INTERACTING SUPERNOVAE AND SUPERNOVA IMPOSTORS: SN 2009ip, IS THIS THE END?

Pastorello, A.; Cappellaro, E.; Inserra, C.; Smartt, S. J.; Pignata, G.; Benetti, S.; Valenti, S.; Fraser, M.; Takáts, K.; Benitez, S.; Botticella, M. T.; Brimacombe, J.; Bufano, F.; Cellier-Holzem, F.; Costado, M. T.; Cupani, G.; Curtis, Ivan A.; Elias‐Rosa, N.; Ergon, M.; Fynbo, J. P. U.; Hambsch, Franz-Josef; Hamuy, M.; Harutyunyan, A.; Ivarson, K.; Kankare, E.; Martin, John; Kotak, R.; Lacluyzé, A.; Maguire, K.; Mattila, S.; Maza, J.; McCrum, M.; Miluzio, M.; Nørgaard-Nielsen, H. U.; Nysewander, M.; Ochner, P.; Pan, Y. C.; Pumo, M. L.; Reichart, D. E.; Tan, T. G.; Taubenberger, S.; Tomasella, L.; Turatto, M.; Wright, D. E.

doi:10.1088/0004-637x/767/1/1

Cited by 233 publications

(343 citation statements)

References 73 publications

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“…The optical photometry was calibrated based on the SDSS DR9 ugriz magnitudes of 15 field stars. For the Johnson-Cousins filters, (Pastorello et al 2013;Fraser et al 2013Fraser et al , 2015, black curve: JD = 2 456 155 corresponds to day 0, no shift in magnitude; and green curve: day 0 epoch JD = 2 456 195, +3.0 mag shift) emphasizing the similar evolution between some of the key phases. b) Colour evolution of SNHunt248.…”

Section: Observationsmentioning

confidence: 99%

On the triple peaks of SNHunt248 in NGC 5806

Kankare

Kotak

Pastorello

et al. 2015

A&A

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We present our findings on a supernova (SN) impostor, SNHunt248, based on optical and near-IR data spanning ∼15 yr before discovery, to ∼1 yr post-discovery. The light curve displays three distinct peaks, the brightest of which is at M R ∼ −15.0 mag. The post-discovery evolution is consistent with the ejecta from the outburst interacting with two distinct regions of circumstellar material. The 0.5-2.2 μm spectral energy distribution at −740 d is well-matched by a single 6700 K blackbody with log(L/L ) ∼ 6.1. This temperature and luminosity support previous suggestions of a yellow hypergiant progenitor; however, we find it to be brighter than the brightest and most massive Galactic late-F to early-G spectral type hypergiants. Overall the historical light curve displays variability of up to ∼±1 mag. At current epochs (∼1 yr post-outburst), the absolute magnitude (M R ∼ −9 mag) is just below the faintest observed historical absolute magnitude ∼10 yr before discovery.

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Section: Observationsmentioning

confidence: 99%

On the triple peaks of SNHunt248 in NGC 5806

Kankare

Kotak

Pastorello

et al. 2015

A&A

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“…Most of these come from the inference of large amounts of circumstellar material in the close vicinity of the progenitor star, such as in SN 2006gy (Smith et al 2007). (Smith et al 2010;Mauerhan et al 2013;Foley et al 2011;Pastorello et al 2013), and SN 2010jl (Smith et al 2011b). The high luminosity of the progenitor has been used as evidence for the star having initial masses M ini > 50 M .…”

Section: When Lbvs Are Sn Progenitors and Their Sn Typesmentioning

confidence: 99%

Fundamental properties of core-collapse supernova and GRB progenitors: predicting the look of massive stars before death

Groh

Meynet

Georgy

et al. 2013

A&A

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We investigate the fundamental properties of core-collapse supernova (SN) progenitors from single stars at solar metallicity. For this purpose, we combine Geneva stellar evolutionary models with initial masses of M ini = 20−120 M with atmospheric and wind models using the radiative transfer code CMFGEN. We provide synthetic photometry and high-resolution spectra of hot stars at the pre-SN stage. For models with M ini = 9−20 M , we supplement our analysis using publicly available MARCS model atmospheres of RSGs to estimate their synthetic photometry. We employ well-established observational criteria of spectroscopic classification and find that, depending on their initial mass and rotation, massive stars end their lives as red supergiants (RSG), yellow hypergiants (YHG), luminous blue variables (LBV), and Wolf-Rayet (WR) stars of the WN and WO spectral types. For rotating models, we obtained the following types of SN progenitors:, and RSGs (9 ≤ M ini ≤ 18 M ). For non-rotating models, we found spectral types WO1-, and RSGs (9 ≤ M ini ≤ 20 M ). Our rotating models indicate that SN IIP progenitors are all RSG, SN IIL/b progenitors are 56% LBVs and 44% YHGs, SN Ib progenitors are 96% WN10-11 and 4% WOs, and SN Ic progenitors are all WO stars. We find that the most massive and luminous SN progenitors are not necessarily the brightest ones in a given filter, since this depends on their luminosity, temperature, wind density, and the way the spectral energy distribution compares to a filter bandpass. We find that SN IIP progenitors (RSGs) are bright in the RIJHK S filters and faint in the UB filters. SN IIL/b progenitors (LBVs and YHGs), and SN Ib progenitors (WNs) are relatively bright in optical/infrared filters, while SN Ic progenitors (WOs) are faint in all optical filters. We argue that SN Ib and Ic progenitors from single stars should be undetectable in the available pre-explosion images with the current magnitude limits, in agreement with observational results.

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“…The progenitor of Type IIn SN 2005gl is found to have an absolute brightness of M V −10 mag and it belongs to the most luminous class of stars. The progenitor of Type IIn SN 2009ip provided us with more remarkable information about the progenitors' activities (e.g., Margutti et al 2014;Smith et al 2014;Mauerhan et al 2013;Prieto et al 2013; but see also Fraser et al 2013a;Pastorello et al 2013). The luminosity of the progenitor was again close to M V = −10 mag, and it is presumed to be near the Eddington luminosity.…”

Section: Introductionmentioning

confidence: 98%

Mass loss of massive stars near the Eddington luminosity by core neutrino emission shortly before their explosion

Moriya

2014

A&A

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We present a novel mechanism for enhancing the mass-loss rates of massive stars shortly before their explosion. The neutrino luminosities of the stellar core of massive stars increase as they get closer to the time of the core collapse. As emitted neutrinos escape freely from the core, the core mass is significantly reduced when the neutrino luminosity is high. If a star is near the Eddington luminosity when the neutrino luminosity is high, the star can exceed the Eddington luminosity because of the core neutrino mass loss. We suggest that the stellar surface mass-loss rates due to the core neutrino emission can be higher than 10 −4 M yr −1 from ∼1 year before the core collapse. The mass-loss rates can exceed 10 −2 M yr −1 ∼ 10 days before the core collapse. This mass-loss mechanism may be able to explain the enhanced mass loss observed in some supernova progenitors shortly before their explosion. Even if the star is not close enough to the Eddington luminosity to enhance the mass loss, the star can still expand because of the reduced gravitational force. This mechanism can be activated in Wolf-Rayet stars, and it can create the hydrogen-poor, as well as hydrogen-rich, dense circumstellar media observed in some supernovae.

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INTERACTING SUPERNOVAE AND SUPERNOVA IMPOSTORS: SN 2009ip, IS THIS THE END?

Cited by 233 publications

References 73 publications

On the triple peaks of SNHunt248 in NGC 5806

On the triple peaks of SNHunt248 in NGC 5806

Fundamental properties of core-collapse supernova and GRB progenitors: predicting the look of massive stars before death

Mass loss of massive stars near the Eddington luminosity by core neutrino emission shortly before their explosion

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