Statistics – Methodology
Scientific paper
Oct 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003phdt.........9m&link_type=abstract
Thesis (PhD). COLUMBIA UNIVERSITY, Source DAI-B 64/04, p. 1766, Oct 2003, 159 pages.
Statistics
Methodology
2
Scientific paper
This thesis consists of a theoretical study of neutron star atmospheres and its application to recent X-ray data on the isolated neutron star 1E1207.4-5209, which shows absorption features. Although the study of pulsars has been carried out mostly in the radio band for many years, spectroscopy study by recent X-ray telescopes provides a powerful tool for describing the interior of neutron stars. In particular, a unique determination of mass and radius from a single neutron star severely constrains the equation of state and composition of the core region of neutron stars. In the first part of my thesis, theoretical work on neutron star atmosphere models is presented. Intensive study of atomic structure in strong magnetic fields typical of neutron stars was undertaken. A novel atomic calculation which computes transition energies and oscillator strengths with sufficient accuracy to analyze high energy resolution data on Chandra and XMM-Newton was performed. In the second part of my thesis, a methodology was established to identify spectral features from strongly- magnetized dense plasmas. Based on the application of the atomic code and methodology to the Chandra data from the isolated neutron star 1E1207.4-5209, it was shown that the observed absorption features are due to Helium-like Oxygen or Neon at B ˜ 1012 G. This led to a simultaneous determination of the surface composition, the magnetic field strength and, more importantly, the gravitational redshift. Further constraints on the atmosphere, as well as the neutron star equation of state, can be inferred under the assumption that the neutron star mass is near the canonical value of 1.4 M&sun; . In that case Neon is ruled out, and the atmosphere is unambiguously Oxygen. The corresponding gravitational redshift for the Oxygen atmosphere constrains the equation of state of the interior of 1E1207.4-5209 to be quite stiff.
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