Dust formation in embryonic pulsar-aided supernova remnants

Conor M.B. Omand, Kazumi Kashiyama, Kohta Murase

Research output: Contribution to journalArticlepeer-review

16 Scopus citations


We investigate effects of energetic pulsar wind nebulae (PWNe) on dust formation and evolution. Dust emission has been observed in many supernova remnants that also have neutron stars as compact remnants. We study the dependence of dust formation time and size on properties of the ejecta and central pulsar. We find that a pulsar with an initial spin period P ∼ 1-10 ms and a dipole magnetic field B ∼ 1012-15 G can either accelerate or delay dust formation, with a time-scale of several months to over 10 yr, and reduce the average size of dust by a factor of ∼10 or more compared to the non-pulsar case. We also find that infrared dust emission may be detectable in typical superluminous supernovae out to ∼100-1000 Mpc in 2-5 yr after the explosion, although this depends sensitively on the spectral index of non-thermal emission from the nebula. We discuss implications to previous supernova observations. Some discrepancies between dust formation models and observations, such as the formation time in SN1987A or the dust size in the Crab Nebula, could be explained by the influence of a pulsar, and knowledge of the dust emission will be important for future ALMA observations of superluminous supernovae.

Original languageEnglish (US)
Pages (from-to)5468-5483
Number of pages16
JournalMonthly Notices of the Royal Astronomical Society
Issue number4
StatePublished - Apr 21 2019

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science


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