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Littérature scientifique sur le sujet « Astronomia X »

Auteur : Grafiati

Publié le 9 mars 2023

Mis à jour le 10 mars 2023

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Articles de revues sur le sujet "Astronomia X"

Lopes, C. E. F., et M. G. Pereira. « Astronomia no Infravermelho de Estrelas Variáveis ». Sitientibus Série Ciências Físicas 1 (20 décembre 2005) : 52–58. http://dx.doi.org/10.13102/sscf.v1i.5254.

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Este trabalho tem por objetivo fazer um estudo fotométrico de estrelas variáveis utilizando dados fotométricos do projeto 2 Micron All Sky Survey. Foram analisados dados de fotometria infravermelho nas bandas JHKs de cinco tipos de estrelas variáveis: Wolf Rayet, RS Canum Venaticorum, Sistemas Binários de Raios-X, Fontes Super Soft e Estrelas Simbióticas. As materializações de diagramas Cor-Cor permitiram um estudo das propriedades fotométricas infravermelho intrínsecas destas fontes, e assim obteve-se uma ferramenta para identificação de alvos para estudos mais detalhados a serem realizados posteriormente com telescópios de maior porte.

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Lopes, C. E. F., et M. G. Pereira. « Astronomia no Infravermelho de Estrelas Variáveis ». Sitientibus Série Ciências Físicas 1 (20 décembre 2005) : 52. http://dx.doi.org/10.13102/sscf.v1i0.5254.

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Este trabalho tem por objetivo fazer um estudo fotométrico de estrelas variáveis utilizando dados fotométricos do projeto 2 Micron All Sky Survey. Foram analisados dados de fotometria infravermelho nas bandas JHKs de cinco tipos de estrelas variáveis: Wolf Rayet, RS Canum Venaticorum, Sistemas Binários de Raios-X, Fontes Super Soft e Estrelas Simbióticas. As materializações de diagramas Cor-Cor permitiram um estudo das propriedades fotométricas infravermelho intrínsecas destas fontes, eassim obteve-se uma ferramenta para identificação de alvos para estudos mais detalhados a serem realizados posteriormente com telescópios de maior porte.

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Pereira, Ana Carolina Costa, Antonia Naiara de Sousa Batista et Isabelle Coelho da Silva. « A matemática incorporada na construção do quadrante descrito na obra Libros del Saber de Astronomía ». Revemat : Revista Eletrônica de Educação Matemática 12, n^o 1 (13 septembre 2017) : 173. http://dx.doi.org/10.5007/1981-1322.2017v12n1p173.

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Dentre as várias alternativas de inserir a história da matemática no ensino, vislumbramos os instrumentos matemáticos, em especial, o quadrante em um quarto de círculo, ou quadrante náutico, utilizado na astronomia de posição, como um recurso que incorpora, manipula e dissemina diversos conceitos. Dessa forma, o artigo tem o intuito de apresentar a matemática presente na construção do quadrante na busca por interfaces que permitam a articulação de conceitos matemáticos em sala de aula. A construção do quadrante está baseada na obra Libros del saber de Astronomía compilado pelo Rei D. Afonso X de Cartilha, escrita entre 1276 e 1279. Esse instrumento apresenta propriedades geométricas que podem ser incorporadas nas aulas de matemática, principalmente, envolvendo a construção de desenhos geométricos, semelhança de triângulos e conceitos fundamentais de trigonometria. Consideramos que a competência didática do instrumento matemático para o ensino é algo palpável e possível de ser introduzido na sala de aula. Contudo, precisamos observá-lo como um elemento que agrega conhecimentos, e não apenas o entendimento das relações matemática envolvidas na sua construção e utilização, mas a compreensão dos motivos de certas construções serem realizadas dessa forma ou estarem naquele local.

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Parmar, A. N., M. Bavdaz, F. Favata, T. Oosterbroek, A. Orr, A. Owens, U. Lammers et D. Martin. « Early Results from the Low-Energy Concentrator Spectrometer on-board BeppoSAX ». Symposium - International Astronomical Union 188 (1998) : 71–74. http://dx.doi.org/10.1017/s0074180900114457.

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SAX, an acronym for “Satellite Italiano per Astronomia a raggi X”, now renamed “BeppoSAX” in honor of Giuseppe Occhialini, is the first X-ray mission sensitive in the very broad energy range between 0.1 and 300 keV (Boella et al. 1997a). The Narrow Field Instruments (NFI) have approximately 1° fields of view and consist of the imaging low- and medium-energy concentrator spectrometers (LECS, 0.1-10 keV, Parmar et al. 1997; and MECS, 1-10 keV, Boella et al. 1997b), and the non-imaging high pressure gas scintillation proportional counter (HPGSPC, 3-120 keV, Manzo et al. 1997) and Phoswich detector system (PDS, 15-300 keV, Frontera et al. 1997). All the NFI are coaligned and are normally operated simultaneously. In addition, the payload includes two wide field cameras (WFC, 2-30 keV; Jager et al. 1997) which observe in directions perpendicular to the NFI. These allow the detection of X-ray transient phenomena, as well as long-term variability studies.

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De Melo, Enaldo Vieira, et Elton Casado Fireman. « Ensino e aprendizagem de funções trigonométricas por meio do software Geogebra aliado à Modelagem Matemática ». Revista de Ensino de Ciências e Matemática 7, n^o 5 (22 décembre 2016) : 12–30. http://dx.doi.org/10.26843/rencima.v7i5.1182.

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A presente pesquisa qualitativa, delineado por um estudo de caso com pesquisa participante, analisou as contribuições da utilização do software Geogebra aliado à Modelagem Matemática no ensino-aprendizagem das funções trigonométricas seno e cosseno, à luz da Aprendizagem Significativa. O estudo foi aplicado a 18 alunos do segundo ano do Ensino Médio de uma escola pública do município de Marechal Deodoro, Alagoas. A investigação foi regida por uma Sequência Didática de Ensino, produto desta dissertação, na qual foi trabalhado o software junto com a Modelagem Matemática de fenômenos periódicos. Os resultados da pesquisa mostraram que o uso do software Geogebra otimizou o ensino e a aprendizagem de funções trigonométricas; foi possível utilizar a Modelagem Matemática como uma metodologia de ensino para a aprendizagem das funções f(x)=a+bsen(cx+d) e g(x)=a+bcos(cx+d); e que os discentes compreenderam o comportamento dos seus parâmetros a, b, c e d. O estudo tem como principal contribuição, a conexão realizada pelos estudantes entre o conteúdo de funções trigonométricas e o cotidiano, através de sua aplicação na previsão de fenômenos periódicos (altura da maré e fases lunares), entendendo ainda a importância deste assunto para outras áreas do conhecimento, como física, astronomia, biologia e medicina, obtendo assim, uma Aprendizagem Significativa.

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Campos, Guadalupe Do Nascimento, Marcus Granato, Antonieta Middea et Ricardo Tadeu Lopes. « ARQUEOMETRIA APLICADA À CONSERVAÇÃO DO PATRIMÔNIO ARQUEOLÓGICO METÁLICO : UM ESTUDO DE CASO DO SÍTIO FUNERÁRIO DE SÃO GONÇALO GARCIA, RIO DE JANEIRO ». Cadernos do LEPAARQ (UFPEL) 15, n^o 30 (30 novembre 2018) : 290. http://dx.doi.org/10.15210/lepaarq.v15i30.13620.

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O presente trabalho apresenta alguns dos resultados obtidos no âmbito do projeto de pesquisa Conservação e Caracterização Microanalítica de Objetos Arqueológicos Metálicos, desenvolvido no Museu de Astronomia e Ciências Afins - MAST. O projeto tem como objetivo principal estabelecer metodologias de caracterização e conservação do patrimônio arqueológico metálico. Os artefatos selecionados para o estudo de caso são provenientes do Sítio Funerário da Igreja São Gonçalo Garcia (região central do Rio de Janeiro), relacionados aos séculos XVIII e XIX. Para os exames arqueométricos, foram empregadas as seguintes técnicas de caracterização: radiografia digital e microtomografia computadorizada de raios X, microscopias estereoscópica e eletrônica de varredura, espectroscopia de energia dispersiva (MEV/EDS) e difratometria de raios X. Foram obtidas informações sobre a composição dos artefatos (fase metálica e alguns produtos de corrosão), detalhes da morfologia em 3D não visíveis a olho nu, extensão da mineralização, dentre outros aspectos. Abstract: This paper presents some of the achieved results in the "Microanalytical Conservation and Characterization of Metallic Archaeological Objects" research project, developed at the Museum of Astronomy and Related Sciences - MAST. The project's main goal is to establish methodologies for characterization and conservation of the metallic archaeological heritage. The artifacts selected for the case study are from the Funeral Site at São Gonçalo Garcia's Church (Rio de Janeiro's central region), related to the 18th and 19th centuries. For the archaeometric examinations, the following characterization techniques were employed: digital radiography and X ray microtomography, stereoscopic and scanning electron microscopy, energy-dispersive X ray spectroscopy (SEM / EDS) and X ray diffraction. Results were obtained about the artifacts's composition (metallic phase and some corrosion products), 3D morphology details invisible to the naked eye, and the extent of the mineralization, among other aspects.

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LIPPI, DONATELLA. « ASTRONOMIA B. STEPHENSON, M. BOLT, A. F. FRIEDMAN, The universe unveiled. Instruments and Images through History, Cambridge, Cambridge Univ. Press 2000, 152 pp., (ISBN 0-521-79143-X). » Nuncius 16, n^o 1 (1 janvier 2001) : 447–48. http://dx.doi.org/10.1163/221058701x00301.

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Ivorra, Adolfo. « Manlio SODI (ed.), Astronomia e culto. Risposta a domande di attualità, Padova : Edizioni Messaggero Padova («Instant book»), 2009, 151 pp., 11 x 17, ISBN 978-88-250-2145-5. » Scripta Theologica 43, n^o 1 (10 novembre 2015) : 243. http://dx.doi.org/10.15581/006.43.3336.

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Lemoine, Martin, et Guy Perrin. « Les X astronomes ». Bulletin de la Sabix, n^o 35 (1 janvier 2004) : 44–49. http://dx.doi.org/10.4000/sabix.443.

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Palhares, Dario, et Íris Almeida dos Santos. « Astronomic Bioethics : Terraforming X Planetary protection ». Bangladesh Journal of Bioethics 8, n^o 2 (3 novembre 2017) : 1–10. http://dx.doi.org/10.3329/bioethics.v8i2.34474.

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A hard difficulty in Astrobiology is the precise definition of what life is. All living beings have a cellular structure, so it is not possible to have a broader concept of life hence the search for extraterrestrial life is restricted to extraterrestrial cells. Earth is an astronomical rarity because it is difficult for a planet to present liquid water on the surface. Two antagonistic bioethical principles arise: planetary protection and terraforming. Planetary protection is based on the fear of interplanetary cross-infection and possible ecological damages caused by alien living beings. Terraforming is the intention of modifying the environmental conditions of the neighbouring planets in such a way that human colonisation would be possible. The synthesis of this antagonism is ecopoiesis, a concept related to the creation of new ecosystems in other planets. Since all the multicellular biodiversity requires oxygen to survive, only extremophile microorganisms could survive in other planets. So, it could be carried out a simulation of a meteorite by taking to other planets portions of the terrestrial permafrost, or ocean or soil, so that if a single species could grow, a new ecosystem would start, as well as a new Natural History. As a conclusion, ecopoiesis should be the bioethical principle to guide practices and research in Astrobiology.

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Thèses sur le sujet "Astronomia X"

Camero, Arranz Ascension. « Accreting X-Ray pulsars. The high energy picture ». Doctoral thesis, Universitat de València, 2007. http://hdl.handle.net/10803/9484.

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El objetivo principal de esta tesis ha sido el estudio del comportamiento transitorio durante estallidos de distinto tipo, de una selección de pulsares acretores en rayos X, localizados en el plano galáctico.Con ello se pretende haber avanzado hacia una explicación más clara de la naturaleza de estas objetos binarios de alta masa (con estrella de neutrones como objeto compacto), así como de los mecanismos físicos que operan en este escenario. Para todo esto se han analizado datos de dos misiones espaciales:INTEGRA Y RXTE.El segundo objetivo ha sido el estudio de la zona del brazo galactico de Scutum. Al ser esta una región de fuerte absorción se cree de la existencia de sistemas del tipo anteriormente mencionado este todavía escondidos, y los cuales solo pueden ser descubiertos a altas energías. En esta tesis se han podido presentar resultados esperanzadores, con la detección de varios objetos posibles nuevos candidatos a pulsares acretores de rayos X.

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Parisi, Pietro <1982&gt. « Multiwavelength studies of hard X-ray selected sources ». Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2011. http://amsdottorato.unibo.it/3775/1/Parisi_Pietro_tesi.pdf.

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Parisi, Pietro <1982&gt. « Multiwavelength studies of hard X-ray selected sources ». Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2011. http://amsdottorato.unibo.it/3775/.

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Munar, i. Adrover Pere. « High energy processes in young stellar objects and high-mass X-ray binaries ». Doctoral thesis, Universitat de Barcelona, 2014. http://hdl.handle.net/10803/144509.

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The high energy astrophysics, specifically the gamma-ray astrophysics, studies the processes that cannot be caused by hot matter but by other mechanisms colled non thermaland processes, which involve matter with energies above ~ 1 MeV. There are currently a number of instruments able to detect this radiation, such as AGILE and Fermi satellites or Cherenkov telescopes like MAGIC at the Earth's surface. In this thesis we studied two main types of systems that, as it has been observed or theoretically predicted, can produce gamma radiation : young stellar objects and high-mass X-ray binaries. Young stellar objects are found in regions of star formation, which are the cradles where new stars are being formed. The star-forming regions are populated with protostars and young stars, among other objects. Protostars still accrete matter from the parent cloud through an accretion disk, while expelling material through a jet formed by magnetic interaction. In these jets the particles are ejected at high speeds out of the system and in some cases reach relativistic velocities, as evidenced by the detection of non-thermal radio emission in some of these objects. In this thesis we are interested to find more evidence of young stellar objects that present non-thermal emission, either in the range of X-rays or gamma rays. To find new candidates have used the first catalog of the Fermi satellite and the catalogs of young systems in our Galaxy. Besides the search through catalogs, we did a study using archival X-ray XMM-Newton data on the young stellar object IRAS 16547-4247, which is known to display non-thermal radio emission. This object is a protostar still accretes material through an accretion disk and also ejects jets of material through particle. We discovered its X-ray counterpart and studied the interaction of its jets through a theoretical model. Finally, we studied a region of star formation that has been found in spatial coincidence with a second Fermi source catalog, known as Monoceros R2 . We analyzed the Fermi data from this source and our results allow us to say that the detected gamma-ray emission is consistent with that expected by the collective effects of a population of protostars. Among the other large block of this thesis there are high-mass X-ray binares. The most relevant of which we have studied is MWC 656. This system consists of a Be star and a black hole, a combination that has never been detected before. We have observed this source with XMM-Newton in X-rays and with the MAGIC Telescopes in very high energy gamma rays. Our X-ray observation has led to the discovery of the X-ray counterpart of this binary system and has allowed us to classify it as a high-mass X-ray binary, the first composed of a Be star and a black hole. Other systems we studied with MAGIC are HESS J0632 +057 and SS 433. HESS J0632 +057 is a binary system consisting of a Be star and a compact object of unknown nature and was identified by us as a gamma-ray emitter. We have also observed SS 433, the first microquasar ever discovered. We observed this source during 2010 May and June, but it has not been detected. We have calculated upper limits to the emission of very high energy gamma-rays to put constraints on the physical parameters of the system.
L'astrofísica d'altes energies i en concret l'astrofísica de raigs gamma, estudia els processos d'emissió que no poden ser causats per matèria calenta, sinó per altres mecanismes que anomenem no tèrmics i que comporten que la matèria que emet aquesta radiació tingui energies per sobre d'1~MeV. Actualment disposem d'un bon nombre d'instruments capaços de detectar aquesta emissió, com ara els satèl•lits Fermi i AGILE o els telescopis Cherenkov com MAGIC, a la superfície terrestre. En aquesta tesi hem estudiat principalment dos tipus de sistemes que, tal com s'ha observat o predit teòricament, poden produir radiació gamma: els objectes estel•lars joves i els sistemes binaris de raigs X d’alta massa. Els objectes estel•lars joves els trobem a les regions de formació estel•lar, que són els bressols on noves estrelles s'estan formant. Els pobladors de les regions de formació estel•lar són les protoestrelles i les estrelles joves, entre altres objectes celests. Les protoestrelles encara acretem matèria del núvol progenitor a través d'un disc d'acreció, i al mateix temps expulsen material per mitjà d'uns dolls formats per interacció magnètica. En aquests dolls les partícules són expulsades a grans velocitats cap a fora del sistema i en alguns casos assoleixen velocitats relativistes tal com evidencia la detecció d'emissió ràdio no tèrmica en alguns d'aquests objectes. En aquesta tesi ens hem interessat per trobar evidència de més objectes estel•lars joves que presentin emissió no tèrmica, ja sigui en el rang dels raigs X o dels raigs gamma. Per a trobar nous candidats hem aprofitat el primer catàleg del satèl•lit Fermi i l'hem creuat amb catàlegs d'objectes joves de la Galàxia. A més a més de la cerca per mitjà de catàlegs, hem fet un estudi en raigs X a partir de dades d'arxiu disponibles sobre un objecte estel•lar jove del que ja es coneix emissió no tèrmica en ràdio: IRAS 16547-4247. Aquest objecte és una protoestrella que encara acreta material per mitjà d'un disc d'acreció i que alhora expulsa material a través de dolls de partícules. Hem descobert la contrapartida en raigs X d'aquest sistema i l'hem estudiat per mitjà d'un model teòric. Finalment, hem estudiat una regió de formació estel•lar que s'ha trobat en coincidència espacial amb una font del segon catàleg de Fermi, coneguda com Monoceros R2. Hem analitzat les dades de Fermi d'aquesta font i els nostres resultats ens permeten dir que l'emissió gamma detectada és compatible amb el que s'esperaria que produissin un conjunt de protoestrelles. Dins de l'altre gran bloc d'aquesta tesi trobem les estrelles binàries de raigs X d'alta massa. El cas més rellevant dels que hem estudiat és el de MWC 656. Aquest sistema està format per una estrella Be i un forat negre, una combinació que mai s'havia detectat. Nosaltres hem observat aquesta font amb el telescopi de raigs X XMM-Newton i amb els Telescopis MAGIC, en raigs gamma de molt alta energia. La nostra observació de raigs X ha suposat la descoberta de la contrapartida de raigs X d'aquest sistema binari i ens ha permès classificar-la com a binària de raigs X d'alta massa, la primera composada per una estrella Be i un forat negre. Altres sistemes que hem estudiat amb MAGIC són HESS J0632+057 i SS 433. HESS J0632+057 és un sistema binari format per una estrella Be i un objecte compacte de natura desconeguda i va ser detectat per nosaltres com a emissor de raigs gamma. També hem observat SS 433, el primer microquàsar que es va descobrir. Hem observat aquesta font durant els mesos de maig i juny de 2010 però no s'ha detectat. Així, hem calculat límits superiors a l'emissió gamma de molt alta energia que serveixen per a posar restriccions en paràmetres físics.

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Donnarumma, Annamaria <1981&gt. « X-ray and lensing mass estimates in galaxy clusters ». Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2010. http://amsdottorato.unibo.it/2955/1/donnarumma_annamaria_tesi.pdf.

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In this Thesis we have presented our work on the analysis of galaxy clusters through their X-ray emission and the gravitational lensing effect that they induce. Our research work was mainly finalised to verify and possibly explain the observed mismatch between the galaxy cluster mass distributions estimated through two of the most promising techniques, i.e. the X-ray and the gravitational lensing analyses. Moreover, it is an established evidence that combined, multi-wavelength analyses are extremely effective in addressing and explaining the open issues in astronomy: however, in order to follow this approach, it is crucial to test the reliability and the limitations of the individual analysis techniques. In this Thesis we also assessed the impact of some factors that could affect both the X-ray and the strong lensing analyses.

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Donnarumma, Annamaria <1981&gt. « X-ray and lensing mass estimates in galaxy clusters ». Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2010. http://amsdottorato.unibo.it/2955/.

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GIANNI', SILVIA. « X-ray overview of INTEGRAL Blazars ». Doctoral thesis, Università degli Studi di Roma "Tor Vergata", 2010. http://hdl.handle.net/2108/1218.

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I quasars Radio Loud (RL) fanno parte di una piccola percentuale (~10%) di Nuclei Galattici Attivi (AGN) e sono caratterizzati da una forte emissione nella banda radio. Lo scopo del nostro lavoro e’ lo studio dell’emissione nella banda dell’X e dell’hard-X di una sotto-classe di questi oggetti: i Blazars. Gli oggetti di tipo Blazar sono AGN aventi un getto di particelle relativistiche (per lo piu’ elettroni e protoni) orientato a piccoli angoli rispetto alla linea di vista. Questa particolare classe di AGN include oggetti di tipo BL Lacerate (BL Lac) e Flat Spectrum Radio Quasar (FSRQ), che si differenziano per gli spettri ottici e per l’intensita’ della loro emissione: una sorgente BL Lac non presenta righe di emissione ottiche (EW < 5 Amstrong) e viene usualmente classificata come un blazar di bassa potenza (LBol~1046 – 1047 erg s-1), mentre una sorgente FSRQ mostra righe di emissione con significative larghezze equivalenti ed e’ classificata come un blazar di alta potenza (LBol~1048 erg s-1). In generale, lo spettro di un AGN in banda X e’ ben modellato da una legge di potenza con un flusso specifico (per unita’ di intervallo di energia) della forma N(E) ~ E-Gamma, dove E e’ l’energia in keV, N(E) e’ il numero di fotoni in unita’ di s-1 cm-2 keV-1 e Gamma e’ chiamato indice fotonico. Nonostante questa visione chiara e generale, lo spettro X di un Blazar puo’ mostrare alcune deviazioni dalla semplice legge di potenza sopra menzionata. Queste particolari caratteristiche spettrali si manifestano nel soft X con una curvatura dello spettro: un appiattimento (o flattening) e un irripidimento (o steepening) dello spettro. Inoltre, la presenza di componenti di riflessione Compton del continuo intrinseco – piu’ comunemente note come un picco (o Compton reflection hump) a 20-30 keV ed una riga di fluorescenza del ferro K-alpha – in oggetti RL e’ ancora una questione molto dibattuta. Ad oggi non e’ stata ancora trovata una chiara interpretazione fisica di queste caratteristiche spettrali. In questo lavoro riportiamo i risultati di uno studio a larga-banda (0.2-100 keV) dell’emissione nell’X di un campione selezionato di 11 Blazars osservati con INTEGRAL: 1ES 0033+595, 3C 273, 3C 279, 4C 04.42, BL Lac, IGR J22517+2218, PKS 0537-286, PKS 1830-211, PKS 2149-306, QSO B0836-710 e Swift J1656.3-3302. L’osservatorio spaziale INTEGRAL, grazie al largo campo di vista e alla alta risoluzione spettrale dei suoi strumenti, e’ ideale per studiare l’emissione di sorgenti X alle alte energie (oltre i 10 keV). Lo scopo di questo lavoro di Dottorato e’ l’analisi di un campione di Blazars selezionato nell’hard X ed avente dati disponibili provenienti dai satelliti INTEGRAL, Swift e XMM-Newton. Dopo aver eseguito la procedura standard per la riduzione dati nel soft X ci siamo occupati dell’analisi temporale e spettrale dell’intero campione di sorgenti. Riassumiamo di seguito i risultati scientifici ottenuti: • gli spettri a larga banda di tutte le sorgenti – eccetto due, le FSRQs 4C 04.42 e 3C 273 – sono ben riprodotti con un modello a legge di potenza assorbita da una quantita’ di gas in eccesso a quella galattica (NH~1020-23 cm-2). Questo risultato e’ una chiara evidenza del fatto che, utilizzando dati INTEGRAL alle alte energie, le sorgenti pesantemente assorbite possono essere piu’ facilmente rivelate. Inoltre, l’assorbimento sembra provenire da un materiale freddo intrinseco, confermando ed estendendo precedenti risultati presentati in letteratura. Il presente lavoro fornisce un’ulteriore conferma dell’esistenza di una correlazione tra l’NH ed il redshift; • per quanto concerne il continuo di emissione, l’analisi a larga banda del nostro campione di Blazars ha evidenziato la presenza di spettri piu’ hard (con indici fotonici dell’ordine di 1.4) rispetto a quelli di un campione piu’ ampio di oggetti RL analizzato da Page e collaboratori nel 2005 con dati di XMM-Newton. Tale differenza potrebbe risiedere nel fatto che effettivamente INTEGRAL seleziona sorgenti con valori dell’indice fotonico piu’ piatti, come mostrato anche da precedenti risultati; • nella nostra analisi abbiamo trovato due casi (4C 04.42 e 3C 273) di eccesso di conteggi nel soft X rispetto al modello di semplice legge di potenza (in altre parole uno steepening dello spettro), indicando la possibile presenza di un’emissione nel soft X; • non abbiamo trovato evidenza di componenti di riflessione (ne’ di Compton Reflection hump ne’ di una riga di emissione del ferro). La struttura della tesi e’ la seguente: Nei capitoli 1 e 2 riassumiamo le proprieta’ osservative comuni a tutte le sotto-classi di AGN enfatizzando in particolare la classe dei Blazars, diamo una descrizione generale della loro distribuzione spettrale in energia e discutiamo i loro meccanismi di emissione nella banda delle alte energie e le questioni ancora aperte sugli spettri degli oggetti RL. Nel capitolo 3 introduciamo la missione INTEGRAL e ne confrontiamo i rivelatori X a bordo con quelli di altri strumenti quali, BAT e XRT a bordo del satellite Swift e MOS1, MOS2, PN a bordo di XMM-Newton. Nel capitolo 4 riportiamo il metodo di riduzioni dei dati da noi adottato e l’analisi temporale e spettrale del campione selezionato di Blazars. Infine, nel capitolo 5 discutiamo i risultati ottenuti e diamo le nostre conclusioni.
Radio Loud (RL) quasars represent a small percentage (~10%) of all Active Galactic Nuclei (AGN) with a strong radio emission. We aimed to study the X-ray and hard X-ray emission from a subclass of these objects: the Blazars. The Blazar objects are AGNs with a jet of plasma (largely formed by electrons and protons) emitting at low angles with respect the line-ofsight. This class of AGN include BL Lacertae objects (BL Lac) and Flat- Spectrum Radio Quasars (FSRQ). The intrinsic differences between two types of sources are been found in their optical spectra and in the intensity of their emission: a BL Lac source does not show any optical emission lines (EW < 5°A) and this class of objects is essentially a low-power blazar (LBol~1046 − 1047 erg s−1), whereas a FSRQ source shows significant emission line equivalent widths and corresponding to a high-power blazar (LBol~1048 erg s−1). In general, the spectrum of an AGN in the X-rays band is usually well described by a power-law with a specific flux (i.e. per unit energy interval) of the form N(E) / E−Gamma, where E is the energy, N(E) is the number of photons in units of s−1 cm−2 keV−1 and Gamma is called the photon index. Despite this general view, X-ray spectra of the Blazars show some deviations from the simple power-law. These spectral signatures appear in the soft X-ray band with a curvature (a flattening or a steepening of the spectrum). In addition, the presence of Compton reflection components - most notably the Fe K-alpha emission line and the Compton reflection ”hump” peaked at about 20−30 keV - in RL objects is still debated. To date a clear physical interpretation of these features has not yet been found. We report in this work the results of a broad-band (0.2 − 100 keV) study of X- ray emission from a selected sample of 11 Blazars detected by INTEGRAL: 1ES 0033+595, 3C 273, 3C 279, 4C 04.42, BL Lac, IGR J22517+2218, PKS 0537-286, PKS 1830-211, PKS 2149-306, QSO B0836- 710 and Swift J1656.3-3302. The INTEGRAL observatory, because of the large field of view and high spectral resolution of its instruments, is ideal to study the high energy emission (above 10 keV). Present PhD work was aimed to the investigation of this hard X-rays selected sample, by taking advantage of the availability of the INTEGRAL, Swift and XMM-Newton data. After data reduction procedure, we performed a detailed temporal and spectral analysis for all sources in the sample. The scientific results can be summarized as follows: • the broad-band spectra of all selected sources - but two, the FSRQs 4C 04.42 and 3C 273 - are well reproduced with a power-law model absorbed by an amount of gas in excess to the Galactic one (NH ~ 1020 − 1023 cm−2). This result provides plain evidence to the fact that by using the INTEGRAL high-energies data the highly absorbed sources can be more easily detected. Moreover, the absorption seems to be a signature of a cold intrinsic absorber, confirming and extending previous results quoted in the literature. Present work provides a further confirmation of the existence of a NH-redshift trend; • with regard to continuum emission we found that the broad-band analysis of our sample of Blazars revealed a harder spectrum with a photonindex of the order of 1.4, with respect to the mean value of the spectral index obtained by Page et al. (2005) with XMM data of a statistically sizeable sample of RL objects. Such a difference could be due to the hard X-ray selection of our INTEGRAL sample that is clearly biased towards flatter values of the photon index as shown by previous results; • in our analysis we have find two case (4C 04.42 and 3C 273) of excess of soft X-ray counts with respect to the simple power-law model (in other words a steepening of the spectrum), indicating the possible presence of a soft X-ray emission; • we have not found any evidence of reflection components (Reflection ”hump” and iron emission line). The thesis structure is as follows: In Chapters 1 and 2 we summarize the observational properties common to all AGN subclasses emphasizing in particular the Blazar class, we give a general description of their spectral energy distribution and then we discuss their emission mechanisms in the high energy band and the open questions related to the spectra of the RL objects. In Chapter 3 we deal with the INTEGRAL mission overview and a comparison with some X-ray detectors such as, Swift/BAT, Swift/XRT and XMM-Newton. In Chapter 4 we report on the data reduction method and analysis of the Blazar selected sample. Finally, in Chapter 5 we discuss the results and give our conclusions.

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Oss, Valerio. « Telescopi ottici, radio, X : principi e differenze ». Bachelor's thesis, Alma Mater Studiorum - Università di Bologna, 2022. http://amslaurea.unibo.it/25282/.

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In questo elaborato si vuole descrivere il funzionamento generale di telescopi, in banda ottica, radio e X, con un approfondimento sui principi di funzionamento e sulle relative differenze. In generale si può definire un telescopio come uno strumento capace di raccogliere la radiazione elettromagnetica per concentrarla grazie a lenti, specchi o antenne paraboliche, in un’area ristretta, un punto focale in cui si trova un rivelatore, che può essere l’occhio umano, un CCD, un illuminatore ecc. Questi, grazie anche a software dedicati, elaborano la radiazione raccolta fornendo un’immagine della sorgente celeste.

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Santucci, Giulia. « Telescopi ottici, radio, X : principi e differenze ». Bachelor's thesis, Alma Mater Studiorum - Università di Bologna, 2014. http://amslaurea.unibo.it/7200/.

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Per telescopio intendiamo qualsiasi strumento finalizzato alla misura della radiazione proveniente dallo spazio. Tipicamente questo nome viene riservato agli strumenti ottici; tuttavia è utile utilizzare un singolo nome per caratterizzare tutta la classe di strumenti per le osservazioni astronomiche. Un telescopio è uno strumento capace di raccogliere radiazione da una grande superficie, concentrandola in un punto. La luce viene in genere raccolta da uno specchio o antenna, quindi elaborata da vari strumenti, come per esempio un filtro o uno spettrografo, e infine indirizzata ad un rivelatore, che può essere l'occhio umano, una lastra fotografica, un CCD, un rivelatore radio, una camera a scintille etc.

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Fioretti, Valentina <1982&gt. « Background minimization issues for next generation hard X-ray focusing telescopes ». Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2011. http://amsdottorato.unibo.it/3858/1/Fioretti_Valentina_Tesi.pdf.

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The hard X-ray band (10 - 100 keV) has been only observed so far by collimated and coded aperture mask instruments, with a sensitivity and an angular resolution lower than two orders of magnitude as respects the current X-ray focusing telescopes operating below 10 - 15 keV. The technological advance in X-ray mirrors and detection systems is now able to extend the X-ray focusing technique to the hard X-ray domain, filling the gap in terms of observational performances and providing a totally new deep view on some of the most energetic phenomena of the Universe. In order to reach a sensitivity of 1 muCrab in the 10 - 40 keV energy range, a great care in the background minimization is required, a common issue for all the hard X-ray focusing telescopes. In the present PhD thesis, a comprehensive analysis of the space radiation environment, the payload design and the resulting prompt X-ray background level is presented, with the aim of driving the feasibility study of the shielding system and assessing the scientific requirements of the future hard X-ray missions. A Geant4 based multi-mission background simulator, BoGEMMS, is developed to be applied to any high energy mission for which the shielding and instruments performances are required. It allows to interactively create a virtual model of the telescope and expose it to the space radiation environment, tracking the particles along their path and filtering the simulated background counts as a real observation in space. Its flexibility is exploited to evaluate the background spectra of the Simbol-X and NHXM mission, as well as the soft proton scattering by the X-ray optics and the selection of the best shielding configuration. Altough the Simbol-X and NHXM missions are the case studies of the background analysis, the obtained results can be generalized to any future hard X-ray telescope. For this reason, a simplified, ideal payload model is also used to select the major sources of background in LEO. All the results are original contributions to the assessment studies of the cited missions, as part of the background groups activities.

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Livres sur le sujet "Astronomia X"

Riccardo, Giacconi, dir. The x-ray universe. Cambridge, Mass : Harvard University Press, 1985.

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1951-, Mason K. O., Watson M. G. 1952- et White N. E. 1952-, dir. The Physics of accretion onto compact objects : Proceedings of a workshop held in Tenerife, Spain, April 21-25, 1986. Berlin : Springer-Verlag, 1986.

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Center, Goddard Space Flight, et Smithsonian Astrophysical Observatory, dir. Constellation X-Ray Observatory : Unlocking the mysteries of black holes, dark matter, dark energy, and life cycles of matter in the universe. [Greenbelt, Md.] : National Aeronautics and Space Administration, Goddard Space Flight Center, 2004.

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Center, Goddard Space Flight, et Smithsonian Astrophysical Observatory, dir. Constellation X-Ray Observatory : Unlocking the mysteries of black holes, dark matter, dark energy, and life cycles of matter in the universe. [Greenbelt, Md.] : National Aeronautics and Space Administration, Goddard Space Flight Center, 2004.

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Paul, Gorenstein, Hoover Richard B et Society of Photo-optical Instrumentation Engineers., dir. X-ray optics for astronomy : Telescopes, multilayers, spectrometers, and missions : 30 July 2001, San Diego, USA. Bellingham, Wash., USA : SPIE, 2002.

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Silvano, Fineschi, Society of Photo-optical Instrumentation Engineers. et International Commission for Optics, dir. Polarimetry in astronomy : 25-28 August 2002, Waikoloa, Hawaii, USA. Bellingham, Wash : SPIE, 2003.

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W, Siegmund Oswald H., Gummin Mark A et Society of Photo-optical Instrumentation Engineers., dir. EUV, x-ray, and gamma-ray instrumentation for astronomy VIII : 30 July-1 August 1997, San Diego, California. Bellingham, Wash., USA : SPIE, 1997.

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United States. National Aeronautics and Space Administration., dir. EGRET sources at intermediate galactic latitude. [Washington, DC : National Aeronautics and Space Administration, 1996.

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United States. National Aeronautics and Space Administration., dir. EGRET sources at intermediate galactic latitude. [Washington, DC : National Aeronautics and Space Administration, 1996.

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Charles, Philip A. Exploring the X-ray universe. Cambridge : Cambridge University Press, 1995.

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Chapitres de livres sur le sujet "Astronomia X"

Seward, Frederick D. « X-Ray Astronomy ». Dans Allen’s Astrophysical Quantities, 183–206. New York, NY : Springer New York, 2002. http://dx.doi.org/10.1007/978-1-4612-1186-0_9.

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Beckman, John Etienne. « X-Ray Astronomy ». Dans Astronomers' Universe, 145–75. Cham : Springer International Publishing, 2021. http://dx.doi.org/10.1007/978-3-030-68372-6_5.

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Grupen, Claus. « X-ray Astronomy ». Dans essentials, 17–20. Wiesbaden : Springer Fachmedien Wiesbaden, 2021. http://dx.doi.org/10.1007/978-3-658-32547-3_3.

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Kitchin, Chris. « X ». Dans Illustrated Dictionary of Practical Astronomy, 254. London : Springer London, 2002. http://dx.doi.org/10.1007/978-1-4471-0175-8_24.

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Pottschmidt, Katja, et Michael König. « Analyzing X-Ray Variability of Cygnus X-1 ». Dans Astronomical Time Series, 187–90. Dordrecht : Springer Netherlands, 1997. http://dx.doi.org/10.1007/978-94-015-8941-3_20.

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Poggiani, Rosa. « Ultraviolet and X-Ray Astronomy ». Dans UNITEXT for Physics, 81–89. Cham : Springer International Publishing, 2016. http://dx.doi.org/10.1007/978-3-319-44729-2_11.

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Makino, F. « X-Ray Astronomy Satellite Ginga ». Dans Observatories in Earth Orbit and Beyond, 41–48. Dordrecht : Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-011-3454-5_7.

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Porter, F. S., G. V. Brown et J. Cottam. « X-Ray Astronomy and Astrophysics ». Dans Topics in Applied Physics, 359–416. Berlin, Heidelberg : Springer Berlin Heidelberg, 2005. http://dx.doi.org/10.1007/10933596_8.

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Mertz, Lawrence. « X-ray Telescopes ». Dans Excursions in Astronomical Optics, 25–45. New York, NY : Springer New York, 1996. http://dx.doi.org/10.1007/978-1-4612-2386-3_2.

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Hjellming, R. M. « Radio-X-Ray Connection for X-Ray Transients and Binaries ». Dans Highlights of Astronomy, 767–70. Dordrecht : Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-011-4778-1_51.

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Actes de conférences sur le sujet "Astronomia X"

Da Costa, Luiz A. Nicolaci, Angelo Fausti Neto, Marcio A. G. Maia, Ricardo L. C. Ogando et Riccardo Campisano. « Laboratório Interinstitucional de e-Astronomia : passado, presente, e futuro ». Dans X Brazilian e-Science Workshop. Sociedade Brasileira de Computação - SBC, 2020. http://dx.doi.org/10.5753/bresci.2016.9127.

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Descrevemos como o LIneA foi criado, e o que produziu em termos de software e hardware nos últimos 10 anos de trabalho no Dark Energy Survey e em preparação para vários outros levantamentos, tal como o LSST, quando um centro de e-ciência no Brasil será necessário para atender seu grande volume, velocidade, e variabilidade de dados. Paralelismo, proveniência, e visualização são alguns dos desafios encarados pelo LIneA a fim de gerar produtos e alcançar os resultados científicos.

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Massadar, Hanna Beatriz Melo. « Olimpíadas científicas e atividades didáticas como proposta para divulgação da Astronomia ». Dans X SEMACIT, Anais da IX Jornada Científica e II Jornada de Extensão do IFRJ campus Duque de Caxias. Recife, Brasil : Even3, 2020. http://dx.doi.org/10.29327/126933.1-1.

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Hudec, R. « Digitized astronomical plates : Optical data for X-ray astronomy ». Dans X-RAY ASTRONOMY : Stellar Endpoints,AGN, and the Diffuse X-ray Background. AIP, 2001. http://dx.doi.org/10.1063/1.1434708.

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Golub, Leon. « Soft-x-ray astronomy : results and future missions ». Dans OSA Annual Meeting. Washington, D.C. : Optica Publishing Group, 1990. http://dx.doi.org/10.1364/oam.1990.tumm2.

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Softx-ray astronomy began with detection of x-rays from the sun in the late 1940s and continues to have strong ties to study of the solar emission. Because it is intrinsically interesting and is the strongest x-ray source, studies of the sun remain the testing ground for new techniques and the development of new instrumentation, such as multilayer coatings for near-normal incidence imaging and high resolution electronic array detectors. The continued development of grazing incidence techniques and associated instrumental recording devices, combined with improvements in sensitivity and resolution, have allowed x-ray astronomy to detect and study a large variety of "normal" astronomical features in addition to the rare and unusual objects which were first detected. Current missions in the soft x-ray and XUV are carrying out extensive mainstream studies in all areas of astronomy, and future missions call for studies directed at the most fundamental cosmological questions.

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Holt, Stephen S. « Telescope systems for x-ray astronomy ». Dans OSA Annual Meeting. Washington, D.C. : Optica Publishing Group, 1987. http://dx.doi.org/10.1364/oam.1987.wp2.

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Because of the opacity of the atmosphere, x-ray astronomy must be conducted from space. Twenty-five years ago, the first detections of nonsolar x rays were made with simple proportional counters from sounding rockets. Collimated counters aboard rockets and satellites were used to follow up these discoveries, and more recently true x-ray telescopes have been used for the study of x rays from the cosmos. There are now thousands of cataloged x-ray sources ranging from nearby stars to distant quasars. The primary advantages afforded by telescopes for x-ray astronomy are twofold: direct imagery allows finer angular resolution than otherwise possible, and it also betters the sensitivity of the x-ray detectors via the minimization of nonsource background. The primary disadvantages are associated with the necessary grazing-incidence geometry: the effective focal length is limited by the actual telescope length, and the short-wavelength response is, therefore, sharply limited by the shallowness of the grazing angle. Examples are presented of important astronomical results that have been obtained from x-ray telescopes in space. Also presented are conceptual designs (and prototypical test results) from three different types of next-generation telescope for x-ray astronomy.

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Aschenbach, Bernd. « X-Ray scattering from grazing incidence telescopes ». Dans Surface Roughness and Scattering. Washington, D.C. : Optica Publishing Group, 1992. http://dx.doi.org/10.1364/surs.1992.smb1.

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For almost 30 years grazing incidence telescopes for astronomical observations have been developed and matured to low scattering performance. A culmination point was reached with the launch of the X-ray astronomy satellite ROSAT, which is in operation since 2 years. ROSAT carries two grazing incidence telescopes covering the XUV (~50 - 750Å) and the soft X-ray (~5 - 120Å) spectral regions, separately. The Wolter type I X-ray telescope consists of 4 nested mirror pairs with a maximum aperture of 835mm and 2.4m focal length, characterized by a half energy width of <4 arcsec and extremely low scattering wings due to the superb mirror surface microroughness of <2.8Å. The point spread function, which has been measured on ground in a 130m long beam test facility prior to launch, will be compared with the performance obtained in orbit. Future grazing incidence X-ray telescopes aim at improved angular resolution, larger collecting area and broader spectral coverage. This is pursued in various projects including SAX, BBXRT, ASTRO-D, Spectrum-X, SOHO-CDS, AXAF and XMM, requiring new fabrication techniques and metrology.

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Zhang, Yuheng, Mingzhi Wei, Qian Song et Quan Sun. « The Signal Processing ASIC for astronomical CCD controller ». Dans X-Ray, Optical, and Infrared Detectors for Astronomy X, sous la direction de Andrew D. Holland et James Beletic. SPIE, 2022. http://dx.doi.org/10.1117/12.2627230.

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Zhu, Jie, Hong-Fei Zhang, Yihao Zhang, Yujing Tang, Zeyu Zhu, Jun Zhang, Feng Zeng, Hao Liu, Jian Wang et Jian Ge. « Design of a scientific CMOS camera for astronomical observation ». Dans X-Ray, Optical, and Infrared Detectors for Astronomy X, sous la direction de Andrew D. Holland et James Beletic. SPIE, 2022. http://dx.doi.org/10.1117/12.2629345.

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HOLT, STEPHEN S. « X-RAY ASTRONOMICAL SPECTROSCOPY ». Dans A Festschrift in Honor of Ricardo Giacconi. WORLD SCIENTIFIC, 2000. http://dx.doi.org/10.1142/9789812792174_0006.

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Collura, Alfonso, Marco Barbera, Giuseppe Inzerillo, Filippo Mirabello, Salvatore Sciortino et Salvatore Serio. « X-ray Astronomy Calibration and Testing Facility (XACT) at Osservatorio Astronomico di Palermo G.S. Vaiana ». Dans SPIE's 1994 International Symposium on Optics, Imaging, and Instrumentation, sous la direction de Oswald H. W. Siegmund et John V. Vallerga. SPIE, 1994. http://dx.doi.org/10.1117/12.186814.

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Rapports d'organisations sur le sujet "Astronomia X"

Saz Parkinson, P. X-ray Astronomy at SLAC. Office of Scientific and Technical Information (OSTI), avril 2005. http://dx.doi.org/10.2172/839834.

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Mizuno, T. Beam Test of a Prototype Detector Array for the PoGO Astronomical Hard X-Ray/ Soft Gamma-Ray Polarimeter. Office of Scientific and Technical Information (OSTI), novembre 2004. http://dx.doi.org/10.2172/839629.

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