Shock Breakout in Three-dimensional Red Supergiant Envelopes

Goldberg, Jared A.; Jiang, Yan-Fei; Bildsten, Lars

doi:10.3847/1538-4357/ac75e3

Cited by 27 publications

(12 citation statements)

References 59 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…When heated by the shock at breakout, these layers are immediately ionized and become optically thick, and their high density becomes immediately inadequate for radiation transport. While realistic 3D RSG models are the way forward (Goldberg et al 2022b), one may in 1D, and for a start, extend the RSG atmospheres out to low density to allow for a proper physical handling of the breakout phase. Davies et al (2022) argued that a decade-long increase in mass loss at the RSG surface could lead to a dramatic and prolonged extinction of the underlying star until core collapse.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Radiative-transfer modeling of nebular-phase type II supernovae

Dessart

Hillier

2020

A&A

View full text Add to dashboard Cite

Nebular phase spectra of core-collapse supernovae (SNe) provide critical and unique information on the progenitor massive star and its explosion. We present a set of 1-D steady-state non-local thermodynamic equilibrium radiative transfer calculations of type II SNe at 300 d after explosion. Guided by results for a large set of stellar evolution simulations, we craft ejecta models for type II SNe from the explosion of a 12, 15, 20, and 25 M star. The ejecta density structure and kinetic energy, the 56 Ni mass, and the level of chemical mixing are parametrized. Our model spectra are sensitive to the adopted line Doppler width, a phenomenon we associate with the overlap of Fe ii and O i lines with Ly α and Ly β. Our spectra show a strong sensitivity to 56 Ni mixing since it determines where decay power is absorbed. Even at 300 d after explosion, the H-rich layers reprocess the radiation from the inner metal rich layers. In a given progenitor model, variations in 56 Ni mass and distribution impact the ejecta ionization, which can modulate the strength of all lines. Such ionization shifts can quench Ca ii line emission. In our set of models, the [O i] λλ 6300, 6364 doublet strength is the most robust signature of progenitor mass. However, we emphasize that convective shell merging in the progenitor massive star interior can pollute the O-rich shell with Ca, which will weaken the O i doublet flux in the resulting nebular SN II spectrum. This process may occur in Nature, with a greater occurrence in higher mass progenitors, and may explain in part the preponderance of progenitor masses below 17 M inferred from nebular spectra.

show abstract

Section: Conclusion and Discussionmentioning

confidence: 99%

Radiative-transfer modeling of nebular-phase type II supernovae

Dessart

Hillier

2020

A&A

View full text Add to dashboard Cite

show abstract

“…However, alternate pathways regarding the initial rise times and enhanced luminosity are being studied theoretically. The detailed studies of the hydrogen-rich layer in 3D models (Goldberg et al 2022) could also reveal the initial behavior of the peak if other shreds of evidence are scarce.…”

Section: Introductionmentioning

confidence: 99%

SN 2018gj: A Short Plateau Type II Supernova with Persistent Blueshifted Ha Emission

Teja,

Singh,

Sahu

et al. 2023

ApJ

View full text Add to dashboard Cite

We present an extensive, panchromatic photometric (UV, optical, and near-IR) and low-resolution optical spectroscopic coverage of a Type IIP supernova SN 2018gj that occurred on the outskirts of the host galaxy NGC 6217. From the V-band light curve, we estimate the plateau length to be ∼ 70 ± 2 days, placing it among the very few well-sampled short plateau supernovae (SNe). With V-band peak absolute magnitude M V ≤ −17.0 ± 0.1 mag, it falls in the middle of the luminosity distribution of the Type II SNe. The color evolution is typical to other Type II SNe except for an early elbow-like feature in the evolution of V − R color owing to its early transition from the plateau to the nebular phase. Using the expanding photospheric method, we present an independent estimate of the distance to SN 2018gj. We report the spectral evolution to be typical of a Type II SNe. However, we see a persistent blueshift in emission lines until the late nebular phase, not ordinarily observed in Type II SNe. The amount of radioactive nickel (56Ni) yield in the explosion was estimated to be 0.026 ± 0.007 M ⊙. We infer from semianalytical modeling, nebular spectrum, and 1D hydrodynamical modeling that the probable progenitor was a red supergiant with a zero-age-main-sequence mass ≤13 M ⊙. In the simulated hydrodynamical model light curves, reproducing the early optical bolometric light curve required an additional radiation source, which could be the interaction with the proximal circumstellar matter.

show abstract

“…The star formation rate and the mass of cNE are consistent with some of the hosts of SGRBs and LGRBs (orange circles and yellow circles, respectively, in the right panel of Figure 5). An SBO origin of the XRT 210423 is very unlikely, given the low probability to have such a high peak luminosity (L X,peak  10 45 erg s −1 for supernova SBOs; Soderberg et al 2008;Waxman & Katz 2017;Goldberg et al 2022), offset (see Figure 5; Kelly & Kirshner 2012;Uddin et al 2020;Schulze et al 2021), M * , and SFR (see Figure 5; Galbany et al 2014).…”

Section: Assuming Cne Is the Host Galaxy For Xrt 210423mentioning

confidence: 99%

The Fast X-Ray Transient XRT 210423 and Its Host Galaxy

Eappachen

Jonker

Levan

et al. 2023

ApJ

View full text Add to dashboard Cite

Fast X-ray Transients (FXTs) are X-ray flares with durations ranging from a few hundred seconds to a few hours. Possible origins include the tidal disruption of a white dwarf by an intermediate-mass black hole, a supernova shock breakout, or a binary neutron star merger. We present the X-ray light curve and spectrum as well as deep optical imaging of the FXT XRT 210423, which has been suggested to be powered by a magnetar produced in a binary neutron star merger. Our Very Large Telescope and Gran Telescopio Canarias (GTC) observations began on 2021 May 6, thirteen days after the onset of the flare. No transient optical counterpart is found in the 1.″ (3σ) X-ray uncertainty region of the source to a depth g s = 27.0 AB mag. (We use the word “counterpart” for any transient light in a wave band other than the original X-ray detection wave band, whereas the word “host” refers to the host galaxy.) A candidate host lies within the 1.″ X-ray uncertainty region with a magnitude of 25.9 ± 0.1 in the GTC/HiPERCAM g s filter. Due to its faintness, it was not detected in other bands, precluding a photometric redshift determination. We detect two additional candidate host galaxies: one with z spec = 1.5082 ± 0.0001 and an offset of 4.″2 ± 1.″ (37 ± 9 kpc) from the FXT, and another one with z phot = 1.04 − 0.14 + 0.22 and an offset of 3.″6 ± 1.″ (30 ± 8 kpc). Based on the properties of all the prospective hosts, we favor a binary neutron star merger, as previously suggested in the literature, as the explanation for XRT 210423.

show abstract

Shock Breakout in Three-dimensional Red Supergiant Envelopes

Cited by 27 publications

References 59 publications

Radiative-transfer modeling of nebular-phase type II supernovae

Radiative-transfer modeling of nebular-phase type II supernovae

SN 2018gj: A Short Plateau Type II Supernova with Persistent Blueshifted Ha Emission

The Fast X-Ray Transient XRT 210423 and Its Host Galaxy

Contact Info

Product

Resources

About