An Approach for Estimating the Deformation of Pulsar Included in Binary-System PSR B 1913+16 | ||||
| Egyptian Journal of Physics | ||||
| Article 11, Volume 47, Issue 1, June 2019, Page 45-55 PDF (1.05 MB) | ||||
| Document Type: Original Article | ||||
| DOI: 10.21608/ejphysics.2018.6174.1015 | ||||
 View on SCiNiTO | ||||
| Authors | ||||
Mohammed Hasan M. Soleiman  1; Magdi mohamed elgogary2; Sayed Saleh Abdel-AZIZ Saleh2; Ahmed Imsaery Omar3
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| 1Physics Department, Faculty of Science, Cairo University, Giza, Egypt. | ||||
| 2Physics Department, Faculty of Science, Cairo University, Giza 12613, Egypt. | ||||
| 3Physics Department, Faculty of Science, Cairo University, Giza 12613, Egypt, and Physics Department, Faculty of Science, Sebha University, Sebha, Libya. | ||||
| Abstract | ||||
| Discovery of pulsars included in binary systems (BS) is dated to 1974, when Hulse and Taylor announced the parameters of pulsar PSR B 1913+16. It inspires great motivations for possible new physical measurements of the properties of neutron stars (NSs). We present a simple model to estimate the deformation in shape of two neutron stars bounded to each other in a binary system due to their mutual gravity. The model predicts the Bulk modulus of the pulsar – as an infinite nuclear matter. In particular, the model determines the stress and the strain of a pulsar included in PSR B 1913+16 binary system within the frame of Newtonian theory of gravity. The calculations show that, our approach is consistent with the model of two spherical neutron stars up to the eccentricity-squared. The model could evaluate the axial elongation of the observed NS as well as the eccentricity. The eccentricity is found to be of order 10^(-5) and the elongation is of the order 10^(-9) km. | ||||
| Keywords | ||||
| Infinite Nuclear Matter; Neutron Star; Pulsar; Buk Modulus; Compressibility; Companion Star | ||||
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