Evidence for a Mid-Atomic-Number Atmosphere in the Neutron Star 1E1207.4-5209

Details Evidence for a Mid-Atomic-Number Atmosphere in the Neutron Star 1E1207.4-5209 Evidence for a Mid-Atomic-Number Atmosphere in the Neutron Star 1E1207.4-5209

2002-07-26

arxiv.org/abs/astro-ph/0207590v2

Astrophys.J. 578 (2002) L133-L136

Astronomy and Astrophysics

Astrophysics

5 pages, AASTeX, Revised version. Accepted for publication in ApJ Letters

Scientific paper

10.1086/344716

Recently Sanwal et al. (2002) reported the first clear detection of absorption features in an isolated neutron star, 1E1207.4-5209. Remarkably their spectral modeling demonstrates that the atmosphere cannot be Hydrogen. They speculated that the neutron star atmosphere is indicative of ionized Helium in an ultra-strong (~1.5x10^{14} G) magnetic field. We have applied our recently developed atomic model (Mori & Hailey 2002) for strongly-magnetized neutron star atmospheres to this problem. We find that this model, along with some simp le atomic physics arguments, severely constrains the possible composition of the atmosphere. In particular we find that the absorption features are naturally associated with He-like Oxygen or Neon in a magnetic field of ~10^{12} G, comparable to the magnetic field derived from the spin parameters of the neutron star. This interpretation is consistent with the relative line strengths and widths and is robust. Our model predicts possible substructure in the spectral features, which has now been reported by XMM-Newton (Mereghetti et al. 2002). However we show the Mereghetti et al. claim that the atmosphere is Iron or some comparable high-Z element at ~ 10^{12} G is easily ruled out by the Chandra and XMM-Newton data.

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