Ejection of the Massive Hydrogen-rich Envelope Timed with the Collapse of the Stripped SN 2014C

Margutti, R.; Kamble, A.; Milisavljevic, Dan; Zapartas, Emmanouil; Mink, S. E. de; Drout, M. R.; Chornock, R.; Risaliti, G.; Zauderer, B. A.; Bietenholz, M. F.; Cantiello, Matteo; Chakraborti, Sayan; Chomiuk, Laura; Fong, W.; Grefenstette, Brian W.; Guidorzi, C.; Kirshner, R.; Parrent, J.; Patnaude, Daniel; Söderberg, A. M.; Gehrels, N.; Harrison, Fiona A.

doi:10.3847/1538-4357/835/2/140

Cited by 171 publications

(308 citation statements)

References 147 publications

(234 reference statements)

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“…It also, unusually, kept brightening in X-rays till t ∼ 1 yr (Margutti et al 2017), and Hα emission was still detected as late as t 892 d (Vinko et al 2017). In the mid-infrared, it had an almost constant brightness till t ∼ 800 d, with even a possible slight re-brightening near t ∼ 250 d (Tinyanont et al 2016).…”

Section: Introductionmentioning

confidence: 93%

“…We adopt the updated Cepheid distance of D = 15.1 ± 0.7 Mpc from Saha et al (2006). We also adopt an explosion date, t = 0, of 2013 December 30.0 (UT) = MJD 56656.0, as determined by Margutti et al (2017) from bolometric lightcurve modelling.…”

Section: Introductionmentioning

confidence: 99%

“…A 16-GHz radio lightcurve from the Arcminute Microkelvin Imager was presented by Anderson et al (2017), who found a very unusual two-peaked lightcurve, with the first peak at t 80 d, and a second at t 400 d. A paper on our multi-frequency flux-density monitoring of SN 2014C with the Jansky Very Large Array is in preparation (Kamble et al). Milisavljevic et al (2015) and Margutti et al (2017) suggest a scenario where SN 2014C's progenitor exploded inside a relatively low-density cavity, but within a year, the expanding shock encountered a massive H-rich shell (probably ∼ 1 M ) at radius, r16 ∼ 6, where r16 is a dimensionless radius, and r16 = r/(10 16 cm). Such a shell is not expected from the standard metallicity-dependent line-driven mass-loss scenario (Kudritzki & Puls 2000;Nugis & Lamers 2000), and requires a different, highly time-dependent massloss mechanism that is active during the last centuries before the explosion.…”

Section: Introductionmentioning

confidence: 99%

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SN 2014C: VLBI images of a supernova interacting with a circumstellar shell

Bietenholz

Kamble

Margutti³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We report on VLBI measurements of supernova 2014C at several epochs between t = 384 and 1057 days after the explosion. SN 2014C was an unusual supernova that initially had Type Ib optical spectrum, but after t = 130 d it developed a Type IIn spectrum with prominent Hα lines, suggesting the onset of strong circumstellar interaction. Our first VLBI observation was at t = 384 d, and we find that the outer radius of SN 2014C was (6.40 ± 0.26) × 10 16 cm (for a distance of 15.1 Mpc), implying an average expansion velocity of 19300 ± 790 km s −1 up to that time. At our last epoch, SN 2014C was moderately resolved and shows an approximately circular outline but with an enhancement of the brightness on the W side. The outer radius of the radio emission at t = 1057 d is (14.9 ± 0.6) × 10 16 cm. We find that the expansion between t = 384 and 1057 d is well described by a constant velocity expansion with v = 13600 ± 650 km s −1 . SN 2014C had clearly been substantially decelerated by t = 384 d. Our measurements are compatible with a scenario where the expanding shock impacted upon a shell of dense circumstellar material during the first year, as suggested by the observations at other wavelengths, but had progressed through the dense shell by the time of the VLBI observations.

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Section: Introductionmentioning

confidence: 93%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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SN 2014C: VLBI images of a supernova interacting with a circumstellar shell

Bietenholz

Kamble

Margutti³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…It seems that the pre-explosion outbursts of CCSNe are common (e.g., Moriya et al 2014;Ofek et al 2014;Svirski & Nakar 2014;Tartaglia et al 2016;Yaron et al 2017), with about one in ten CCSNe suffering a pre-explosion outburst (e.g., Margutti et al 2017). The outburst might result from a single-star process, e.g., strong convection in the pre-collapsing core (Quataert & Shiode 2012;Shiode & Quataert 2014).…”

Section: Observational Consequencesmentioning

confidence: 99%

The two promising scenarios to explode core collapse supernovae

Soker

2017

Res. Astron. Astrophys.

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I compare to each other what I consider to be the two most promising scenarios to explode core-collapse supernovae (CCSNe). Both are based on the negative jet feedback mechanism (JFM). In the jittering jets scenario a collapsing core of a single slowly-rotating star can launch jets. The accretion disk or belt (a sub-Keplerian accretion flow concentrated toward the equatorial plane) that launches the jets is intermittent with varying directions of the axis. Instabilities, such as the standing accretion shock instability (SASI), lead to stochastic angular momentum variations that allow the formation of the intermittent accretion disk/belt. According to this scenario no failed CCSNe exist. According to the fixed axis scenario, the core of the progenitor star must be spun up during its late evolutionary phases, and hence all CCSNe are descendants of strongly interacting binary systems, most likely through a common envelope evolution (whether the companion survives or not). Due to the strong binary interaction, the axis of the accretion disk that is formed around the newly born neutron star has a more or less fixed direction. According to the fixed axis scenario, accretion disk/belt are not formed around the newly born neutron star of single stars; they rather end in failed CCSNe. I also raise the possibility that the jittering jets scenario operates for progenitors with initial mass of 8M ⊙ M ZAMS 18M ⊙ , while the fixed axis scenario operates for M ZAMS 18M ⊙ . For the first time these two scenarios are compared to each other, as well as to some aspects of neutrino-driven explosion mechanism. These new comparisons further suggest that the JFM plays a major role in exploding massive stars.

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“…The recent study on SN 2014C, which appeared as a SN Ib initially and evolved into a SN IIn over one year, indicates that the progenitor experienced a mass eruption about 100 years before the SN explosion (Milisavljevic et al 2015;Margutti et al 2016). A situation similar to this case may have occurred with Cas A.…”

Section: Impostor Of the Cas A Supernova?mentioning

confidence: 95%

The Korean 1592-1593 Record of a Guest Star: An 'Impostor' of the Cassiopeia a Supernova?

Park¹,

Yoon²,

Koo³

2016

Journal of The Korean Astronomical Society

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Abstract:The missing historical record of the Cassiopeia A (Cas A) supernova (SN) event implies a large extinction to the SN, possibly greater than the interstellar extinction to the current SN remnant. Here we investigate the possibility that the guest star that appeared near Cas A in 1592-1593 in Korean history books could have been an 'impostor' of the Cas A SN, i.e., a luminous transient that appeared to be a SN but did not destroy the progenitor star, with strong mass loss to have provided extra circumstellar extinction. We first review the Korean records and show that a spatial coincidence between the guest star and Cas A cannot be ruled out, as opposed to previous studies. Based on modern astrophysical findings on core-collapse SN, we argue that Cas A could have had an impostor and derive its anticipated properties. It turned out that the Cas A SN impostor must have been bright (M V = −14.7 ± 2.2 mag) and an amount of dust with visual extinction of ≥ 2.8 ± 2.2 mag should have formed in the ejected envelope and/or in a strong wind afterwards. The mass loss needs to have been spherically asymmetric in order to see the light echo from the SN event but not the one from the impostor event.

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Ejection of the Massive Hydrogen-rich Envelope Timed with the Collapse of the Stripped SN 2014C

Cited by 171 publications

References 147 publications

SN 2014C: VLBI images of a supernova interacting with a circumstellar shell

SN 2014C: VLBI images of a supernova interacting with a circumstellar shell

The two promising scenarios to explode core collapse supernovae

The Korean 1592-1593 Record of a Guest Star: An 'Impostor' of the Cassiopeia a Supernova?

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