Shock Dynamics in Stellar Outbursts. I. Shock Formation

@article{Ro2016ShockDI,
  title={Shock Dynamics in Stellar Outbursts. I. Shock Formation},
  author={S. Ro and Christopher D. Matzner},
  journal={The Astrophysical Journal},
  year={2016},
  volume={841}
}
  • S. Ro, C. Matzner
  • Published 28 December 2016
  • Physics
  • The Astrophysical Journal
Wave-driven outflows and non-disruptive explosions have been implicated in pre-supernova outbursts, supernova impostors, luminous blue variable eruptions, and some narrow-line and superluminous supernovae. To model these events, we investigate the dynamics of stars set in motion by strong acoustic pulses and wave trains, focusing on nonlinear wave propagation, shock formation, and an early phase of the development of a weak shock. We identify the shock formation radius, showing that a heuristic… 

Figures and Tables from this paper

Wave-driven Shocks in Stellar Outbursts: Dynamics, Envelope Heating, and Nascent Blast Waves

We address the shocks from acoustic pulses and wave trains in general one-dimensional flows, with an emphasis on the application to super-Eddington outbursts in massive stars. Using approximate

Weak Shock Propagation with Accretion. II. Stability of Self-similar Solutions to Radial Perturbations

Coughlin et al. derived and analyzed a new regime of self-similarity that describes weak shocks (Mach number of order unity) in the gravitational field of a point mass. These solutions are relevant

Hydrodynamic Simulations of Pre-supernova Outbursts in Red Supergiants: Asphericity and Mass Loss

The activity of a massive star approaching core-collapse can strongly affect the appearance of the star and its subsequent supernova. Late-phase convective nuclear burning generates waves that

Pre-supernova outbursts via wave heating in massive stars – I. Red supergiants

Early observations of supernovae (SNe) indicate that enhanced mass-loss and pre-SN outbursts may occur in progenitors of many types of SNe. We investigate the role of energy transport via waves

3D Hydrodynamics of Pre-supernova Outbursts in Convective Red Supergiant Envelopes

Eruptive mass loss likely produces the energetic outbursts observed from some massive stars before they become core-collapse supernovae (SNe). The resulting dense circumstellar medium may also cause

A physical model of mass ejection in failed supernovae

During the core collapse of massive stars, the formation of the protoneutron star is accompanied by the emission of a significant amount of mass-energy ($\sim 0.3 \, M_{\odot}$) in the form of

Pre-supernova outbursts via wave heating in massive stars – II. Hydrogen-poor stars

Pre-supernova (SN) outbursts from massive stars may be driven by hydrodynamical wave energy emerging from the core of the progenitor star during late nuclear-burning phases. Here, we examine the

The Formation and Dissipation of Current Sheets and Shocks due to Compressive Waves in a Stratified Atmosphere Containing a Magnetic Null

We study the propagation and dissipation of magnetohydrodynamic waves in a set of numerical models that each includes a solar-like stratified atmosphere and a magnetic field with a null point. All

Simulating the formation of η Carinae’s surrounding nebula through unstable triple evolution and stellar merger-induced eruption

η Carinae is an extraordinary massive star famous for its 19th century Great Eruption and the surrounding Homunculus nebula ejected in that event. The cause of this eruption has been the centre of

The Betelgeuse Project II: asteroseismology

We explore the question of whether the interior state of massive red supergiant supernova progenitors can be effectively probed with asteroseismology. We have computed a suite of ten models with ZAMS

References

SHOWING 1-10 OF 36 REFERENCES

OBLIQUE SHOCK BREAKOUT IN SUPERNOVAE AND GAMMA-RAY BURSTS. II. NUMERICAL SOLUTIONS FOR NON-RELATIVISTIC PATTERN SPEEDS

Non-spherical explosions develop non-radial flows as the pattern of shock emergence progresses across the stellar surface. In supernovae, these flows can limit ejecta speeds, stifle shock breakout

OBLIQUE SHOCK BREAKOUT IN SUPERNOVAE AND GAMMA-RAY BURSTS. I. DYNAMICS AND OBSERVATIONAL IMPLICATIONS

In a non-spherical stellar explosion, non-radial motions become important near the stellar surface. For realistic deviations from spherical symmetry, non-radial flow dramatically alters the dynamics

PREPARING FOR AN EXPLOSION: HYDRODYNAMIC INSTABILITIES AND TURBULENCE IN PRESUPERNOVAE

Both observations and numerical simulations are discordant with predictions of conventional stellar evolution codes for the latest stages of a massive star's life before core collapse. The most

Shock‐heating of stellar envelopes: a possible common mechanism at the origin of explosions and eruptions in massive stars

Observations of transient phenomena in the Universe reveal a spectrum of mass-ejection properties associated with massive stars, covering from Type II/Ib/Ic core-collapse supernovae (SNe) to giant

Wave-driven stellar expansion and binary interaction in pre-supernova outbursts

We suggest that the main outcome of energy leakage carried by waves from the core to the envelope of pre-collapse massive stars is envelope expansion rather than major mass ejection. We show that the

SETTING THE STAGE FOR CIRCUMSTELLAR INTERACTION IN CORE-COLLAPSE SUPERNOVAE. II. WAVE-DRIVEN MASS LOSS IN SUPERNOVA PROGENITORS

Supernovae (SNe) powered by interaction with circumstellar material provide evidence for intense stellar mass loss during the final years before core collapse. We have argued that during and after

Deflagration-to-detonation transition by amplification of acoustic waves in type Ia supernovae

We study a new mechanism for deflagration to detonation transition in thermonuclear supernovae (SNe Ia), based on the formation of shocks by amplification of sound waves in the steep density

Wave‐driven mass loss in the last year of stellar evolution: setting the stage for the most luminous core‐collapse supernovae

During the late stages of stellar evolution in massive stars (C fusion and later), the fusion luminosity in the core of the star exceeds the star’s Eddington luminosity. This can drive vigorous

Shock formation in the presence of entropy gradients

The steepening of a normal compression wave into a shock in a homentropic flow field is understood well through the method of characteristics. In a non-homentropic flow field, however, shock

A blast wave from the 1843 eruption of η Carinae

TLDR
Observations of much faster material with speeds up to 3,500–6,000 km s-1 indicate that the eruption of η Carinae may have been powered by a deep-seated explosion rivalling a supernova, perhaps triggered by the pulsational pair instability.