SN 2009N: linking normal and subluminous Type II-P SNe

Takáts, K.; Pumo, M. L.; Elias‐Rosa, N.; Pastorello, A.; Pignata, G.; Paillas, Enrique; Zampieri, L.; Anderson, J. P.; Vinkó, J.; Benetti, S.; Botticella, M. T.; Bufano, F.; Campillay, A.; Cartier, R.; Ergon, M.; Folatelli, G.; Foley, R. J.; Förster, F.; Hamuy, M.; Hentunen, V. P.; Kankare, E.; Leloudas, G.; Morrell, N.; Nissinen, M.; Phillips, M. M.; Smartt, S. J.; Stritzinger, M. D.; Taubenberger, S.; Valenti, S.; Dyk, Schuyler D. Van; Haislip, J.; Lacluyzé, A.; Moore, J. P.; Reichart, D.

doi:10.1093/mnras/stt2203

Cited by 69 publications

(61 citation statements)

References 78 publications

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“…This event was not as luminous as a normal Type IIP SN, but it was brighter than the underluminous SN 2005cs. Hydrodynamic modeling was presented by Takáts et al (2014) who applied the code of Pumo et al (2010) and Pumo & Zampieri (2011). In Table 4, we summarize our results as well as the properties from hydrodynamic simulations.…”

Section: Sn 2009nmentioning

confidence: 95%

“…For better comparison, we used d = 8.4 Mpc for the distance of M51, Tsvetkov et al (2006). Takáts et al (2014). which was adopted by Tsvetkov et al (2006). However, we also calculated the quasi-bolometric light curve with d = 7.1 Mpc (Takáts & Vinkó 2006).…”

Section: Sn 2005csmentioning

confidence: 99%

“…SN 2009N was discovered in NGC 4487 having a distance of 21.6 Mpc (Takáts et al 2014). The first images were taken by Itagaki on 2009 Jan. 24.86 and 25.62 UT (Nakano et al 2009).…”

Section: Sn 2009nmentioning

confidence: 99%

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A semianalytical light curve model and its application to type IIP supernovae

Nagy

Ordasi

Vinkó

et al. 2014

A&A

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The aim of this work is to present a semianalytical light curve model code that can be used for estimating physical properties of core collapse supernovae (SNe) in a quick and efficient way. To verify our code we fit light curves of Type II SNe and compare our best parameter estimates to those from hydrodynamical calculations. For this analysis, we use quasi-bolometric light curves of five different Type IIP SNe. In each case, we obtain appropriate results for initial pre-supernova parameters. We conclude that this semianalytical light curve model is useful to obtaining approximate physical properties of Type II SNe without using time-consuming numerical hydrodynamic simulations.

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Section: Sn 2009nmentioning

confidence: 95%

Section: Sn 2005csmentioning

confidence: 99%

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A semianalytical light curve model and its application to type IIP supernovae

Nagy

Ordasi

Vinkó

et al. 2014

A&A

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“…Also the code computes the fallback of material on the central compact object and consequently determines the amount of 56 Ni in the ejected envelope at late times. The code has been widely used to model the observations of core-collapse SNe (e.g., Pastorello et al 2012;Dall'Ora et al 2014;Spiro et al 2014;Takáts et al 2014), having also the capability of simulating the bolometric lightcurve and the time evolution of the photospheric velocity and temperature.…”

Section: Modeling the Post-explosion Evolution Of The Snmentioning

confidence: 99%

Modeling SNR Cassiopeia a From the Supernova Explosion to Its Current Age: The Role of Post-Explosion Anisotropies of Ejecta

Orlando

Miceli

Pumo

et al. 2016

ApJ

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113

138

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The remnants of core-collapse supernovae (SNe) have complex morphologies that may reflect asymmetries and structures developed during the progenitor SN explosion. Here we investigate how the morphology of the supernova remnant Cassiopeia A (Cas A) reflects the characteristics of the progenitor SN with the aim of deriving the energies and masses of the post-explosion anisotropies responsible for the observed spatial distribution of Fe and Si/S. We model the evolution of Cas A from the immediate aftermath of the progenitor SN to the three-dimensional interaction of the remnant with the surrounding medium. The post-explosion structure of the ejecta is described by small-scale clumping of material and larger-scale anisotropies. The hydrodynamic multi-species simulations consider an appropriate post-explosion isotopic composition of the ejecta. The observed average expansion rate and shock velocities can be well reproduced by models with ejecta mass M ej ≈4M e and explosion energy E SN ≈2.3×10 51 erg. The post-explosion anisotropies (pistons) reproduce the observed distributions of Fe and Si/ S if they had a total mass of ≈0.25 M e and a total kinetic energy of ≈1.5×10 50 erg. The pistons produce a spatial inversion of ejecta layers at the epoch of Cas A, leading to the Si/S-rich ejecta physically interior to the Fe-rich ejecta. The pistons are also responsible for the development of the bright rings of Si/S-rich material which form at the intersection between the reverse shock and the material accumulated around the pistons during their propagation. Our result supports the idea that the bulk of asymmetries observed in Cas A are intrinsic to the explosion.

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“…The left panel of Fig.5 compares the photospheric velocity of the model Ldep5d39uni to that of the model without the pre-SN energy injection. Also shown here are the observational data of several SNe IIP (Takáts & Vinkó 2012;Takáts et al 2014;Tomasella et al 2013) The model Ldep5d39uni has a relatively constant photospheric velocity during the first ∼ 50 days from the explosion. After that, it gradually declines.…”

Section: Photospheric Velocitymentioning

confidence: 97%

Constraining Massive Star Activities in the Final Years through Properties of Supernovae and Their Progenitors

Ouchi

Maeda

2020

Proceedings of the 15th International Symposium on Origin of Matter and Evolution of Galaxies (OMEG15)

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Recent observations of supernovae (SNe) just after the explosion suggest that a good fraction of SNe have the confined circumstellar material (CSM) in the vicinity, and the pre-SN enhanced mass loss may be a common property. The physical mechanism of this phenomenon is still unclarified, and the energy deposition into the envelope has been proposed as a possible cause of the confined CSM. In this work, we have calculated the response of the envelope to various types of sustained energy deposition starting from a few years before the core collapse. We have further investigated how the resulting progenitor structure would affect appearance of the ensuing supernova. While it has been suspected that a super-Eddington energy deposition may lead to a strong and/or eruptive mass loss to account for the confined CSM, we have found that a highly super-Eddington energy injection into the envelope changes the structure of the progenitor star substantially, and the properties of the resulting SNe become inconsistent with usual SNe. This argument constrains the energy budget involved in the possible stellar activity in the final years to be at most one order of magnitude higher than the Eddington luminosity. Such an energy generation however would not dynamically develop a strong wind in the time scale of a few years. We therefore propose that a secondary effect (e.g., pulsation or binary interaction) triggered by the moderate envelope inflation, which is caused by sub-Eddington energy injection, likely induces the mass loss.

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SN 2009N: linking normal and subluminous Type II-P SNe

Cited by 69 publications

References 78 publications

A semianalytical light curve model and its application to type IIP supernovae

A semianalytical light curve model and its application to type IIP supernovae

Modeling SNR Cassiopeia a From the Supernova Explosion to Its Current Age: The Role of Post-Explosion Anisotropies of Ejecta

Constraining Massive Star Activities in the Final Years through Properties of Supernovae and Their Progenitors

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