Abstract
By studying composite supernova remnants (SNRs), remnants which contain a pulsar wind nebula (PWN), it is possible to estimate physical properties of the progenitor explosion, central neutron star, and its pulsar wind that are difficult to measure directly. This is best done by fitting the dynamical and broadband spectral properties of a PWN with an evolutionary model for a PWN inside an SNR. We apply such a model to the composite SNR Kes 75, whose associated pulsar PSR J1846-0258 is thought to have an extremely strong surface magnetic field. If ∼3 M⊙ of mass was ejected in the supernova, our model suggests a normal or slightly subenergetic supernova in a low density environment. Additionally, for the measured pre-outburst braking index of p = 2.65, our model prefers an age of ∼430 years and an initial spin period P0 ∼ 0.2 s. Lastly, the magnetization of the pulsar wind and energy spectrum of particles injected at the termination shock are similar to those observed from other PWNe powered by less magnetized neutron stars. While further study is needed to verify these results, they are nominally inconsistent with strong neutron star magnetic fields resulting from very fast initial rotation.
Original language | English (US) |
---|---|
Pages (from-to) | 318-323 |
Number of pages | 6 |
Journal | Astronomische Nachrichten |
Volume | 335 |
Issue number | 3 |
DOIs | |
State | Published - Mar 2014 |
Keywords
- ISM: (Kes 75)
- Pulsars: individual (J1846-0258)
- Supernova remnants
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science