and study their thermodynamic topology. We observe that for a given value of the parameters &lt;/span&gt;&lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;mo&gt;≤&lt;/mo&gt;&lt;mi&gt;z&lt;/mi&gt;&lt;mo&gt;&lt;&lt;/mo&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;, &lt;span&gt;&lt;math&gt;&lt;mover&gt;&lt;mrow&gt;&lt;mi&gt;θ&lt;/mi&gt;&lt;/mrow&gt;&lt;mo&gt;¯&lt;/mo&gt;&lt;/mover&gt;&lt;/math&gt;&lt;/span&gt;, and other free parameters, there exist two total topological charges &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mo&gt;(&lt;/mo&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;Q&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;t&lt;/mi&gt;&lt;mi&gt;o&lt;/mi&gt;&lt;mi&gt;t&lt;/mi&gt;&lt;mi&gt;a&lt;/mi&gt;&lt;mi&gt;l&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mo&gt;−&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;mo&gt;)&lt;/mo&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; with the same phase structure for the &lt;span&gt;&lt;math&gt;&lt;mi&gt;T&lt;/mi&gt;&lt;/math&gt;&lt;/span&gt; method and total topological numbers &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mo&gt;(&lt;/mo&gt;&lt;mi&gt;W&lt;/mi&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mo&gt;+&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;mo&gt;)&lt;/mo&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; for the generalized Helmholtz free energy method. Additionally, we summarize the results for each study as photon sphere, temperature, and generalized Helmholtz free energy in some f","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"156 ","pages":"Article 102920"},"PeriodicalIF":3.5,"publicationDate":"2023-12-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139031341","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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":"Ancestral spin information in gravitational waves from black hole mergers","authors":"O. Barrera,&nbsp;I. Bartos","doi":"10.1016/j.astropartphys.2023.102919","DOIUrl":"10.1016/j.astropartphys.2023.102919","url":null,"abstract":"<div><p><span>The heaviest black holes discovered through gravitational waves have masses that are difficult to explain with current standard </span>stellar models. This discrepancy may be due to a series of hierarchical mergers, where the observed black holes are themselves the products of previous mergers. Here we present a method to estimate the masses and spins of previous generations of black holes based on the masses and spins of black holes in a binary. Examining the merger GW190521, we find that assuming black hole spins that are consistent with those of merger remnants will alter the reconstructed ancestral spins when compared to results with uninformed priors. At the same time, the inclusion of black hole spins does not significantly affect the mass distributions of the ancestral black holes.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"156 ","pages":"Article 102919"},"PeriodicalIF":3.5,"publicationDate":"2023-12-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138567469","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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":"Forecasts analysis on varying-α theories from gravitational wave standard sirens","authors":"L.R. Colaço ,&nbsp;R.F.L. Holanda ,&nbsp;Rafael C. Nunes ,&nbsp;J.E. Gonzalez","doi":"10.1016/j.astropartphys.2023.102911","DOIUrl":"https://doi.org/10.1016/j.astropartphys.2023.102911","url":null,"abstract":"<div><p><span>Motivated by future gravitational waves observations, we perform forecasts analysis to constrain a possible time variation of the fine structure constant (</span><span><math><mi>α</mi></math></span><span>) within the context of the so-called runaway dilaton model. For this purpose, some gravitational-wave standard sirens mock data within the perspective of Einstein Telescope and LISA mission were considered jointly with current strong gravitational lensing systems observations. We find that future standard sirens observations can also play an important role in the search for possible variations of </span><span><math><mi>α</mi></math></span> within the methodology presented in this work.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"155 ","pages":"Article 102911"},"PeriodicalIF":3.5,"publicationDate":"2023-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"49761351","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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":"Enabling kilonova science with Nancy Grace Roman Space Telescope","authors":"Igor Andreoni ,&nbsp;Michael W. Coughlin ,&nbsp;Alexander W. Criswell ,&nbsp;Mattia Bulla ,&nbsp;Andrew Toivonen ,&nbsp;Leo P. Singer ,&nbsp;Antonella Palmese ,&nbsp;E. Burns ,&nbsp;Suvi Gezari ,&nbsp;Mansi M. Kasliwal ,&nbsp;R. Weizmann Kiendrebeogo ,&nbsp;Ashish Mahabal ,&nbsp;Takashi J. Moriya ,&nbsp;Armin Rest ,&nbsp;Dan Scolnic ,&nbsp;Robert A. Simcoe ,&nbsp;Jamie Soon ,&nbsp;Robert Stein ,&nbsp;Tony Travouillon","doi":"10.1016/j.astropartphys.2023.102904","DOIUrl":"https://doi.org/10.1016/j.astropartphys.2023.102904","url":null,"abstract":"<div><p><span><span><span><span>Binary neutron star mergers and neutron star–black hole mergers are multi-messenger sources that can be detected in </span>gravitational waves and in </span>electromagnetic radiation<span>. The low electron fraction of neutron star merger ejecta favors the production of heavy elements such as </span></span>lanthanides and actinides via rapid neutron capture (</span><span><math><mi>r</mi></math></span>-process). The decay of these unstable nuclei powers an infrared-bright transient called a “kilonova”. The discovery of a population of kilonovae will allow us to determine if neutron star mergers are the dominant sites for <span><math><mi>r</mi></math></span><span><span>-process element nucleosynthesis, constrain the equation of state<span><span> of nuclear matter, and make independent measurements of the Hubble constant. The Nancy Grace Roman Space Telescope (Roman) will have a unique combination of depth, near-infrared sensitivity, and wide </span>field of view. These characteristics will enable Roman’s discovery of GW counterparts that will be missed by </span></span>optical telescopes, such as kilonova that are associated with large distances, high lanthanide fractions, high binary mass-ratios, large dust extinction in the line of sight, or that are observed from equatorial viewing angles. In preparation for Roman’s launch and operations, our analysis suggests to (i) make available a rapid (</span><span><math><mrow><mo>∼</mo><mn>1</mn></mrow></math></span> week) Target of Opportunity mode for GW follow-up; (ii) include observations of the High Latitude Time-Domain survey footprint in at least two filters (preferably the F158 and F213 filters) with a cadence of <span><math><mrow><mo>≲</mo><mn>8</mn></mrow></math></span> days; (iii) operate in synergy with Rubin Observatory. Following these recommendations, we expect that 1–6 kilonovae can be identified by Roman via target of opportunity observations of well localized (<span><math><mrow><mi>A</mi><mo>&lt;</mo><mn>10</mn></mrow></math></span> <!--> <!-->deg<span><math><msup><mrow></mrow><mrow><mn>2</mn></mrow></msup></math></span>, 90% C.I.) neutron star mergers during 1.5 years of the LIGO-Virgo-KAGRA fifth (or <span><math><mo>∼</mo></math></span>4–21 in during the sixth) observing run. A sample of 5–40 serendipitously discovered kilonovae can be collected in a 5-year high latitude survey.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"155 ","pages":"Article 102904"},"PeriodicalIF":3.5,"publicationDate":"2023-10-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"49710379","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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":"Tensor fluctuations in the early universe","authors":"F. Melia","doi":"10.1016/j.astropartphys.2023.102876","DOIUrl":"10.1016/j.astropartphys.2023.102876","url":null,"abstract":"<div><p><span><span>In standard inflationary cosmology, scalar and tensor perturbations grew as the Universe expanded and froze when their wavelengths exceeded the Hubble horizon, producing a tell-tale signature in the fluctuation spectrum and amplitude of the cosmic microwave background (CMB). But there are now very good reasons to examine whether structure formation could also have begun via the seeding of </span>quantum fluctuations in a non-inflationary field. In this </span><em>Letter</em><span>, we study and compare the scalar and tensor modes produced in these two scenarios, and demonstrate that upcoming observations to measure the B-mode polarization of the CMB may be able to differentiate between them. Whereas both scalar and tensor modes should be observable if the field was inflationary, only scalar modes would be present in the CMB if it were not. Should gravity be purely classical, however, the tensor modes would have avoided canonical quantization in all cases, resulting in unmeasurably weak gravitational waves. A non-detection of B-mode polarization would thus not completely rule out inflation.</span></p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"152 ","pages":"Article 102876"},"PeriodicalIF":3.5,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"48310613","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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 cosmogenic activation above ground for the DarkSide-20k experiment","authors":"A. Elersich ,&nbsp;P. Agnes ,&nbsp;I. Ahmad ,&nbsp;S. Albergo ,&nbsp;I.F.M. Albuquerque ,&nbsp;T. Alexander ,&nbsp;A.K. Alton ,&nbsp;P. Amaudruz ,&nbsp;M. Atzori Corona ,&nbsp;M. Ave ,&nbsp;I.Ch. Avetisov ,&nbsp;O. Azzolini ,&nbsp;H.O. Back ,&nbsp;Z. Balmforth ,&nbsp;A. Barrado-Olmedo ,&nbsp;P. Barrillon ,&nbsp;A. Basco ,&nbsp;G. Batignani ,&nbsp;V. Bocci ,&nbsp;W.M. Bonivento ,&nbsp;M.P. Zykova","doi":"10.1016/j.astropartphys.2023.102878","DOIUrl":"https://doi.org/10.1016/j.astropartphys.2023.102878","url":null,"abstract":"<div><p>The activation of materials due to exposure to cosmic rays may become an important background source for experiments investigating rare event phenomena. DarkSide-20k, currently under construction at the Laboratori Nazionali del Gran Sasso, is a direct detection experiment for galactic dark matter particles, using a two-phase liquid-argon Time Projection Chamber (TPC) filled with 49.7 tonnes (active mass) of Underground Argon (UAr) depleted in ³⁹Ar. Despite the outstanding capability of discriminating <span><math><mi>γ</mi></math></span>/<span><math><mi>β</mi></math></span> background in argon TPCs, this background must be considered because of induced dead time or accidental coincidences mimicking dark-matter signals and it is relevant for low-threshold electron-counting measurements. Here, the cosmogenic activity of relevant long-lived radioisotopes induced in the experiment has been estimated to set requirements and procedures during preparation of the experiment and to check that it is not dominant over primordial radioactivity; particular attention has been paid to the activation of the 120 t of UAr used in DarkSide-20k. Expected exposures above ground and production rates, either measured or calculated, have been considered in detail. From the simulated counting rates in the detector due to cosmogenic isotopes, it is concluded that activation in copper and stainless steel is not problematic. The activity of ³⁹Ar induced during extraction, purification and transport on surface is evaluated to be 2.8% of the activity measured in UAr by DarkSide-50 experiment, which used the same underground source, and thus considered acceptable. Other isotopes in the UAr such as ³⁷Ar and ³H are shown not to be relevant due to short half-life and assumed purification methods.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"152 ","pages":"Article 102878"},"PeriodicalIF":3.5,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"49709788","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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":"MOONRAY: A permanent high-energy cosmic-ray observatory on the surface of the Moon","authors":"P.S. Marrocchesi","doi":"10.1016/j.astropartphys.2023.102879","DOIUrl":"10.1016/j.astropartphys.2023.102879","url":null,"abstract":"<div><p>The forthcoming decades will see a rapid development of space programs aiming at the implementation of habitats on our satellite. Therefore it makes sense to evaluate the feasibility of a permanent cosmic-ray (CR) observatory on the Moon. Its large sensitive area would allow to carry out a very rich observational program over a time span of a few decades with an unprecedented energy reach. A thorough exploration of the energy region around the CR spectral anomaly located at a few PeV, also known as the “knee”, will become possible.</p><p>In this paper we propose an innovative concept of a <em>modular</em> lunar observatory designed to overcome the limitations of the present generation of cosmic-ray telescopes in Low Earth Orbit. It consists of an array of fully independent modules with limited individual size and weight. This would allow an ample flexibility in the gradual deployment of a progressively larger active volume, while ensuring the collection of meaningful scientific data during the intermediate stages of its implementation. Each independent module consists of three main instruments: a combined Charge and Time-of-Flight detector to identify individual elements from proton to nickel (and beyond), a tracker providing the direction and impact point of the incident particle, and a calorimeter to measure its kinetic energy. The design of each instrument contains innovative solutions that are well within the reach of the present technology.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"152 ","pages":"Article 102879"},"PeriodicalIF":3.5,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"45041951","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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 longitudinal development of air showers in the knee energy range","authors":"Feng Zhang ,&nbsp;Hu Liu ,&nbsp;Fengrong Zhu ,&nbsp;Jacob Oloketuyi","doi":"10.1016/j.astropartphys.2023.102877","DOIUrl":"10.1016/j.astropartphys.2023.102877","url":null,"abstract":"<div><p><span>Ground-based cosmic ray experiments detect cosmic ray mainly by measuring the longitudinal and lateral distribution of secondary particles produced in the extensive air shower<span> (EAS). The EAS of cosmic ray in the knee energy region is simulated via CORSIKA software. Several simulation samples with different energy, composition and zenith angles were carried out to understand the longitudinal development of electron, muon and Cherenkov light in EAS. All the results presented were obtained assuming an observation plane at an altitude of 4400 m a.s.l. The differences of longitudinal development between electron and Cherenkov light were studied, and the reconstruction uncertainty of shower maximum for electron from Cherenkov light was estimated to be 10–15 g/cm</span></span><span><math><msup><mrow></mrow><mrow><mn>2</mn></mrow></msup></math></span> for nuclei above 1 PeV. The performances of energy measurement and the composition discrimination ability based on longitudinal development were studied and compared with that from lateral distribution. It was found that number of electron per depth at its shower maximum has the smallest shower-to-shower fluctuations, but the shower-to-shower fluctuations of electron density measured at observation level was very close to it when the appropriate zenith angle was employed. The shower-to-shower fluctuations of shower maximum for electron is 50–55 g/cm<span><math><msup><mrow></mrow><mrow><mn>2</mn></mrow></msup></math></span> for proton, and 20–25 g/cm<span><math><msup><mrow></mrow><mrow><mn>2</mn></mrow></msup></math></span> for iron, but the composition discrimination ability between nuclei from muon density measured at observation level is much better than the shower maximum variable from longitudinal development. The hadronic model dependencies of the longitudinal development and lateral distribution were also discussed.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"152 ","pages":"Article 102877"},"PeriodicalIF":3.5,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"47737687","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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":"Evaluations of uncertainties in simulations of propagation of ultrahigh-energy cosmic-ray nuclei derived from microscopic nuclear models","authors":"E. Kido ,&nbsp;T. Inakura ,&nbsp;M. Kimura ,&nbsp;N. Kobayashi ,&nbsp;S. Nagataki ,&nbsp;N. Shimizu ,&nbsp;A. Tamii ,&nbsp;Y. Utsuno","doi":"10.1016/j.astropartphys.2023.102866","DOIUrl":"10.1016/j.astropartphys.2023.102866","url":null,"abstract":"<div><p>Photodisintegration is a main energy loss process for ultrahigh-energy cosmic-ray (UHECR) nuclei in intergalactic space. Therefore, it is crucial to understand systematic uncertainty in photodisintegration when simulating the propagation of UHECR nuclei. In this work, we calculated the cross sections using the random phase approximation (RPA) of density functional theory (DFT), a microscopic nuclear model. We calculated the <span><math><mrow><mi>E</mi><mn>1</mn></mrow></math></span> strength of 29 nuclei using three different density functionals. We obtained the cross sections of photonuclear reactions, including photodisintegration, with the <span><math><mrow><mi>E</mi><mn>1</mn></mrow></math></span> strength. Then, we implemented the cross sections in the cosmic-ray propagation code CRPropa. We found that assuming certain astrophysical parameter values, the difference between UHECR energy spectrum predictions using the RPA calculation and the default photodisintegration model in CRPropa can be more than the statistical uncertainty of the spectrum. We also found that the differences between the RPA calculations and CRPropa default in certain astrophysical parameters obtained by a combined fit of UHECR energy spectrum and composition data assuming a phenomenological model of UHECR sources can be more than the uncertainty of the data.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"152 ","pages":"Article 102866"},"PeriodicalIF":3.5,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"43038931","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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}