Özel, Feryal и др. On the Mass Distribution and Birth Masses of Neutron Stars // The Astrophysical Journal 757 (1). септември 2012. DOI:10.1088/0004-637X/757/1/55. с. 13.
Chamel, N. и др. On the Maximum Mass of Neutron Stars // International Journal of Modern Physics 1 (28). 19 ноември 2013. DOI:10.1142/S021830131330018X. с. 1330018.
Ozel, Feryal и др. Masses, Radii, and the Equation of State of Neutron Stars // Annu. Rev. Astron. Astrophys. 54 (1). 2016. DOI:10.1146/annurev-astro-081915-023322. с. 401 – 440.
Kaspi, V. M. и др. (Anomalous) X-ray Pulsars // Nuclear Physics B: Proceedings Supplements 132. 2004. DOI:10.1016/j.nuclphysbps.2004.04.080. с. 456 – 465.
Hessels, Jason W. T и др. Neutron Star Structure and the Equation of State // The Astrophysical Journal 550 (426). 2001. DOI:10.1086/319702. с. 426 – 442.
Pons, José A. и др. Too much „pasta“ for pulsars to spin down // Nature Physics 9 (7). 2013. DOI:10.1038/nphys2640. с. 431 – 434.
De Luca, Andrea. Central Compact Objects in Supernova Remnants // AIP Conference Proceedings 983. 2008. DOI:10.1063/1.2900173. с. 311 – 319.
Klochkov, D. и др. A non-pulsating neutron star in the supernova remnant HESS J1731-347 / G353.6 – 0.7 with a carbon atmosphere // Astronomy & Astrophysics 556. 2013. DOI:10.1051/0004-6361/201321740. с. A41.
Brazier, K. T. S. и др. The implications of radio-quiet neutron stars // Monthly Notices of the Royal Astronomical Society 305 (3). август 2013. DOI:10.1046/j.1365-8711.1999.02490.x. с. 671.
Hessels, Jason W. T и др. A Radio Pulsar Spinning at 716 Hz // Science 311 (5769). 2006. DOI:10.1126/science.1123430. с. 1901 – 1904.
Posselt, B. и др. Searching for substellar companions of young isolated neutron stars // Astronomy and Astrophysics 496 (2). март 2009. DOI:10.1051/0004-6361/200810156. с. 533 – 545.
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7. Pulsars at Other Wavelengths // Frontiers of Modern Astronomy. Jodrell Bank Centre for Astrophysics. Посетен на 6 април 2016.
Zahn, Corvin. Tempolimit Lichtgeschwindigkeit // 1990-10-09. Посетен на 9 октомври 2009. Durch die gravitative Lichtablenkung ist mehr als die Hälfte der Oberfläche sichtbar. Masse des Neutronensterns: 1, Radius des Neutronensterns: 4, ... dimensionslosen Einheiten (c, G = 1) (на немски)