X-ray studies of radio-silent neutron stars in the remnants of supernova explosions. (arXiv:2107.09506v2 [astro-ph.HE] UPDATED)

X-ray studies of radio-silent neutron stars in the remnants of supernova explosions. (arXiv:2107.09506v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Collazos_J/0/1/0/all/0/1">J. Alfredo Collazos</a>

The present work is devoted to the study of the supernova remnant and its
neutron star XMMU J172054. 5-372652. The paper analyzes observations in 2009
and 2018, data for this system obtained by the Chandra x ray observatory. The
analysis showed that the neutron star G350. 1-0. 3 with M = 1, 4 Msun, R = 13
MS, dist = 4, 5 KPC, we also measured its temperature in two groups: the first
group, including observations made in 2009, and the second group, including 5
observations made at different times of the year 2018. In addition, in this
work, we study all important aspects of the supernova remnants of G350. 1-0. 3,
and obtain their spectra using the collided plasma, nonequilibrium, constant
temperature (VNEI) model, which assumes a constant temperature and a single
ionization parameter. It gives a characteristic of the spectrum, but is not a
physical model, we will precede the spectra obtained using this model.

The present work is devoted to the study of the supernova remnant and its
neutron star XMMU J172054. 5-372652. The paper analyzes observations in 2009
and 2018, data for this system obtained by the Chandra x ray observatory. The
analysis showed that the neutron star G350. 1-0. 3 with M = 1, 4 Msun, R = 13
MS, dist = 4, 5 KPC, we also measured its temperature in two groups: the first
group, including observations made in 2009, and the second group, including 5
observations made at different times of the year 2018. In addition, in this
work, we study all important aspects of the supernova remnants of G350. 1-0. 3,
and obtain their spectra using the collided plasma, nonequilibrium, constant
temperature (VNEI) model, which assumes a constant temperature and a single
ionization parameter. It gives a characteristic of the spectrum, but is not a
physical model, we will precede the spectra obtained using this model.

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