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Artykuły w czasopismach na temat "Coronographe de Lyot"
Smartt, Raymond N., Serge Koutchmy i Jacques-Clair NoëNs. "Near-IR Solar Coronal Observations with New-Technology Reflecting Coronographs". Symposium - International Astronomical Union 154 (1994): 603–8. http://dx.doi.org/10.1017/s0074180900124908.
Pełny tekst źródłaDavoust, Emmanuel. "Le coronographe de Bernard Lyot au Pic du Midi". BibNum, 1.08.2009. http://dx.doi.org/10.4000/bibnum.699.
Pełny tekst źródłaRozprawy doktorskie na temat "Coronographe de Lyot"
Alagao, Mary Angelie. "Characterization and optimization of the Evanescent Wave Coronagraph". Electronic Thesis or Diss., Saint-Etienne, 2023. http://www.theses.fr/2023STET0060.
Pełny tekst źródłaDirect imaging of exoplanets remains challenging due to the high contrast and the small angular separation between the star and the planet. It requires suppressing the blinding glare from the star and ensuring that the planet's faint light is not buried deep in various noises. Successful detection depends on the technological readiness and maturity of techniques and algorithms employed while considering the significant trade-offs on raw contrast, inner working angle, and throughput. One of its key components is the use of coronagraphs – instruments with the sole purpose of blocking/reducing the light from the star. This work presents a new type of Lyot coronagraph, invented by Dr. Yves Rabbia, that relies on the frustrated total internal reflection (FTIR) principle to suppress the starlight. This coronagraph is aptly called the Evanescent Wave Coronagraph (EvWaCo) owing to its nature that its focal plane mask, comprising a lens and a prism, reflects the off-axis source (planet) and transmits the on-axis source (star) by capturing the evanescent waves. This thesis aims to provide the reader with the groundwork that highlights EvWaCo's three main advantages: i) the mask is inherently achromatic, ii) the size of the mask is adjustable by changing the pressure between the lens and the prism, and iii) both the stellar light and the planet light can be collected simultaneously for low-order wavefront sensing, and proper stellar light centering. The performance of EvWaCo is assessed through experiments in a laboratory and then compared to numerical simulations. The experimental results show a raw contrast equal to a few 10-4 at 3 ��/�� over the full I-band (��c = 800 nm, ∆��/�� ≈ 20%) and at 4 ��/�� over the full R-band (��c = 650 nm, ∆��/�� ≈ 23%). The simulations confirm the achromatic rejection capability of EvWaCo as it showed a raw contrast of 10-4 at the same radial distance over both bandpasses. This thesis concludes with the status of its testbed and future perspectives
Venet, Melanie. "Coronographes spatiaux : Solar Orbiter / Metis, Smese / Lyot, Proba-3 / Aspiics". Thesis, Aix-Marseille 1, 2011. http://www.theses.fr/2011AIX10011.
Pełny tekst źródłaThe solar corona is the part of the Sun's atmosphere that extends from the photosphere (solar surface where the photons are emitted) into the interplanetary medium. Its understanding is a major issue because it is the source of phenomena that can disrupt telecommunications, living beings and even climate. The most appropriate tool to observe it is the coronagraph, an optical system obscuring the solar disk in favor of the corona, a million times fainter. My thesis deals with its review, particularly through the spaceprojects :- Solar Orbiter, which will approach the Sun at 0.2 astronomical unit (distance between Earth and Sun), allowing a very high spatial resolution ;- SMESE, in cooperation with China, which should study the corona in the Lymanalpha (and far infrared) ;- and ASPIICS, which will observe the corona in conditions close to a natural solar eclipse, with its occulting disk located at 150 m from the imaging instrument.The first point tackled is the rejection of instrumental stray light, whose optimization is one of the major problems in coronagraphy. The second concerns the methods of observation and imaging in white light, monochromatic imaging, and interferometry, in particular the Fabry Perot. The development and improvement of these techniques will allow considerable progress in terms of resolution and access to the corona ever closer to the Sun's surface, the location yet little known where the solar activity originates
Streszczenia konferencji na temat "Coronographe de Lyot"
Maadadi, S., S. Djabi, M. Rahmani, N. Mebarki i J. Mimouni. "Simulation of the Lyot Coronograph". W THE THIRD ALGERIAN WORKSHOP ON ASTRONOMY AND ASTROPHYSICS. AIP, 2010. http://dx.doi.org/10.1063/1.3518341.
Pełny tekst źródłaWatson, Steven M., i James P. Mills. "Incorporating coronographs with segmented telescopic systems for extrasolar planetary imaging". W OSA Annual Meeting. Washington, D.C.: Optica Publishing Group, 1989. http://dx.doi.org/10.1364/oam.1989.wv2.
Pełny tekst źródłaBabin, A. N., i A. N. Koval. "LARGE LYOT-CORONOGRAPH OF NIKOLSKY-SAZANOV DESIGN AT THE CRIMEAN ASTROPHYSICAL OBSERVATORY". W All-Russia Conference on Solar and Solar-Terrestrial Physics. The Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo, 2019. http://dx.doi.org/10.31725/0552-5829-2019-27-30.
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