Statistical Analysis of Neutron Star Cooling: Implications for the Nuclear Equation of State and Nucleon Pairing
Year: 2026
Type: preprint
Abstract: This dataset contains the theoretical neutron star (NS) cooling curves generated with the public code NSCool (Page 2016) that underlie the statistical analysis presented in Ávila, Ferreira & Sagun, "Statistical Analysis of Neutron Star Cooling: Implications for the Nuclear Equation of State and Nucleon Pairing" (2026). Cooling curves (redshifted photon luminosity as a function of stellar age) were computed for five purely nucleonic equations of state (EoS): APR4: Akmal, Pandharipande & Ravenhall (1998) IST: Induced Surface Tension EoS, Set B (Sagun et al. 2019, 2020) FSU2R: Tolos et al. (2017) DD2: Typel et al. (2010) NL3ωρ: Horowitz & Piekarewicz (2001); Pais & Providência (2016) For each EoS, curves were generated over a grid of gravitational masses (0.10 M☉ steps, up to ~2.00 MSun for APR4/FSU2R/IST and up to ~2.40–2.60 MSun for DD2/NL3ωρ) and envelope compositions (parametrized by η = ΔM/M), combined with different neutron-singlet (¹S₀), proton-singlet (¹S₀), and neutron-triplet (³P₂) pairing gap models following the modified-Gaussian parametrization of Yanagi (2019) (see Table 2 and Section 2.3 of the paper). File structure The data are organized into two archives, each containing one subfolder per EoS (APR, IST, F2R = FSU2R, DD2, NL3wr = NL3ωρ): Pairings_Singlets.zip — Cooling curves for unpaired matter (0-0-0) and for models with only singlet-channel pairing: neutron ¹S₀ pairing alone, or neutron ¹S₀ combined with proton ¹S₀ pairing. Pairings_Triplets.zip — Cooling curves with neutron ³P₂ (triplet) pairing always active, combined with the two extrema singlet models (in each of the neutron ¹S₀ and proton ¹S₀ channels) tested alongside triplet pairing. Each file is named Teff_<EOS>_Cat_<Mass>Msun_<i-j-k>_ETA<xx>.dat, where i-j-k encodes the neutron singlet, neutron triplet, and proton singlet pairing model (using NSCool's internal superfluidity codes), and ETA<xx> gives the envelope composition (η = 10E-{xx}). A full key to the naming convention and the file's data columns is provided in the accompanying README. Full details on the pairing gap parametrization, the mass/envelope grids sampled per EoS, and the physical motivation for the model selection are given in the paper (Sections 2.2–3.2 and Table 2). Citation If you use this dataset, please cite: Ávila, A., Ferreira, R. Z., & Sagun, V. (2026), Statistical Analysis of Neutron Star Cooling: Implications for the Nuclear Equation of State and Nucleon Pairing.
Source: arXiv (Cornell University)
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: green
OpenAlex ID: W7222928759