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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

Probing Elastic Quark Phases in Hybrid Stars with Radius Measurements

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Pereira, Jonas P. [1] ; Bejger, Michal [1] ; Tonetto, Lucas [2, 3, 4] ; Lugones, German [2] ; Haensel, Pawel [1] ; Zdunik, Julian Leszek [1] ; Sieniawska, Magdalena [5]
Total Authors: 7
[1] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw - Poland
[2] Univ Fed ABC, Ctr Ciencias Nat & Humanas, Ave Estados 5001, BR-09210580 Santo Andre, SP - Brazil
[3] Sapienza Univ Roma, Dipartimento Fis, PA Moro 5, I-00185 Rome - Italy
[4] Sez INFN Roma1, PA Moro 5, I-00185 Rome - Italy
[5] Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw - Poland
Total Affiliations: 5
Document type: Journal article
Source: ASTROPHYSICAL JOURNAL; v. 910, n. 2 APR 2021.
Web of Science Citations: 0

The internal composition of neutron stars is currently largely unknown. Due to the possibility of phase transitions in quantum chromodynamics, stars could be hybrid and have quark cores. We investigate some imprints of elastic quark phases (only when perturbed) on the dynamical stability of hybrid stars. We show that they increase the dynamical stability window of hybrid stars in the sense that the onset of instabilities happens at larger central densities than the ones for maximum masses. In particular, when the shear modulus of a crystalline quark phase is taken at face value, the relative radius differences between elastic and perfect-fluid hybrid stars with null radial frequencies (onset of instability) would be up to 1%-2%. Roughly, this would imply a maximum relative radius dispersion (on top of the perfect-fluid predictions) of 2%-4% for stars in a given mass range exclusively due to the elasticity of the quark phase. In the more agnostic approach where the estimates for the quark shear modulus only suggest its possible order of magnitude (due to the many approximations taken in its calculation), the relative radius dispersion uniquely due to a quark phase elasticity might be as large as 5%-10%. Finally, we discuss possible implications of the above dispersion of radii for the constraint of the elasticity of a quark phase with electromagnetic missions such as NICER, eXTP, and ATHENA. (AU)

FAPESP's process: 18/04281-8 - Compact star oscillations in the gravitational wave era
Grantee:Lucas Tonetto Coimbra
Support type: Scholarships in Brazil - Master
FAPESP's process: 17/21384-2 - Asteroseismology of quasi-periodic oscillations and constraints to hybrid neutron star models
Grantee:Jonas Pedro Pereira
Support type: Scholarships abroad - Research Internship - Post-doctor
FAPESP's process: 19/15124-3 - Linking the dense matter equation of state with quasi-normal modes of compact stars
Grantee:Lucas Tonetto Coimbra
Support type: Scholarships abroad - Research Internship - Master's degree
FAPESP's process: 15/04174-9 - Some consequences of the microphysics of volumes and surfaces in compact systems
Grantee:Jonas Pedro Pereira
Support type: Scholarships in Brazil - Post-Doctorate