Oblique Shock Breakout in Supernovae and Gamma-Ray Bursts. Ii. Numerical Solutions for Non-Relativistic Pattern Speeds

Salbi, Pegah; Matzner, Christopher D.; Ro, Stephen; Levin, Y.

doi:10.1088/0004-637x/790/1/71

Cited by 21 publications

(21 citation statements)

References 20 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…It also engenders ejecta-ejecta collisions in the equatorial disk. All of these features conform to the theoretical expectations of Matzner et al (2013) and Salbi et al (2014), and are consistent with the outcome of earlier numerical works such as those by Couch et al (2009). We note that reducing the aphericity can lead to mildy aspherical explosions which are more realistic for larger progenitors such as RSGs.…”

Section: Summary and Discussionsupporting

confidence: 91%

“…In top right plot, the bipolar shock is emerged from the pole. The bottom left panel depicts the spray of the ejecta outside the stellar surface and exhibits the kink in the shock front as was previously shown bySalbi et al (2014). The bottom right panel marks the time when the shock has completely traversed the progenitor and the circumstellar collisions is happening along the equator.…”

mentioning

confidence: 68%

“…Couch et al (2009) and Couch et al (2011) perform adiabatic, axisymmetric simulations of jet-driven explosions and analyze the results to infer properties of the early light. Examining the breakout dynamics, Matzner et al (2013) point out that aspherical explosions can undergo a transition to distinctly different behavior, predictions Salbi et al (2014) verify on the basis of simulations that address a small zone near the stellar surface. Most recently, Suzuki et al (2016) simulate a mildly aspherical explosion using a radiation hydrodynamics calculation.…”

Section: Introductionmentioning

confidence: 95%

See 2 more Smart Citations

Aspherical Supernovae: Effects on Early Light Curves

Afsariardchi

Matzner

2018

ApJ

Self Cite

View full text Add to dashboard Cite

Early light from core-collapse supernovae, now detectable in high-cadence surveys, holds clues to a star and its environment just before it explodes. However, effects that alter the early light have not been fully explored. We highlight the possibility of non-radial flows at the time of shock breakout. These develop in sufficiently non-spherical explosions if the progenitor is not too diffuse. When they do develop, non-radial flows limit ejecta speeds and cause ejecta-ejecta collisions. We explore these phenomena and their observational implications, using global, axisymmetric, non-relativistic FLASH simulations of simplified polytropic progenitors, which we scale to representative stars. We develop a method to track photon production within the ejecta, enabling us to estimate band-dependent light curves from adiabatic simulations. Immediate breakout emission becomes hidden as an oblique flow develops. Non-spherical effects lead the shock-heated ejecta to release a more constant luminosity at a higher, evolving color temperature at early times, effectively mixing breakout light with the early light curve. Collisions between non-radial ejecta thermalize a small fraction of the explosion energy; we address emission from these collisions in a subsequent paper.

show abstract

Section: Summary and Discussionsupporting

confidence: 91%

mentioning

confidence: 68%

Section: Introductionmentioning

confidence: 95%

See 1 more Smart Citation

Aspherical Supernovae: Effects on Early Light Curves

Afsariardchi

Matzner

2018

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…This is true even when one accounts for the shallow relativistic slope described here and in previous works (e.g., Tan et al 2001). This probably implies that the explosion is not fully spherical (e.g., Couch et al 2011;Matzner et al 2013;Salbi et al 2014), or that the stellar structure is different than in typical SNe, or a combination of the two. A likely explanation for this point is discussed in a future work (Nakar, in preparation).…”

Section: Constraints On the X-ray Sourcementioning

confidence: 51%

The afterglow of a relativistic shock breakout and low-luminosity GRBs

Duran¹,

Nakar²,

Piran³

et al. 2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The prompt emission of low luminosity gamma-ray bursts (llGRBs) indicates that these events originate from a relativistic shock breakout. In this case, we can estimate, based on the properties of the prompt emission, the energy distribution of the ejecta. We develop a general formalism to estimate the afterglow produced by synchrotron emission from the forward shock resulting from the interaction of this ejecta with the circum-burst matter. We assess whether this emission can produce the observed radio and X-ray afterglows of the available sample of 4 llGRBs. All 4 radio afterglows can be explained within this model, providing further support for shock breakouts being the origin of llGRBs. We find that in one of the llGRBs (GRB 031203), the predicted X-ray emission, using the same parameters that fit the radio, can explain the observed one. In another one (GRB 980425), the observed X-rays can be explained if we allow for a slight modification of the simplest model. For the last two cases (GRBs 060218 and 100316D), we find that, as is the case for previous attempts to model these afterglows, the simplest model that fits the radio emission underpredicts the observed X-ray afterglows. Using general arguments, we show that the most natural location of the X-ray source is, like the radio source, within the ejecta-external medium interaction layer but that emission is due to a different population of electrons or to a different emission process.

show abstract

“…Cooling and recombination may cause the stream to fragment, resulting in the formation of discrete clumps within the stream (Roos 1992; ), but will not affect the vertical spread in velocity as the stream will not be self-gravitating after its first return to periapse. However, heating of the stream through an oblique shock at periapse (Matzner et al 2013;Salbi et al 2014) may increase this vertical spread, this would increase the typical stream widths and would result in streams that self-intersect after fewer windings than what is presented here. Lastly, the magnetic fields that permeate the star likely thread through the stellar debris and potentially become dynamically relevant once the gas pressure drops sufficiently, this additional pressure support may also increase the width of the stream.…”

Section: Discussionmentioning

confidence: 73%

A Dark Year for Tidal Disruption Events

Guillochon

Ramírez-Ruiz

2015

ApJ

204

241

View full text Add to dashboard Cite

Main-sequence disruptions of stars by supermassive black holes result in the production of an extended, geometrically thin debris stream winding repeatedly around the black hole. In the absence of black hole spin, in-plane relativistic precession causes this stream to intersect with itself after a single winding. In this paper we show that relativistic precessions arising from black hole spin can induce deflections out of the original orbital plane that prevent the stream from self-intersecting even after many windings. This naturally leads to a "dark period" in which the flare is not observable for some time, persisting for up to a dozen orbital periods of the most bound material, which translates to years for disruptions around black holes with masses ∼ 10 7 M . When the stream eventually self-intersects, the distance from the black hole and the angle at which this collision occurs determines the rate of energy dissipation. We find that more-massive black holes (M h 10 7 M ) tend to have more violent stream self-intersections, resulting in prompt accretion. For these tidal disruption events (TDEs), the accretion rate onto the black hole should still closely follow the original fallback rate after a fixed delay time t delay ,Ṁ acc (t + t delay ) =Ṁ fb (t). For lower black hole masses (M h 10 6 ), we find that flares are typically slowed down by about an order of magnitude, resulting in the majority of TDEs being sub-Eddington at peak. This also implies that current searches for TDEs are biased towards prompt flares, with slowed flares likely having been unidentified.

show abstract

Oblique Shock Breakout in Supernovae and Gamma-Ray Bursts. Ii. Numerical Solutions for Non-Relativistic Pattern Speeds

Cited by 21 publications

References 20 publications

Aspherical Supernovae: Effects on Early Light Curves

Aspherical Supernovae: Effects on Early Light Curves

The afterglow of a relativistic shock breakout and low-luminosity GRBs

A Dark Year for Tidal Disruption Events

Contact Info

Product

Resources

About