The properties of the progenitor, neutron star, and pulsar wind in the supernova remnant Kes 75

Joseph (Yosi) Gelfand, P. O. Slane, T. Temim

Research output: Contribution to journalArticle

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 languageEnglish (US)
Pages (from-to)318-323
Number of pages6
JournalAstronomische Nachrichten
Volume335
Issue number3
DOIs
StatePublished - Mar 1 2014

Fingerprint

supernova remnants
pulsars
neutron stars
nebulae
supernovae
magnetic field
composite materials
braking
magnetization
outburst
explosion
magnetic fields
physical property
explosions
energy spectra
physical properties
shock
broadband
energy
estimates

Keywords

  • ISM: (Kes 75)
  • Pulsars: individual (J1846-0258)
  • Supernova remnants

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

The properties of the progenitor, neutron star, and pulsar wind in the supernova remnant Kes 75. / Gelfand, Joseph (Yosi); Slane, P. O.; Temim, T.

In: Astronomische Nachrichten, Vol. 335, No. 3, 01.03.2014, p. 318-323.

Research output: Contribution to journalArticle

@article{41e19c8086ee49658c66c4a2d5a47cbf,
title = "The properties of the progenitor, neutron star, and pulsar wind in the supernova remnant Kes 75",
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.",
keywords = "ISM: (Kes 75), Pulsars: individual (J1846-0258), Supernova remnants",
author = "Gelfand, {Joseph (Yosi)} and Slane, {P. O.} and T. Temim",
year = "2014",
month = "3",
day = "1",
doi = "10.1002/asna.201312039",
language = "English (US)",
volume = "335",
pages = "318--323",
journal = "Astronomische Nachrichten",
issn = "0004-6337",
publisher = "Wiley-VCH Verlag",
number = "3",

}

TY - JOUR

T1 - The properties of the progenitor, neutron star, and pulsar wind in the supernova remnant Kes 75

AU - Gelfand, Joseph (Yosi)

AU - Slane, P. O.

AU - Temim, T.

PY - 2014/3/1

Y1 - 2014/3/1

N2 - 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.

AB - 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.

KW - ISM: (Kes 75)

KW - Pulsars: individual (J1846-0258)

KW - Supernova remnants

UR - http://www.scopus.com/inward/record.url?scp=84894758540&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84894758540&partnerID=8YFLogxK

U2 - 10.1002/asna.201312039

DO - 10.1002/asna.201312039

M3 - Article

AN - SCOPUS:84894758540

VL - 335

SP - 318

EP - 323

JO - Astronomische Nachrichten

JF - Astronomische Nachrichten

SN - 0004-6337

IS - 3

ER -