Millisecond radio pulsars with known masses: Parameter values and equation of state models |
| |
| Institution: | 1. Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Mumbai 400005, India;2. Dipartimento di Fisica, Università di Pisa, Largo B. Pontecorvo, 3 I-56127 Pisa, Italy;3. INFN, Sezione di Pisa, Largo B. Pontecorvo, 3 I-56127 Pisa, Italy;4. Astroparticle Physics and Cosmology Division, Saha Institute of Nuclear Physics, HBNI, 1 / AF Bidhannagar, Kolkata-700064, India;5. Department of Physics, St. Joseph’s College, 36 Lalbagh Road, Bangalore 560027, India;6. Inter-University Centre for Astronomy and Astrophysics (IUCAA), Post Bag 4, Ganeshkhind, Savitribai Phule Pune University, Campus, Pune 411007, India;1. Yunnan Observatories, Chinese Academy of Sciences, P.O. Box 110, Kunming 650216, PR China;2. Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, PR China;3. Graduate University of Chinese Academy of Sciences, Beijing, PR China;4. Department of Theoretical Physics and Astrophysics, Masaryk University, Kotlár̆ská 2, Brno 611 37, Czech Republic;1. Department of Telematics Engineering, Universitat Politècnica de Catalunya (UPC), E-08034, Barcelona, Spain;2. Centre Tecnològic de Telecomunicacions de Catalunya (CTTC), E-08860, Castelldefels, Barcelona, Spain;3. Scytl Secure Electronic Voting, E-08006, Barcelona, Spain |
| |
| Abstract: | The recent fast growth of a population of millisecond pulsars with precisely measured mass provides an excellent opportunity to characterize these compact stars at an unprecedented level. This is because the stellar parameter values can be accurately computed for known mass and spin rate and an assumed equation of state (EoS) model. For each of the 16 such pulsars and for a set of EoS models from nucleonic, hyperonic, strange quark matter and hybrid classes, we numerically compute fast spinning stable stellar parameter values considering the full effect of general relativity. This first detailed catalogue of the computed parameter values of observed millisecond pulsars provides a testbed to probe the physics of compact stars, including their formation, evolution and EoS. We estimate uncertainties on these computed values from the uncertainty of the measured mass, which could be useful to quantitatively constrain EoS models. We note that the largest value of the central density ρc in our catalogue is ∼5.8 times the nuclear saturation density ρsat, which is much less than the expected maximum value 13ρsat. We argue that the ρc-values of at most a small fraction of compact stars could be much larger than 5.8ρsat. Besides, we find that the constraints on EoS models from accurate radius measurements could be significantly biased for some of our pulsars, if stellar spinning configurations are not used to compute the theoretical radius values. |
| |
| Keywords: | |
| 本文献已被 ScienceDirect 等数据库收录！ |
|
