SN 2009ib: a Type II-P supernova with an unusually long plateau

Takáts, K.; Pignata, G.; Pumo, M. L.; Paillas, Enrique; Zampieri, L.; Elias‐Rosa, N.; Benetti, S.; Bufano, F.; Cappellaro, E.; Ergon, M.; Fraser, M.; Hamuy, M.; Inserra, C.; Kankare, E.; Smartt, S. J.; Stritzinger, M. D.; Dyk, Schuyler D. Van; Haislip, J.; Lacluyzé, A.; Moore, J. P.; Reichart, D.

doi:10.1093/mnras/stv857

Cited by 67 publications

(35 citation statements)

References 90 publications

(131 reference statements)

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…The only SN for which our results can strongly constrain the mixing is SN 2009ib for which ηNi = 2.6. The light curve of SN 2009ib shows a long 130-day very smooth plateau (Takáts et al 2015). This light curve is very different than those that we see in our simulations where the 56 Ni is concentrated in the centre.…”

Section: Light Curvescontrasting

confidence: 96%

The role of radioactive nickel in shaping the plateau phase of Type II supernovae

Kozyreva

Nakar

Waldman

2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

In the present study, we systematically explore the effect of the radioactive 56 Ni and its mixing properties in the ejecta on the plateau of Type IIP supernovae (SNe). We evaluate the importance of 56 Ni in shaping light curves of SNe IIP by simulating light curves for two red supergiant models using different amounts of 56 Ni and with different types of mixing: uniform distribution of 56 Ni out to different fractions of the envelope and "boxcar" distribution of 56 Ni. We find, similarly to previous studies, that 56 Ni extends duration of the plateau. We find a formula to estimate the extension based on the observed bolometric light curves and show that for most SNe IIP 56 Ni extends the plateau by about 20 %. Another effect of 56 Ni consists in reduction of the plateau decline rate, i.e. 56 Ni presented in the ejecta flattens the plateau. Our simulations suggest that for typical SNe IIP it can reduce the decline rate by about 1 mag/100 day. We find that for the contribution of 56 Ni seen in most SNe our simulated bolometric light curves resemble observed ones for various types of 56 Ni mixing. We thereby cannot determine the level of 56 Ni mixing in these SNe based on the light curve alone. However, for SN 2009ib we find that only a model where 56 Ni is mixed significantly throughout most of the hydrogen envelope is consistent with the observed light curve. Our light curves are available via link https://wwwmpa.mpa-garching.mpg.de/ ccsnarchive/data/Kozyreva2018/.

show abstract

Section: Light Curvescontrasting

confidence: 96%

The role of radioactive nickel in shaping the plateau phase of Type II supernovae

Kozyreva

Nakar

Waldman

2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…One is that the end of the plateau phase ( 140 days after the explosion) is later than those of other LL SNe IIP for which good data covering the plateau available; ∼110 days in SNe 2003Z and 2009md (Spiro et al 2014;Fraser et al 2011). In fact, this epoch is still later than that of SN 2009ib (Takáts et al 2015), which shows the longest plateau length (∼130 days) among normal SNe IIP.…”

Section: Light Curvesmentioning

confidence: 92%

The Low-luminosity Type IIP Supernova 2016bkv with Early-phase Circumstellar Interaction

Nakaoka

Kawabata

Maeda

et al. 2018

ApJ

View full text Add to dashboard Cite

We present optical and near-infrared observations of a low-luminosity Type IIP supernova (SN) 2016bkv from the initial rising phase to the plateau phase. Our observations show that the end of the plateau is extended to 140 days since the explosion, indicating that this SN takes one of the longest time to finish the plateau phase. among Type IIP SNe (SNe IIP), including low-luminosity (LL) SNe IIP. The line velocities of various ions at the middle of the plateau phase are as low as 1,000-1,500 km s −1 , which is the lowest even among LL SNe IIP. These measurements imply that the ejecta mass in SN 2016bkv is larger than that of the well-studied LL IIP SN 2003Z. In the early phase, SN 2016bkv shows a strong bump in the light curve. In addition, the optical spectra in this bump phase exhibit a blue continuum accompanied with a narrow Hα emission line. These features indicate an interaction between the SN ejecta and the circumstellar matter (CSM) as in SNe IIn. Assuming the ejecta-CSM interaction scenario, the mass loss rate is estimated to be ∼1.7 × 10 −2 M ⊙ yr −1 within a few years before the SN explosion. This is comparable to or even larger than the largest mass loss rate observed for the Galactic red supergiants (∼10 −3 M ⊙ yr −1 for VY CMa). We suggest that the progenitor star of SN 2016bkv experienced a violent mass loss just before the SN explosion.

show abstract

“…Near-infrared photometry for the current sample will be presented in a separate paper. These data have been used previously for the study of specific objects (Schmidt et al 1994b;Zampieri et al 2003;Hamuy et al 2009;Krisciunas et al 2009;Mazzali et al 2009;Bersten et al 2011;Takáts et al 2015;Kleiser et al 2011). The subsample of SNeIIP has been used for the determination of distances using the "Expanding Photosphere Method" (Schmidt et al 1994a;Jones et al 2009) and the "Standardized Candle Method" (Hamuy & Pinto 2002;Nugent et al 2006;Poznanski et al 2009;Hamuy 2004;Olivares et al 2010;Rodríguez et al 2014), and for the determination of bolometric corrections (Bersten & Hamuy 2009).…”

Section: Introductionmentioning

confidence: 99%

UBVRIz LIGHT CURVES OF 51 TYPE II SUPERNOVAE

et al. 2016

View full text Add to dashboard Cite

We present a compilation of UBVRIz light curves of 51 type II supernovae discovered during the course of four different surveys during 1986-2003: the Cerro Tololo Supernova Survey, the Calán/Tololo Supernova Program (C&T), the Supernova Optical and Infrared Survey (SOIRS), and the Carnegie Type II Supernova Survey (CATS). The photometry is based on template-subtracted images to eliminate any potential host galaxy light contamination, and calibrated from foreground stars. This work presents these photometric data, studies the color evolution using different bands, and explores the relation between the magnitude at maximum brightness and the brightness decline parameter (s) from maximum light through the end of the recombination phase. This parameter is found to be shallower for redder bands and appears to have the best correlation in the B band. In addition, it also correlates with the plateau duration, being shorter (longer) for larger (smaller) s values.

show abstract

SN 2009ib: a Type II-P supernova with an unusually long plateau

Cited by 67 publications

References 90 publications

The role of radioactive nickel in shaping the plateau phase of Type II supernovae

The role of radioactive nickel in shaping the plateau phase of Type II supernovae

The Low-luminosity Type IIP Supernova 2016bkv with Early-phase Circumstellar Interaction

UBVRIz LIGHT CURVES OF 51 TYPE II SUPERNOVAE

Contact Info

Product

Resources

About