Atomic Nuclear Physics

Isolated Neutron Stars: from the Surface to the Interior (V. by Silvia Zane, Roberto Turolla, Dany Page

By Silvia Zane, Roberto Turolla, Dany Page

This publication collects the contributions offered on the convention remoted Neutron Stars: From the skin to the internal, held in London in April 2006. 40 years after the invention of radio pulsars it offers an up to date description of the recent imaginative and prescient of remoted neutron stars that has emerged in recent times with the improvement of multi-wavelength observations. the good number of remoted neutron stars, from pulsars to magnetars, a few of them found very lately and plenty of of them now not detectable in radio wavelengths, is abundantly lined via descriptions of contemporary observational effects and displays of the most recent theoretical interpretation of those data.

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J. : Astrophys. J. : Astron. Astrophys. : Astrophys. J. : Astrophys. J. : Mon. Not. Roy. Astron. Soc. : Astrophys. J. : Astrophys. J. : Astrophys. J. : In: Compact Stellar X-ray Sources, p. 547. V. 2007 Abstract We present a systematic analysis of all the BeppoSAX data of SGR1900+14. The observations spanning five years show that the source was brighter than usual on two occasions: ∼20 days after the August 1998 giant flare and during the 105 s long X-ray afterglow following the April 2001 intermediate flare.

The total fluency of the IR enhancement between June and October 2004 is about 1041 erg (we assumed AV = 29 ± 2; see Eikenberry et al. 2004), a factor of about 100 smaller than that in the 2–10 keV band. Based on the above reported findings we note that the SGR 1806–20 emission varies in a similar fashion (in terms of timescale and amplitude of variation) over more than five orders of magnitude in photon energy. The similar flux variation in the IR and X-ray bands suggests that the emission in the two bands has a similar, if not the same, origin.

Although extremely strong, such a field is fully plausible given that a (mainly toroidal) field in excess of 1016 G is required to power the SGR 1806–20 flux during its whole life if one speculate that repeated giant flares of this magnitude over the ∼104 yr lifetime occurred in the past. Motivated by our discovery of QPOs (or GSOs) in the X-ray flux of SGR 1806–20, Strohmayer and Watts (2005) looked for such kind of QPOs in the X-ray flux of the giant flare of SGR 1900+14, serendipitously recorded again by RXTE on 28th August 1998.

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