Enhanced mass-loss rate evolution of stars with ≳18 M⊙ and missing optically observed type II core-collapse supernovae

Gofman, Roni Anna; Gluck, Naomi; Soker, Noam

doi:10.1093/mnras/staa1085

Cited by 6 publications

(3 citation statements)

References 85 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This is roughly consistent with the rate estimate from Eldridge et al (2018) (∼ 4.7%; see §4.3). Recently, Gofman et al (2020) apply enhanced mass-loss rates to RSGs and found that massive RSGs (M ZAMS 20-21 M ) with a similar M Henv range (∼ 0.8-1.8 M ) to that of our short-plateau SN models end up as dustunobscured SNe II. They roughly estimate a rate of this class to be 2-4% of all SNe II, which is similar to our estimate of short-plateau SNe.…”

Section: Implications For the Rsg Problemmentioning

confidence: 54%

Luminous Type II Short-Plateau Supernovae 2006Y, 2006ai, and 2016egz: A Transitional Class from Stripped Massive Red Supergiants

Hiramatsu

Howell

Moriya

et al. 2021

ApJ

View full text Add to dashboard Cite

The diversity of Type II supernovae (SNe II) is thought to be driven mainly by differences in their progenitor’s hydrogen-rich (H-rich) envelope mass, with SNe IIP having long plateaus (∼100 days) and the most massive H-rich envelopes. However, it is an ongoing mystery why SNe II with short plateaus (tens of days) are rarely seen. Here, we present optical/near-infrared photometric and spectroscopic observations of luminous Type II short-plateau SNe 2006Y, 2006ai, and 2016egz. Their plateaus of about 50–70 days and luminous optical peaks (≲−18.4 mag) indicate significant pre-explosion mass loss resulting in partially stripped H-rich envelopes and early circumstellar material (CSM) interaction. We compute a large grid of MESA+STELLA single-star progenitor and light-curve models with various progenitor zero-age main-sequence (ZAMS) masses, mass-loss efficiencies, explosion energies, 56Ni masses, and CSM densities. Our model grid shows a continuous population of SNe IIP–IIL–IIb-like light-curve morphology in descending order of H-rich envelope mass. With large 56Ni masses (≳0.05 M ⊙), short-plateau SNe II lie in a confined parameter space as a transitional class between SNe IIL and IIb. For SNe 2006Y, 2006ai, and 2016egz, our findings suggest high-mass red supergiant (RSG) progenitors (M ZAMS ≃ 18–22 M ⊙) with small H-rich envelope masses ( ) that have experienced enhanced mass loss ( ) for the last few decades before the explosion. If high-mass RSGs result in rare short-plateau SNe II, then these events might ease some of the apparent underrepresentation of higher-luminosity RSGs in observed SN II progenitor samples.

show abstract

Section: Implications For the Rsg Problemmentioning

confidence: 54%

Luminous Type II Short-Plateau Supernovae 2006Y, 2006ai, and 2016egz: A Transitional Class from Stripped Massive Red Supergiants

Hiramatsu

Howell

Moriya

et al. 2021

ApJ

View full text Add to dashboard Cite

show abstract

“…Pre-SN outbursts are often observed especially in Type IIn that display narrow emission lines for extended times after the explosion (e.g., Ofek et al 2014) as a consequence of the shock interaction between the slow-moving circumstellar medium (CSM) and the ejected material of the explosion (Smith 2014). However, the underlying physical mechanism that triggers those outbursts and the mass loss rates involved remain elusive (e.g., Beasor et al 2020;Gofman et al 2020;Humphreys et al 2020;Hosseinzadeh et al 2022;Ou et al 2023). Direct identification of progenitors and the environments of stars via preexplosion imaging becomes crucial in understanding these unsolved questions.…”

Section: Introductionmentioning

confidence: 99%

The Preexplosion Environments and the Progenitor of SN 2023ixf from the Hobby–Eberly Telescope Dark Energy Experiment (HETDEX)

Liu,

Chen,

et al. 2023

ApJL

View full text Add to dashboard Cite

Supernova (SN) 2023ixf was discovered on 2023 May 19. The host galaxy, M101, was observed by the Hobby–Eberly Telescope Dark Energy Experiment collaboration over the period 2020 April 30–2020 July 10, using the Visible Integral-field Replicable Unit Spectrograph (3470 ≲ λ ≲ 5540 Å) on the 10 m Hobby–Eberly Telescope. The fiber filling factor within ±30″ of SN 2023ixf is 80% with a spatial resolution of 1″. The r < 5.″5 surroundings are 100% covered. This allows us to analyze the spatially resolved preexplosion local environments of SN 2023ixf with nebular emission lines. The two-dimensional maps of the extinction and the star formation rate (SFR) surface density (ΣSFR) show weak increasing trends in the radial distributions within the r < 5.″5 regions, suggesting lower values of extinction and SFR in the vicinity of the progenitor of SN 2023ixf. The median extinction and that of the surface density of SFR within r < 3″ are E(B − V) = 0.06 ± 0.14, and Σ SFR = 10 − 5.44 ± 0.66 M ☉ yr − 1 arcsec − 2 . There is no significant change in extinction before and after the explosion. The gas metallicity does not change significantly with the separation from SN 2023ixf. The metal-rich branch of the R 23 calculations indicates that the gas metallicity around SN 2023ixf is similar to the solar metallicity (∼Z ☉). The archival deep images from the Canada–France–Hawaii Telescope Legacy Survey (CFHTLS) show a clear detection of the progenitor of SN 2023ixf in the z band at 22.778 ± 0.063 mag, but nondetections in the remaining four bands of CFHTLS (u, g, r, i). The results suggest a massive progenitor of ≈22 M ☉.

show abstract

“…To the contrary, the collapse of the core to form a black hole will probably lead to a super-energetic CCSN, i.e., an explosion energy of E exp > 10 52 erg (Gilkis et al 2016). The two explosion mechanisms differ in some of their other predictions (e.g., Gofman et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Simulating the inflation of bubbles by late jets in core collapse supernova ejecta

Akashi,

Soker

2020

Preprint

Self Cite

View full text Add to dashboard Cite

We conducted three-dimensional hydrodynamical simulations to study the interaction of two late opposite jets with the ejecta of a core collapse supernova (CCSN), and study the bipolar structure that results from this interaction as the jets inflate hot-low-density bubbles. The newly born central object, a neutron star (NS; or a black hole), launches these jets at about 50 to 100 days after explosion. The bubbles cross the photosphere in the polar directions at much earlier times than the regions at the same radii near the equatorial plane. The hot bubbles releases more radiation and the photosphere recedes more rapidly in the tenuous bubble. Our results strengthen earlier claims that were based on toy models that such an interaction might lead to a late peak in the light curve, and that an equatorial observer might see a rapid drop in the light curve. Our results have implications to much earlier jets that explode the star, either jets that the newly born NS launches in a CCSN, or jets that a NS companion that merges with the core of a massive star launches in a common envelope jets supernova (CEJSN) event. Our results add indirect support to the CEJSN scenario for fast blue optical transients, e.g.,

show abstract

Enhanced mass-loss rate evolution of stars with ≳18 M⊙ and missing optically observed type II core-collapse supernovae

Cited by 6 publications

References 85 publications

Luminous Type II Short-Plateau Supernovae 2006Y, 2006ai, and 2016egz: A Transitional Class from Stripped Massive Red Supergiants

Luminous Type II Short-Plateau Supernovae 2006Y, 2006ai, and 2016egz: A Transitional Class from Stripped Massive Red Supergiants

The Preexplosion Environments and the Progenitor of SN 2023ixf from the Hobby–Eberly Telescope Dark Energy Experiment (HETDEX)

Simulating the inflation of bubbles by late jets in core collapse supernova ejecta

Contact Info

Product

Resources

About