The dynamical and radiative evolution of clumpy supernova ejecta

M. C. Anderson; T. W. Jones; L. Rudnick; I. L. Tregillis; Hyesung Kang

doi:10.1086/187180

The dynamical and radiative evolution of clumpy supernova ejecta

M. C. Anderson, T. W. Jones, L. Rudnick, I. L. Tregillis, Hyesung Kang

Physics and Astronomy (Twin Cities)

Research output: Contribution to journal › Article › peer-review

40 Scopus citations

Abstract

Numerical simulations describing the dynamical and radiative evolution of clumpy supernova ejecta are compared with observations of optical and radio emission knots in SNR Cassiopeia A. Three major phases are identified in the evolution of clumpy ejecta: a bow-shock phase, an instability phase, and a dispersal phase. The phenomenological and radiative signatures of each phase are discussed and compared with multi-epoch measurements of small-scale features in Cas A. Good correspondence is found between theory and observations. Both support the premise that compact radio emission features are controlled more by magnetic field amplification triggered in the instability phase than by in situ acceleration of new relativistic particles.

Original language	English (US)
Pages (from-to)	L31-L34
Journal	Astrophysical Journal
Volume	421
Issue number	1 PART 2
DOIs	https://doi.org/10.1086/187180
State	Published - Jan 20 1994

Keywords

Acceleration of particles
Shock waves
Supernova remnants

Publisher link

10.1086/187180

Find It

Find It at U of M Libraries

Cite this

@article{85a284ab25624c248771daa1643c8567,

title = "The dynamical and radiative evolution of clumpy supernova ejecta",

abstract = "Numerical simulations describing the dynamical and radiative evolution of clumpy supernova ejecta are compared with observations of optical and radio emission knots in SNR Cassiopeia A. Three major phases are identified in the evolution of clumpy ejecta: a bow-shock phase, an instability phase, and a dispersal phase. The phenomenological and radiative signatures of each phase are discussed and compared with multi-epoch measurements of small-scale features in Cas A. Good correspondence is found between theory and observations. Both support the premise that compact radio emission features are controlled more by magnetic field amplification triggered in the instability phase than by in situ acceleration of new relativistic particles.",

keywords = "Acceleration of particles, Shock waves, Supernova remnants",

author = "Anderson, {M. C.} and Jones, {T. W.} and L. Rudnick and Tregillis, {I. L.} and Hyesung Kang",

year = "1994",

month = jan,

day = "20",

doi = "10.1086/187180",

language = "English (US)",

volume = "421",

pages = "L31--L34",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "1 PART 2",

}

TY - JOUR

T1 - The dynamical and radiative evolution of clumpy supernova ejecta

AU - Anderson, M. C.

AU - Jones, T. W.

AU - Rudnick, L.

AU - Tregillis, I. L.

AU - Kang, Hyesung

PY - 1994/1/20

Y1 - 1994/1/20

N2 - Numerical simulations describing the dynamical and radiative evolution of clumpy supernova ejecta are compared with observations of optical and radio emission knots in SNR Cassiopeia A. Three major phases are identified in the evolution of clumpy ejecta: a bow-shock phase, an instability phase, and a dispersal phase. The phenomenological and radiative signatures of each phase are discussed and compared with multi-epoch measurements of small-scale features in Cas A. Good correspondence is found between theory and observations. Both support the premise that compact radio emission features are controlled more by magnetic field amplification triggered in the instability phase than by in situ acceleration of new relativistic particles.

AB - Numerical simulations describing the dynamical and radiative evolution of clumpy supernova ejecta are compared with observations of optical and radio emission knots in SNR Cassiopeia A. Three major phases are identified in the evolution of clumpy ejecta: a bow-shock phase, an instability phase, and a dispersal phase. The phenomenological and radiative signatures of each phase are discussed and compared with multi-epoch measurements of small-scale features in Cas A. Good correspondence is found between theory and observations. Both support the premise that compact radio emission features are controlled more by magnetic field amplification triggered in the instability phase than by in situ acceleration of new relativistic particles.

KW - Acceleration of particles

KW - Shock waves

KW - Supernova remnants

UR - http://www.scopus.com/inward/record.url?scp=12044252551&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=12044252551&partnerID=8YFLogxK

U2 - 10.1086/187180

DO - 10.1086/187180

M3 - Article

AN - SCOPUS:12044252551

SN - 0004-637X

VL - 421

SP - L31-L34

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 PART 2

ER -

The dynamical and radiative evolution of clumpy supernova ejecta

Abstract

Keywords

Publisher link

Find It

Other files and links

Fingerprint

Cite this