变形词
发表于 2025-3-23 13:23:03
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Preserve
发表于 2025-3-23 14:23:19
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Engaging
发表于 2025-3-23 18:32:24
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从容
发表于 2025-3-23 22:29:46
Book 2016ues, which are critical to advances in many areas of astronomy. As reflected in the book, these techniques can be divided into direct methods, interferometry, and reconstruction methods, and can be applied to a huge variety of astrophysical systems, ranging from planets, single stars and binaries to
Feedback
发表于 2025-3-24 03:52:23
Lucky Imaging in Astronomy,y Imaging is a passive observing technique with individual integration times comparable to the atmospheric coherence time. Thanks to the advent of essentially noise free “Electron multiplying CCD” detectors, Lucky Imaging saw a renewed interest in the past decade. It is now routinely used at a numbe
thalamus
发表于 2025-3-24 08:24:02
Adaptive Optics in High-Contrast Imaging,ging is a very rich and complementary method that can reveal the orbital motion of the planet, the spectrophotometry of its atmosphere but also the architecture and properties of its circumstellar environment. It can unveil possible interactions with a disc, whether a proto-planetary disc in case of
AORTA
发表于 2025-3-24 13:39:39
Aperture Masking Imaging,ux, zero read-noise regime and offering superior calibration in the bright regime. Since adaptive optics has become commonplace on large telescopes, the key advantage of aperture-mask interferometry is in calibration, particularly of low spatial-frequency phase aberrations that cause quasi-static sp
摘要记录
发表于 2025-3-24 15:57:31
Optical Long Baseline Interferometry,les (interferometric phase and contrast) and the image of the source is a Fourier transform expressed first by van Cittert and Zernike. Depending on the source size and the amount of information collected, the analysis of these Fourier components allows a measurement of the typical source size, a pa
Ostrich
发表于 2025-3-24 20:04:25
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平躺
发表于 2025-3-25 00:33:09
Velocity Fields in Stellar Atmospheres Probed by Tomography,ing at given, pre-specified ranges of optical depths. Different masks thus probe different line-formation depths in the stellar atmosphere. The masks are cross-correlated with the observed spectrum to yield cross-correlation functions (CCFs). The cross-correlation has two advantages: (i) to overcome