What does this research mean for the field?

Using low-mass X-ray binaries (LMXB) timing observations and NICER mass-radius constraints, the shear and bulk viscous dissipation time scales for r-mode damping in hybrid stars can be estimated, which in turn determine the minima of the star's rotation frequency. Novelty: ClaimNovelty.INCREMENTAL. Consensus alignment: ConsensusAlignment.NEUTRAL.

What question did this study set out to answer?

To model the dissipative dynamics of r-mode oscillations in hybrid stars with mixed hadronic and quark matter and estimate the associated viscous dissipation timescales.

September 14, 2026The European Physical Journal COpen Access

Modelling dissipative dynamics of r-mode instability in hybrid stars

View Full Paper

Ask AI

Bookmark

Authors

KZKhushbu Zala SSSreemoyee Sarkar

Discussion

Member takes

Overview

Bayesian modeling reveals viscous dissipation timescales in hybrid stars, suggesting rotation frequency limits for compact objects.

Key Points

To model the dissipative dynamics of r-mode oscillations in hybrid stars with mixed hadronic and quark matter and estimate the associated viscous dissipation timescales.
Applied a Bayesian inference framework to a two-layer hybrid star model incorporating a mixed phase of hadronic and quark matter.
Constrained viscous damping parameters using observational timing data from low-mass X-ray binaries (LMXBs) alongside mass-radius measurements from the NICER mission.
Estimated shear viscous dissipation timescale at τ_s = (4.99 +0.49/-0.52) × 10^8 T^(5/3) s.
Estimated bulk viscous dissipation timescale at τ_B = (2.150 +1.23/-0.60) × 10^19 (T^4 10^-12 + T^2 10^-6)^(-1) Ω^(-2) s.
Derived rotation frequency minima of Ω = 451.87 Hz at T = 0.259 MeV for a 1.5 M_⊙ star, and Ω = 517.47 Hz at T = 0.234 MeV for a 1.75 M_⊙ star.

Cite This Study

Zala et al. (2026) studied this question.

synapsesocial.com/papers/6aa7b23b0926e14a848b0a06 https://doi.org/10.1140/epjc/s10052-026-16199-6

View Full Paper

Ask AI

Bookmark

September 14, 2026The European Physical Journal COpen Access

Modelling dissipative dynamics of r-mode instability in hybrid stars

View Full Paper

Ask AI

Bookmark

Authors

KZKhushbu Zala SSSreemoyee Sarkar

Discussion

Member takes

Overview

Bayesian modeling reveals viscous dissipation timescales in hybrid stars, suggesting rotation frequency limits for compact objects.

Key Points

To model the dissipative dynamics of r-mode oscillations in hybrid stars with mixed hadronic and quark matter and estimate the associated viscous dissipation timescales.
Applied a Bayesian inference framework to a two-layer hybrid star model incorporating a mixed phase of hadronic and quark matter.
Constrained viscous damping parameters using observational timing data from low-mass X-ray binaries (LMXBs) alongside mass-radius measurements from the NICER mission.
Estimated shear viscous dissipation timescale at τ_s = (4.99 +0.49/-0.52) × 10^8 T^(5/3) s.
Estimated bulk viscous dissipation timescale at τ_B = (2.150 +1.23/-0.60) × 10^19 (T^4 10^-12 + T^2 10^-6)^(-1) Ω^(-2) s.
Derived rotation frequency minima of Ω = 451.87 Hz at T = 0.259 MeV for a 1.5 M_⊙ star, and Ω = 517.47 Hz at T = 0.234 MeV for a 1.75 M_⊙ star.

Cite This Study

Zala et al. (2026) studied this question.

synapsesocial.com/papers/6aa7b23b0926e14a848b0a06 https://doi.org/10.1140/epjc/s10052-026-16199-6

Also Consider

Synapse has enriched 5 closely related papers on similar clinical questions. Consider them for comparative context:

View Full Paper

Ask AI

Bookmark