星形平衡：从BNG到TOV

IF 4.8 2区物理与天体物理 Q2 PHYSICS, PARTICLES & FIELDS

The European Physical Journal C Pub Date : 2025-04-15 DOI:10.1140/epjc/s10052-025-14095-z

Roberto Casadio, Octavian Micu

{"title":"星形平衡：从BNG到TOV","authors":"Roberto Casadio, Octavian Micu","doi":"10.1140/epjc/s10052-025-14095-z","DOIUrl":null,"url":null,"abstract":"<div><p>We study the role of the equilibrium equation in bootstrapped Newtonian gravity (BNG) by including terms inspired by the post-Newtonian expansion of the Tolman–Oppenheimer–Volkov (TOV) equation. We then compare (approximate) BNG solutions for homogenous stars with their Newtonian and General Relativistic exact solutions. Regardless of the additional terms from the conservation equation, BNG stars do not exhibit a Buchdahl limit. However, specific extra terms added to this equation can cause the pressure to become negative inside stars with compactness smaller than the critical values for BNG black hole formation.\n</p></div>","PeriodicalId":788,"journal":{"name":"The European Physical Journal C","volume":"85 4","pages":""},"PeriodicalIF":4.8000,"publicationDate":"2025-04-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1140/epjc/s10052-025-14095-z.pdf","citationCount":"0","resultStr":"{\"title\":\"Star equilibrium: from BNG to TOV\",\"authors\":\"Roberto Casadio, Octavian Micu\",\"doi\":\"10.1140/epjc/s10052-025-14095-z\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"<div><p>We study the role of the equilibrium equation in bootstrapped Newtonian gravity (BNG) by including terms inspired by the post-Newtonian expansion of the Tolman–Oppenheimer–Volkov (TOV) equation. We then compare (approximate) BNG solutions for homogenous stars with their Newtonian and General Relativistic exact solutions. Regardless of the additional terms from the conservation equation, BNG stars do not exhibit a Buchdahl limit. However, specific extra terms added to this equation can cause the pressure to become negative inside stars with compactness smaller than the critical values for BNG black hole formation.\\n</p></div>\",\"PeriodicalId\":788,\"journal\":{\"name\":\"The European Physical Journal C\",\"volume\":\"85 4\",\"pages\":\"\"},\"PeriodicalIF\":4.8000,\"publicationDate\":\"2025-04-15\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"https://link.springer.com/content/pdf/10.1140/epjc/s10052-025-14095-z.pdf\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"The European Physical Journal C\",\"FirstCategoryId\":\"4\",\"ListUrlMain\":\"https://link.springer.com/article/10.1140/epjc/s10052-025-14095-z\",\"RegionNum\":2,\"RegionCategory\":\"物理与天体物理\",\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"Q2\",\"JCRName\":\"PHYSICS, PARTICLES & FIELDS\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"The European Physical Journal C","FirstCategoryId":"4","ListUrlMain":"https://link.springer.com/article/10.1140/epjc/s10052-025-14095-z","RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q2","JCRName":"PHYSICS, PARTICLES & FIELDS","Score":null,"Total":0}

引用次数: 0

摘要

我们通过引入受托尔曼-奥本海默-沃尔科夫（TOV）方程后牛顿展开启发的项，研究了平衡方程在自举牛顿引力（BNG）中的作用。然后，我们将齐次恒星的（近似）BNG解与其牛顿和广义相对论精确解进行比较。不考虑守恒方程中的附加项，BNG星不存在布赫达尔极限。然而，在这个方程中加入特定的额外项可能会导致恒星内部的压力变为负，而致密度小于BNG黑洞形成的临界值。

本文章由计算机程序翻译，如有差异，请以英文原文为准。

查看原文本刊更多论文

Star equilibrium: from BNG to TOV

We study the role of the equilibrium equation in bootstrapped Newtonian gravity (BNG) by including terms inspired by the post-Newtonian expansion of the Tolman–Oppenheimer–Volkov (TOV) equation. We then compare (approximate) BNG solutions for homogenous stars with their Newtonian and General Relativistic exact solutions. Regardless of the additional terms from the conservation equation, BNG stars do not exhibit a Buchdahl limit. However, specific extra terms added to this equation can cause the pressure to become negative inside stars with compactness smaller than the critical values for BNG black hole formation.

求助全文

通过发布文献求助，成功后即可免费获取论文全文。去求助

来源期刊

The European Physical Journal C 物理-物理：粒子与场物理

CiteScore

8.10

自引率

15.90%

发文量

1008

审稿时长

2-4 weeks

期刊介绍： Experimental Physics I: Accelerator Based High-Energy Physics Hadron and lepton collider physics Lepton-nucleon scattering High-energy nuclear reactions Standard model precision tests Search for new physics beyond the standard model Heavy flavour physics Neutrino properties Particle detector developments Computational methods and analysis tools Experimental Physics II: Astroparticle Physics Dark matter searches High-energy cosmic rays Double beta decay Long baseline neutrino experiments Neutrino astronomy Axions and other weakly interacting light particles Gravitational waves and observational cosmology Particle detector developments Computational methods and analysis tools Theoretical Physics I: Phenomenology of the Standard Model and Beyond Electroweak interactions Quantum chromo dynamics Heavy quark physics and quark flavour mixing Neutrino physics Phenomenology of astro- and cosmoparticle physics Meson spectroscopy and non-perturbative QCD Low-energy effective field theories Lattice field theory High temperature QCD and heavy ion physics Phenomenology of supersymmetric extensions of the SM Phenomenology of non-supersymmetric extensions of the SM Model building and alternative models of electroweak symmetry breaking Flavour physics beyond the SM Computational algorithms and tools...etc.