Relevant bibliographies by topics / Supernovae

Academic literature on the topic 'Supernovae'

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Published: 4 June 2021
Last updated: 28 July 2024

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Journal articles on the topic "Supernovae"

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Arcavi, Iair. "Type II SN Light Curves from the Caltech Core Collapse Project." Proceedings of the International Astronomical Union 7, S285 (September 2011): 431–53. http://dx.doi.org/10.1017/s1743921312001329.

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We presented our analysis of a sample of type II supernova (SN) light curves measured by the Caltech Core Collapse Project (CCCP). CCCP is a large observational program which made use of the robotic 60-in and the Hale 200-in telescopes to obtain optical photometry, spectroscopy and IR photometry of 49 nearby core-collapse supernovae (SNe). It provides a fair sample of core-collapse events, with well-defined selection criteria, and uniform, high-quality optical/IR observations. Our goal is to characterize the little-studied properties of core-collapse supernovae as a population. Preliminary data indicate a diverse set of sub-populations including “standard” type IIP supernovæ, declining supernovæ (at different rates) and slowly rising peculiar supernovæ. Work is in progress to map and quantify that diversity better. It is hoped that a single tunable formula will be able to describe most light-curve shapes, thereby helping us attain a better understanding of the physical mechanisms underlying these results.
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Nomoto, Ken'ichi. "Core Collapse Supernova Models and Nucleosynthesis." Proceedings of the International Astronomical Union 9, S296 (January 2013): 27–36. http://dx.doi.org/10.1017/s1743921313009198.

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AbstractAfter the Big Bang, production of heavy elements in the early Universe takes place in the first stars and their supernova explosions. The nature of the first supernovae, however, has not been well understood. The signature of nucleosynthesis yields of the first supernovae can be seen in the elemental abundance patterns observed in extremely metal-poor stars. Interestingly, those abundance patterns show some peculiarities relative to the solar abundance pattern, which should provide important clues to understanding the nature of early generations of supernovae. We review the recent results of the nucleosynthesis yields of massive stars. We examine how those yields are affected by some hydrodynamical effects during the supernova explosions, namely, explosion energies from those of hypernovae to faint supernovae, mixing and fallback of processed materials, asphericity, etc. Those parameters in the supernova nucleosynthesis models are constrained from observational data of supernovae and metal-poor stars.
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Wang, Lifan, Dietrich Baade, and Ferdinando Patat. "Spectropolarimetric Diagnostics of Thermonuclear Supernova Explosions." Science 315, no. 5809 (November 30, 2006): 212–14. http://dx.doi.org/10.1126/science.1121656.

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Even at extragalactic distances, the shape of supernova ejecta can be effectively diagnosed by spectropolarimetry. We present results for 17 type Ia supernovae that allow a statistical study of the correlation among the geometric structures and other observable parameters of type Ia supernovae. These observations suggest that type Ia supernova ejecta typically consist of a smooth, central, iron-rich core and an outer layer with chemical asymmetries. The degree of this peripheral asphericity is correlated with the light-curve decline rate of type Ia supernovae. These results lend strong support to delayed-detonation models of type Ia supernovae.
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Murphey, C. Tanner, Jacob W. Hogan, Brian D. Fields, and Gautham Narayan. "Witnessing history: sky distribution, detectability, and rates of naked-eye Milky Way supernovae." Monthly Notices of the Royal Astronomical Society 507, no. 1 (July 29, 2021): 927–43. http://dx.doi.org/10.1093/mnras/stab2182.

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ABSTRACT The Milky Way hosts on average a few supernova explosions per century, yet in the past millennium only five supernovae have been identified confidently in the historical record. This deficit of naked-eye supernovae is at least partly due to dust extinction in the Galactic plane. We explore this effect quantitatively, developing a formalism for the supernova probability distribution in space and on the sky, accounting for dust and for the observer’s flux limit. We then construct a fiducial axisymmetric model for the spatial supernova and dust densities, featuring an exponential dependence on galactocentric radius and height, with core-collapse events in a thin disc and Type Ia events including a thick disc component. When no flux limit is applied, our model predicts that on the sky, supernovae are intrinsically concentrated in the Galactic plane, with Type Ia events extending to higher latitudes. We then apply a flux limit and include dust effects, to predict the sky distribution of historical supernovae. We use well-observed supernovae as light-curve templates, and introduce naked-eye discovery criteria. The resulting sky distributions are strikingly inconsistent with the locations of confident historical supernovae, none of which lie near our model’s central peaks. Indeed, SN 1054 lies off the plane almost exactly in the anticentre, and SN 1181 is in the second Galactic quadrant. We discuss possible explanations for these discrepancies. We calculate the percentage of all supernovae bright enough for historical discovery: $\simeq 13{{\ \rm per\ cent}}$ of core-collapse and $\simeq 33{{\ \rm per\ cent}}$ of Type Ia events. Using these and the confident historical supernovae, we estimate the intrinsic Galactic supernova rates, finding general agreement with other methods. Finally, we urge searches for supernovae in historical records from civilizations in the Southern hemisphere.
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Weiler, Kurt W., and Richard A. Sramek. "Supernovae and Supernova Remnants." Annual Review of Astronomy and Astrophysics 26, no. 1 (September 1988): 295–341. http://dx.doi.org/10.1146/annurev.aa.26.090188.001455.

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Green, D. A. "Historical Supernovae and their Remnants." Highlights of Astronomy 12 (2002): 350–53. http://dx.doi.org/10.1017/s1539299600013721.

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AbstractHistorical records are available for nine supernova explosions seen in our Galaxy over the last two millennia. The observations of these ‘historical’ supernovae are very useful for the modern astrophysical interpretation of the remnants of these supernovae. The ages of the remnants of these historical supernovae are definitively known, which greatly aids understanding of the nature of the remnants. Also, the fact that the parent supernova was seen implies that it was relatively nearby in the Galaxy, giving further constraints on the distance, and hence other properties of their remnants. Here I briefly review the historical supernovae in our Galaxy, in the context of our understanding of their remnants from modern observations.
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Waldman, Roni. "Around the Pair Instability Valley – Massive SN Progenitors." Proceedings of the International Astronomical Union 4, S252 (April 2008): 329–32. http://dx.doi.org/10.1017/s1743921308023120.

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AbstractThe discovery of the extremely luminous supernova SN 2006gy, possibly interpreted as a pair instability supernova, renewed the interest in very massive stars. We explore the evolution of these objects, which end their life as pair instability supernovae or as core collapse supernovae with relatively massive iron cores, up to about 3 M⊙.
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Nomoto, Ken'ichi, and Tomoharu Suzuki. "Supernova Yields for Chemical Evolution Modeling." Proceedings of the International Astronomical Union 9, S298 (May 2013): 154–66. http://dx.doi.org/10.1017/s1743921313006327.

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AbstractWe review the recent results of the nucleosynthesis yields of massive stars. We examine how those yields are affected by some hydrodynamical effects during the supernova explosions, namely, explosion energies from those of hypernovae to faint supernovae, mixing and fallback of processed materials, asphericity, etc. Those parameters in the supernova nucleosynthesis models are constrained from observational data of supernovae and metal-poor stars. The elemental abundance patterns observed in extremely metal-poor stars show some peculiarities relative to the solar abundance pattern, which suggests the important contributions of hypernovae and faint supernovae in the early chemical enrichment of galaxies. These constraints on supernova nucleosynthesis are taken into account in the latest yield table for chemical evolution modeling.
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Abe, S., S. Asami, M. Eizuka, S. Futagi, A. Gando, Y. Gando, T. Gima, et al. "Search for Supernova Neutrinos and Constraint on the Galactic Star Formation Rate with the KamLAND Data." Astrophysical Journal 934, no. 1 (July 1, 2022): 85. http://dx.doi.org/10.3847/1538-4357/ac7a3f.

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Abstract We present the results of a search for core-collapse supernova neutrinos, using long-term KamLAND data from 2002 March 9 to 2020 April 25. We focus on the electron antineutrinos emitted from supernovae in the energy range of 1.8–111 MeV. Supernovae will make a neutrino event cluster with the duration of ∼10 s in the KamLAND data. We find no neutrino clusters and give the upper limit on the supernova rate to be 0.15 yr−1 with a 90% confidence level. The detectable range, which corresponds to a >95% detection probability, is 40–59 kpc and 65–81 kpc for core-collapse supernovae and failed core-collapse supernovae, respectively. This paper proposes to convert the supernova rate obtained by the neutrino observation to the Galactic star formation rate. Assuming a modified Salpeter-type initial mass function, the upper limit on the Galactic star formation rate is <(17.5–22.7) M ⊙ yr−1 with a 90% confidence level.
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Gomez, H. L., S. A. Eales, and L. Dunne. "Smoking supernovae." International Journal of Astrobiology 6, no. 2 (February 28, 2007): 159–67. http://dx.doi.org/10.1017/s1473550407003552.

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AbstractThe question ‘Are supernovae important sources of dust?’ is a contentious one. Observations with the Infrared Astronomical Satellite (IRAS) and the Infrared Space Observatory (ISO) only detected very small amounts of hot dust in supernova remnants. Here, we review observations of two young Galactic remnants with the Submillimetre Common User Bolometer Array (SCUBA), which imply that large quantities of dust are produced by supernovae. The association of dust with the Cassiopeia A remnant is in question owing to the contamination of foreground material. In this paper, we compare the emission from cold dust with CO emission towards Kepler’s supernova remnant. We detect very little CO at the location of the submillimetre peaks. A comparison of masses from the CO and the dust clouds are made, and we estimate the 3σ upper limit on the gas-to-dust ratios to be in the range 20–60. These results suggest that we cannot yet rule out freshly-formed or swept-up circumstellar dust in Kepler’s supernova remnant.
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Dissertations / Theses on the topic "Supernovae"

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Tartaglia, Leonardo. "Interacting supernovae and supernova impostors." Doctoral thesis, Università degli studi di Padova, 2016. http://hdl.handle.net/11577/3427226.

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Massive stars are thought to end their lives with spectacular explosions triggered by the gravitational collapse of their cores. Interacting supernovae are generally attributed to supernova explosions occurring in dense circumstellar media, generated through mass-loss which characterisie the late phases of the life of their progenitors. In the last two decades, several observational evidences revealed that mass-loss in massive stars may be related to violent eruptions involving their outer layers, such as the luminous blue variables. Giant eruptions of extragalactic luminous blue variables, similar to that observed in $\eta$~Car in the 19th century, are usually labelled `SN impostors', since they mimic the behaviour of genuine SNe, but are not the final act of the life of the progenitor stars. The mechanisms producing these outbursts are still not understood, although the increasing number of observed cases triggered the efforts of the astronomical community to find possible theoretical interpretations. More recently, a number of observational evidences suggested that also lower-mass stars can experience pre-supernova outbursts, hence becoming supernova impostors. Even more interestingly, there is growing evidence of a connection among massive stars, their outbursts and interacting supernovae. All of this inspired this research, which has been focused in particular on the characterisation of supernova impostors and the observational criteria that may allow us to safely discriminate them from interacting supernovae. Moreover, the discovery of peculiar transients, motivated us to explore the lowest range of stellar masses that may experience violent outbursts. Finally, the quest for the link among massive stars, their giant eruptions and interacting supernovae, led us to study the interacting supernova LSQ13zm, which possibly exploded a very short time after an LBV-like major outburst.
Le stelle massive terminano la loro vita con spettacolari esplosioni innescate dal collasso gravitazionale del loro nucleo. Le supernove interagenti sono tipicamente associate a questo tipo di esplosioni in mezzi circumstellari densi, generati da episodi di perdita di massa durante le fasi finali dell'evoluzione dei loro progenitori. Negli ultimi due decenni, diverse evidenze osservative hanno rivelato come questi episodi siano spesso correlati ad eruzioni violente che coinvolgono gli strati esterni degli inviluppi di stelle massive, come le `luminous blue variables'. In qualche caso questi eventi sono stati osservati come `supernova impostors' (impostori), transienti che imitano il comportamento di supernove reali, ma non costituiscono l'atto finale della vita dei loro progenitori. Questi sono spesso associati alle eruzioni giganti di luminous blue variable extragalattiche. I meccanismi che innescano queste eruzioni non sono ancora del tutto compresi, nonostante il crescente numero di casi osservati abbia attirato l'attenzione della comunit\'a astronomica nel tentativo di trovare delle spiegazioni teoriche a questi fenomeni. P\'iu di recente, un certo di numero di evidenze osservative ha portato ad ipotizzare che anche stelle meno massive possano mostrare eruzioni giganti che imitano gli osservabili delle supernove interagenti. Tutto questo, unitamente alla possibile connessione recentemente proposta tra le stelle massive, le loro eruzioni giganti e alcune supernove interagenti, ha ispirato questo lavoro di ricerca, che si \'e focalizzato in particolare sulla caratterizzazione del fenomeno degli impostori e sui possibili criteri osservativi che permettono di distinguere con sicurezza le supernove interagenti dagli impostori. Inoltre, la scoperta di oggetti peculiari ci ha motivato nell'analisi dell'estremo inferiore dell'intervallo di masse interessate da episodi eruttivi violenti. La caccia al collegamento tra le stelle massive, le loro eruzioni giganti e le supernove interagenti, ha portato alla scoperta della supernova peculiare LSQ13zm, che potrebbe essere esplosa poco tempo dopo un'eruzione gigante simile a quelle osservate nelle luminous blue variables.
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Graham, J. R. "Dust in supernovae and supernova remnants." Thesis, Imperial College London, 1985. http://hdl.handle.net/10044/1/37710.

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Petrushevska, Tanja. "Supernovae seen through gravitational telescopes." Doctoral thesis, Stockholms universitet, Fysikum, 2017. http://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-141633.

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Galaxies, and clusters of galaxies, can act as gravitational lenses and magnify the light of objects behind them. The effect enables observations of very distant supernovae, that otherwise would be too faint to be detected by existing telescopes, and allows studies of the frequency and properties of these rare phenomena when the universe was young. Under the right circumstances, multiple images of the lensed supernovae can be observed, and due to the variable nature of the objects, the difference between the arrival times of the images can be measured. Since the images have taken different paths through space before reaching us, the time-differences are sensitive to the expansion rate of the universe. One class of supernovae, Type Ia, are of particular interest to detect. Their well known brightness can be used to determine the magnification, which can be used to understand the lensing systems. In this thesis, galaxy clusters are used as gravitational telescopes to search for lensed supernovae at high redshift. Ground-based, near-infrared and optical search campaigns are described of the massive clusters Abell 1689 and 370, which are among the most powerful gravitational telescopes known. The search resulted in the discovery of five photometrically classified, core-collapse supernovae at redshifts of 0.671<z<1.703 with significant magnification from the cluster. Owing to the power of the lensing cluster, the volumetric core-collapse supernova rates for 0.4 ≤ z < 2.9 were calculated, and found to be in good agreement with previous estimates and predictions from cosmic star formation history. During the survey, two Type Ia supernovae in A1689 cluster members were also discovered, which allowed the Type Ia explosion rate in galaxy clusters to be estimated. Furthermore, the expectations of finding lensed supernovae at high redshift in simulated search campaigns that can be conducted with upcoming ground- and space-based telescopes, are discussed. Magnification from a galaxy lens also allows for detailed studies of the supernova properties at high redshift that otherwise would not be possible. Spectroscopic observations of lensed high-redshift supernovae Type Ia are of special interest since they can be used to test for evolution of the standard candle nature of these objects. If systematic redshift-dependent properties are found, their utility for future surveys could be challenged. In the thesis it is shown that the strongly lensed and very distant supernova Type Ia PS1-10afx at z=1.4, does not deviate from the well-studied nearby and intermediate populations of normal supernovae Type Ia. In a different study, the discovery of the first resolved multiply-imaged gravitationally lensed supernova Type Ia is also reported.

At the time of the doctoral defense, the following papers were unpublished and had a status as follows: Paper 3: Manuscript. Paper 4: Manuscript.

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Mitra, Ayan. "Gravitational Lensing of the supernovae from the Supernova Legacy Survey." Thesis, Paris 6, 2016. http://www.theses.fr/2016PA066331.

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La presence d’inhomogénéite de matière le long de la ligne de visée d’une source lumineuseprovoque la déviation des rayons lumineux : c’est l’effet de lentille gravitationnelle. Dans cette thèse, nous etudions l’effet de lentille gravitationnelle qui affecte les supernovae détectées par le Supernova Legacy Survey et induit une dispersion supplémentaire dans leur distribution en magnitude observée. Cet effet est mis en évidence par la mesure d’une corrélation positive entre : d’une part, le résidu au diagramme de Hubble c’est-à -dire à l’ajustement de la dépendance en redshift de la magnitude de la supernova ; d’autre part, la magnification calculée en modélisant les halos galactiques présents le long de la ligne de visée. Une corrélation positive est estimée, en utilisant les données à cinq ans du Supernova Legacy Survey. Le résultat obtenu est compatible avec les résultats précédemments obtenus sur un lot de supernovae plus restreint
The presence of mass inhomogeneities along the line of sight of propagation of light fromdistant objects can induce deflection in the flight path of the photon. This phenomenon is called as gravitational lensing. Lensing can have both distortion (shear) and isotropic magnification effects on the source. We studied the effect of lensing magnification on supernova (SN) Ia in this thesis. Presence of lensing would introduce a source of contamination to the brightness distribution of the source (SN Ia in our case). Thus it also enables one to compute the lensing effect indirectly from the Hubble diagram (i.e. from the residual to the Hubble diagram). In this thesis we computed the correlation between these two effects : the Hubble residual and the computed lensing magnification for the SN by the line of sight foreground dark matter haloes. A detection of positive correlation between these two would signify the positivity of lensing signal detection. The data sample is the spectroscopic SNe Ia sample from the five years full SNLS data and the Hubble resiudals are those of the preliminary cosmology analysis performed on SNLS5 data. We obtain a signal of _ = 0.177 at 2.51_. This result is consistent with the previous SNLS three years data lensing analysis results
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Kilpatrick, Charles Donald, and Charles Donald Kilpatrick. "New Observational Insight on Shock Interactions Toward Supernovae and Supernova Remnants." Diss., The University of Arizona, 2016. http://hdl.handle.net/10150/621574.

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Supernovae (SNe) are energetic explosions that signal the end of a star's life. These events and the supernova remnants (SNRs) they leave behind play a central role in stellar feedback by adding energy and momentum and metals to the interstellar medium (ISM). Emission associated with these feedback processes, especially atomic and molecular line emission as well as thermal and nonthermal continuum emission is known to be enhanced in regions of high density, such as dense circumstellar matter (CSM) around SNe and molecular clouds (MCs). In this thesis, I begin with a brief overview of the physics of SN shocks in Chapter 1, focusing on a foundation for studying pan-chromatic signatures of interactions between SNe and dense environments. In Chapter 2, I examine an unusual SN with signatures of CSM interaction in the form of narrow lines of hydrogen (Type IIn) and thermal continuum emission. This SN appears to belong to a class of Type Ia SNe that shares spectroscopic features with Type IIn SNe. I discuss the difficulties of decomposing spectra in a regime where interaction occurs between SN ejecta and CSM, potentially confusing the underlying SN type. This is followed by a discussion of rebrightening that occurred at late-time in 𝐵 and 𝑉 band photometry of this SN, possibly associated with clumpy or dense CSM at large distances from the progenitor. In Chapter 3, I examine synchrotron emission from Cassiopeia A, observed in the 𝐾ₛ band over multiple epochs. The synchrotron emission is generally diffuse over the remnant, but there is one location in the southwest portion of the remnant where it appears to be enhanced and entrained as knots of emission in the SNR ejecta. I evaluate whether the 𝐾ₛ band knots are dominated by synchrotron emission by comparing them to other infrared and radio imaging that is known to be dominated by synchrotron emission. Concluding that they are likely synchrotron-emitting knots, I measure the magnetic field strength and electron density required for their evolution over the ~ 10 yr baseline they were observed and find 𝐵 ≈ 1.3-5.8 mG and 𝑛ₑ≈ 1,000-15,000 cm⁻³. The magnetic field strengths appear enhanced beyond values required by the adiabatic strong shock limit, arguing in favor of other forms of magnetic field amplification in the shock. In Chapter 4, I again discuss Cassiopeia A and interaction between the remnant and nearby MCs as seen at mid-infrared and millimeter wavelengths. I report detection of a SNR-MC interaction and analyze its signatures in broadened molecular lines. I extend this analysis in Chapter 5 to a large survey for SNR-MC interactions in the ¹²CO 𝐽=2-1 line. Although broadened ¹²CO 𝐽=2-1 line emission should be detectable toward virtually all SNR-MC interactions, I find relatively few examples; therefore, the number of interactions is low. This result favors mechanisms other than supernova feedback as the basic trigger for star formation. In addition, I find no significant association between TeV gamma-ray sources and MC interactions, contrary to predictions that SNR-MC interfaces are the primary venues for cosmic ray acceleration. I end this dissertation in Chapter 6 with a brief summary of my results and two extensions of this work: examining the late-time radio light curves of CSM-interacting SNe for signatures of radio synchrotron emission and dense or clumpy CSM at large distances from the progenitor and re-observing SNR-MC interactions in ¹²CO 𝐽=3-2 in order to verify the presence of shock-heated molecular gas and perform a census on the densities and temperatures of post-shock molecular gas.
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Heereman, von Zuydtwyck David. "HitSpooling: an improvement for the supernova neutrino detection system in icecube." Doctoral thesis, Universite Libre de Bruxelles, 2015. http://hdl.handle.net/2013/ULB-DIPOT:oai:dipot.ulb.ac.be:2013/209179.

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The IceCube Neutrino Observatory consists of a lattice of 5160 photomultiplier tubes (PMTs)

which monitor one cubic kilometer of deep Antarctic ice at the geographic South Pole.

IceCube was primarily designed to detect neutrinos of energies greater than O(100 GeV).

Due to subfreezing ice temperatures, the photomultipliers' dark noise rates are particularly

low which enables IceCube to search for neutrinos from galactic supernovae by detecting

bursts of MeV neutrinos emitted during the core collapse and for several seconds following.

For that purpose, a dedicated online supernova DAQ system records the total number of hits

in the detector, without any further information from the PMTs, and generates supernova

candidate triggers in case of a significant detector rate enhancement. A new feature to the

standard DAQ, called HitSpooling, was implemented in IceCube during this thesis. The

HitSpooling system is implemented in the standard DAQ system and buffers the complete

raw data stream of the photomultipliers for several hours or days. By reading out time periods

of HitSpool data around supernova candidate triggers, generated by the online supernova

DAQ system, we overcome the limitations of the latter and have access to the entire information

of the detector in case of a supernova. Furthermore, HitSpool data is a powerful

source for studying and understanding the noise behavior of the detector as well as background

processes coming from atmospheric muons. The idea of HitSpooling was developed in the

scope of this thesis and is the basis of the work at hand. The developed interface between the

standard DAQ and the supernova DAQ system is presented. The correlated dark noise component

in optical modules of IceCube is quantified for the first time and possible explanations

are discussed. The possibility of identifying triggering and subthreshold atmospheric muons

in HitSpool data and subtracting them from a possible supernova signal is analyzed. Furthermore,

the conversion from HitSpool data to supernova DAQ type data was developed

which allows for a comparison of both data types with respect to lightcurves and significances

of selected supernova candidate triggers.
Doctorat en Sciences
info:eu-repo/semantics/nonPublished

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López, Hermoso Rosario. "Modelos de curva de luz de las supernovas de tipo I." Doctoral thesis, Universitat de Barcelona, 1985. http://hdl.handle.net/10803/665979.

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En el presente trabajo se han conectado unos fenómenos pertenecientes al campo de la observación (las supernovas de tipo 1, SN 1) con los procesos físicos que tienen lugar en fases evolutivas avanzadas de los sistemas binarios compactos en los que hay una enana blanca de carbono-oxigeno que acreta materia. El estudio llevado a cabo muestra que el fenómeno observacional de las SN 1 es la consecuencia última de que dichos procesos se verifiquen bajo unas condiciones específicas y que es posible reproducir las características más notables de las supernovas de tipo 1 en el escenario a que nos referimos si se considera de forma realista las condiciones físicas existentes en el interior de la enana que da origen al fenómeno. El trabajo ha sido estructurado de la forma que se indica a continuación: El primer capítulo se dedica a analizar las observaciones de SN 1 disponibles con objeto de establecer las restricciones que deben imponerse a los modelos que se formulen así como a los resultados que de ellos se obtengan. En el segundo capítulo se discuten los diversos modelos que se han ido realizando hasta la fecha para explicar el fenómeno de las SN I, señalando los problemas que plantean y que los hacen inviables a la hora de dar una explicación totalmente satisfactoria del mismo. Se acaba con la presentación de las relaciones dimensionales obtenidas a partir de los modelos analíticos de Arnett, de gran importancia para entender el origen de las dificultades con que tropiezan los modelos teóricos de formulación más reciente. Posteriormente, se presenta un escenario general que sirve de base para el desarrollo de las supernovas de tipo 1: los sistemas binarios compactos que poseen enanas blancas masivas las cuales han desarrollado un núcleo Sólido de carbono-oxígeno. En el marco del citado escenario, se construyen modelos para simular numéricamente las curvas de luz de las SN 1. Los modelos se han formulado teniendo en cuenta las relaciones dimensionales de Arnett y resultados previos de cálculos sobre explosión de objetos compactos. La integración numérica de las ecuaciones de conservación y de transporte bajo unas hipótesis físicas bastante generales permite obtener la evolución temporal de cada modelo y su comparación con 105 observables. Todo ello, marco astrofísico y método de construcción de los modelos, se expone en el tercer capítulo del trabajo. El capítulo cuarto recoge y analiza los resultados de los cálculos que se han llevado a cabo. Se destacan en él los efectos que tiene el considerar como progenitores de las supernovas enanas blancas totalmente fluidas o, por el contrario, con un núcleo Sólido. Se muestra mediante dos secuencias de modelos, una para cada caso, las consecuencias observacionales a que da lugar el que la explosión deje o no un residuo ligado, en especial en lo que se refiere a poder reproducir el efecto Pskovski-Branch. Adicionalmente, se indican las incertidumbres que padecen los modelos y se estudian las consecuencias que supondría cambiar el valor de algunos parámetros no bien conocidos. Asimismo, se discuten las implicaciones cosmológicas del modelo de explosión de supernova que se presenta en lo relativo a su compatibilidad con determinados valores de la constante de Hubble. Finalmente, se indican las posibles vías de continuación del trabajo.
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Mori, Masamitsu. "Long time supernova simulation and search for supernovae in Super-Kamiokande IV." Doctoral thesis, Kyoto University, 2021. http://hdl.handle.net/2433/263465.

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Melinder, Jens. "The Frequency of Supernovae in the Early Universe." Doctoral thesis, Stockholms universitet, Institutionen för astronomi, 2011. http://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-56000.

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Supernovae are cosmic explosions of cataclysmic proportion that signify the death of a star. While being interesting phenomena in their own right, their brightness also make them excellent probes of the early universe. Depending on the type of the progenitor star and the origin of the explosion different subjects can be investigated. In this dissertation the work I have done on the detection, characterisation and rate measurements of supernovae in the Stockholm VIMOS Supernova Search is presented. We have discovered 16 supernovae that exploded billions of years ago (or, equivalently, at high redshift, z). The observed brightness and colour evolution have been used to classify the supernovae into either thermonuclear (type Ia) or core collapse (type II) supernovae. The accuracy of the classification code is high, only about 5% of the supernovae are mistyped, similar to other codes of the same kind. By comparing the observed frequency of supernovae to simulations the underlying supernova rate at these high redshifts have been measured. The main result reported in this thesis is that the core collapse supernova rate at high redshift matches the rates estimated from looking at the star formation history of the universe, and agree well with previous studies. The rate of Ia supernovae at high redshift have been investigated by several projects, our results show a somewhat higher rate of Ia supernovae than expected. Proper estimates of the systematic errors of rate measurements are found to be very important. Furthermore, by using novel techniques for reducing and stacking images, we have obtained a galaxy sample containing approximately 50,000 galaxies. Photometric redshifts have been obtained for most of the galaxies, the resulting accuracy below z=1 is on the order of 10%. The galaxy sample has also been used to find high redshift sources, so called Lyman Break Galaxies, at z=3-5.
At the time of the doctoral defense, the following papers were unpublished and had a status as follows: Paper 2: Submitted. Paper 3: Manuscript. Paper 4: Manuscript.
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Polshaw, Joseph Stephan Wilfrid. "Exploring extreme supernovae." Thesis, Queen's University Belfast, 2016. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.709695.

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The study of supernovae (SNe) has greatly advanced in recent years, in particular due to the successes of wide-field transient surveys. The ever-increasing quantity of data has led to the discoveries of a large number of peculiar SNe with extreme properties, which both challenge and illuminate the current understanding of massive star evolution. In this thesis, I present detailed analyses of three SNe, each of which can be considered to be extreme in some way. The analysis highlights the multiple competing physical effects that the properties of massive stars at the end of their lives have on the resulting explosion. The understanding of this is one of the key goals of SNe research.
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Books on the topic "Supernovae"

1

Marschall, Laurence A. The supernova story. New York: Plenum Press, 1988.

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Marschall, Laurence A. The supernova story. Princeton, N.J: Princeton University Press, 1994.

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Efe, Yazgan, and Ankay Askin, eds. Neutron stars, supernovae and supernova remnants. New York: Nova Science Publishers, 2007.

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Bykov, Andrei, Chevalier Roger, John Raymond, Friedrich-Karl Thielemann, Maurizio Falanga, and Rudolf von Steiger, eds. Supernovae. Dordrecht: Springer Netherlands, 2019. http://dx.doi.org/10.1007/978-94-024-1581-0.

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Woosley, S. E., ed. Supernovae. New York, NY: Springer New York, 1991. http://dx.doi.org/10.1007/978-1-4612-2988-9.

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Petschek, Albert G., ed. Supernovae. New York, NY: Springer New York, 1990. http://dx.doi.org/10.1007/978-1-4612-3286-5.

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Ecole, d'été de physique théorique (54th 1990 Les Houches Haute-Savoie France). Supernovae. Amsterdam: North-Holland, 1994.

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Albert, Petschek, ed. Supernovae. New York: Springer-Verlag, 1990.

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G, Petschek Albert, ed. Supernovae. New York: Springer-Verlag, 1990.

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Lesley, Murdin, and Murdin Paul, eds. Supernovae. Cambridge [Cambridgeshire]: Cambridge University Press, 1985.

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Book chapters on the topic "Supernovae"

1

Tsunemi, Hiroshi. "Supernovae and supernova remnants." In The Century of Space Science, 937–60. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-010-0320-9_41.

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Sarangi, A., M. Matsuura, and E. R. Micelotta. "Dust in Supernovae and Supernova Remnants I: Formation Scenarios." In Supernovae, 313–60. Dordrecht: Springer Netherlands, 2018. http://dx.doi.org/10.1007/978-94-024-1581-0_13.

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Vink, Jacco. "Supernovae." In Astronomy and Astrophysics Library, 5–31. Cham: Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-030-55231-2_2.

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Lemmer, Boris, Benjamin Bahr, and Rina Piccolo. "Supernovae." In Quirky Quarks, 83–86. Berlin, Heidelberg: Springer Berlin Heidelberg, 2016. http://dx.doi.org/10.1007/978-3-662-50259-4_20.

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Fransson, Claes, and George Sonneborn. "Supernovae." In Astrophysics and Space Science Library, 249–63. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-0794-5_26.

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Bahr, Benjamin, Boris Lemmer, and Rina Piccolo. "Supernovae." In Quirky Quarks, 82–85. Berlin, Heidelberg: Springer Berlin Heidelberg, 2016. http://dx.doi.org/10.1007/978-3-662-49509-4_20.

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Lang, Kenneth R. "Supernovae." In Astrophysical Data, 701–8. New York, NY: Springer US, 1992. http://dx.doi.org/10.1007/978-1-4684-0640-5_26.

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Powell, Jonathan. "Supernovae." In Astronomers' Universe, 39–79. Cham: Springer International Publishing, 2019. http://dx.doi.org/10.1007/978-3-030-31688-4_5.

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Heyssler, Matthias. "Supernovae." In Das Leben der Sterne, 25–39. Wiesbaden: Springer Fachmedien Wiesbaden, 2015. http://dx.doi.org/10.1007/978-3-658-10650-8_3.

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Röpke, Friedrich. "Supernovae." In Explodierende Vielfalt, 65–75. Berlin, Heidelberg: Springer Berlin Heidelberg, 2019. http://dx.doi.org/10.1007/978-3-662-58334-0_8.

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Conference papers on the topic "Supernovae"

1

Semenikhin, T. A., and M. V. Pruzhinskaya. "Bolometric light curves and parameters of superbright supernova explosions." In Всероссийская с международным участием научная конференция студентов и молодых ученых, посвященная памяти Полины Евгеньевны Захаровой «Астрономия и исследование космического пространства». Ural University Press, 2021. http://dx.doi.org/10.15826/b978-5-7996-3229-8.47.

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The goal of this work is to obtain bolometric light curves of superluminous supernovae using data from the Open Supernova Catalog of and vector-valued Gaussian processes. With the help of theoretical and analytical simulations, parameters of supernova explosions, such as the explosion energy and the mass of the produced radioactive elements, will be extracted from the obtained bolometric light curves.
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Moiseenko, S. G., G. S. Bisnovatyi-Kogan, Stefan Immler, and Kurt Weiler. "Magnetorotational supernovae." In SUPERNOVA 1987A: 20 YEARS AFTER: Supernovae and Gamma-Ray Bursters. AIP, 2007. http://dx.doi.org/10.1063/1.2803576.

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Moiseenko, S. G., G. S. Bisnovatyi-Kogan, Stefan Immler, and Kurt Weiler. "Magnetorotational supernovae." In SUPERNOVA 1987A: 20 YEARS AFTER: Supernovae and Gamma-Ray Bursters. AIP, 2007. http://dx.doi.org/10.1063/1.3682915.

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Chevalier, Roger A. "Supernovae and supernova remnants at high energies." In High−Energy Astrophysics in the 21st Century. AIP, 1990. http://dx.doi.org/10.1063/1.39667.

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SATO, KATSUHIKO, KEITARO TAKAHASHI, SHIN'ICHIRO ANDO, and KEI KOTAKE. "SUPERNOVA EXPLOSIONS AND NEUTRINO BURSTS FROM SUPERNOVAE." In Proceedings of the KIAS–APCTP International Symposium on Astro-Hadron Physics. WORLD SCIENTIFIC, 2004. http://dx.doi.org/10.1142/9789812702524_0040.

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Tartaglia, L. "Interacting supernovae and supernova impostors: Evidence of incoming supernova explosions?" In EXOTIC NUCLEI AND NUCLEAR/PARTICLE ASTROPHYSICS (V). FROM NUCLEI TO STARS: Carpathian Summer School of Physics 2014. AIP Publishing LLC, 2015. http://dx.doi.org/10.1063/1.4909612.

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Chevalier, Roger A., Stefan Immler, and Kurt Weiler. "Circumstellar Interaction around Supernovae." In SUPERNOVA 1987A: 20 YEARS AFTER: Supernovae and Gamma-Ray Bursters. AIP, 2007. http://dx.doi.org/10.1063/1.2803564.

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Panagia, Nino, Stefan Immler, and Kurt Weiler. "ULTRAVIOLET OBSERVATIONS OF SUPERNOVAE." In SUPERNOVA 1987A: 20 YEARS AFTER: Supernovae and Gamma-Ray Bursters. AIP, 2007. http://dx.doi.org/10.1063/1.2803569.

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Weiler, Kurt W., Nino Panagia, Richard A. Sramek, Schuyler D. Van Dyk, Christopher L. Williams, Christopher J. Stockdale, Matthew T. Kelley, Stefan Immler, and Kurt Weiler. "Radio Emission from Supernovae." In SUPERNOVA 1987A: 20 YEARS AFTER: Supernovae and Gamma-Ray Bursters. AIP, 2007. http://dx.doi.org/10.1063/1.2803571.

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Chevalier, Roger A., Stefan Immler, and Kurt Weiler. "Circumstellar Interaction around Supernovae." In SUPERNOVA 1987A: 20 YEARS AFTER: Supernovae and Gamma-Ray Bursters. AIP, 2007. http://dx.doi.org/10.1063/1.3682904.

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Reports on the topic "Supernovae"

1

Albert, J., G. Aldering, S. Allam, W. Althouse, R. Amanullah, J. Annis, P. Astier, et al. Supernova Acceleration Probe: Studying Dark Energy with Type Ia Supernovae. Office of Scientific and Technical Information (OSTI), August 2005. http://dx.doi.org/10.2172/878833.

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Stockdale, Christopher J., Kurt W. Weiler, Nino Panagia, Richard A. Sramek, Schuyler D. Van Dyk, Stefan Immler, Dave Pooley, et al. Radio Supernovae: Circum-Stellar Investigation (C.S.I.) of Supernova Progenitor Stars. Fort Belvoir, VA: Defense Technical Information Center, February 2009. http://dx.doi.org/10.21236/ada520162.

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Kasen, Daniel Nathan. Aspherical supernovae. Office of Scientific and Technical Information (OSTI), January 2004. http://dx.doi.org/10.2172/825138.

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Cooperstein, J. Nuclear astrophysics of supernovae. Office of Scientific and Technical Information (OSTI), January 1988. http://dx.doi.org/10.2172/6034283.

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Fryer, Christopher. Understanding Core-Collapse Supernovae. Office of Scientific and Technical Information (OSTI), March 2024. http://dx.doi.org/10.2172/2323505.

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Miller, Douglas Scott. Convection in Type 2 supernovae. Office of Scientific and Technical Information (OSTI), October 1993. http://dx.doi.org/10.2172/10139321.

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Brown, W. K. High explosive simulations of supernovae and the supernova shell fragmentation model of solar system formation. Office of Scientific and Technical Information (OSTI), September 1987. http://dx.doi.org/10.2172/6019760.

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Jones, Samuel. Constraining simulations of stars and supernovae. Office of Scientific and Technical Information (OSTI), September 2018. http://dx.doi.org/10.2172/1469481.

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Tandon, Suyash, Nicholas William Stegmeier, Vasu Jaganath, Jennifer Helen Ranta, Rathish Previn Ratnasingam, Elizabeth Anne Carlson, Julien Loiseau, Vinay Bharadwaj Ramakrishnaiah, and Robert Stephen Pavel. Core-Collapse Supernovae Simulations using FleCSPH. Office of Scientific and Technical Information (OSTI), December 2019. http://dx.doi.org/10.2172/1579683.

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Haxton, W. C. Neutrino nucleosynthesis in supernovae: Shell model predictions. Office of Scientific and Technical Information (OSTI), January 1989. http://dx.doi.org/10.2172/5022225.

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