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Готові списки джерел за темами / Astrophysics Technique

Добірка наукової літератури з теми "Astrophysics Technique"

Автор: Grafiati

Опубліковано: 4 червня 2021

Оновлено: 31 січня 2023

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Статті в журналах з теми "Astrophysics Technique":

1

Shen, Yang-Ping, Bing Guo, and Wei-Ping Liu. "An indirect technique in nuclear astrophysics: alpha-cluster transfer reaction." EPJ Web of Conferences 260 (2022): 01001. http://dx.doi.org/10.1051/epjconf/202226001001.

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Helium(4He, or α)is the second most abundant element in the observable Universe. The α-particle induced reactions such as(α, γ), (α, n) and (α, p) play a crucial role in nuclear astrophysics, especially for understanding stellar heliumburning. Because of the strong Coulomb repulsion, it is greatly hindered to directly measure the cross sections for these α-capture reactions at stellar energies. Alpha-cluster transfer reaction is a powerful tool for investigation of astrophysical(α, γ), (α, n)and(α, p)reactions since it can preferentially populate the natural-parity states with an α-cluster structure which dominantly contribute to these astrophysical α-capture reactions during stellar heliumburning. In this paper, we reviewthe theoretical scheme, theexperimental technique, astrophysical applications and the future perspectives of such approach based on α-cluster transfer reactions.

2

Rahma, Siti Nur, Suliyanah Suliyanah, and Abdul Halim. "How do Astrophysics and the Qur'an Perceive the Extraterrestrial Life? A Qualitative Study." Jurnal Pendidikan Fisika 10, no. 2 (April 20, 2022): 107–22. http://dx.doi.org/10.26618/jpf.v10i2.7433.

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The topic of extraterrestrial life is still only a theory and the truth is still being investigated. Therefore, this research aims to analyze the beginning formation of the universe according to astrophysics and the Qur’an, astrophysics discoveries about extraterrestrial life, and letters in the Qur’an that hint at extraterrestrial life, as well as analyzing the relationship between astrophysics and letters in the Qur’an related to extraterrestrial life. This research is qualitative research with a method consisting of library research and interviews. The primary data of this research comes from scientific articles of previous research, relevant books, and interpretations of Qur’an verses. The secondary data were obtained through the results of interviews with experts. The data analysis technique in this study was adapted from the analysis technique of Miles Huberman, while the verses of the Qur’an used the Kemenag interpretation with a scientific interpretation style. The results show that in line with the astrophysical discoveries, the creation of the universe and the existence of extraterrestrial life are also hinted at in the Qur'an. In addition, the alleged presence of water on other planets also supports the signs in the Qur'an. Based on the results, it can be concluded that there is no dichotomy between astrophysical discoveries and signs in the Qur'an regarding extraterrestrial life.

3

Longair, Malcolm. "Radio astronomy and the rise of high-energy astrophysics two anniversaries." International Journal of Modern Physics D 28, no. 02 (January 2019): 1930004. http://dx.doi.org/10.1142/s0218271819300040.

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This paper celebrates the 100th anniversary of the birth of Martin Ryle and the 50th anniversary of the discovery of pulsars by Jocelyn Bell and Antony Hewish. Ryle and Hewish received the 1974 Nobel Prize in Physics, the first in the area of astrophysics. Their interests strongly overlapped, one of the key papers on the practical implementation of the technique of aperture synthesis being co-authored by Ryle and Hewish. The discovery of pulsars and the roles played by Hewish and Bell are described. These key advances were at the heart of the dramatic rise of high-energy astrophysics in the 1960s and led to the realization that general relativity is central to the understanding of high-energy astrophysical phenomena.

4

Mukhamedzhanov, A. M., L. D. Blokhintsev, B. F. Irgaziev, A. S. Kadyrov, M. La Cognata, C. Spitaleri, and R. E. Tribble. "Trojan Horse as an indirect technique in nuclear astrophysics." Journal of Physics G: Nuclear and Particle Physics 35, no. 1 (December 13, 2007): 014016. http://dx.doi.org/10.1088/0954-3899/35/1/014016.

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5

Spitaleri, Claudio. "Trojan Horse technique to measure nuclear astrophysics rearrangement reactions." Journal of Physics: Conference Series 420 (March 25, 2013): 012137. http://dx.doi.org/10.1088/1742-6596/420/1/012137.

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6

Tumino, A., C. Spitaleri, S. Cherubini, V. Crucillà, C. Fu, Z. Elekes, Z. Fülöp, et al. "The trojan horse method as indirect technique in nuclear astrophysics." Journal of Physics: Conference Series 111 (May 1, 2008): 012033. http://dx.doi.org/10.1088/1742-6596/111/1/012033.

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7

Minier, Vincent, Gilles Durand, Pierre-Olivier Lagage, and M. Talvard. "CAMISTIC: THz/submm astronomy at Dome C in Antarctica." Proceedings of the International Astronomical Union 2, no. 14 (August 2006): 709–10. http://dx.doi.org/10.1017/s1743921307012367.

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Submillimetre (submm) astronomy is the prime technique to unveil the birth and early evolution of a broad range of astrophysical objects. It is a relatively new branch of observational astrophysics which focuses on studies of the cold Universe, i.e., objects radiating a significant – if not dominant – fraction of their energy at wavelengths ranging from ∼ 100 μm to ∼ 1 mm. Submm continuum observations are particularly powerful to measure the luminosities, temperatures and masses of cold dust emitting objects. Examples of such objects include star-forming clouds in our Galaxy, prestellar cores and deeply embedded protostars, protoplanetary disks around young stars, as well as nearby starburst galaxies and dust-enshrouded high-redshift galaxies in the early Universe.

8

Bukvić, S., Dj Spasojević, and V. Žigman. "Advanced fit technique for astrophysical spectra." Astronomy & Astrophysics 477, no. 3 (November 12, 2007): 967–77. http://dx.doi.org/10.1051/0004-6361:20065969.

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9

Crossland, Tom, Pontus Stenetorp, Sebastian Riedel, Daisuke Kawata, Thomas D. Kitching, and Rupert A. C. Croft. "Towards machine-assisted meta-studies: the Hubble constant." Monthly Notices of the Royal Astronomical Society 492, no. 3 (December 23, 2019): 3217–28. http://dx.doi.org/10.1093/mnras/stz3400.

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ABSTRACT We present an approach for automatic extraction of measured values from the astrophysical literature, using the Hubble constant for our pilot study. Our rules-based model – a classical technique in natural language processing – has successfully extracted 298 measurements of the Hubble constant, with uncertainties, from the 208 541 available arXiv astrophysics papers. We have also created an artificial neural network classifier to identify papers in arXiv which report novel measurements. From the analysis of our results we find that reporting measurements with uncertainties and the correct units is critical information when distinguishing novel measurements in free text. Our results correctly highlight the current tension for measurements of the Hubble constant and recover the 3.5σ discrepancy – demonstrating that the tool presented in this paper is useful for meta-studies of astrophysical measurements from a large number of publications.

10

SINNIS, GUS. "TeV ASTROPHYSICS WITH THE MILAGRO AND HAWC OBSERVATORIES." International Journal of Modern Physics D 22, no. 11 (September 2013): 1360010. http://dx.doi.org/10.1142/s0218271813600109.

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Ground-based gamma-ray astronomy has historically implemented two dramatically different techniques. One method employs Imaging Atmospheric Cherenkov Telescope(s) (IACT) that detect the Cherenkov light generated in the atmosphere by extensive air showers. The other method employs particle detectors that directly detect the particles that reach ground level — known as Extensive Air Shower (EAS) arrays. Until recently, the IACT method had been the only technique to yield solid detections of TeV gamma-ray sources. Utilizing water Chernkov technology, Milagro, was the first EAS array to discover new gamma-ray sources and demonstrated the power of and need for an all-sky high duty cycle instrument in the TeV energy regime. The transient nature of many TeV sources, the enormous number of potential sources, and the existence of TeV sources that encompass large angular areas all point to the need for an all-sky, high duty-factor instrument with even greater sensitivity than Milagro. The High Altitude Water Cherenkov (HAWC) Observatory will be over an order of magnitude more sensitive than Milagro. In this paper we will discuss the results from Milagro and the design of the HAWC instrument and its experimental sensitivity.

Більше джерел

Дисертації з теми "Astrophysics Technique":

1

MacRae, John Hamish Kenneth. "The detection of very high energy cosmic gamma rays using the atmospheric Cerenkov technique." Thesis, Durham University, 1985. http://etheses.dur.ac.uk/7854/.

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This thesis is concerned with the detection of very high energy cosmic gamma rays using the atmospheric Cerenkov technique. A general introduction to gamma ray detection techniques is followed by a detailed discussion of the principles of the atmospheric Cerenkov technique and the history of its use prior to this work. The design and operation of the University of Durham facility in Dugway, Utah is described in depth. Monte Carlo computer simulations have been developed to assist in both the understanding of the equipment and the analysis of the results for the Durham facility. The variation of the response of the array with zenith angle and detector threshold has been investigated and the aperture function of a single telescope calculated. The latter has been found to be a complicated function of both zenith angle and detector threshold. Computer simulations have also been developed to aid in the design of a camera to record two-dimensional Cerenkov light images from small extensive air showers, and to provide a means of testing analysis routines; these are discussed. The camera is located at the F.L. Whipple Observatory in Arizona. The techniques employed in the analysis of data recorded by the Dugway facility are discussed, and a computer package developed to aid in the routine aspects of the analysis is described. Results of observations from two sources, Cygnus X-3 and PSR0531, are presented, with particular reference to periodicities inherent in the sources and to bursts of gamma ray emission. The discussion of the results includes a review of the various models which have been proposed for Cygnus X-3.

2

Tisserand, Patrick. "Recherches d'astres sombres massifs du halo galactique par la technique des microlentilles gravitationnelles avec les caméras d'EROS-2." Phd thesis, Université de Nice Sophia-Antipolis, 2004. http://tel.archives-ouvertes.fr/tel-00008267.

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Le problème de la masse manquante galactique prend sa source dans l'étude des courbes de rotation des galaxies spirales. Une des hypothèses privilégiées durant les vingt dernières années est la présence d'un halo entourant chaque galaxie composé d'objets compacts sombres (les machos) qui peuvent être détectés indirectement par le phénomène gravitationnel de microlentille. Le travail présenté dans cette thèse concerne l'analyse des courbes de lumière de plus de 55 millions d'étoiles des deux Nuages de Magellan, observées de juin 1996 à février 2003, avec les caméras de l'expérience EROS2. Deux études différentes ont été menées dans le but de détecter d'éventuels objets de 10^(-4) à 1000 masses solaires, complétant ainsi les contraintes déjà posées par EROS entre 10^(-7) et 10 masses solaires. Les candidats découverts sont en nombre insuffisant pour rendre compte de la masse manquante et ne permettent pas non plus de confirmer le signal présenté par le groupe MACHO.

3

Filip, Münz. "La simulation électronique de CELESTE : étude des biais et application à l'obsevation de la Nébuleuse de Crabe." Phd thesis, Université Paris-Diderot - Paris VII, 2003. http://tel.archives-ouvertes.fr/tel-00003334.

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Cette thèse présente le domaine de l'astronomie gamma et les principales sources de notre Galaxie (pulsars et SNRs) et celles situées à des distances cosmologiques (noyaux actifs de galaxie). La technique Cerenkov permet aux observatoires au sol de détecter des rayons gamma d'énergie du GeV absorbés dans l'atmosphère après avoir développé une cascade électromagnétique. Le projet CELESTE a atteint le but d'un seuil bas de 30 GeV, utilisant une grande surface de collection de l'ancienne centrale solaire de Thémis (Pyrénées Orientales). Une étude des principaux éléments du dispositif - un système de déclenchement mixte analogique-digital et un échantillonnage à haute fréquence du signal enregistré en plusieurs points du champ - représente la partie essentielle de cette thèse. Le code développé pour la simulation de la chaîne électronique de l'expérience a été vérifié profondément en faisant des comparaisonsavec les données réelles.
L'incertitude de la calibration en amplitude et de la mise-en-temps pour le déclenchement se traduit en erreurs sur la détermination du seuil en énergie et la surface effective. Les sources des biais éventuels sont étudiées (sur les différents points de la chaîne de simulation). Ces considérations sont appliquées aux observations de la Nébuleuse de Crabe, détectée par CELESTE déjà en 2000.

4

Kreckelbergh, Stephane. "Contrôle longitudinal et caractérisation optique du détecteur Virgo." Phd thesis, Université Paris Sud - Paris XI, 2005. http://tel.archives-ouvertes.fr/tel-00012159.

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Le détecteur Virgo est constitué d'un interféromètre de Michelson avec des cavités Fabry-Perot de 3 km de long dans les bras et utilise la technique de recyclage de puissance. Il a pour but la détection directe des ondes gravitationnelles émises par des sources astrophysiques.
Pour atteindre sa sensibilité, Virgo doit être emmené à son point de fonctionnement par des asservissements tant longitudinaux qu'angulaires. Pour cela, nous avons mis en place un algorithme de contrôle longitudinal ("lock") qui partant d'un interféromètre libre l'emmène à son point de fonctionnement. Pour arriver à ce résultat, nous utilisons la technique de Pound-Drever qui nous permet d'avoir un signal sensible à la variation de la position d'une cavité optique par rapport à la résonance.
Nous avons developpé deux algorithmes. Le premier s'inspire de celui utilisé par la collaboration LIGO. Nous arrivons au point de fonctionnement en contrôlant successivement les quatres longueurs caractéristiques de Virgo. L'application de cet algorithme sur l'instrument s'est soldé par un échec dont les causes sont liées aux différences entre Virgo et LIGO. Le deuxième algorithme nous permet de contrôler simultanément ces quatres longueurs en étant sur la mi frange de l'interféromètre de Michelson. Nous emmenons ensuite l'interféromètre en quelques minutes à son point de fonctionnement de manière déterministe.
Une autre partie de la thèse consiste en la mesure in situ des paramètres optiques nécessaires à la compréhension de l'instrument. Ceci nous a permis à la fois de faire accorder la simulation avec les données et de préparer l'algorithme d'acquisition du lock de Virgo.
Enfin, nous nous intéressons à l'impact de la technique d'Anderson utilisée pour le contrôle angulaire des miroirs sur le contrôle longitudinal des cavités optiques. Nous en montrons le mécanisme et évaluons son impact sur le lock de Virgo.

5

Platts, Emma. "Computational analysis techniques using fast radio bursts to probe astrophysics." Doctoral thesis, Faculty of Science, 2021. http://hdl.handle.net/11427/33921.

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This thesis focuses on Fast Radio Bursts (FRBs) and presents computational techniques that can be used to understand these enigmatic events and the Universe around them. Chapter 1 provides a theoretical overview of FRBs; providing a foundation for the chapters that follow. Chapter 2 details current understandings by providing a review of FRB properties and progenitor theories. In Chapter 3, we implement non-parametric techniques to measure the elusive baryonic halo of the Milky Way. We show that even with a limited data set, FRBs and an appropriate set of statistical tools can provide reasonable constraints on the dispersion measure of the Milky Way halo. Further, we expect that a modest increase in data (from fewer than 100 FRB detections to over 1000) will significantly tighten constraints, demonstrating that the technique we present may offer a valuable complement to other analyses in the near future. In Chapter 4, we study the fine time-frequency structure of the most famous FRB: FRB 121102. Here, we use autocorrelation functions to maximise the structure of 11 pulses detected with the MeerKAT radio telescope. The study is motivated by the low time-resolution of MeerKAT data, which presents a challenge to more traditional techniques. The burst profiles that are unveiled offer unique insight into the local environment of the FRB, including a possible deviation from the expected cold plasma dispersion relationship. The pulse features and their possible physical mechanisms are critically discussed in a bid to uncover the nature and origin of these transients.

6

Lindgren, Sara. "Metallicity determination of M dwarfs." Doctoral thesis, Uppsala universitet, Observationell astrofysik, 2017. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-332102.

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M dwarfs constitute around 70% of all stars in the local Galaxy. Their multitude together with their long main-sequence lifetimes make them important for studies of global properties of the Galaxy such as the initial mass function or the structure and kinematics of stellar populations. In addition, the exoplanet community is showing an increasing interest for those small, cold stars. However, very few M dwarfs are well characterized, and in the case of exoplanetary systems the stellar parameters have a direct influence on the derived planet properties. Stellar parameters of M dwarfs are difficult to determine because of their low surface temperatures that result in an optical spectrum dominated by molecular lines. Most previous works have therefore relied on empirical calibrations. High-resolution spectrographs operating in the infrared, a wavelength region less affected by molecular lines, have recently opened up a new window for the investigation of M dwarfs. In the two first papers of this thesis we have shown that we can determine the metallicity, and in some cases the effective temperature, using synthetic spectral fitting with improved accuracy. This method is time consuming and therefore not practical or even feasible for studies of large samples of M dwarfs. When comparing our results from the high-resolution studies with available photometric calibrations we find systematic differences. In the third paper we therefore used our sample to determine a new photometric metallicity calibration. Compared to previous calibrations our new photometric calibration shows improved statistical characteristics, and our calibration gives similar results as spectroscopic calibrations. In a comparison with theoretical calculations we find a good agreement of the shapes and slopes of iso-metallicity lines with our empirical relation. Applying the photometric calibration to a sample of M dwarfs with confirmed exoplanets we find a possible giant planet-metallicity correlation for M dwarfs.

7

Sajjad, Saeeda. "Développement d'outils de simulation et de reconstruction de gerbes de particules pour l'astronomie gamma avec les futurs imageurs Tcherenkov." Phd thesis, Université Montpellier II - Sciences et Techniques du Languedoc, 2007. http://tel.archives-ouvertes.fr/tel-00408835.

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Le futur de l'astronomie gamma au sol repose sur l'utilisation de grands réseaux d'imageurs Tcherenkov atmosphériques (IACT) avec des capacités améliorées : seuil en énergie plus bas, meilleure sensibilité, meilleurs résolution et pouvoir de rejet. Pour concevoir ces systèmes et optimiser leurs caractéristiques, il est nécessaire de comprendre les gerbes atmosphériques et de disposer d'outils de simulation adaptés permettant d'évaluer les performances des réseaux. La première partie de cette thèse traite des gerbes atmosphériques, des propriétés de la lumière Tcherenkov qu'elles émettent et de leur simulation. La seconde partie présente les outils que nous avons développés pour la simulation des télescopes à imagerie Tcherenkov atmosphérique et les caractéristiques des images qu'ils obtiennent. La troisième partie de cette thèse contient une présentation des outils dévéloppés pour la reconstruction de la source, du pied de gerbe et de l'énergie ainsi que des propositions pour la séparation gamma-hadrons. Dans la dernière partie, ces outils sont utilisés pour étudier deux grands réseaux de télescopes à deux altitudes différentes et pour donner leurs performances pour la détection des rayons gamma.

8

Popescu, Marcel. "Techniques d'observation spectroscopique d'astéroïdes." Phd thesis, Observatoire de Paris, 2012. http://tel.archives-ouvertes.fr/tel-00785991.

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L'objectif fondamental des sciences planétaires est la compréhension de la formation et de l'évolution du Système Solaire. Pour atteindre cet objectif les astéroïdes présentent un intérêt tout particulier pour la communauté scientifique. En effet, nous pouvons regarder la population astéroïdale comme une fenêtre vers le passée, par laquelle nous regardons les débuts de la formation du système planétaire. Ils sont les témoins des premiers moments de la formation des planètes gardant dans leur structure la complexité chimique de la nébuleuse primordiale. Pour cette raison, les études physiques et dynamiques de ces corps nous apportent des informations essentielles sur l'histoire et l'évolution de notre Système Solaire et plus généralement sur la formation des systèmes planétaires. Pendant ma thèse j'ai développé l'application Modelling for Asteroids (acronyme M4AST). M4AST est un service en libre service sur internet permettant la modélisation des surfaces d'astéroïdes en utilisant plusieurs approches théoriques. M4AST est composé d'une base de données contenant quelques 2500 spectres d'astéroïdes et d'une bibliothèque de routines permettant la modélisation et l'obtention de plusieurs paramètres minéralogiques. La base de données est accessible aussi bien par les biais des protocoles de l'Observatoire Virtuel (OV-Paris) que par sa propre interface. Le service est accessible depuis l'adresse http:// cardamine.imcce.fr/m4ast. M4AST permet plusieurs types d'analyses : classification taxonomique, modélisation de l'altération spatiale, comparaison avec les spectres des météorites et des minéraux terrestres, calculs des centres et des surfaces des bandes. J'ai participé à plus de 10 campagnes d'observations pour la caractérisation physique et dynamique des astéroïdes. Les observations spectroscopiques ont servi à la caractérisation minéralogique des surfaces d'astéroïdes. L'astrométrie a plutôt servi à la confirmation et la sécurisation de nouvelles découvertes d'astéroïdes. Pendant la thèse, j'ai observé et caractérisé les spectres en infrarouge proche de huit astéroïdes géocroiseurs : 1917, 8567, 16960, 164400, 188452, 2010 TD54, 5620, and 2001 SG286. Ces observations ont été obtenues avec le télescope IRTF et du spectrographe SpeX, en employant l'infrastructure CODAM de l'Observatoire de Paris. Pour chaque astéroïde j'ai proposé des solutions minéralogiques. Une révision de leur taxonomie a aussi été effectuée pour cinq astéroïdes de mon échantillon. Quatre des objets sont des objets à faible delta-V, qui sont des cibles souhaitables/possibles pour des missions spatiales. L'astéroïde (5620) Jasonwheeler montre un spectre similaire à ceux des météorites chondritiques. J'ai observé et modélisé six astéroïdes de la ceinture principale. (9147) Kourakuen, (854) Frostia, (10484) Hecht and (31569) 1999 FL18 montrent des caractéristiques des astéroïdes du type V; (1333) Cevenola, (3623) Chaplin sont du type taxonomique S. Quelques astéroïdes de cet échantillon sont particuliers : (854) Frostia est un astéroïde binaire, (10484) Hecht et (31569) 1999 FL18 ont des gémeaux dynamiques, (1333) Cevenola et (3623) Chaplin sont des objets avec des courbes de lumières à grandes amplitudes. La classification taxonomique, la comparaison avec les météorites, permettent l'établissement des solutions minéralogiques intéressantes et des ressemblances avec les météorites de la classe des howardites, eucrites et diogenites.

9

Adamakis, Sotiris. "Application of statistical analysis techniques to solar and stellar phenomena." Thesis, University of Central Lancashire, 2009. http://clok.uclan.ac.uk/20908/.

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Currently, solar observers are investigating spectroscopic images of the Sun's outermost atmosphere (the corona), which are challenging long-held views on the density and temperature structure of this environment. The corona is "filled" with magnetic strands but determining their precise nature is not straightforward. One way of revealing the nature of the coronal heating mechanism is by comparing simple theoretical one dimensional hydrostatic loop models with observations of the temperature and/or density structure along these features. The most wellknown method for dealing with comparisons like that is the x2 approach. In this research we consider the restrictions imposed by this approach and present an alternative way for making model comparisons using Bayesian statistics. In order to quantify our beliefs we use Bayes factors and information criteria such as AIC and BIC. Three simulated data-sets are analysed in order to validate the procedure and assess the effects of varying error bar size. Another three datasets (Ugarte-Urra ci at., 2005; Priest ci at., 2000; Young ci al., 2007) are analysed using the method described above. For the Ugarte-Urra ci at. and Young ci al. data-sets, we conclude apex dominant heating is the likely heating candidate, whereas the Priest ci al. data-set implies basal heating. Note that these new results (regarding the Ugarte-Urra ci at. and Priest ci at. data-sets) are different from those obtained using the chi-squared statistic. The second research project involves extensive model comparison against solar flare plasma observed cooling curves. After a solar flare erupts, flare-loops form which cool over thousands of seconds. How the plasma cools over time is investigated. In this case, we test the adequacy of the zero-dimensional EBTEL (Enthalpy-Based Thermal Evolution of Loops) model as introduced by Klimchuk, Patsourakos, and Cargill (2008). An interesting approach here is to define the form of the non-thermal heating input to the system and compare it with the thermal heating input. For the data-set under investigation (Raftery et al., 2009) a Full-Gaussian energy profile is proposed. Also, from the data it is not possible to distinguish which of the thermal or non-thermal heat flux is more dominant, so both can be equally considered for temperature, density and pressure evolution of the system. Finally, the last part of this research is dedicated to recurrent nova outbursts. RS Ophiuehi is a nova produced by a white dwarf star and a red giant. In this case the white dwarf will steadily acerete gases on its surface from the red giant's outer atmosphere. About every twenty years, enough material will be accreted on the white dwarf's surface in order to produce an eruption. Over the past one hundred years at least five such outbursts have been observed. As another application of Bayesian model comparison techniques, curve fitting models are tested against light curves of RS Ophiuchi outbursts in order to decide upon the one that best describes the data. Furthermore, the magnitude of the star is analysed using wavclet analysis techniques. Ways of deriving the Cone of Influence are presented. An outcome of this analysis is that we can quantitatively confirm that an outburst occurred around November 26, 1945, which was not recorded due to the observational seasonal gaps. This was originally proposed by Oppenheimer and Mattei (1993) but was never accepted as a confirmed outburst. Also, this method reveals a pre-outburst signal in the light curve. For this, the way in which the wavelet analysis can be beneficial for future outburst predictions is presented.

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Hills, Graeme Lawrence. "The application of polarimetric techniques to gamma ray astronomy." Thesis, University of Southampton, 1996. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.243187.

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Книги з теми "Astrophysics Technique":

1

Smith, Robert C. Observational astrophysics. Cambridge: Cambridge University Press, 1995.

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2

P, Ehrenfreund, ed. Laboratory astrophysics and space research. Boston: Kluwer Academic Publishers, 1999.

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3

International, School of Physics "Enrico Fermi" (1989 Varenna Italy). Solid-state astrophysics: 27 June-7 July 1989. Amsterdam: North-Holland, 1991.

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4

Kitchin, C. R. Astrophysical techniques. 5th ed. Boca Raton: CRC Press, 2008.

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5

Kitchin, C. R. Astrophysical techniques. 4th ed. Bristol: Institute of Physics Pub., 2003.

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6

Kitchin, C. R. Astrophysical techniques. 3rd ed. Bristol: Institute of Physics Pub., 1998.

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7

Kitchin, C. R. Astrophysical techniques. 2nd ed. Bristol [England]: IOP Pub., 1991.

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8

Italy) European Summer School on Experimental Nuclear Astrophysics (5th 2009 Acireale. Fifth European Summer School on Experimental Nuclear Astrophysics, Santa Tecla, Sicily, Italy, 20-27 September 2009. Edited by Spitaleri C. (Claudio), Rolfs Claus E, and Pizzone Rosario Gianluca. Melville, N.Y: American Institute of Physics, 2010.

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9

Astrophysics School (4th 1991 Graz, Austria). Galactic high-energy astrophysics ; High-accuracy timing and positional astronomy: Lectures held at the Astrophysics School IV, organized by the European Astrophysics Doctoral Network (EADN) in Graz, Austria, 19-31 August 1991. Berlin: Springer-Verlag, 1993.

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10

Liège International Astrophysical Colloquium (27th 1987). Observational astrophysics with high precision data: Proceedings of the 27th Liège International Astrophysical Colloquium, June 23-26, 1987. Cointe-Ougrée, Belgique: Université de Liège, Institut d'astrophysique, 1987.

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Частини книг з теми "Astrophysics Technique":

1

Rowe, B. R., J. B. Marquette, and G. Dupeyrat. "Measurements Of Ion-Molecule Reaction Rate Coefficients Between 8 and 160 K by the Cresu Technique." In Molecular Astrophysics, 631–38. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5432-8_31.

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2

Porter, N. A. "The Atmospheric Čerenkov Technique in the Search for PBH." In TeV Gamma-Ray Astrophysics, 67–69. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0171-1_6.

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3

Fors, O., and J. Núñez. "CCD Scanning Technique Applied to Millisecond Photometric Observations." In Highlights of Spanish Astrophysics II, 293–96. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-017-1776-2_68.

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4

Weekes, Trevor C. "The Atmospheric Cherenkov Technique in Very High Energy Gamma-Ray Astronomy." In TeV Gamma-Ray Astrophysics, 1–15. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0171-1_1.

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5

Singh, Puneet, Amit Chatterjee, Vimal Bhatia, and Shashi Prakash. "Viability Assessment of Kidney Bean Seed (Phaseolus Vulgaris sp.) Using Robust Biospeckle Indexing Technique." In Computational Mathematics, Nanoelectronics, and Astrophysics, 189–95. Singapore: Springer Singapore, 2021. http://dx.doi.org/10.1007/978-981-15-9708-4_18.

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6

Champavert, N., and H. Wozniak. "A New Chemodynamical Tool to Study the Evolution of Galaxies in the Local Universe: a Quick and Accurate Numerical Technique to Compute the Gas Cooling Rate for any Chemical Composition." In Eso Astrophysics Symposia, 409–11. Berlin, Heidelberg: Springer Berlin Heidelberg, 2007. http://dx.doi.org/10.1007/978-3-540-73484-0_75.

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7

Lestrade, Jean-François, Alan E. E. Rogers, Arthur E. Niell, and Robert A. Preston. "Astrometry of Millijansky Sources using a Phase Reference VLBI Technique." In The Impact of VLBI on Astrophysics and Geophysics, 323–24. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2949-4_109.

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8

Kankainen, A., Yu N. Novikov, H. Schatz, and C. Weber. "Mass measurements of neutron-deficient nuclei and their implications for astrophysics." In Three decades of research using IGISOL technique at the University of Jyväskylä, 345–63. Dordrecht: Springer Netherlands, 2012. http://dx.doi.org/10.1007/978-94-007-5555-0_27.

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9

Gupta, Sumit, Devendra Kumar, Jagdev Singh, and Sushila. "An Efficient Computational Technique for Nonlinear Emden-Fowler Equations Arising in Astrophysics and Space Science." In 4th International Conference on Computational Mathematics and Engineering Sciences (CMES-2019), 76–98. Cham: Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-030-39112-6_5.

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10

Wood, Matt. "Numerical Techniques in Astrophysics." In Planets, Stars and Stellar Systems, 481–502. Dordrecht: Springer Netherlands, 2013. http://dx.doi.org/10.1007/978-94-007-5618-2_11.

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Тези доповідей конференцій з теми "Astrophysics Technique":

1

Mukha, Ivan, Hajime Susa, Marcel Arnould, Sydney Gales, Tohru Motobayashi, Christoph Scheidenberger, and Hiroaki Utsunomiya. "2p radioactivity studied by tracking technique." In TOURS SYMPOSIUM ON NUCLEAR PHYSICS AND ASTROPHYSICS—VII. AIP, 2010. http://dx.doi.org/10.1063/1.3455942.

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2

Ivashchenko, Ganna, Olga Sergijenko, and Olena Torbaniuk. "Improved technique for quasar composite spectra generation." In VI European Summer School on Experimental Nuclear Astrophysics. Trieste, Italy: Sissa Medialab, 2013. http://dx.doi.org/10.22323/1.148.0007.

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3

Garcia, Iskya. "Water Cherenkov Detector installation by the Vertical Muon Equivalent technique." In 4th School on Cosmic Rays and Astrophysics. Trieste, Italy: Sissa Medialab, 2011. http://dx.doi.org/10.22323/1.118.0009.

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4

Hadinia, B. "First Identification of γ-rays in 106Te Using Recoil Decay Tagging Technique". У FRONTIERS IN NUCLEAR STRUCTURE, ASTROPHYSICS, AND REACTIONS - FINUSTAR. AIP, 2006. http://dx.doi.org/10.1063/1.2200981.

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5

Brown, J. R., M. A. Bentley, M. J. Taylor, P. Aldrich, D. Bazin, J. M. Cook, C. A. Diget, et al. "Mirrored Fragmentation Reactions—A New Technique for Probing Isospin Symmetry in Exotic Nuclei." In FRONTIERS IN NUCLEAR STRUCTURE, ASTROPHYSICS, AND REACTIONS: FINUSTAR 2. AIP, 2008. http://dx.doi.org/10.1063/1.2939325.

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6

Doukellis, G., G. Galios, S. Kossionides, and Themis Paradellis. "Novel technique for measurements of neutron cross sections and its application to nuclear astrophysics." In 4th International Conference on Applications of Nuclear Techniques: Neutrons and their Applications, edited by George Vourvopoulos and Themis Paradellis. SPIE, 1995. http://dx.doi.org/10.1117/12.204199.

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Kwak, Kyujin. "Numerical Simulation of 2-D Relativistic Hydrodynamics Using Adaptive Mesh Refinement Technique." In GAMMA-RAY BURSTS IN THE SWIFT ERA: Sixteenth Maryland Astrophysics Conference. AIP, 2006. http://dx.doi.org/10.1063/1.2207878.

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8

Karimabadi, H. "A New Simulation Technique for Study of Collisionless Shocks: Self-Adaptive Simulations." In THE PHYSICS OF COLLISIONLESS SHOCKS: 4th Annual IGPP International Astrophysics Conference. AIP, 2005. http://dx.doi.org/10.1063/1.2032675.

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BOYLE, PATRICK J. "DEVELOPMENT OF THE IMAGING ATMOSPHERIC CHERENKOV TECHNIQUE AT THE WHIPPLE OBSERVATORY." In Proceedings of the 13th Course of the International School of Cosmic Ray Astrophysics. WORLD SCIENTIFIC, 2004. http://dx.doi.org/10.1142/9789812702968_0028.

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Connors, Riley, David van Eijnatten, Chiara Ceccobello, and Sera Markoff. "Using a joint spectral fitting technique to explore the outflow geometry of GX 339-4 during the hard state." In 11th INTEGRAL Conference Gamma-Ray Astrophysics in Multi-Wavelength Perspective. Trieste, Italy: Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.285.0071.

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