works on

From the 1 of 8 linked papers with an AI index.

activity
20242026
collaborators

8 papers

nucl-th2026

The petit four of color-superconducting phases in proto-neutron star evolution

Selina Kunkel, Ishfaq Ahmad Rather, Hosein Gholami +2

The paper studies how color‑superconducting phases may appear and evolve in proto‑neutron stars, tracking the star’s transition from a hot, neutrino‑trapped state to a cold, neutri…

nucl-th2026

Studying the QCD Matter produced in Heavy-Ion Collisions using the MUSES Calculation Engine

Johannes Jahan, Kevin P. Pala, Yumu Yang +42

The equation of state of hot and dense matter is essential for describing heavy-ion collisions at all collision energies. Here, we explore the capabilities of the latest version of…

astro-ph.HE2025

A finite temperature framework for quark matter with color-superconducting phases

Hosein Gholami, Marco Hofmann, Débora Mroczek +1

Current observations of neutron stars and measurements of gravitational waves only provide constraints on the zero temperature () equation of state (EoS) of dense matter. The…

nucl-th2025

Neutrino absorption in two-flavor color-superconducting quark matter

Mark G. Alford, Liam Brodie, Michael Buballa +3

We calculate the absorption mean free paths of electron and muon neutrinos in two-flavor color-superconducting (2SC) quark matter in the density and temperature range that is relev…

hep-ph2025

Removing cutoff artifacts in the NJL model by a Renormalization Group consistent treatment

Hosein Gholami, Marco Hofmann, Michael Buballa

We summarize how a renormalization-group (RG)-consistent treatment removes well-known artifacts in NJL-model descriptions of color-superconducting quark matter. We introduce two RG…

astro-ph.HE2025

Comprehensive Analysis of Constructing Hybrid Stars with an RG-consistent NJL Model

Jan-Erik Christian, Ishfaq Ahmad Rather, Hosein Gholami +1

In this work, we investigate the properties of hadronic and quark matter that would allow for a first order phase transition between them within neutron stars. To this end, we use…