LRS Bianchi Type-I String Cosmological Models in f Q IF 0.7 Q2 MATHEMATICS Muenster Journal of Mathematics Pub Date : 2023-06-27 DOI:10.1155/2023/7016804 Mukesh Kumar, Manvinder Singh, Mohit Bajaj, Hossam Kotb, Djeudjo Temene Hermann 求助PDF {"title":"LRS Bianchi Type-I String Cosmological Models in <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M1\">\n <mi>f</mi>\n <mfenced open=\"(\" close=\")\" separators=\"|\">\n <mrow>\n <mi>Q</mi>\n </m","authors":"Mukesh Kumar, Manvinder Singh, Mohit Bajaj, Hossam Kotb, Djeudjo Temene Hermann","doi":"10.1155/2023/7016804","DOIUrl":null,"url":null,"abstract":"<jats:p>In the current study, we studied a <jats:inline-formula>\n <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M2\">\n <mi>f</mi>\n <mfenced open=\"(\" close=\")\" separators=\"|\">\n <mrow>\n <mi>Q</mi>\n </mrow>\n </mfenced>\n </math>\n </jats:inline-formula>-gravitational, anisotropic, locally rotationally symmetric (LRS), Bianchi type-I spacetime universe. We have adopted the freely chosen function <jats:inline-formula>\n <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M3\">\n <mi>f</mi>\n <mfenced open=\"(\" close=\")\" separators=\"|\">\n <mrow>\n <mi>Q</mi>\n </mrow>\n </mfenced>\n <mo>=</mo>\n <mi>Q</mi>\n <mo>+</mo>\n <mi>α</mi>\n <msqrt>\n <mi>Q</mi>\n </msqrt>\n </math>\n </jats:inline-formula>, where <jats:inline-formula>\n <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M4\">\n <mi>α</mi>\n </math>\n </jats:inline-formula> is a model-free parameter. We assumed that the universe is filled with dusty string fluid and that the shear scalar (<jats:inline-formula>\n <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M5\">\n <mi>σ</mi>\n </math>\n </jats:inline-formula>) and the expansion scalar (<jats:inline-formula>\n <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M6\">\n <mi>θ</mi>\n </math>\n </jats:inline-formula>) are proportional to each other in order to solve field equations for the average Hubble parameter (<jats:inline-formula>\n <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M7\">\n <mi>H</mi>\n </math>\n </jats:inline-formula>). The resultant Hubble function has been fitted with observational datasets <jats:inline-formula>\n <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M8\">\n <mi>H</mi>\n <mfenced open=\"(\" close=\")\" separators=\"|\">\n <mrow>\n <mi>z</mi>\n </mrow>\n </mfenced>\n </math>\n </jats:inline-formula> and SNe Ia datasets of apparent magnitude <jats:inline-formula>\n <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M9\">\n <mi>m</mi>\n <mfenced open=\"(\" close=\")\" separators=\"|\">\n <mrow>\n <mi>z</mi>\n </mrow>\n </mfenced>\n </math>\n </jats:inline-formula> in order to obtain the best fit values for the cosmological parameters. Utilizing these best fit values throughout the analysis, many cosmic phenomena are examined. We have investigated cosmographic coefficients such as <jats:inline-formula>\n <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M10\">\n <mi>H</mi>\n <mo>,</mo>\n <mi>q</mi>\n <mo>,</mo>\n <mi>j</mi>\n <mo>,</mo>\n <mi mathvariant=\"normal\">a</mi>\n <mi mathvariant=\"normal\">n</mi>\n <mi mathvariant=\"normal\">d</mi>\n <mtext> </mtext>\n <mi>s</mi>\n </math>\n </jats:inline-formula> to see if an accelerated transit phase dark energy model of the cosmos exists. Also, we have classified the dark energy models that are explored using Om diagnostic analysis; our universe model is a quintessential dark energy model. The age of the universe as it exists right now has been roughly calculated by the model.</jats:p>","PeriodicalId":43667,"journal":{"name":"Muenster Journal of Mathematics","volume":null,"pages":null},"PeriodicalIF":0.7000,"publicationDate":"2023-06-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"Muenster Journal of Mathematics","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.1155/2023/7016804","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q2","JCRName":"MATHEMATICS","Score":null,"Total":0} 引用次数: 0 引用 批量引用 Abstract In the current study, we studied a f Q -gravitational, anisotropic, locally rotationally symmetric (LRS), Bianchi type-I spacetime universe. We have adopted the freely chosen function f Q = Q + α Q , where α is a model-free parameter. We assumed that the universe is filled with dusty string fluid and that the shear scalar ( σ ) and the expansion scalar ( θ ) are proportional to each other in order to solve field equations for the average Hubble parameter ( H ). The resultant Hubble function has been fitted with observational datasets H z and SNe Ia datasets of apparent magnitude m z in order to obtain the best fit values for the cosmological parameters. Utilizing these best fit values throughout the analysis, many cosmic phenomena are examined. We have investigated cosmographic coefficients such as H , q , j , a n d s to see if an accelerated transit phase dark energy model of the cosmos exists. Also, we have classified the dark energy models that are explored using Om diagnostic analysis; our universe model is a quintessential dark energy model. The age of the universe as it exists right now has been roughly calculated by the model. 分享 查看原文 本刊更多论文 fq 在本研究中，我们研究了一个fq -引力、各向异性、局部旋转对称(LRS)、Bianchi - i型时空宇宙。我们采用自由选择的函数f Q = Q + α Q，其中α是无模型参数。为了求解平均哈勃参数H的场方程，我们假设宇宙充满了尘埃弦流体，并且剪切标量(σ)和膨胀标量(θ)彼此成正比。所得的哈勃函数用观测数据集H z和视星等m z的超新星Ia数据集进行了拟合以获得宇宙学参数的最佳拟合值。在整个分析过程中利用这些最佳拟合值，对许多宇宙现象进行了检验。我们已经研究了宇宙系数，如H, q, j, a和s，看看是否存在宇宙的加速过渡阶段暗能量模型。此外，我们还对使用Om诊断分析探索的暗能量模型进行了分类;我们的宇宙模型是一个典型的暗能量模型。现在宇宙的年龄已经被这个模型粗略地计算出来了。 本文章由计算机程序翻译，如有差异，请以英文原文为准。 求助全文 约1分钟内获得全文 求助全文 来源期刊 Muenster Journal of Mathematics MATHEMATICS- 自引率 0.00% 发文量 0 相关文献 × 引用 GB/T 7714-2015 复制 MLA 复制 APA 复制 导出至 BibTeX EndNote RefMan NoteFirst NoteExpress × 求助内容： 期刊论文 学位论文 图书 其他 (专利、报告等) 只需要正文 仅需补充材料 应助结果提醒方式： 微信（请自行确认已关注Book学术公众号） 邮件 保存 保存后同步修改账户信息中的邮箱 确认发布求助 × 处理提示 您的部分求助已有人上传文件，您还尚未处理，请先处理完毕再发起新的求助 点击查看 × 努力提交中 提交成功 继续求助查看详情 × 提示 您的信息不完整，为了账户安全，请先补充。 现在去补充 × 没积分了 多种获得积分方式，供你选择！ 查看如何获取积分 × 提示 您因"违规操作" 具体请查看互助需知 我知道了 × 提示 现在去查看 取消 × 提示 确定 × 快捷登录 密码登录 用户名： 密码： 验证码： 两周内记住我 忘记密码？ 手机号： 验证码： 没有帐号？现在注册 请完成安全验证× 微信好友 朋友圈 QQ好友 复制链接 取消 已复制链接 快去分享给好友吧! 我知道了 点击右上角分享 0 $(function () { var title = $("#title").val(); var id = $("#id").val(); $.post("/Literature/GetRelatedLiterature", { id: id, title: title }, function (result) { if (result != null) { var html = ``; for (var i = 0; i < result.length; i++) { html += `<div class="sslist">`; html += `<a class="caption" href="` + $("#url1").val() + result[i].ArticleID + `.htm">` + result[i].Title + `</a>`; html += ` <div class="substance">`; html += `<span class="IF">IF ` + result[i].PeriodicalIF + ` </span>`; if (result[i].RegionNum > 0) { html += `<span class="fq` + result[i].RegionNum + `">` + result[i].RegionNum + `区 ` + result[i].RegionCategory + `</span>`; } //var EmployDataBaseShoreName = result[i].EmployDataBaseShoreName; //if (EmployDataBaseShoreName != "" && EmployDataBaseShoreName!=null) { // var names = EmployDataBaseShoreName.split('||') // for (var j = 0; j < names.length; j++) { // html += `<span class="fq5">` + names[j] + `</span>`; // } //} //html += ``; html += `</div>`; html += `<div class="substance">`; html += `<a href="` + $("#url2").val() + "_d" + result[i].PeriodicalID + `.htm" target="_blank">` + result[i].PeriodicalName + `</a>`; html += `<span class="Pub">Pub Date : ` + result[i].PublishDate + `</span>`; html += `</div>`; html += ` <div class="author">`; html += result[i].AuthorName; html += `</div>`; html += `</div>`; } if (html.length > 0) { $("#xglist").show(); $("#xglist").append(html); } } }); getReferenceCount(); }); function getReferenceCount() { var LocalId = localStorage.getItem("referenceName"); if (LocalId != null) { $.get("/Literature/GetBatchReferenceCountByLocalId", { LocalId: LocalId }, function (result) { $("#referencecount").html(result.Code); }, "json"); } else { $("#referencecount").html('0'); } } wx.config({ debug: false, appId: 'wx999b2eb01732df2e', timestamp: '1730904052', nonceStr: 'ka3Xw7Be4t7OTic1', signature: 'b408360e746609f9a9d8a0dfcfa45f067c1b842a', jsApiList: [ 'onMenuShareTimeline', 'onMenuShareAppMessage', 'hideMenuItems' ] });

Abstract

In the current study, we studied a $f\left(Q\right)$ -gravitational, anisotropic, locally rotationally symmetric (LRS), Bianchi type-I spacetime universe. We have adopted the freely chosen function $f\left(Q\right)=Q+\alpha \sqrt{Q}$ , where $\alpha$ is a model-free parameter. We assumed that the universe is filled with dusty string fluid and that the shear scalar ( $\sigma$ ) and the expansion scalar ( $\theta$ ) are proportional to each other in order to solve field equations for the average Hubble parameter ( $H$ ). The resultant Hubble function has been fitted with observational datasets $H\left(z\right)$ and SNe Ia datasets of apparent magnitude $m\left(z\right)$ in order to obtain the best fit values for the cosmological parameters. Utilizing these best fit values throughout the analysis, many cosmic phenomena are examined. We have investigated cosmographic coefficients such as $H,q,j,\mathrm{a}\mathrm{n}\mathrm{d}s$ to see if an accelerated transit phase dark energy model of the cosmos exists. Also, we have classified the dark energy models that are explored using Om diagnostic analysis; our universe model is a quintessential dark energy model. The age of the universe as it exists right now has been roughly calculated by the model.