Handbook of Supernovae

Alsabti, Abdul Athem

doi:10.1007/978-3-319-20794-0

Cited by 8 publications

(1 citation statement)

References 105 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Subtleties in neutrino interactions, oscillations, and transport play a surprisingly large role. For a compilation on many aspects of supernova research see Alsabti & Murdin (2017).…”

Section: Supernovae and Neutrinosmentioning

confidence: 99%

Search for Unstable Sterile Neutrinos with the IceCube Neutrino Observatory

Abbasi¹,

Ackermann²,

Adams³

et al. 2022

Phys. Rev. Lett.

View full text Add to dashboard Cite

The IceCube Neutrino Observatory has been continuously taking data to search for O(0.5−10) s long neutrino bursts since 2007. Even if a Galactic core-collapse supernova is optically obscured or collapses to a black hole instead of exploding, it will be detectable via the O(10) MeV neutrino burst emitted during the collapse. We discuss a search for such events covering the time between April 17, 2008 and December 31, 2019. Considering the average data taking and analysis uptime of 91.7 % after all selection cuts, this is equivalent to 10.735 years of continuous data taking. In order to test the most conservative neutrino production scenario, the selection cuts were optimized for a model based on a 8.8 solar mass progenitor collapsing to an O-Ne-Mg core. Conservative assumptions on the effects of neutrino oscillations in the exploding star were made. The final selection cut was set to ensure that the probability to detect such a supernova within the Milky Way exceeds 99 %. No such neutrino burst was found in the data after performing a blind analysis. Hence, a 90 % C.L. upper limit on the rate of core-collapse supernovae out to distances of ≈ 25 kpc was determined to be 0.23/yr. For the more distant Magellanic Clouds, only high neutrino luminosity supernovae will be detectable by IceCube, unless external information on the burst time is available. We determined a model-independent limit by parameterizing the dependence on the neutrino luminosity and the energy spectrum.

show abstract

“…Subtleties in neutrino interactions, oscillations, and transport play a surprisingly large role. For a compilation on many aspects of supernova research see Alsabti & Murdin (2017).…”

Section: Supernovae and Neutrinosmentioning

confidence: 99%

Search for Unstable Sterile Neutrinos with the IceCube Neutrino Observatory

Abbasi¹,

Ackermann²,

Adams³

et al. 2022

Phys. Rev. Lett.

View full text Add to dashboard Cite

show abstract

New regimes in the observation of core-collapse supernovae

2019

View full text Add to dashboard Cite

Core-collapse Supernovae (CCSNe) mark the deaths of stars more massive than about eight times the mass of the sun (M ) and are intrinsically the most common kind of catastrophic cosmic explosions. They can teach us about many important physical processes, such as nucleosynthesis and stellar evolution, and thus, they have been studied extensively for decades. However, many crucial questions remain unanswered, including the most basic ones regarding which kinds of massive stars achieve which kind of explosions and how. Observationally, this question is related to the open puzzles of whether CCSNe can be divided into distinct types or whether they are drawn from a population with a continuous set of properties, and of what progenitor characteristics drive the diversity of observed explosions. Recent developments in wide-field surveys and rapid-response followup facilities are helping us answer these questions by providing two new tools: (1) large statistical samples which enable population studies of the most common SNe, and reveal rare (but extremely informative) events that question our standard understanding of the explosion physics involved, and (2) observations of early SNe emission taken shortly after explosion which carries signatures of the progenitor structure and mass loss history. Future facilities will increase our capabilities and allow us to answer many open questions related to these extremely energetic phenomena of the Universe.We focus this short review on a few open questions which are being tackled by new facilities for quick discovery and rapidresponse followup, as well as for studying CCSNe in large numbers. For a more exhaustive review of the field see recent compilations such as the Handbook of Supernovae [1]. The CCSN Classification LandscapeSN classification has been a challenge since the 1940's [2], but especially recently, as innovative surveys have brought a large increase of new and debated types. Classification schemes are important as physically motivated ones can give crucial insight into the explosion physics and stellar evolution pathways that lead to the different kinds of important explosions.The classical classification scheme [e.g., 3, 4] relies mostly on spectra and has two main types: Type I SNe (SNe I) which do not show hydrogen lines, and Type II SNe (SNe II) which do.In Figure 1 (left panel), we present spectra around peak brightness of the main CCSN classes. Among them, SNe II are perhaps the most heterogeneous class with a large range of observed photometric and spectroscopic properties. Because of this diversity, they can be further divided into several subclasses. The first historical subclassification was based on the light curve shape: SNe showing a linear decline (in magnitudes) in their light curve were named SNe IIL, while SNe showing a quasiconstant luminosity or a plateau for several weeks were called SNe IIP [13]. Later it was discovered that Type IIP and IIL SNe can also be distinguished by a subtle difference in their spectra, with SNe IIP showing deeper absor...

show abstract

Detection of optical emission from the supernova remnant G7.7–3.7

Domček,

Hernández Santisteban,

Chiotellis

et al. 2023

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present the first optical study of the supernova remnant (SNR) G7.7–3.7, with the aim of determining its evolutionary phase since it has been suggested to be the remnant of SN 386 AD. We obtained narrow-band images in the filters H α + [N ii], H β, [O iii], [S ii] that revealed faint optical emission in the southern region of the SNR consisting of two filaments elongated in the east–west direction aligned with the X-ray emitting region of the remnant. The filaments were seen in H α + [N ii], [O iii] images and marginally in the [S ii] images, with a non-detection in H β. Long-slit spectroscopy of the three regions along one filament revealed large ratios of [S ii]/H α = (1.6–2.5), consistent with that expected for a shock-heated SNR. The [S ii] doublet ratio observed in two of the regions implies an upper limit for the electron density of the gas, with estimates falling below 400 cm−3 and 600 cm−3 in the respective areas. We discuss potential physical mechanisms that formed the observed optical filaments and we suggest that most likely they resulted by a collision of the SNR with a dense circumstellar shell lying at the southern region of the remnant.

show abstract

Handbook of Supernovae

Cited by 8 publications

References 105 publications

Search for Unstable Sterile Neutrinos with the IceCube Neutrino Observatory

Search for Unstable Sterile Neutrinos with the IceCube Neutrino Observatory

New regimes in the observation of core-collapse supernovae

Detection of optical emission from the supernova remnant G7.7–3.7

Contact Info

Product

Resources

About