969 resultados para Läs*
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A continuació s’indiquen algunes orientacions dirigides a facilitar la comprensió i l’ús d’aquesta guia, tant per als estudiants com per als docents. La guia consta de set capítols: capítol 1, “Fitxes de pràctiques” composta per 12 pràctiques; capítol 2, “Estudi de casos pràctics” compost per 13 casos; capítol 3, “Estils de referència”; capítol 4, “Dinàmica de grups”; capítol 5, “Sistema d’avaluació”; capítol 6, “Bibliografia general” i un capítol 7 d’annexos.
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Quan parlem de les TIC estem fent referència a un concepte relativament modern sobre les tecnologies de la informació i la comunicació, com per exemple l’ús de l’ordinador, Internet, la càmera digital, els mòbils de tercera generació, l’ús de la pissarra digital i un llarg etcètera. En les últimes dècades s’ha produït un increment molt gran de l’ús de les TIC en quasi tot el món. Espanya no s’ha quedat al marge i a través de diferents estudis publicats es constata que les noves tecnologies ja formen part de la vida quotidiana de les famílies espanyoles. Com que la família és el primer agent de socialització del xiquet o xiqueta, factors com l’actitud de la família vers l’ús de les TIC i els recursos socioeconòmics de la família, influenciaran el desenvolupament evolutiu del xiquet o xiqueta. Al llarg d’aquesta pràctica, l’alumnat reflexionarà sobre els avantatges i desavantatges de l’ús de les TIC en xiquets i adolescents a través del capítol de Carl Honoré (2009), i duran a terme una anàlisi sobre els hàbits dels xiquets d’educació infantil sobre l’ús de les TIC i de l’actitud dels pares i les mares vers aquestes. Per a fer aquesta anàlisi hauran de fer unes enquestes a les famílies amb aquesta finalitat.
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Only a few binary systems with compact objects display TeV emission. The physical properties of the companion stars represent basic input for understanding the physical mechanisms behind the particle acceleration, emission, and absorption processes in these so-called gamma-ray binaries. Here we present high-resolution and high signal-to-noise optical spectra of LS 2883, the Be star forming a gamma-ray binary with the young non-accreting pulsar PSR B1259-63, showing it to rotate faster and be significantly earlier and more luminous than previously thought. Analysis of the interstellar lines suggests that the system is located at the same distance as (and thus is likely a member of) Cen OB1. Taking the distance to the association, d = 2.3 kpc, and a color excess of E(B – V) = 0.85 for LS 2883 results in MV ≈ –4.4. Because of fast rotation, LS 2883 is oblate (R eq sime 9.7 R ☉ and R pole sime 8.1 R ☉) and presents a temperature gradient (T eq≈ 27,500 K, log g eq = 3.7; T pole≈ 34,000 K, log g pole = 4.1). If the star did not rotate, it would have parameters corresponding to a late O-type star. We estimate its luminosity at log(L */L ☉) sime 4.79 and its mass at M * ≈ 30 M ☉. The mass function then implies an inclination of the binary system i orb ≈ 23°, slightly smaller than previous estimates. We discuss the implications of these new astrophysical parameters of LS 2883 for the production of high-energy and very high-energy gamma rays in the PSR B1259-63/LS 2883 gamma-ray binary system. In particular, the stellar properties are very important for prediction of the line-like bulk Comptonization component from the unshocked ultrarelativistic pulsar wind.
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Context. It appears that most (if not all) massive stars are born in multiple systems. At the same time, the most massive binaries are hard to find owing to their low numbers throughout the Galaxy and the implied large distances and extinctions. Aims. We want to study LS III +46 11, identified in this paper as a very massive binary; another nearby massive system, LS III +46 12; and the surrounding stellar cluster, Berkeley 90. Methods. Most of the data used in this paper are multi-epoch high S/N optical spectra, although we also use Lucky Imaging and archival photometry. The spectra are reduced with dedicated pipelines and processed with our own software, such as a spectroscopic-orbit code, CHORIZOS, and MGB. Results. LS III +46 11 is identified as a new very early O-type spectroscopic binary [O3.5 If* + O3.5 If*] and LS III +46 12 as another early O-type system [O4.5 V((f))]. We measure a 97.2-day period for LS III +46 11 and derive minimum masses of 38.80 ± 0.83 M⊙ and 35.60 ± 0.77 M⊙ for its two stars. We measure the extinction to both stars, estimate the distance, search for optical companions, and study the surrounding cluster. In doing so, a variable extinction is found as well as discrepant results for the distance. We discuss possible explanations and suggest that LS III +46 12 may be a hidden binary system where the companion is currently undetected.
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Questions and answers on the topic of Imamat for students of Shia Imami Ismaili schools.
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"HRDI-04/08-05(1M)E"--P. [4] of cover.
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Mode of access: Internet.
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18 have imprint: Budán.
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Mode of access: Internet.
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Available on demand as hard copy or computer file from Cornell University Library.
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Mode of access: Internet.
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Extrait du tome VI des Memoires de la Société des antiquaires de la Morinie.
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"5 June 1961."
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"August 1955."
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"20 July 1961."