Relevant bibliographies by topics / Close — supernovae

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  1. Journal articles
  2. Dissertations / Theses
  3. Book chapters
  4. Conference papers

Academic literature on the topic 'Close — supernovae'

Author: Grafiati
Published: 4 June 2025
Last updated: 23 June 2025

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Journal articles on the topic "Close — supernovae"

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Uenishi, Tatsuhiro, Ken'ichi Nomoto, and Izumi Hachisu. "Evolution of Rotating White Dwarfs in Close Binaries and Diversity of Type Ia Supernovae." Symposium - International Astronomical Union 208 (2003): 459–60. http://dx.doi.org/10.1017/s0074180900207754.

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Type Ia supernovae are very good, but not perfect, standard candles, because their observed brightness shows a little diversity. The origin of this dibersity needs to be understood for the application to cosmology.In close binary systems, a white dwarf must be rotating faster and faster as it gains angular momentum from the accretion disk. Its rapid rotation affects its final mass and strucure just before a supernova expolosion. Brightness of supernovae can be changed if mass of their progenitors have some diversity.
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Joss, P. C. "Type II Supernovae in Binary Systems." Symposium - International Astronomical Union 165 (1996): 141–49. http://dx.doi.org/10.1017/s0074180900055637.

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The presence of a close binary companion can affect the evolution of a massive star through one or more episodes of mass transfer, or by merger in a common-envelope phase. Monte Carlo calculations indicate that ∼20–35% of all massive supernovae are affected by such processes, and that a substantial fraction of these events will be supernovae of type II. The properties of the progenitor star, the distribution of circumstellar material, the peak supernova luminosity, the shape of the supernova light curve, and other observable features of the supernova event can be affected by prior binary membership. Binary interactions may be the cause of much of the variability among type II supernova light curves. In particular, many of the peculiarities of SN 1987A and SN 1993J may well have resulted from the prior duplicity of the progenitors.
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Nomoto, K., K. Iwamoto, T. Suzuki, et al. "The Origin of Type Ib-Ic-IIb-IIL Supernovae and Binary Star Evolution." Symposium - International Astronomical Union 165 (1996): 119–34. http://dx.doi.org/10.1017/s0074180900055613.

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Supernovae are classified as type I and type II and further subdivided into Ia, Ib, Ic, II-P, II-L, and IIb. The origin of this observational diversity has not been well understood. The recent nearby supernovae SN 1993J and SN 1994I have provided particularly useful material to clarify the supernova — progenitor connection. For a progenitor of type IIb supernova 1993J, we propose that merging of two stars in a close binary is responsible for the formation of a thin H-rich envelope. As a progenitor of type Ic supernova 1994I, we propose a bare C+O star that has lost both its H and He envelope after a common-envelope phase. By generalizing these scenarios, we show that common-envelope evolution in massive close binary stars leads to various degrees of stripping off of the envelope of a massive star. This naturally leads to an explanation of the origin of type II-L, IIn, IIb, Ib, and Ic in a unified manner. The binary hypothesis to explain the diversity of supernovae can be substantiated with new information on SN IIb 1993J and SN Ic 1994I. Model light curves are compared with observations. Since extensive mass loss is essential for the binary scenario, circumstellar interactions are examined for comparison with X-ray observations.
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Angloher, G., M. R. Bharadwaj, M. Cababie, et al. "Neutrino flux sensitivity to the next galactic core-collapse supernova in COSINUS." Journal of Cosmology and Astroparticle Physics 2025, no. 03 (2025): 037. https://doi.org/10.1088/1475-7516/2025/03/037.

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Abstract While neutrinos are often treated as a background for many dark matter experiments, these particles offer a new avenue for physics: the detection of core-collapse supernovae. Supernovae are extremely energetic, violent and complex events that mark the death of massive stars. During their collapse stars emit a large number of neutrinos in a short burst. These neutrinos carry 99% of the emitted energy which makes their detection fundamental in understanding supernovae. This paper illustrates how COSINUS (Cryogenic Observatory for SIgnatures seen in Next-generation Underground Searches), a sodium iodide (NaI) based dark matter search, will be sensitive to the next galactic core-collapse supernova. The experiment is composed of two separate detectors which will respond to far away and nearby supernovae. The inner core of the experiment will consist of NaI crystals operating as scintillating calorimeters. These crystals will mainly be sensitive to the Coherent Elastic Neutrino-Nucleus Scattering (CEνNS) against Na and I nuclei. The low mass of the cryogenic detectors enables the experiment to identify close supernovae within 1 kpc without pileup. The crystals will see up to hundreds of CEνNS events from a supernova happening at 200 pc. They reside at the center of a large cylindrical 230 T water tank, instrumented with 30 photomultiplier tubes. This tank acts simultaneously as a passive and active shield able to detect the Cherenkov radiation induced by impinging charged particles from ambient and cosmogenic radioactivity. A supernova near the Milky Way Center (10 kpc) will be easily detected inducing ∼60 measurable events, and the water tank will have a 3σ sensitivity to supernovae up to 22 kpc, seeing ∼10 events. This paper shows how, even without dedicated optimization, modern dark matter experiments will also be able to play their part in the multi-messenger effort to detect the next galactic core-collapse supernova.
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Sternberg, Assaf. "Evidence for Circumstellar Material in Type Ia Supernovae via Sodium Absorption Features." Proceedings of the International Astronomical Union 7, S281 (2011): 299–302. http://dx.doi.org/10.1017/s1743921312015232.

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AbstractType Ia supernovae are very good tools for measuring distances on a cosmic scale. The consensus view is that mass transfer onto a white dwarf in a close binary system leads to a thermonuclear explosion, though the nature of the mass donor is still uncertain. In the single-degenerate model it is a main-sequence star or an evolved star. In the double-degenerate model it is another white dwarf. We study the velocity structure of absorbing material along the line of sight to 35 Type Ia supernovae and find a statistical preference for blueshifted structures, likely arising in gas outflows from the supernova progenitor systems, consistent with a single-degenerate progenitor for a substantial fraction of Type Ia supernovae in nearby spiral galaxies.
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Meynet, G., J. Groh, C. Georgy, H. Saio, and R. Kudritzki. "Supernovae from yellow, blue supergiants: origin and consequences for stellar evolution." Proceedings of the International Astronomical Union 11, A29B (2015): 211. http://dx.doi.org/10.1017/s1743921316004932.

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AbstractA few core collapse supernovae progenitors have been found to be yellow or blue supergiants. Weshall discuss possible scenarios involving single and close binary evolution allowing to explain this kind of corecollapse supernova progenitors. According to stellar models for both single and close binaries, blue supergiants, at theend of their nuclear lifetimes and thus progenitors of core collapse supernovae, present very different characteristicsfor what concerns their surface compositions, rotational surface velocities and pulsational properties with respect toblue supergiants in their core helium burning phase. We discuss how the small observed scatter of the flux-weightedgravity-luminosity (FWGL) relation of blue supergiants constrains the evolution of massive stars after the Main-Sequence phase and the nature of the progenitors of supernovae in the mass range between 12 and 40 solarmasses. The present day observed surface abundances of blue supergiants, of their pulsational properties, as well asthe small scatter of the FWGL relation provide strong constraints on both internal mixing and mass loss in massivestars and therefore on the end point of their evolution.
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de Angelis, Alessandro, and Selenia Broccio. "First Observations of SN 1604 (Kepler’s Supernova)." Universe 7, no. 11 (2021): 430. http://dx.doi.org/10.3390/universe7110430.

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A supernova close enough to the Earth is a spectacular event: it can appear as a “new star” as luminous as Venus, or even more, visible for several days. The rate of Galactic supernovae is expected to be of about one in 30 years, with a fraction visible to the naked eye; however in all the history of human civilization only seven supernovae in the Milky Way have been reported, the last two (1572 and 1604) during Galilei’s life. The supernova of 1604, today called Kepler’s Supernova, was observed by Galilei, Kepler and other astronomers in Europe, Korea, China, Arabia. Like the supernova SN1572, today called Tycho’s supernova, it has been the subject of extensive studies, and inspired observational measurements and philosophical considerations on the nature of the heavens. The remnant of SN1604 has been indicated by recent X- and gamma-ray data to be a likely site of cosmic ray acceleration. The first recorded data of optical observations, together with new data, can still tell us a lot about the early evolution of this supernova.
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Arbutina, B., D. Urošević, and B. Vukotić. "High supernova rate and enhanced star-formation triggered in M81-M82 encounter." Proceedings of the International Astronomical Union 2, S237 (2006): 391. http://dx.doi.org/10.1017/s1743921307001792.

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It is a general belief that the starburst activity of a nearby galaxy M82 was triggered in a close encounter with its massive companion M81, a few tens of million years ago. Despite the lack of supernovae observed, multiwavelength radio observations of M82 discovered a considerable number of compact supernova remnant candidates. We use these remnants to estimate the supernova rate (SNR) and the enhanced star-formation (SFR) rate in M82, and compare them with rates in normal galaxies.
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Napiwotzki, R., C. Karl, G. Nelemans, et al. "Close Binary White Dwarfs and Supernovae la." International Astronomical Union Colloquium 194 (2004): 113–16. http://dx.doi.org/10.1017/s0252921100152121.

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AbstractWe report on the current status of radial velocity surveys for white dwarf binaries (double degenerates DDs) including SPY (ESO Supernovae la progenitor survey) recently carried out at the VLT. A large sample of DD will allow us to put strong constraints on the phases of close binary evolution of the progenitor systems and to perform an observational test of the DD scenario for Supernovae of type Ia.
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PAULUCCI, L., and J. E. HORVATH. "NU-PROCESS IN EXOTIC MODELS." International Journal of Modern Physics D 19, no. 08n10 (2010): 1731–35. http://dx.doi.org/10.1142/s0218271810017238.

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The exact physical conditions generating the abundances of r-elements in environments such as supernovae explosions are still under debate. We evaluated the characteristics expected for the neutrino wind in the proposed model of type-II supernova driven by conversion of nuclear matter to strange matter. Neutrinos will change the final abundance of elements after freeze out of r-process nucleosynthesis, specially those close to mass peaks.
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Dissertations / Theses on the topic "Close — supernovae"

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Batta, Aldo, Enrico Ramirez-Ruiz, and Chris Fryer. "The Formation of Rapidly Rotating Black Holes in High-mass X-Ray Binaries." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/625738.

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High-mass X-ray binaries (HMXRBs), such as Cygnus X-1, host some of the most rapidly spinning black holes (BHs) known to date, reaching spin parameters a greater than or similar to 0.84. However, there are several effects that can severely limit the maximum BH spin parameter that could be obtained from direct collapse, such as tidal synchronization, magnetic core-envelope coupling, and mass loss. Here, we propose an alternative scenario where the BH is produced by a failed supernova (SN) explosion that is unable to unbind the stellar progenitor. A large amount of fallback material ensues, whose interaction with the secondary naturally increases its overall angular momentum content, and therefore the spin of the BH when accreted. Through SPH hydrodynamic simulations, we studied the unsuccessful explosion of an 8 M-circle dot pre-SN star in a close binary with a 12 M-circle dot companion with an orbital period of approximate to 1.2 days, finding that it is possible to obtain a BH with a high spin parameter a greater than or similar to 0.8 even when the expected spin parameter from direct collapse is a less than or similar to 0.3. This scenario also naturally explains the atmospheric metal pollution observed in HMXRB stellar companions.
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Zapartas, E., S. E. de Mink, S. D. Van Dyk, et al. "Predicting the Presence of Companions for Stripped-envelope Supernovae: The Case of the Broad-lined Type Ic SN 2002ap." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624948.

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Many young, massive stars are found in close binaries. Using population synthesis simulations. we predict the likelihood of a companion star being present when these massive stars end their lives as core-collapse supernovae (SNe). We focus on stripped-envelope SNe, whose progenitors have lost their outer hydrogen and possibly helium layers before explosion. We use these results to interpret new Hubble Space Telescope observations of the site of the broad-lined Type. Ic SN 2002ap, 14 years post-explosion. For a subsolar metallicity consistent with SN 2002ap, we expect a main-sequence (MS) companion present in about two thirds of all stripped-envelope SNe and a compact companion (likely a stripped helium star or a white dwarf/neutron star/black hole) in about 5% of cases. About a quarter of progenitors are single at explosion (originating from initially single stars, mergers, or disrupted systems). All of the latter scenarios require a massive progenitor, inconsistent with earlier studies of SN 2002ap. Our new, deeper upper limits exclude the presence of an MS companion star > 8-10 M., ruling out about 40% of all stripped-envelope SN channels. The most likely scenario for SN 2002ap includes nonconservative binary interaction of a primary star initially. 23 M.. Although unlikely (< 1% of the scenarios), we also discuss the possibility of an exotic reverse merger channel for broadlined Type. Ic events. Finally, we explore how our results depend on the metallicity and the model assumptions and discuss how additional searches for companions can constrain the physics that govern. the evolution of SN progenitors.
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Cai, Yongzhi. "Intermediate Luminosity Optical Transients." Doctoral thesis, Università degli studi di Padova, 2019. http://hdl.handle.net/11577/3424674.

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Beyond supernovae (SNe), very few cosmic explosions can release an amount of kinetic energy of the order of 10ˆ{51} erg (1 foe). In past years, modern all-sky surveys discovered numerous peculiar transients releasing much lower energies. With the label of Intermediate Luminosity Optical Transients or Gap Transients, we refer to objects fainter than typical SNe but brighter than classical novae (i.e., they lay in the magnitude range -10< Mv < -15 mag). In this poorly populated luminosity range (the “gap”), we find several types of stellar transients, including faint supernovae, giant eruptions of massive stars including luminous blue variables (LBVs), intermediate-luminosity red transients (ILRTs), and luminous red novae (LRNe). These gap transients may originate from various physical mechanisms, and sometimes the classification is a tricky task. A major goal of this research work is characterising the observational properties and correlating the physical parameters of gap transients, shedding light on their nature. In this thesis project, I studied in detail a recent faint and red transient, AT 2017be, classified as an ILRT, and show that an electron-capture supernova (EC SN) is the most likely scenario to explain the observed outburst. In-depth analysis on a large ILRT sample favours the same explosion mechanism for all of them. Finally, I studied an unprecedented object, AT 2018hso, that reveals transitional observational properties between ILRTs and LRNe, making its precise classification dubious. However, follow-up observations support it to be a LRN, hence most likely a transient produced by a stellar merging event.<br>Oltre alle supernove (SNe), pochissime esplosioni cosmiche sono in grado di rilasciare una quantità di energia cinetica dell’ordine di 1051 erg (1 foe). Negli anni passati, moderne “all-sky surveys” hanno permesso di scoprire numerosi transienti peculiari che rilasciavano energie molto più modeste. Con il nome di transienti ottici di luminosità intermedia o transienti nel “gap”, ci riferiamo ad oggetti che sono più deboli delle tipiche SNe ma più luminosi delle classiche novae (cio`e hanno magnitudine nell’intervallo -10< MV < -15 mag). In questo intervallo di luminosità scarsamente popolato (il “gap”), troviamo diversi tipi di transienti stellari, tra cui supernove deboli, eruzioni giganti di stelle massicce incluse le Variabili Luminose Blu (LBV), i transienti rossi di luminosità intermedia (ILRTs) e le novae rosse luminose (LRNe). Questi transienti di “gap” possono essere prodotti da diversi meccanismi fisici, e talvolta la loro classificazione è un compito arduo. Uno degli obiettivi principali di questo studio è caratterizzare le proprietà osservative e correlare i parametri fisici dei transienti di “gap”, svelandone la natura. In questo lavoro di tesi, ho studiato in dettaglio un recente evento transiente debole e rosso, AT 2017be, classificato come ILRT, e ho mostrato come una supernova prodotta da cattura elettronica (EC SN) sia lo scenario più probabile per spiegare l’evento eruttivo osservato. Un’analisi approfondita su un grande campione di ILRTs favorisce lo stesso meccanismo di esplosione per tutti questi transienti. Infine, ho studiato un oggetto senza precedenti, AT 2018hso, che rivela proprietà osservative intermedie tra quelle degli ILRT e le LRNe, e che rendono una sua precisa classificazione incerta. Tuttavia, le osservazioni di follow-up supportano la tesi che sia un LRN, quindi probabilmente un transiente prodotto da un evento di coalescenza stellare.
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Book chapters on the topic "Close — supernovae"

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Marsden, Brian G. "Supernovae up close." In Supernovae as Distance Indicators. Springer Berlin Heidelberg, 1985. http://dx.doi.org/10.1007/3-540-15206-7_63.

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Bragaglia, Angela. "The Elusive Close Binary White Dwarfs." In Thermonuclear Supernovae. Springer Netherlands, 1997. http://dx.doi.org/10.1007/978-94-011-5710-0_15.

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Benvenuto, Omar G., and Melina C. Bersten. "Close Binary Stellar Evolution and Supernovae." In Handbook of Supernovae. Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-20794-0_124-1.

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Benvenuto, Omar G., and Melina C. Bersten. "Close Binary Stellar Evolution and Supernovae." In Handbook of Supernovae. Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-21846-5_124.

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Eldridge, J. J. "Population Synthesis of Massive Close Binary Evolution." In Handbook of Supernovae. Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-20794-0_125-1.

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Eldridge, J. J. "Population Synthesis of Massive Close Binary Evolution." In Handbook of Supernovae. Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-21846-5_125.

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den Heuvel, Edward P. J. van. "Supernovae and the Evolution of Close Binary Systems." In Handbook of Supernovae. Springer International Publishing, 2016. http://dx.doi.org/10.1007/978-3-319-20794-0_75-1.

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van den Heuvel, Edward P. J. "Supernovae and the Evolution of Close Binary Systems." In Handbook of Supernovae. Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-21846-5_75.

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Hicks, Ken. "It Came from Outer Space." In Nature’s Balancing Act. Oxford University PressNew York, NY, 2025. https://doi.org/10.1093/9780197771471.003.0007.

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Abstract Life on Earth continually faces dangers from outer space that have the potential to cause mass extinctions. Examples are asteroid impacts, nearby supernova explosions, gamma-ray bursts, or rogue black holes. Supernovae have occurred nearby in the past. Gamma-ray bursts, if pointing toward us, can deliver lethal amounts of radiation. If our solar system were located closer to the galactic center, it is likely that life would have been wiped out. The proof that a large asteroid impact killed off most dinosaurs is now overwhelming. Impacts like this happen every fifty to one hundred million years. The fact that life continues to flourish over the eons despite these dangers speaks to how lucky our existence is. Every time life on Earth has reached a balance point, it has tipped in our favor.
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Boothm, Roy S., and Susanne Aalto. "Molecular Gas, Starbursts and Active Galactic Nuclei." In The Molecular Astrophysics of Stars and Galaxies. Oxford University PressOxford, 1998. http://dx.doi.org/10.1093/oso/9780198501589.003.0020.

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Abstract Active centres of galaxies range from extremely compact active galactic nuclei (AGNs) powered by mass accretion on to black holes to extended starbursts of more modest power. In some extreme cases, e.g. Arp 220, the star-powered luminosity may rival that of a compact AGN. Interest in the connection between the starburst phenomenon and the central AGN has been stimulated by the fact that some galaxies with central AGNs, e.g. NGC 1068 and Centaurus A, contain significant amounts of circumnuclear gas. Molecular gas fuels the star-forming activity and responds physically and chemically to the ultraviolet radiation and supernovae produced in a young population of massive stars. Molecular clouds collide dissipatively and thus sink readily towards the centres of galactic gravitational potentials and may fuel the black holes. The high velocity resolution together with the modest angular resolution achievable in millimetre wave emission line measurements have made molecular emissions useful reddening-free tracers of the central kinematics of galaxies. Indeed, more recent high velocity, high angular resolution VLBI observations of molecular masers have revealed a very close connection between molecules and accretion discs surrounding AGN black holes.
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Conference papers on the topic "Close — supernovae"

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Sokolov, Vladimir V. "On the Observed Mass Distribution of Compact Stellar Remnants in Close Binary Star Systems and Possible Explanations Proposed for the Time Being." In Quark Phase Transition in Compact Objects and Multimessenger Astronomy: Neutrino Signals, Supernovae and Gamma-Ray Bursts. СНЕГ, 2016. http://dx.doi.org/10.26119/sao.2020.1.51263.

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Nava, Lara, and Stefano Gabici. "Cosmic ray diffusion close to supernova remnants: Isotropic vs anisotropic model." In HIGH ENERGY GAMMA-RAY ASTRONOMY: 5th International Meeting on High Energy Gamma-Ray Astronomy. AIP, 2012. http://dx.doi.org/10.1063/1.4772244.

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Ergin, Tulun, Aytap Sezer, Ryo Yamazaki, Hidetoshi Sano, Yasuo Fukui, and Shuta Tanaka. "Detection of an Unidentified Extended Gamma-ray Source Close to the Galactic Supernova Remnant 3C 400.2." In 7th International Fermi Symposium. Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.312.0103.

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