التفاصيل البيبلوغرافية
| العنوان: |
Constraining the Dense Matter Equation of State with New NICER Mass–Radius Measurements and New Chiral Effective Field Theory Inputs |
| المؤلفون: |
Rutherford, N., Mendes , M., Svensson , I., Schwenk, A., Watts, A., Hebeler, K., Keller, J., Prescod-Weinstein, C., Choudhury , D., Raaijmakers, G., Salmi, T., Timmerman, P., Vinciguerra, S., Guillot, S., Lattimer, J. |
| المصدر: |
The Astrophysical Journal Letters |
| سنة النشر: |
2024 |
| المجموعة: |
Max Planck Society: MPG.PuRe |
| مصطلحات موضوعية: |
Starke Wechselwirkung und exotische Kerne – Abteilung Blaum |
| الوصف: |
Pulse profile modeling of X-ray data from the Neutron Star Interior Composition Explorer is now enabling precision inference of neutron star mass and radius. Combined with nuclear physics constraints from chiral effective field theory ( X EFT), and masses and tidal deformabilities inferred from gravitational-wave detections of binary neutron star mergers, this has led to a steady improvement in our understanding of the dense matter equation of state (EOS). Here, we consider the impact of several new results: the radius measurement for the 1.42 M ☉ pulsar PSR J0437−4715 presented by Choudhury et al., updates to the masses and radii of PSR J0740+6620 and PSR J0030+0451, and new X EFT results for neutron star matter up to 1.5 times nuclear saturation density. Using two different high-density EOS extensions—a piecewise-polytropic (PP) model and a model based on the speed of sound in a neutron star (CS)—we find the radius of a 1.4 M ☉ (2.0 M ☉ ) neutron star to be constrained to the 95% credible ranges 12.28 -0.76 +0.50 km (12.33 -1.34 +0.70 km) for the PP model and 12.01 -0.75 +0.56 km (11.55 -1.09 +0.94 km) for the CS model. The maximum neutron star mass is predicted to be 2.15 -0.16 +0.14 M ☉ and 2.08 -0.16 +0.28 M ☉ for the PP and CS models, respectively. We explore the sensitivity of our results to different orders and different densities up to which X EFT is used, and show how the astrophysical observations provide constraints for the pressure at intermediate densities. Moreover, we investigate the difference R 2.0 − R 1.4 of the radius of 2 M ☉ and 1.4 M ☉ neutron stars within our EOS inference. |
| نوع الوثيقة: |
article in journal/newspaper |
| اللغة: |
unknown |
| Relation: |
http://hdl.handle.net/21.11116/0000-000F-B326-C |
| الاتاحة: |
http://hdl.handle.net/21.11116/0000-000F-B326-C |
| رقم الانضمام: |
edsbas.F99D9B97 |
| قاعدة البيانات: |
BASE |