Fortschritte Der Physik-Progress of Physics最新文献

{"title":"Issue Information: Fortschritte der Physik 6 / 2024","authors":"","doi":"10.1002/prop.202400905","DOIUrl":"https://doi.org/10.1002/prop.202400905","url":null,"abstract":"","PeriodicalId":55150,"journal":{"name":"Fortschritte Der Physik-Progress of Physics","volume":"72 6","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-06-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/prop.202400905","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141286800","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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":"One-Loop Effective Potential in Scherk–Schwarz Compactifications of Pure \u0000 \u0000 \u0000 d\u0000 =\u0000 5\u0000 \u0000 $d=5$\u0000 Supergravities","authors":"Gianguido Dall'Agata, Fabio Zwirner","doi":"10.1002/prop.202400087","DOIUrl":"10.1002/prop.202400087","url":null,"abstract":"<p>We perform a systematic analysis of the one-loop effective potential of pure <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>d</mi>\u0000 <mo>=</mo>\u0000 <mn>5</mn>\u0000 </mrow>\u0000 <annotation>$d=5$</annotation>\u0000 </semantics></math> supergravities, with supersymmetry fully broken by a Scherk–Schwarz compactification on the circle, as a function of the radial modulus. We discuss the precise correspondence between the effective potential <span></span><math>\u0000 <semantics>\u0000 <msub>\u0000 <mi>V</mi>\u0000 <mn>1</mn>\u0000 </msub>\u0000 <annotation>$V_1$</annotation>\u0000 </semantics></math> in the full compactified theory and its counterpart <span></span><math>\u0000 <semantics>\u0000 <msub>\u0000 <mi>V</mi>\u0000 <mrow>\u0000 <mn>1</mn>\u0000 <mo>,</mo>\u0000 <mi>r</mi>\u0000 <mi>e</mi>\u0000 <mi>d</mi>\u0000 </mrow>\u0000 </msub>\u0000 <annotation>$V_{1,red}$</annotation>\u0000 </semantics></math> in the reduced theory. We confirm that <span></span><math>\u0000 <semantics>\u0000 <msub>\u0000 <mi>V</mi>\u0000 <mn>1</mn>\u0000 </msub>\u0000 <annotation>$V_1$</annotation>\u0000 </semantics></math> is finite for any <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>N</mi>\u0000 <mo>></mo>\u0000 <mn>0</mn>\u0000 </mrow>\u0000 <annotation>$N>0$</annotation>\u0000 </semantics></math>, in contrast to <span></span><math>\u0000 <semantics>\u0000 <msub>\u0000 <mi>V</mi>\u0000 <mrow>\u0000 <mn>1</mn>\u0000 <mo>,</mo>\u0000 <mi>r</mi>\u0000 <mi>e</mi>\u0000 <mi>d</mi>\u0000 </mrow>\u0000 </msub>\u0000 <annotation>$V_{1,red}$</annotation>\u0000 </semantics></math>. We find that for broken <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>N</mi>\u0000 <mo>=</mo>\u0000 <mn>8</mn>\u0000 </mrow>\u0000 <annotation>$N=8$</annotation>\u0000 </semantics></math> supergravity <span></span><math>\u0000 <semantics>\u0000 <msub>\u0000 <mi>V</mi>\u0000 <mn>1</mn>\u0000 </msub>\u0000 <annotation>$V_1$</annotation>\u0000 </semantics></math> is negative definite even after accounting for the Kaluza–Klein states. We outline a program for future work where the study of a different kind of Scherk-Schwarz compactifications, still at the field theory level but with at least three extra dimensions, could lead to qualita","PeriodicalId":55150,"journal":{"name":"Fortschritte Der Physik-Progress of Physics","volume":"72 7-8","pages":""},"PeriodicalIF":5.6,"publicationDate":"2024-06-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141378106","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":"Species Scale and Primordial Gravitational Waves","authors":"Marco Scalisi","doi":"10.1002/prop.202400033","DOIUrl":"10.1002/prop.202400033","url":null,"abstract":"<p>The species scale is a field-dependent UV cut-off for any effective field theory weakly coupled to gravity. In this letter, it is shown that in the context of inflationary cosmology, a detection of primordial gravitational waves will set an upper bound on the decay rate <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mrow>\u0000 <mo>|</mo>\u0000 </mrow>\u0000 <msubsup>\u0000 <mi>Λ</mi>\u0000 <mi>s</mi>\u0000 <mo>′</mo>\u0000 </msubsup>\u0000 <mo>/</mo>\u0000 <msub>\u0000 <mi>Λ</mi>\u0000 <mi>s</mi>\u0000 </msub>\u0000 <mrow>\u0000 <mo>|</mo>\u0000 </mrow>\u0000 </mrow>\u0000 <annotation>$|Lambda ^{prime }_s/Lambda _s|$</annotation>\u0000 </semantics></math> of the species scale. Specifically, this is derived in terms of the tensor-to-scalar ratio <span></span><math>\u0000 <semantics>\u0000 <mi>r</mi>\u0000 <annotation>$r$</annotation>\u0000 </semantics></math> of power spectra of primordial perturbations. Given the targets of current and next generation experiments, it is shown that any successful detection would signify that this upper limit is of the order of unity, which is consistent with recent discussions in the literature.</p>","PeriodicalId":55150,"journal":{"name":"Fortschritte Der Physik-Progress of Physics","volume":"72 6","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-05-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/prop.202400033","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140930060","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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":"Issue Information: Fortschritte der Physik 5 / 2024","authors":"","doi":"10.1002/prop.202400904","DOIUrl":"https://doi.org/10.1002/prop.202400904","url":null,"abstract":"","PeriodicalId":55150,"journal":{"name":"Fortschritte Der Physik-Progress of Physics","volume":"72 5","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-05-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/prop.202400904","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140880993","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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":"Dynamics and Stability via Thin-Shell of Approximated Black Holes in \u0000 \u0000 \u0000 f\u0000 (\u0000 Q\u0000 )\u0000 \u0000 $f(mathbb {Q})$\u0000 Gravity","authors":"Faisal Javed,&nbsp;Ji Lin,&nbsp;Ghulam Mustafa,&nbsp;Ferdous M. O. Tawfiq","doi":"10.1002/prop.202300081","DOIUrl":"10.1002/prop.202300081","url":null,"abstract":"<p>The current study is devoted to exploring the geometrical configuration of a thin-shell in the background of symmetric teleparallel gravity. For this purpose, the well-known cut-and-paste approach by matching the inner flat and outer newly calculated class of approximated black hole (BH) solutions in symmetric teleparallel gravity are considered, i.e., uncharged, charged, and anti-de-Sitter BHs. The dynamical analysis of thin-shell configuration by adopting the massive and massless scalar field via Klein-Gordon's equation of motion is discussed. The effective potential and proper time derivative of shell radius for both massive and massless scalar shells are used to discuss the collapse, expansion, and oscillatory behavior. The stable configuration of thin-shell is observed through the linearized radial perturbation approach with a phantomlike equation of state, i.e., quintessence, dark energy, and phantom energy. It is noted that stable/unstable behavior of thin-shell is found after the expected position of the event horizon of an exterior manifold. It is concluded that the stability of a thin-shell is greater for <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>f</mi>\u0000 <mo>(</mo>\u0000 <mi>Q</mi>\u0000 <mo>)</mo>\u0000 </mrow>\u0000 <annotation>$f(mathbb {Q})$</annotation>\u0000 </semantics></math> BH with cosmological constant as compared to the uncharged and charged <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>f</mi>\u0000 <mo>(</mo>\u0000 <mi>Q</mi>\u0000 <mo>)</mo>\u0000 </mrow>\u0000 <annotation>$f(mathbb {Q})$</annotation>\u0000 </semantics></math> BHs.</p>","PeriodicalId":55150,"journal":{"name":"Fortschritte Der Physik-Progress of Physics","volume":"72 6","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-05-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140827842","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":"Quasinormal Spectrum of \u0000 \u0000 \u0000 (\u0000 2\u0000 +\u0000 1\u0000 )\u0000 \u0000 $(2+1)$\u0000 -Dimensional Asymptotically Flat, dS and AdS Black Holes","authors":"Milena Skvortsova","doi":"10.1002/prop.202400036","DOIUrl":"10.1002/prop.202400036","url":null,"abstract":"<p>While <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>(</mo>\u0000 <mn>2</mn>\u0000 <mo>+</mo>\u0000 <mn>1</mn>\u0000 <mo>)</mo>\u0000 </mrow>\u0000 <annotation>$(2+1)$</annotation>\u0000 </semantics></math>-dimensional black holes in the Einstein theory allow for only the anti-de Sitter (AdS) asymptotic, when the higher curvature correction is tuned on, the asymptotically flat, de Sitter, and AdS cases are included. Here, a detailed study of the stability and quasinormal spectra of the scalar field perturbations around such black holes with all three asymptotics is proposed. Calculations of the frequencies are fulfilled with the help of the 6th order Wentzel–Kramers–Brillouin (WKB) method with Pade approximants, Bernstein polynomial method, and time-domain integration. Results obtained by all three methods are in a very good agreement in their common range of applicability. When the multipole moment <span></span><math>\u0000 <semantics>\u0000 <mi>k</mi>\u0000 <annotation>$k$</annotation>\u0000 </semantics></math> is equal to zero, the purely imaginary, i.e., non-oscillatory, modes dominate in the spectrum for all types of the asymptotic behavior, while the spectrum at higher <span></span><math>\u0000 <semantics>\u0000 <mi>k</mi>\u0000 <annotation>$k$</annotation>\u0000 </semantics></math> resembles that in four-dimensional spacetime with the corresponding asymptotic.</p>","PeriodicalId":55150,"journal":{"name":"Fortschritte Der Physik-Progress of Physics","volume":"72 6","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-04-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140801883","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":"Bouncing Cosmology in \u0000 \u0000 \u0000 f\u0000 (\u0000 R\u0000 ,\u0000 G\u0000 )\u0000 \u0000 $f(R,mathcal {G})$\u0000 Gravity with Thermodynamic Analysis","authors":"Shaily,&nbsp;Jainendra Kumar Singh,&nbsp;Akanksha Singh","doi":"10.1002/prop.202300244","DOIUrl":"10.1002/prop.202300244","url":null,"abstract":"&lt;p&gt;The evolution of the universe in a modified gravity theory that includes the terms Ricci scalar (&lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mi&gt;R&lt;/mi&gt;\u0000 &lt;annotation&gt;$ R$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;) and the Gauss-Bonnet invariant (&lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mi&gt;G&lt;/mi&gt;\u0000 &lt;annotation&gt;$mathcal {G}$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;) is studied. The function &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;f&lt;/mi&gt;\u0000 &lt;mo&gt;(&lt;/mo&gt;\u0000 &lt;mi&gt;R&lt;/mi&gt;\u0000 &lt;mo&gt;,&lt;/mo&gt;\u0000 &lt;mi&gt;G&lt;/mi&gt;\u0000 &lt;mo&gt;)&lt;/mo&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$f(R,mathcal {G})$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; is obtained using the e-folding number and reconstruction technique by assuming an appropriate parameterization of the scale factor &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mi&gt;a&lt;/mi&gt;\u0000 &lt;annotation&gt;$ a$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;. In this model, the various cosmological parameters are analyzed to explicate the bouncing scenario of the universe with the help of the contraction and expansion phases of the universe before and after the bouncing point of the model, respectively. A violation of the null energy condition is found. Additionally, the ghost condensate nature of the model in the neighborhood of the bouncing point (&lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;t&lt;/mi&gt;\u0000 &lt;mo&gt;=&lt;/mo&gt;\u0000 &lt;mn&gt;0&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$ t=0$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;) is seen. Furthermore, the deceleration parameter is not defined at the bouncing point, i.e., &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;q&lt;/mi&gt;\u0000 &lt;mo&gt;→&lt;/mo&gt;\u0000 &lt;mi&gt;∞&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$q rightarrow infty$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; at &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;t&lt;/mi&gt;\u0000 &lt;mo&gt;=&lt;/mo&gt;\u0000 &lt;mn&gt;0&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$t=0$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; and approaches a finite value &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;q&lt;/mi&gt;\u0000 &lt;mo&gt;→&lt;/mo&gt;\u0000 &lt;mo&gt;−&lt;/mo&gt;\u0000 &lt;mn&gt;1&lt;/mn&gt;\u0000 &lt;mo&gt;+&lt;/mo&gt;\u0000 &lt;mfrac&gt;\u0000 &lt;mn&gt;1&lt;/mn&gt;\u0000 &lt;mi&gt;β&lt;/mi&gt;\u0000 &lt;/mfrac&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$ q rightarrow -1+frac{1}{beta }$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; in later times (&lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;t&lt;/mi&gt;\u0000 &lt;mo&gt;→&lt;/mo&gt;\u0000 ","PeriodicalId":55150,"journal":{"name":"Fortschritte Der Physik-Progress of Physics","volume":"72 6","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-04-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140685638","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":"Issue Information: Fortschritte der Physik 4 / 2024","authors":"","doi":"10.1002/prop.202400903","DOIUrl":"https://doi.org/10.1002/prop.202400903","url":null,"abstract":"","PeriodicalId":55150,"journal":{"name":"Fortschritte Der Physik-Progress of Physics","volume":"72 4","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-04-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/prop.202400903","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140537914","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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":"A New 2D Formulation of Modified General Relativity","authors":"Christian G. Böhmer,&nbsp;Erik Jensko","doi":"10.1002/prop.202300216","DOIUrl":"10.1002/prop.202300216","url":null,"abstract":"<p>It is well known that the Einstein–Hilbert action in two dimensions is topological and yields an identically vanishing Einstein tensor. Consequently one is faced with difficulties when formulating a non-trivial gravity model. The authors present a new, intrinsically two-dimensional, approach to this problem based on the Einstein action. This yields a well defined variational approach which results in new field equations that break diffeomorphism invariance. This proposed approach does not require the introduction of additional scalar fields, nor the use of conformal transformations. However, how including conformal counter terms leads to equivalent results is shown. In doing so, an explanation for why previous approaches worked can be provided. Solutions to the field equations are briefly discussed.</p>","PeriodicalId":55150,"journal":{"name":"Fortschritte Der Physik-Progress of Physics","volume":"72 6","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-04-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/prop.202300216","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140564174","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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":"Dynamical System Approach and Thermodynamical Perspective of Hořava-Lifshitz Gravity","authors":"Amit Samaddar,&nbsp;S. Surendra Singh","doi":"10.1002/prop.202400006","DOIUrl":"10.1002/prop.202400006","url":null,"abstract":"<p>The authors have examined a Friedmann Robertson Walker cosmological model in Hořava-Lifshitz gravity by using a dynamical system approach. A set of autonomous equations is derived and their solutions are calculated. The critical points from these equations and find the characteristics values with the analysis of the physical interpretation of the phase space for this system are assessed. Three stable critical points are found and the values of the physical parameters and the scale factor's expressions at each critical points are displayed in Tables 1, 2, and 3. A hybrid scale factor to develop the model, which results in a phase transition from deceleration to acceleration is used. The suitable values of the parameters are governed by applying the Monte Chain Monte Carlo method technique to the Hubble 46 and joint Hubble 46 and Baryon Acoustic Oscillations 15 datasets. In contrast to the negative behavior of pressure, the positive behavior of energy density and <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>q</mi>\u0000 <mo>=</mo>\u0000 <mo>−</mo>\u0000 <mn>1</mn>\u0000 </mrow>\u0000 <annotation>$q=-1$</annotation>\u0000 </semantics></math> illustrate the Universe's acceleration epoch and the <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>Λ</mi>\u0000 <mi>CDM</mi>\u0000 </mrow>\u0000 <annotation>$Lambda{rm CDM}$</annotation>\u0000 </semantics></math> model is represented by the EoS parameter <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>ω</mi>\u0000 <mo>=</mo>\u0000 <mo>−</mo>\u0000 <mn>1</mn>\u0000 </mrow>\u0000 <annotation>$omega =-1$</annotation>\u0000 </semantics></math>. The authors investigated that the energy conditions and their model violates the strong energy condition. Utilizing <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>O</mi>\u0000 <mi>m</mi>\u0000 </mrow>\u0000 <annotation>$Om$</annotation>\u0000 </semantics></math> diagnostic test, it is found that the model represents phantom behavior. The thermodynamical perspective for the model is also examined. The model accurately explained the Universe's propagation history and fits well with contemporary cosmic data.</p>","PeriodicalId":55150,"journal":{"name":"Fortschritte Der Physik-Progress of Physics","volume":"72 6","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140564175","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}