A model for SNR evolution in a cloudy medium and its application to N49

Shull, Peter; Dyson, J. E.; Kahn, F. D.; West, K. A.

doi:10.1093/mnras/212.4.799

Cited by 38 publications

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“…Motivated by evidence for interaction between supernovae and molecular clouds such as N49 (Shull 1983), a few analytical studies have been performed (Shull et al 1985;Chevalier 1999). More recently, hydrodynamical numerical simulations of a supernova explosion taking place in a dense clump have been performed by Rogers & Pittard (2013).…”

Section: Introductionmentioning

confidence: 99%

Mutual influence of supernovae and molecular clouds

Iffrig

Hennebelle

2015

A&A

130

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Context. Molecular clouds are known to be turbulent and strongly affected by stellar feedback. Moreover, stellar feedback is believed to drive turbulence at large scales in galaxies. Aims. We study the role played by supernovae in molecular clouds and the influence of the magnetic field on this process. Methods. We performed three-dimensional numerical simulations of supernova explosions, in and near turbulent self-gravitating molecular clouds. In order to study the influence of the magnetic field, we performed both hydrodynamical and magnetohydrodynamical simulations. We also ran a series of simple uniform density medium simulations and developed a simple analytical model. Results. We find that the total amount of momentum that is delivered during supernova explosions typically varies by a factor of about 2, even when the gas density changes by 3 orders of magnitude. However, the amount of momentum delivered to the dense gas varies by almost a factor of 10 if the supernova explodes within or outside the molecular cloud. The magnetic field has little influence on the total amount of momentum injected by the supernova explosions but increases the momentum injected into the dense gas. Conclusions. Supernovae that explode inside molecular clouds remove a significant fraction of the cloud mass. Supernovae that explode outside have a limited influence on the cloud but nevertheless remove a substantial amount of gas at densities between 1 cm −3 and 100 cm −3 , that would be forming stars later. It is thus essential to know sufficiently well the correlation between supernovae and the surrounding dense material in order to know whether supernovae can regulate star formation effectively.

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Section: Introductionmentioning

confidence: 99%

Mutual influence of supernovae and molecular clouds

Iffrig

Hennebelle

2015

A&A

130

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“…Data from this intermediate-temperature gas are essential for discriminating among the many theoretical models which have been advanced to explain the X-ray and optical morphology of SNRs. Several models have been proposed to describe the cloud-shock processes : thermal evaporation of dense clouds inside an SNR (McKee & Ostriker 1977), radiative cooling by shocks driven into small dense clouds (i.e., "" cloud crushing ÏÏ ; Cox 1979), collision of a blast wave with a large cloud (possibly a shell created by the SN progenitor ; Shull et al 1985), a bow shock where a blast wave encounters a small cloud (e.g., Klein, McKee, & Collela 1994), thermally unstable cooling of a Sedov blast wave (Gaetz, Edgar, & Chevalier 1988), or turbulent mixing of hot and cool material by shear instabilities ("" mixing layer models ÏÏ ; Slavin, Shull, & Begelman 1993). These models are compared in Raymond & Curiel (1994 We present the parameters of the observations that constitute this work in°2.…”

Section: Introductionmentioning

confidence: 99%

[Nev] Imaging of the Cygnus Loop

Szentgyorgyi

Raymond

Hester

et al. 2000

ApJ

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We present continuum-subtracted images of a 20@ ] 20@ region of the eastern Cygnus Loop (NGC 6995) in the 3425 forbidden line of Ne V. The images reveal bright linear Ðlaments which are associ-A ated with, but not positionally coincident with, bright features seen in Ha, [O III], and other narrowband images. In some areas, the [Ne V] Ðlaments deÐne the edge of X-rayÈemitting regions. The Ðlaments exhibit a peak surface brightness of 1.2 ] 10~4 photons cm~2 s~1 arcsec~2 at the top of the atmosphere in images with typical detection limits of D10~5 photons cm~2 s~1 arcsec~2. We present arguments that these structures are produced by radiative shock waves and discuss implications for the shock velocities and the three-dimensional structure of this section of the Cygnus Loop. We place limits on the importance of thermal conductionÈdriven evaporation as a contribution to the mass of X-rayÈemitting gas. Lack of evidence of [Ne V] emission resulting from thermal evaporation may have signiÐcance for supernova remnants and interstellar medium models that rely heavily on the importance of thermal evaporation. 5 ] 104 K) and the high-temperature regime imaged in X-rays (T º 106 K). The ionization potential of Ne IV is 97.11 eV, so the concentration of Ne V peaks at a temperature of D3 ] 105 K in collisionally ionized equilibrium plasmas. While there are alternative plasma diagnostics in this temperature regime (e.g., O VI, N V), only the forbidden Ne V lines at jj3345.8, 3425.9, corresponding to the 2p2 3PÈ2p2 1D transition, are observable at ground-based optical telescopes ; all other bright emission features formed near this temperature are well shortward of the atmospheric cuto † near 3000 or in the thermal infrared and thus are A the exclusive province of exoatmospheric telescopes. The j3425.9 feature (henceforth integerized to j3425) is preferred for narrowband imaging, since the transition probability is 2.7 times that of j3345.8 transition (Giles 1979 ;Nussbaumer & Rusca 1979 Rowlands et al. (1989) have obtained spectra at the 24.28 km Ðne-structure transition of Ne V in PNs from the Kuiper Airborne Observatory. A key advantage of observing in the [Ne V] j3425 line is that this wavelength is detectable with blue-optimized, backside-illuminated charge-coupled devices (CCDs) on ground-based telescopes of moderate aperture with standard reÑective coatings (aluminum) and ultraviolet (UV) transmissive refractive elements (fused silica or calcium Ñuoride). The images we present in this paper are the Ðrst continuum-subtracted astronomical images in [Ne V] j3425.While photoionized plasmas are characterized by highionization states and low temperatures, collisionally ionized plasma, as exempliÐed by SNR shocks, may have quite high temperatures. The requisite temperatures for strong Ne V concentrations occur behind shock with velocities 190È250 km s~1. For faster shocks, [Ne V] images "" connect ÏÏ hightemperature X-ray images to images of cooler plasmas in the postshock regions of the Ñow (Fig. 1). The morphology exhi...

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“…If the progenitor was a massive star then an H  region and a wind blown shell will have been set up around the star. Shull et al (1985) discussed the effects of an SN explosion in a cloudy medium around a massive star. The formation of the H  region destroys any H  clouds and thus the SN explosion takes place in a cavity created by the star and then encounters a clumpy shell.…”

Section: Energeticsmentioning

confidence: 99%

The kinematics of the bi-lobal supernova remnant G 65.3+5.7. II.

Boumis

Meaburn

López³

et al. 2004

A&A

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Abstract. Further deep, narrow-band images in the light of [O ] 5007 Å have been added to the previous mosaic of the faint galactic supernova remnant G 65.3+5.7. Additionally, long-slit spatially resolved [O ] 5007 Å line profiles have been obtained at sample positions using the Manchester Echelle Spectrometer at the San Pedro Martir observatory. The remnant is shown to be predominantly bi-lobal with an EW axis. However, a faint additional northern lobe has now been revealed. The splitting of the profiles along the slit lengths, when extrapolated to the centre of the remnant, although uncertain, suggests that the expansion velocity of this remnant is between 124 and 187 km s −1 i.e. much lower than the 400 km s −1 previously predicted for the forward shock velocity from the X-ray emission. An expansion proper motion measurement of 2.1 ± 0.4 arcsec in 48 years for the remnant's filamentary edge in the light of Hα + [N ] 6548 and 6584 Å has also been made. This is combined with an expansion velocity of ≈155 km s −1 , a distance of ≈800 pc is derived. Several possibilities are considered for the large difference in the expansion velocity measured here and the 400 km s −1 shock velocity required to generate the X-ray emission. It is also suggested that the morphology of the remnant may be created by a tilt in the galactic magnetic field in this vicinity.

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A model for SNR evolution in a cloudy medium and its application to N49

Cited by 38 publications

References 0 publications

Mutual influence of supernovae and molecular clouds

Mutual influence of supernovae and molecular clouds

[Nev] Imaging of the Cygnus Loop

The kinematics of the bi-lobal supernova remnant G 65.3+5.7. II.

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