Helium Shell Detonations on Low-Mass White Dwarfs as a Possible Explanation for Sn 2005e

Waldman, Roni; Sauer, Daniel; Livne, Eli; Perets, Hagai B.; Glasner, Ariella; Mazzali, P. A.; Truran, J. W.; Gal‐Yam, A.

doi:10.1088/0004-637x/738/1/21

Cited by 126 publications

(231 citation statements)

References 44 publications

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“…If the progenitor system is not a NS-WD binary but rather a WD-WD binary (e.g., Perets et al 2010;Waldman et al 2011;Sim et al 2012;Dessart & Hillier 2015), then the remote locations require a different origin than SN kicks. One possibility, as noted above, is that group and cluster environments have a large proportion of stars in ICL, resulting from galaxy-galaxy stripping and galaxy mergers in the formation of the cluster.…”

Section: Discussionmentioning

confidence: 99%

“…Perets et al (2010) suggested SN 2005E may be the result of He detonation from accretion from a He white dwarf onto a CO white dwarf, one of several variants of WD-WD progenitors proposed (Waldman et al 2011;Sim et al 2012;Dessart & Hillier 2015). Another possibility is the tidal detonation of a He white dwarf by a neutron star or stellar-mass black hole (Metzger 2012;Sell et al 2015).…”

Section: Introductionmentioning

confidence: 99%

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Two New Calcium-rich Gap Transients in Group and Cluster Environments

Lunnan

Kasliwal

Cao

et al. 2017

ApJ

111

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We present the Palomar Transient Factory discoveries and the photometric and spectroscopic observations of PTF11kmb and PTF12bho. We show that both transients have properties consistent with the class of calcium-rich gap transients, specifically lower peak luminosities and rapid evolution compared to ordinary supernovae, and a nebular spectrum dominated by [Ca II] emission. A striking feature of both transients is their host environments: PTF12bho is an intracluster transient in the Coma Cluster, while PTF11kmb is located in a loose galaxy group, at a physical offset ∼150 kpc from the most likely host galaxy. Deep Subaru imaging of PTF12bho rules out an underlying host system to a limit of > -M 8.0 mag R , while Hubble Space Telescope imaging of PTF11kmb reveals a marginal counterpart that, if real, could be either a background galaxy or a globular cluster. We show that the offset distribution of Ca-rich gap transients is significantly more extreme than that seen for SNe Ia or even short-hard gamma-ray bursts (sGRBs). Thus, if the offsets are caused by a kick, they require higher kick velocities and/or longer merger times than sGRBs. We also show that almost all Ca-rich transients found to date are in group and cluster environments with elliptical host galaxies, indicating a very old progenitor population; the remote locations could partially be explained by these environments having the largest fraction of stars in the intragroup/ intracluster light following galaxy-galaxy interactions.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Two New Calcium-rich Gap Transients in Group and Cluster Environments

Lunnan

Kasliwal

Cao

et al. 2017

ApJ

111

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“…References for individual Ca-rich gap transients are provided in the main text. SN 2005E could also be reproduced by a combination of mostly 48 Cr, 52 Fe and 44 Ti decay, in which case, however, a ridiculously high 44 Ti mass in excess of 1 M would be needed (Waldman et al, 2011;Kasliwal et al, 2012). Without a more precise knowledge of the ejecta mass, this degeneracy cannot be resolved easily.…”

Section: Light Curves and Peak Luminositymentioning

confidence: 99%

“…An acceptable match to the bolometric light curves of Ca-rich transients can probably be obtained if these parameters are chosen accordingly. For instance, Waldman et al (2011) found that the detonation of a 0.2 M He shell on top of a 0.45 M WD provides a good match to the bolometric peak of SN 2005E, but a somewhat too rapid decline. For the same initial conditions, Sim et al (2012) obtained a slightly more complete nucleosynthesis, favouring the production of the short-lived 48 Cr at the expense of 44 Ti, resulting in a significantly brighter light-curve peak.…”

Section: Explosion Modelsmentioning

confidence: 99%

The Extremes of Thermonuclear Supernovae

Taubenberger¹

2016

Handbook of Supernovae

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The majority of thermonuclear explosions in the Universe seem to proceed in a rather standardised way, as explosions of carbon-oxygen (CO) white dwarfs in binary systems, leading to 'normal' Type Ia supernovae (SNe Ia). However, over the years a number of objects have been found which deviate from normal SNe Ia in their observational properties, and which require different and not seldom more extreme progenitor systems. While the 'traditional' classes of peculiar SNe Ia -luminous '91T-like' and faint '91bg-like' objects -have been known since the early 1990s, other classes of even more unusual transients have only been established 20 years later, fostered by the advent of new wide-field SN surveys such as the Palomar Transient Factory. These include the faint but slowly declining '02es-like' SNe, 'Ca-rich' transients residing in the luminosity gap between classical novae and supernovae, extremely short-lived, fast-declining transients, and the very luminous so-called 'super-Chandrasekhar' SNe Ia. Not all of them are necessarily thermonuclear explosions, but there are good arguments in favour of a thermonuclear origin for most of them. The aim of this chapter is to provide an overview of the zoo of potentially thermonuclear transients, reviewing their observational characteristics and discussing possible explosion scenarios.

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“…The relatively large abundances of intermediate elements such as 44 Ti can provide a more unique signature for He-rich collisions, though high abundances of these components can also be produced in the SD sub-Chandrasekhar and .Ia explosion models (Woosley et al 1986;Livne & Glasner 1991;Bildsten et al 2007;Shen & Bildsten 2009;Perets et al 2010;Waldman et al 2011)). Interestingly, recent observations (Troja et al 2014) suggest that the 44 Ti abundances in Tycho SN remnant are comparable with the abundances we find in the Helium rich collisions (even those with low-mass He-layer).…”

Section: Comparison With Other Models Of Type Iamentioning

confidence: 99%

Supernovae From Direct Collisions of White Dwarfs and the Role of Helium Shell Ignition

Papish

Perets

2016

ApJ

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Models for supernovae (SNe) arising from thermonuclear explosions of white dwarfs (WDs) have been extensively studied over the last few decades, mostly focusing on the single degenerate (accretion of material of a WD) and double degenerate (WD-WD merger) scenarios. In recent years it was suggested that WD-WD direct collisions provide an additional channel for such explosions. Here we extend the studies of such explosions, and explore the role of Helium-shells in affecting the thermonuclear explosions. We study both the impact of low-mass helium (∼ 0.01 M ⊙ ) shells, as well as high mass shells (≥ 0.1 M ⊙ ). We find that detonation of the massive helium layers precede the detonation of the WD Carbon-Oxygen (CO) bulk during the collision and can change the explosive evolution and outcomes for the cases of high mass He-shells. In particular, the He-shell detonation propagates on the WD surface and inefficiently burns material prior to the CO detonation that later follows in the central parts of the WD. Such evolution leads to larger production of intermediate elements, producing larger yields of 44 Ti and 48 Cr relative to the pure CO-CO WD collisions. Collisions of WDs with a low-mass He-shell do not give rise to helium detonation, but helium burning does precede the CO bulk detonation. Such collisions produce a high velocity, low-mass of ejected burned material enriched with intermediate elements, with smaller changes to the overall explosion outcomes. The various effects arising from the contribution of low/high mass He layers change the kinematics and the morphological structure of collision-induced SNe and may thereby provide unique observational signatures for such SNe, and play a role in the chemical enrichment of galaxies and the production of intermediate elements and positrons from their longer-term decay.

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Helium Shell Detonations on Low-Mass White Dwarfs as a Possible Explanation for Sn 2005e

Cited by 126 publications

References 44 publications

Two New Calcium-rich Gap Transients in Group and Cluster Environments

Two New Calcium-rich Gap Transients in Group and Cluster Environments

The Extremes of Thermonuclear Supernovae

Supernovae From Direct Collisions of White Dwarfs and the Role of Helium Shell Ignition

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