001445687 000__ 05127cam\a2200553Ii\4500
001445687 001__ 1445687
001445687 003__ OCoLC
001445687 005__ 20230310003844.0
001445687 006__ m\\\\\o\\d\\\\\\\\
001445687 007__ cr\un\nnnunnun
001445687 008__ 220402s2022\\\\gw\\\\\\ob\\\\000\0\eng\d
001445687 019__ $$a1306525856$$a1308394882$$a1308796914$$a1310338913
001445687 020__ $$a9783658368418$$q(electronic bk.)
001445687 020__ $$a3658368411$$q(electronic bk.)
001445687 020__ $$z3658368403
001445687 020__ $$z9783658368401
001445687 0247_ $$a10.1007/978-3-658-36841-8$$2doi
001445687 035__ $$aSP(OCoLC)1309038285
001445687 040__ $$aEBLCP$$beng$$erda$$epn$$cEBLCP$$dGW5XE$$dGZM$$dOCLCO$$dYDX$$dOCLCF$$dUKAHL$$dOCLCQ
001445687 049__ $$aISEA
001445687 050_4 $$aQB812
001445687 08204 $$a523.8/874$$223
001445687 1001_ $$aManoharan, Praveen.
001445687 24510 $$aUniversal relations for binary neutron star mergers with long-lived remnants /$$cPraveen Manoharan.
001445687 264_1 $$aWiesbaden :$$bSpringer Spektrum,$$c2022.
001445687 300__ $$a1 online resource (77 pages).
001445687 336__ $$atext$$btxt$$2rdacontent
001445687 337__ $$acomputer$$bc$$2rdamedia
001445687 338__ $$aonline resource$$bcr$$2rdacarrier
001445687 4901_ $$aBestMasters
001445687 504__ $$aIncludes bibliographical references.
001445687 5050_ $$aIntro -- Abstract -- Contents -- Abbreviations & Notation -- List of Figures -- List of Tables -- 1 Introduction -- 1.1 Problem Statement -- 1.2 Outline -- 2 Related Work -- 2.1 Neutron Star Oscillation Modes -- 2.1.1 Non-rotating Neutron Stars -- 2.1.2 Rotating Neutron Stars -- 2.2 Tidal Deformability -- 2.2.1 Relations Between Tidal Deformability and Oscillation Modes -- 2.3 Other Universal Relations -- 2.4 Binary Neutron Stars -- 2.4.1 Binary Love Relations -- 2.4.2 Effective Tidal Deformability and Chirp Mass -- 2.4.3 Tidal Coupling Constant -- 2.4.4 High Resolution Simulations
001445687 5058_ $$a2.5 Discussion -- 3 Theory -- 3.1 Neutron Star Equilibrium Model and TOV Equations -- 3.2 Neutron Star Bulk Properties -- 3.3 Tidal Deformability of Neutron Stars -- 3.3.1 The Tidal Love Number -- 3.3.2 Computing the Tidal Love Number -- 3.3.3 Binary Tidal Deformability -- 3.4 Quasi-normal Modes of Neutron Stars -- 3.4.1 Quasi-normal modes of Rotating Neutron Stars -- 3.5 Goodness of Fit and Error Estimates -- 4 Methodology -- 4.1 Data Set of Rotating Neutron Stars -- 4.2 Relating Tidal Deformability to f-mode Frequency -- 4.3 Binary Neutron Star Mergers -- 4.3.1 Post-merger Remnant -- 5 Results
001445687 5058_ $$a5.1 Revisiting Existing Universal Relations -- 5.2 Universal Relations for Single Neutron Stars -- 5.3 f-mode Relations for BNS Mergers -- 5.3.1 Co-rotating f-mode -- 5.3.2 Counter-rotating f-mode -- 5.4 Combined eta Relation for BNS Mergers -- 5.5 Direct eta Relation for BNS Mergers -- 5.5.1 Direction Relation with soft EoSs -- 5.5.2 Reintroducing stiff EoSs -- 5.6 Direct Relation with Constraints -- 6 Discussion & Conclusion -- 6.1 Future Directions -- A Bibliography
001445687 506__ $$aAccess limited to authorized users.
001445687 520__ $$aIn the last 25 years, an extensive body of work has developed various equation of state independent - or (approximately) universal - relations that allow for the inference of neutron star parameters from gravitational wave observations. These works, however, have mostly been focused on singular neutron stars, while our observational efforts at the present, and in the near future, will be focused on binary neutron star (BNS) mergers. In light of these circumstances, the last five years have also given rise to more attempts at developing universal relations that relate BNS pre-merger neutron stars to stellar parameters of the post-merger object, mostly driven by numerical relativity simulations. In this thesis a first attempt at perturbatively deriving universal relations for binary neutron star mergers with long-lived neutron star remnants is presented. The author succeeds in confirming previous results relating pre-merger binary tidal deformabilities to the f-mode frequency of the post-merger object. Combining this result with recent advances of computing the f-mode frequency of fast rotating neutron stars, he also derives a combined relation that relates the pre-merger binary tidal deformability of a BNS to the effective compactness of a long-lived neutron star remnant. Finally, he also proposes a direct relation between these quantities with improved accuracy. About the author Praveen Manoharan is PhD student at Tubingen University, Institute for Theoretical Astrophysics.
001445687 588__ $$aOnline resource; title from PDF title page (SpringerLink, viewed April 11, 2022).
001445687 650_0 $$aStellar mergers.
001445687 650_0 $$aNeutron stars.
001445687 650_6 $$aÉtoiles à neutrons.
001445687 655_0 $$aElectronic books.
001445687 77608 $$iPrint version:$$aManoharan, Praveen$$tUniversal Relations for Binary Neutron Star Mergers with Long-Lived Remnants$$dWiesbaden : Springer Fachmedien Wiesbaden GmbH,c2022$$z9783658368401
001445687 830_0 $$aBestMasters.
001445687 852__ $$bebk
001445687 85640 $$3Springer Nature$$uhttps://univsouthin.idm.oclc.org/login?url=https://link.springer.com/10.1007/978-3-658-36841-8$$zOnline Access$$91397441.1
001445687 909CO $$ooai:library.usi.edu:1445687$$pGLOBAL_SET
001445687 980__ $$aBIB
001445687 980__ $$aEBOOK
001445687 982__ $$aEbook
001445687 983__ $$aOnline
001445687 994__ $$a92$$bISE