Bibliografías temáticas / Stars: supernovae

Literatura académica sobre el tema "Stars: supernovae"

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Publicado: 11 de marzo de 2023

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Artículos de revistas sobre el tema "Stars: supernovae"

1

Nomoto, Ken'ichi. "Core Collapse Supernova Models and Nucleosynthesis". Proceedings of the International Astronomical Union 9, S296 (enero de 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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2

Jones, Samuel, Raphael Hirschi, Falk Herwig, Bill Paxton, Francis X. Timmes y Ken'ichi Nomoto. "Progenitors of electron-capture supernovae". Proceedings of the International Astronomical Union 7, S279 (abril de 2011): 341–42. http://dx.doi.org/10.1017/s1743921312013257.

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AbstractWe investigate the lowest mass stars that produce Type-II supernovae, motivated by recent results showing that a large fraction of type-II supernova progenitors for which there are direct detections display unexpectedly low luminosity (for a review see e.g. Smartt 2009). There are three potential evolutionary channels leading to this fate. Alongside the standard ‘massive star’ Fe-core collapse scenario we investigate the likelihood of electron capture supernovae (EC-SNe) from super-AGB (S-AGB) stars in their thermal pulse phase, from failed massive stars for which neon burning and other advanced burning stages fail to prevent the star from contracting to the critical densities required to initiate rapid electron-capture reactions and thus the star's collapse. We find it indeed possible that both of these relatively exotic evolutionary channels may be realised but it is currently unclear for what proportion of stars. Ultimately, the supernova light curves, explosion energies, remnant properties (see e.g. Knigge et al. 2011) and ejecta composition are the quantities desired to establish the role that these stars at the lower edge of the massive star mass range play.
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3

Nomoto, Ken'ichi y Tomoharu Suzuki. "Supernova Yields for Chemical Evolution Modeling". Proceedings of the International Astronomical Union 9, S298 (mayo de 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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4

Maund, Justyn R., Paul A. Crowther, Hans-Thomas Janka y Norbert Langer. "Bridging the gap: from massive stars to supernovae". Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 375, n.º 2105 (18 de septiembre de 2017): 20170025. http://dx.doi.org/10.1098/rsta.2017.0025.

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Almost since the beginning, massive stars and their resultant supernovae have played a crucial role in the Universe. These objects produce tremendous amounts of energy and new, heavy elements that enrich galaxies, encourage new stars to form and sculpt the shapes of galaxies that we see today. The end of millions of years of massive star evolution and the beginning of hundreds or thousands of years of supernova evolution are separated by a matter of a few seconds, in which some of the most extreme physics found in the Universe causes the explosive and terminal disruption of the star. Key questions remain unanswered in both the studies of how massive stars evolve and the behaviour of supernovae, and it appears the solutions may not lie on just one side of the explosion or the other or in just the domain of the stellar evolution or the supernova astrophysics communities. The need to view massive star evolution and supernovae as continuous phases in a single narrative motivated the Theo Murphy international scientific meeting ‘Bridging the gap: from massive stars to supernovae’ at Chicheley Hall, UK, in June 2016, with the specific purpose of simultaneously addressing the scientific connections between theoretical and observational studies of massive stars and their supernovae, through engaging astronomers from both communities. This article is part of the themed issue ‘Bridging the gap: from massive stars to supernovae’.
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5

Nomoto, K., T. Shigeyama y T. Tsujimoto. "Supernova Abundance Generation". Symposium - International Astronomical Union 145 (1991): 21–38. http://dx.doi.org/10.1017/s007418090022723x.

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Theoretical models of supernova explosions of various types are reviewed to obtain heavy element yields from supernovae. We focus on new models for SN 1987A, and Type Ia, Ib, and Ic supernovae. Maximum brightness and decline rate of their light curves suggest that 12–18 M⊙ stars produce larger amount of 56Ni than more massive stars. We discuss relative roles of various types of supernovae in the chemical evolution of galaxies.
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6

Waldman, Roni. "Around the Pair Instability Valley – Massive SN Progenitors". Proceedings of the International Astronomical Union 4, S252 (abril de 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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7

Magg, Mattis, Anna T. P. Schauer, Ralf S. Klessen, Simon C. O. Glover, Robin G. Tress y Ondrej Jaura. "Metal Mixing in Minihalos: The Descendants of Pair-instability Supernovae". Astrophysical Journal 929, n.º 2 (1 de abril de 2022): 119. http://dx.doi.org/10.3847/1538-4357/ac5aac.

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Abstract The lack of observations of abundance patterns originating in pair-instability supernovae has been a long-standing problem in relation to the first stars. This class of supernovae is expected to have an abundance pattern with a strong odd–even effect, making it substantially different from present-day supernovae. In this study, we use a cosmological radiation hydrodynamics simulation to model such supernovae and the subsequent formation of the second generation of stars. We incorporate streaming velocities for the first time. There are 14 star-forming minihalos in our 1 cMpc h −1 box, leading to 14 supernovae occurring before redshift z = 19.5, where we start reducing the complexity of the simulation. Following the explosions, extremely metal-poor stars form in 10 halos via internal and external enrichment, which makes it the most common outcome. Only one halo does not recollapse during the simulations. This result is at variance with the current (lack of) observations of metal-poor stars with pair-instability supernova abundance patterns, suggesting that these very massive stars might be rare even in the early universe. The results from this simulation also give us insights into what drives different modes of recollapse and what determines the mixing behavior of metals after very energetic supernovae.
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8

Eldridge, John J. "Massive stars in their death throes". Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 366, n.º 1884 (23 de septiembre de 2008): 4441–52. http://dx.doi.org/10.1098/rsta.2008.0160.

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The study of the stars that explode as supernovae used to be a forensic study, working backwards from the remnants of the star. This changed in 1987 when the first progenitor star was identified in pre-explosion images. Currently, there are eight detected progenitors with another 21 non-detections, for which only a limit on the pre-explosion luminosity can be placed. This new avenue of supernova research has led to many interesting conclusions, most importantly that the progenitors of the most common supernovae, type IIP, are red supergiants, as theory has long predicted. However, no progenitors have been detected thus far for the hydrogen-free type Ib/c supernovae, which, given the expected progenitors, is an unlikely result. Also, observations have begun to show evidence that luminous blue variables, which are among the most massive stars, may directly explode as supernovae. These results contradict the current stellar evolution theory. This suggests that we may need to update our understanding.
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9

Chevalier, R. A. "Supernovae and Stellar Mass Loss". Highlights of Astronomy 7 (1986): 599–609. http://dx.doi.org/10.1017/s1539299600007000.

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AbstractType I supernovae can be modeled as the carbon deflagration of white dwarfs and Type II supernovae as the explosions of massive stars with hydrogen envelopes. The massive stars at the ends of their lives are expected to be red supergiants, which are observed to have slow, dense winds. The interaction of the supernova kinetic energy and radiation with the circumstellar gas gives rise to observational phenomena at a range of wavelengths. Additional phenomena, such as a scattered light echo, are predicted. While the light from a Type II supernova near maximum light is probably from energy deposited in the initial explosion, there is now good evidence that the radioactive decay of 56Co powers the emission at late times. It was been noted that the explosions of massive stars without hydrogen envelopes would be quite unlike normal Type II supernovae. There is now good evidence for such explosions – SN1985f and the class of peculiar Type I supernovae. It is suggested that these supernovae be called Type III with the spectroscopic definition of a) no H lines and b) broad [01] lines at late times. That not all very massive star explosions are of this type is indicated by SN1961v, which was probably a very massive explosion, but in which hydrogen was present.
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Neuhäuser, R., F. Gießler y V. V. Hambaryan. "A nearby recent supernova that ejected the runaway star ζ Oph, the pulsar PSR B1706−16, and 60Fe found on Earth". Monthly Notices of the Royal Astronomical Society 498, n.º 1 (23 de septiembre de 2019): 899–917. http://dx.doi.org/10.1093/mnras/stz2629.

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ABSTRACT The detection of ∼1.5–3.2 Myr old 60Fe on Earth indicates recent nearby core-collapse supernovae. For supernovae in multiple stars, the primary stars may become neutron stars, while former companions may become unbound and become runaway stars. We wrote software for tracing back the space motion of runaway and neutron stars to young associations of massive stars. We apply it here to the nearby young Scorpius–Centaurus–Lupus groups, all known runaway stars possibly coming from there, and all 400 neutron stars with known transverse velocity. We find kinematic evidence that the runaway ζ Oph and the radio pulsar PSR B1706−16 were released by a supernova in a binary 1.78 ± 0.21 Myr ago at 107 ± 4 pc distance (for pulsar radial velocity 260 ± 43 km s−1); association age and flight time determine the progenitor mass (16–18 M⊙), which can constrain supernova nucleosynthesis yields and 60Fe uptake on Earth. In addition, we notice that the only high-mass X-ray binary in Scorpius–Centaurus–Lupus (1H11255−567 with μ1 and μ2 Cru) may include a neutron star formed in another SN, up to ∼1.8 Myr ago at 89−112 pc, i.e. also yielding 60Fe detectable on Earth. Our scenario links 60Fe found on Earth to one or two individual supernovae in multiple stars.
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Tesis sobre el tema "Stars: supernovae"

1

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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2

Covarrubias, Ricardo Alberto. "Does the metallicity affect the fate of massive stars? /". Thesis, Connect to this title online; UW restricted, 2007. http://hdl.handle.net/1773/5442.

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Fraser, Morgan. "On dying stars : supernovae and their progenitors". Thesis, Queen's University Belfast, 2012. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.579701.

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In the last fifteen years, searches for the progenitors of core-collapse supernovae (SNe) in archival images have provided the crucial "missing link" between the final stages in the evolution of a massive star, and its explosion as a core-collapse SN. In this thesis, I present new detections and limits for core-collapse SN progenitors, together with a critical re-analysis of those already published. I present detailed studies of the progenitors of three nearby SNe. For the sub- luminous Type IIP SN 2009md, I find a coincident red supergiant progenitor with a mass of ~8 M in archival images, which is consistent with the low mass progenitors found for other faint Type IIP SNe. Such events appear to come from red supergiants at the lower extremum of the mass range for core-collapse. I discuss the intermediate Type IIP /L SN 2009kr, for which I find what appears to be a massive yellow supergiant progenitor. I consider possible explanations for the observed colour of the progenitor candidate at explosion, and the consequences for stellar evolution. I also analyse archival pre-explosion images of the site of the Type Ib SN 2009jf, for which a progenitor was not detected. I attempt to constrain the age of the stellar population in the locale of the SN, and use this to set a limit on the progenitor mass. I also extend the time- and volume-limited sample of core-collapse SNe presented by Smartt et al. (2009). I use this new data, together with an improved re-analysis of the original limits of Smartt et al., to set an upper limit on the mass of Type IIP and Type IIL SN progenitors of 20M, at a 95 per cent confidence level. This limit is lower than the most massive observed red supergiants, providing strong support for suggestions that some of the most massive red supergiants do not produce bright SNe, but rather collapse to form black holes either directly or via fall-back. Finally, I discuss some alternative approaches for understanding core-collapse SNe and their progenitors, including searching for progenitors in X-ray data, a survey for optically faint failed SNe, and a deeper search for a surviving companion to the progenitor of the Galactic SN Cas A.
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Gerke, Jill R. "Failed Supernovae, Dusty Stars and Cepheid Distances". The Ohio State University, 2014. http://rave.ohiolink.edu/etdc/view?acc_num=osu1405528289.

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Reiss, David J. "The rate of supernovae in the nearby and distant universe /". Thesis, Connect to this title online; UW restricted, 1999. http://hdl.handle.net/1773/5441.

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Magill, Lindsay J. "Core-collapse supernovae and the deaths of massive stars". Thesis, Queen's University Belfast, 2013. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.602594.

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In this thesis I present a detailed study of two type IIn supernovae: PTFll iqb and SN 2011jb. I find that PTFll iqb shows complex Ha and H~ profiles, which indicate that the progenitor underwent multiple periods of mass loss . The shells formed by these periods of mass loss are interacting with the ejecta . The measured widths of the narrow components are consistent with a Red Supergiant progenitor. Asymmetric line profiles at late times suggest dust formation. Contrastingly, SN 2011jb appears to be a type Ic supernova which is interacting with a CSM, similarly to SNe 2002ic and SN 2005gj. In these cases the spectra can be modeled as ejecta interacting with a CSM superimposed upon a type la or le spectrum, which appears weak due to the attenuation caused by the dust. I endeavor to conduct a search of all core-collapse supernovae which have exploded within the cryogenic lifetime of Spitzer, within 25Mpc. It is found that type Un SNe were twice as likely to be recovered as other type II supernovae, but due to the low numbers of type Iblc supernovae for which data exists it is not possible. to draw any conclusions about their likelihood of being recovered. The dust which is found in type II supernovae was likely to be caused by a light echo as the ejecta heated the surrounding circumstellar medium. However, dust formation is found to be an equally likely explanation for the presence of dust in other type II supernovae. Lastly, I discuss approaches for furthering our understanding of core-collapse supernovae. These include plans for discovering supernovae more quickly, and studying them more effectively, using surveys such as PESSTO, and pushing the boundaries for the faintest and furthest supernovae we can see using larger telescopes such as the E- ELT.
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Adams, Scott M. "Stellar Death by Weak or Failed Supernovae". The Ohio State University, 2016. http://rave.ohiolink.edu/etdc/view?acc_num=osu1468850125.

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Prieto, Jose L. "Massive Stars: Life and Death". The Ohio State University, 2009. http://rave.ohiolink.edu/etdc/view?acc_num=osu1248987393.

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Gaensler, Bryan Malcolm. "Barrels, jets and smoke-rings: Understanding the bizarre shapes of radio supernova remnants". Thesis, The University of Sydney, 1999. http://hdl.handle.net/2123/399.

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This thesis considers the various morphologies of radio supernova remnants (SNRs), and attempts to determine whether their appearance results from the properties of the progenitor star and its supernova explosion, or from the structure of the interstellar medium (ISM) and ambient magnetic field into which a SNR consequently expands. High-resolution observations of Supernova 1987A show a young remnant whose appearance and evolution are completely dominated by the structure of its progenitor wind. A statistical study of the Galactic population of bilateral SNRs demonstrates that the symmetry axes of these remnants run parallel to the Galactic Plane. This result can be explained by the interaction of main sequence stellar wind-bubbles with the ambient magnetic field; expansion of SNRs into the resulting elongated cavities results in a bilateral appearance with the observed alignment. Radio observations of SNR G296.8-00.3 show a double-ringed morphology which is best explained by expansion either into an anisotropic main-sequence progenitor wind or into multiple cavities in the ISM. Data on SNRs G309.2-00.6 and G320.4-01.2 (MSH 15-52) make a strong case that the appearance of both remnants is significantly affected by collimated outflows from a central source; for G309.2-00.6 the source itself is not detected, but for G320.4-01.2 there is now compelling evidence that the remnant is associated with and is interacting with the young pulsar PSR B1509-58. I conclude that, while the youngest SNRs are shaped by their progenitor's circumstellar material, the appearance of most SNRs reflects the properties of the local ISM and magnetic field. Remnants which interact with an associated pulsar or binary system appear to be rare, and are easily distinguished by their unusual and distorted morphologies.
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Gaensler, Bryan Malcolm. "Barrels, jets and smoke-rings: Understanding the bizarre shapes of radio supernova remnants". University of Sydney, Physics, 1999. http://hdl.handle.net/2123/399.

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This thesis considers the various morphologies of radio supernova remnants (SNRs), and attempts to determine whether their appearance results from the properties of the progenitor star and its supernova explosion, or from the structure of the interstellar medium (ISM) and ambient magnetic field into which a SNR consequently expands. High-resolution observations of Supernova 1987A show a young remnant whose appearance and evolution are completely dominated by the structure of its progenitor wind. A statistical study of the Galactic population of bilateral SNRs demonstrates that the symmetry axes of these remnants run parallel to the Galactic Plane. This result can be explained by the interaction of main sequence stellar wind-bubbles with the ambient magnetic field; expansion of SNRs into the resulting elongated cavities results in a bilateral appearance with the observed alignment. Radio observations of SNR G296.8-00.3 show a double-ringed morphology which is best explained by expansion either into an anisotropic main-sequence progenitor wind or into multiple cavities in the ISM. Data on SNRs G309.2-00.6 and G320.4-01.2 (MSH 15-52) make a strong case that the appearance of both remnants is significantly affected by collimated outflows from a central source; for G309.2-00.6 the source itself is not detected, but for G320.4-01.2 there is now compelling evidence that the remnant is associated with and is interacting with the young pulsar PSR B1509-58. I conclude that, while the youngest SNRs are shaped by their progenitor's circumstellar material, the appearance of most SNRs reflects the properties of the local ISM and magnetic field. Remnants which interact with an associated pulsar or binary system appear to be rare, and are easily distinguished by their unusual and distorted morphologies.
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Libros sobre el tema "Stars: supernovae"

1

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

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Stars and supernovas. New York, N.Y: DK Pub., 2001.

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3

Owen, Ruth. Supernovas. New York: Windmill Books, 2013.

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4

Naeye, Robert. Through the eyes of Hubble: The birth, life, and violent death of stars. Bristol: Institute of Physics Publishing, 1998.

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Through the eyes of Hubble: The birth, life, and violent death of stars. Waukesha, WI: Kalmbach Books, 1998.

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Novye i sverkhnovye zvezdy. 2a ed. Moskva: "Nauka," Glav. red. fiziko-matematicheskoĭ lit-ry, 1985.

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Lupato, Giovanni. SN1054: Una supernova sul medioevo. Galliera Veneta, Italy: Biroma Editore, 1997.

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Lozinskai͡a, T. A. Supernovae and stellar wind in the interstellar medium. New York: American Institute of Physics, 1992.

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Extreme explosions: Supernovae, hypernovae, magnetars, and other unusual cosmic blasts. New York: Springer, 2014.

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School and Workshop on Supernovae and Stellar Evolution (1989 Goa, India). Proceedings of the School and Workshop [on] Supernovae and Stellar Evolution, Goa, India, March 10-17, 1989. Editado por Ray A y Velusamy T. Singapore: World Scientific, 1991.

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Capítulos de libros sobre el tema "Stars: supernovae"

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Hartmann, Dieter. "Neutrino Nucleosynthesis in Massive Stars". En Supernovae, 626–29. New York, NY: Springer New York, 1991. http://dx.doi.org/10.1007/978-1-4612-2988-9_91.

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Langer, Norbert. "Wolf-Rayet Stars as Supernova Precursors". En Supernovae, 549–55. New York, NY: Springer New York, 1991. http://dx.doi.org/10.1007/978-1-4612-2988-9_77.

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Ensman, Lisa y S. E. Woosley. "Type Ib Supernovae Wolf-Rayet Stars". En Supernovae, 556–58. New York, NY: Springer New York, 1991. http://dx.doi.org/10.1007/978-1-4612-2988-9_78.

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El Eid, Mounib F. "Explosion of Massive Wolf-Rayet Stars". En Supernovae, 568–71. New York, NY: Springer New York, 1991. http://dx.doi.org/10.1007/978-1-4612-2988-9_81.

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Winkler, P. Frank, Peter F. Roberts y Robert P. Kirshner. "Spectrophotometry of Cas A: Implications for Nucleosynthesis in Massive Stars". En Supernovae, 652–55. New York, NY: Springer New York, 1991. http://dx.doi.org/10.1007/978-1-4612-2988-9_96.

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Limongi, Marco. "Supernovae from Massive Stars". En Handbook of Supernovae, 1–56. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-20794-0_119-1.

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Meynet, Georges y André Maeder. "Supernovae from Rotating Stars". En Handbook of Supernovae, 1–34. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-20794-0_122-1.

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Limongi, Marco. "Supernovae from Massive Stars". En Handbook of Supernovae, 513–65. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-21846-5_119.

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Meynet, Georges y André Maeder. "Supernovae from Rotating Stars". En Handbook of Supernovae, 601–34. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-21846-5_122.

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Weiler, K. W. "Radio Supernovae". En High Energy Phenomena Around Collapsed Stars, 223–34. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3823-6_10.

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Actas de conferencias sobre el tema "Stars: supernovae"

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Ekström, S., G. Meynet y A. Maeder. "Can Very Massive Stars Avoid Pair‐Instability Supernovae?" En FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905547.

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Suwa, Yudai. "From Supernovae to Neutron Stars". En Proceedings of the Workshop on Quarks and Compact Stars 2017 (QCS2017). Journal of the Physical Society of Japan, 2018. http://dx.doi.org/10.7566/jpscp.20.011020.

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Limongi, Marco. "Presupernova evolution of massive stars". En Supernovae: lights in the darkness. Trieste, Italy: Sissa Medialab, 2008. http://dx.doi.org/10.22323/1.060.0018.

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Tartaglia, L. "Interacting supernovae and supernova impostors: Evidence of incoming supernova explosions?" En 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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Hummel, Jacob A., Andreas H. Pawlik, Miloš Milosavljević y Volker Bromm. "The first supernovae: Source density and observability of pair instability supernovae". En FIRST STARS IV – FROM HAYASHI TO THE FUTURE –. AIP, 2012. http://dx.doi.org/10.1063/1.4754392.

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Modjaz, Maryam, Stefan Immler y Kurt Weiler. "Diverse Deaths of Massive Stars: Properties of SN Ib∕c". En SUPERNOVA 1987A: 20 YEARS AFTER: Supernovae and Gamma-Ray Bursters. AIP, 2007. http://dx.doi.org/10.1063/1.2803600.

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Modjaz, Maryam, Stefan Immler y Kurt Weiler. "Diverse Deaths of Massive Stars: Properties of SN Ib/c". En SUPERNOVA 1987A: 20 YEARS AFTER: Supernovae and Gamma-Ray Bursters. AIP, 2007. http://dx.doi.org/10.1063/1.3682937.

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Farouqi, K., K. ‐L Kratz, J. J. Cowan, L. I. Mashonkina, B. Pfeiffer, C. Sneden, F. ‐K Thielemann y J. W. Truran. "Nucleosynthesis Modes in the High‐Entropy‐Wind Scenario of Type II Supernovae". En FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905568.

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Moriya, T. J., S. I. Blinnikov, N. Tominaga, N. Yoshida, M. Tanaka, K. Maeda y K. Nomoto. "Type IIn superluminous supernovae from collision of supernova ejecta and dense circumstellar medium". En FIRST STARS IV – FROM HAYASHI TO THE FUTURE –. AIP, 2012. http://dx.doi.org/10.1063/1.4754397.

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Woosley, S. E. y Thomas A. Weaver. "Nucleosynthesis and supernovae in massive stars". En The 3rd international symposium on nuclear astrophysics: Nuclei in the Cosmos III. AIP, 1995. http://dx.doi.org/10.1063/1.47368.

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Informes sobre el tema "Stars: supernovae"

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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, febrero de 2009. http://dx.doi.org/10.21236/ada520162.

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

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Wise, J. The Number of Supernovae From Primordial Stars in the Universe. Office of Scientific and Technical Information (OSTI), diciembre de 2004. http://dx.doi.org/10.2172/839784.

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Mathews, G. Hydrodynamics and nucleosynthesis in neutron stars, supernovae, and the early universe. Office of Scientific and Technical Information (OSTI), marzo de 1996. http://dx.doi.org/10.2172/278392.

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Guzik, J. A., P. A. Bradley, A. N. Cox, F. J. Swenson, R. G. Deupree, M. S. Soukup, M. R. Templeton y K. M. Despain. Deriving the structure of pre-supernovae and delta Scuti stars using nonradial oscillations. Office of Scientific and Technical Information (OSTI), noviembre de 1998. http://dx.doi.org/10.2172/674869.

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Haxton, Wick. SHEDDING NEW LIGHT ON EXPLODING STARS: TERASCALE SIMULATIONS OF NEUTRINO-DRIVEN SUPERNOVAE AND THEIR NUCLEOSYNTHESIS. Office of Scientific and Technical Information (OSTI), marzo de 2012. http://dx.doi.org/10.2172/1036022.

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Baker, M. Pauline. VisPort: Web-Based Access to Community-Specific Visualization Functionality [Shedding New Light on Exploding Stars: Visualization for TeraScale Simulation of Neutrino-Driven Supernovae (Final Technical Report)]. Office of Scientific and Technical Information (OSTI), junio de 2007. http://dx.doi.org/10.2172/1054764.

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Dennis C. Smolarski, S. J. Shedding New Light on Exploding Stars: Terascale Simulations of Nuetrino-Dreiven Supernovas and Their Nucleosynthesis. Office of Scientific and Technical Information (OSTI), noviembre de 2004. http://dx.doi.org/10.2172/877197.

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Zilberman, Mark. Shouldn’t Doppler 'De-boosting' be accounted for in calculations of intrinsic luminosity of Standard Candles? Intellectual Archive, septiembre de 2021. http://dx.doi.org/10.32370/iaj.2569.

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Resumen
"Doppler boosting / de-boosting" is a well-known relativistic effect that alters the apparent luminosity of approaching/receding radiation sources. "Doppler boosting" alters the apparent luminosity of approaching light sources to appear brighter, while "Doppler de-boosting" alters the apparent luminosity of receding light sources to appear fainter. While "Doppler boosting / de-boosting" has been successfully accounted for and observed in relativistic jets of AGN, double white dwarfs, in search of exoplanets and stars in binary systems it was ignored in the establishment of Standard Candles for cosmological distances. A Standard Candle adjustment appears necessary for "Doppler de-boosting" for high Z, otherwise we would incorrectly assume that Standard Candles appear dimmer, not because of "Doppler de-boosting" but because of the excessive distance, which would affect the entire Standard Candles ladder at cosmological distances. The ratio between apparent (L) and intrinsic (Lo) luminosities as a function of redshift Z and spectral index α is given by the formula ℳ(Z) = L/Lo=(Z+1)^(α-3) and for Type Ia supernova as ℳ(Z) = L/Lo=(Z+1)^(-2). These formulas are obtained within the framework of Special Relativity and may require adjustments within the General Relativity framework.
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