標(biāo)題: Titlebook: Astronomy at High Angular Resolution; A Compendium of Tech Henri M. J. Boffin,Gaitee Hussain,Linda Schmidtobr Book 2016 Springer Internatio [打印本頁(yè)] 作者: 離開(kāi)浮于空中 時(shí)間: 2025-3-21 16:42
書(shū)目名稱Astronomy at High Angular Resolution影響因子(影響力)
書(shū)目名稱Astronomy at High Angular Resolution影響因子(影響力)學(xué)科排名
書(shū)目名稱Astronomy at High Angular Resolution網(wǎng)絡(luò)公開(kāi)度
書(shū)目名稱Astronomy at High Angular Resolution網(wǎng)絡(luò)公開(kāi)度學(xué)科排名
書(shū)目名稱Astronomy at High Angular Resolution被引頻次
書(shū)目名稱Astronomy at High Angular Resolution被引頻次學(xué)科排名
書(shū)目名稱Astronomy at High Angular Resolution年度引用
書(shū)目名稱Astronomy at High Angular Resolution年度引用學(xué)科排名
書(shū)目名稱Astronomy at High Angular Resolution讀者反饋
書(shū)目名稱Astronomy at High Angular Resolution讀者反饋學(xué)科排名
作者: 無(wú)辜 時(shí)間: 2025-3-21 21:57
0067-0057 next generation of astronomers on how to apply high-resolut.This book offers an essential compendium of astronomical high-resolution techniques. Recent years have seen considerable developments in such techniques, which are critical to advances in many areas of astronomy. As reflected in the book, 作者: 棲息地 時(shí)間: 2025-3-22 02:58 作者: 興奮過(guò)度 時(shí)間: 2025-3-22 06:41 作者: 華而不實(shí) 時(shí)間: 2025-3-22 12:48
https://doi.org/10.1007/BFb0051051pping of the disc flickering sources. This chapter reviews the principles of the method, discusses its performance, limitations, useful error propagation procedures, as well as highlights a selection of applications aimed at showing the possible scientific problems that have been and may be addresses with it.作者: 債務(wù) 時(shí)間: 2025-3-22 13:49
Aperture Masking Imaging, performance. Finally, I will demonstrate the applicability of aperture-masking imaging both to laser-guide star imaging of faint (K??～?14) star systems and bright transition disc stars (e.g. LkCa?15) surrounded by faint (1000:1 dynamic range) structures.作者: Transfusion 時(shí)間: 2025-3-22 18:08 作者: Living-Will 時(shí)間: 2025-3-22 21:48
Eclipse Mapping: Astrotomography of Accretion Discs,pping of the disc flickering sources. This chapter reviews the principles of the method, discusses its performance, limitations, useful error propagation procedures, as well as highlights a selection of applications aimed at showing the possible scientific problems that have been and may be addresses with it.作者: UNT 時(shí)間: 2025-3-23 04:18 作者: 痛苦一生 時(shí)間: 2025-3-23 08:21 作者: 變形詞 時(shí)間: 2025-3-23 13:23 作者: Preserve 時(shí)間: 2025-3-23 14:23 作者: Engaging 時(shí)間: 2025-3-23 18:32 作者: 從容 時(shí)間: 2025-3-23 22:29
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作者: Feedback 時(shí)間: 2025-3-24 03:52
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作者: thalamus 時(shí)間: 2025-3-24 08:24
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作者: AORTA 時(shí)間: 2025-3-24 13:39
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作者: 摘要記錄 時(shí)間: 2025-3-24 15:57
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作者: Ostrich 時(shí)間: 2025-3-24 20:04 作者: 平躺 時(shí)間: 2025-3-25 00:33
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作者: excrete 時(shí)間: 2025-3-25 06:26 作者: Enliven 時(shí)間: 2025-3-25 11:19 作者: ENACT 時(shí)間: 2025-3-25 15:40 作者: insurgent 時(shí)間: 2025-3-25 18:11
Tomographic Imaging of Stellar Surfaces and Interacting Binary Systems,ps allow us to study surface activity, spot and magnetic field variability and map irradiation patterns on secondaries of cataclysmic variable systems (CVs). During the past few years, magnetic fields have been detected and studied on stars throughout the Hertzsprung-Russell diagram. Spectropolarime作者: Omniscient 時(shí)間: 2025-3-25 23:23 作者: Exuberance 時(shí)間: 2025-3-26 00:08
Astronomy at High Angular Resolution978-3-319-39739-9Series ISSN 0067-0057 Series E-ISSN 2214-7985 作者: Aggrandize 時(shí)間: 2025-3-26 08:13 作者: 合群 時(shí)間: 2025-3-26 11:44
H.-J. Cantow,G. Dall’Asta,H. A. Stuarty 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作者: Communal 時(shí)間: 2025-3-26 14:55 作者: intelligible 時(shí)間: 2025-3-26 19:40
H.-G. Elias,R. Bareiss,J. G. Wattersonux, 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作者: Silent-Ischemia 時(shí)間: 2025-3-26 21:18 作者: thrombosis 時(shí)間: 2025-3-27 02:27 作者: 評(píng)論性 時(shí)間: 2025-3-27 08:00
Fortschritte der Hochpolymeren Forschunging 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作者: LEVY 時(shí)間: 2025-3-27 11:12 作者: 小官 時(shí)間: 2025-3-27 14:34
J. Hermans Jr.,D. Lohr,D. Ferrotaclysmic Variables (mCVs)(Potter et?al., MNRAS 297:1261, 1998). I discuss polarisation modelling followed by a summary of the Stokes imaging technique and its application to a real data set. In the final sections I discuss two ongoing developments to Stokes imaging, namely: using a more realistic “作者: Intend 時(shí)間: 2025-3-27 21:19
Fortschritte der Hochpolymeren-Forschungse objects containing complex accretion flows. Limitations of the method will be covered along with how they can be circumvented in some circumstances. We will also present examples of real applications to illustrate the chief areas that Doppler Tomography has had most impact upon.作者: 尾巴 時(shí)間: 2025-3-27 22:56
H.-J. Cantow,G. Dall’Asta,H. A. Stuartps allow us to study surface activity, spot and magnetic field variability and map irradiation patterns on secondaries of cataclysmic variable systems (CVs). During the past few years, magnetic fields have been detected and studied on stars throughout the Hertzsprung-Russell diagram. Spectropolarime作者: 寡頭政治 時(shí)間: 2025-3-28 04:47 作者: 讓步 時(shí)間: 2025-3-28 09:09
Doppler Tomography,se objects containing complex accretion flows. Limitations of the method will be covered along with how they can be circumvented in some circumstances. We will also present examples of real applications to illustrate the chief areas that Doppler Tomography has had most impact upon.作者: orthodox 時(shí)間: 2025-3-28 13:37 作者: 不公開(kāi) 時(shí)間: 2025-3-28 17:09 作者: obsession 時(shí)間: 2025-3-28 21:47
https://doi.org/10.1007/BFb0051606Optical interferometry is now routinely used to image stars and their environments with sub-milliarcsecond resolution. We present here a brief review of model-independent interferometric imaging, discussing the most recent advances in regularisation, optimisation algorithms, and imaging procedures with minimal formalism.作者: Rodent 時(shí)間: 2025-3-29 00:34 作者: 感情脆弱 時(shí)間: 2025-3-29 05:54
Image Reconstruction in Optical Interferometry: An Up-to-Date Overview,Optical interferometry is now routinely used to image stars and their environments with sub-milliarcsecond resolution. We present here a brief review of model-independent interferometric imaging, discussing the most recent advances in regularisation, optimisation algorithms, and imaging procedures with minimal formalism.作者: ACME 時(shí)間: 2025-3-29 10:44 作者: Blemish 時(shí)間: 2025-3-29 14:09 作者: Osmosis 時(shí)間: 2025-3-29 19:04 作者: 佛刊 時(shí)間: 2025-3-29 20:29 作者: 傳染 時(shí)間: 2025-3-30 02:45 作者: pessimism 時(shí)間: 2025-3-30 06:57
Fortschritte der Hochpolymeren Forschunge powerful AGN potentially showing more compact dust structures. Arguably the most exciting discovery was the fact that the bulk of the mid-IR emission in Seyfert galaxies emerges from the polar region of the AGN, which is difficult to reconcile with classical torus models. An alternative model is c作者: 否決 時(shí)間: 2025-3-30 08:32
