Stellar explosions, instabilities, and turbulence

Drake, R. P.; Kuranz, Carolyn; Miles, A. R.; Muthsam, H.; Plewa, T.

doi:10.1063/1.3101816

Cited by 13 publications

(4 citation statements)

References 62 publications

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“…New observational evidence, largely from extensive transient searches (e.g. the Catalina Real-time Transient Survey, the Palomar Transient Factory, PanSTARRS1, La Silla Quest, etc.. Drake et al 2009;Law et al 2009;Tonry et al 2012;Baltay et al 2013, respectively), is shedding new light both at the bright and faint ends of the SN luminosity distribution. In particular, a number of exceptionally luminous objects (SLSNe) are challenging our existing theoretical picture of the late evolution and explosion of massive stars.…”

Section: Introductionmentioning

confidence: 99%

The supernova CSS121015:004244+132827: a clue for understanding superluminous supernovae

Benetti

Nicholl

Pastorello

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present optical photometry and spectra of the super luminous type II/IIn supernova CSS121015:004244+132827 (z=0.2868) spanning epochs from -30 days (rest frame) to more than 200 days after maximum. CSS121015 is one of the more luminous supernova ever found and one of the best observed. The photometric evolution is characterized by a relatively fast rise to maximum (∼ 40 days in the SN rest frame), and by a linear post-maximum decline. The light curve shows no sign of a break to an exponential tail. A broad Hα is first detected at ∼ +40 days (rest-frame). Narrow, barely-resolved Balmer and [O III] 5007Å lines, with decreasing strength, are visible along the entire spectral evolution. The spectra are very similar to other super luminous supernovae (SLSNe) with hydrogen in their spectrum, and also to SN 2005gj, sometimes considered a type Ia interacting with H-rich CSM. The spectra are also similar to a subsample of H-deficient SLSNe. We propose that the properties of CSS121015 are consistent with the interaction of the ejecta with a massive, extended, opaque shell, lost by the progenitor decades before the final explosion, although a magnetar powered model cannot be excluded. Based on the similarity of CSS121015 with other SLSNe (with and without H), we suggest that the shocked-shell scenario should be seriously considered as a plausible model for both types of SLSN.

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Section: Introductionmentioning

confidence: 99%

The supernova CSS121015:004244+132827: a clue for understanding superluminous supernovae

Benetti

Nicholl

Pastorello

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…(2007) used a conical array of wires at the Magpie facility to drive a magnetized jet, and explored the geometry of the deflection shock formed as a jet impacts a crosswind. Laboratory experiments have also recently studied the physics associated with instabilities along supernova blast waves (Kuranz et al 2007;Drake et al 2009), and the dynamics within supernovae explosions (Reighard & Drake 2007).…”

Section: Introductionmentioning

confidence: 99%

Laboratory Experiments, Numerical Simulations, and Astronomical Observations of Deflected Supersonic Jets: Application to Hh 110

Hartigan

Foster

Wilde

et al. 2009

ApJ

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Collimated supersonic flows in laboratory experiments behave in a similar manner to astrophysical jets provided that radiation, viscosity, and thermal conductivity are unimportant in the laboratory jets, and that the experimental and astrophysical jets share similar dimensionless parameters such as the Mach number and the ratio of the density between the jet and the ambient medium. When these conditions apply, laboratory jets provide a means to study their astrophysical counterparts for a variety of initial conditions, arbitrary viewing angles, and different times, attributes especially helpful for interpreting astronomical images where the viewing angle and initial conditions are fixed and the time domain is limited. Experiments are also a powerful way to test numerical fluid codes in a parameter range where the codes must perform well. In this paper we combine images from a series of laboratory experiments of deflected supersonic jets with numerical simulations and new spectral observations of an astrophysical example, the young stellar jet HH 110. The experiments provide key insights into how deflected jets evolve in 3-D, particularly within working surfaces where multiple subsonic shells and filaments form, and along the interface where shocked jet material penetrates into and destroys the obstacle along its path. The experiments also underscore the importance of the viewing angle in determining what an observer will see. The simulations match the experiments so well that we can use the simulated velocity maps to compare the dynamics in the experiment with -2those implied by the astronomical spectra. The experiments support a model where the observed shock structures in HH 110 form as a result of a pulsed driving source rather than from weak shocks that may arise in the supersonic shear layer between the Mach disk and bow shock of the jet's working surface.

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“…These strong spatial perturbations may be related to the Richmyer-Meshkov and Rayleigh-Taylor instabilities which were observed in stellar explosions (e.g. Drake et al, 2009). The perturbations in the plasma density profiles have a spatial scale from 1 R E to a few R E .…”

Section: Global Interaction Between the Interplanetary Transmitted Sh...mentioning

confidence: 88%

Global effects of transmitted shock wave propagation through the Earth's inner magnetosphere: First results from 3-D hybrid kinetic modeling

Lipatov

Sibeck

2016

Planetary and Space Science

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Stellar explosions, instabilities, and turbulence

Cited by 13 publications

References 62 publications

The supernova CSS121015:004244+132827: a clue for understanding superluminous supernovae

The supernova CSS121015:004244+132827: a clue for understanding superluminous supernovae

Laboratory Experiments, Numerical Simulations, and Astronomical Observations of Deflected Supersonic Jets: Application to Hh 110

Global effects of transmitted shock wave propagation through the Earth's inner magnetosphere: First results from 3-D hybrid kinetic modeling

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