標(biāo)題: Titlebook: Coronal Magnetometry; Steven Tomczyk,Jie Zhang,Timothy Bastian Book 2014 Springer Science+Business Media New York 2014 Embedded Systems.Ha [打印本頁(yè)] 作者: firearm 時(shí)間: 2025-3-21 16:05
書目名稱Coronal Magnetometry影響因子(影響力)
書目名稱Coronal Magnetometry影響因子(影響力)學(xué)科排名
書目名稱Coronal Magnetometry網(wǎng)絡(luò)公開度
書目名稱Coronal Magnetometry網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Coronal Magnetometry被引頻次
書目名稱Coronal Magnetometry被引頻次學(xué)科排名
書目名稱Coronal Magnetometry年度引用
書目名稱Coronal Magnetometry年度引用學(xué)科排名
書目名稱Coronal Magnetometry讀者反饋
書目名稱Coronal Magnetometry讀者反饋學(xué)科排名
作者: Largess 時(shí)間: 2025-3-21 21:23
978-1-4939-4983-0Springer Science+Business Media New York 2014作者: adduction 時(shí)間: 2025-3-22 01:14
Transactional Aspects of Workflows, in both the global magnetic-field evolution over a solar cycle, and the local storage of magnetic free energy within coronal plasmas. We address commonly held skepticisms concerning angular ambiguities and line-of-sight confusion. We argue that ambiguities are, in principle, no worse than more fami作者: Ornament 時(shí)間: 2025-3-22 06:35
Micronutrients and Other Trace Elements,r atmosphere has been an important task over the past decades. This task has been made complicated by the difficulties to measure the magnetic field in the corona, while it is currently known with a good accuracy in the photosphere and/or chromosphere. Thus, to determine the coronal magnetic field, 作者: 漫不經(jīng)心 時(shí)間: 2025-3-22 11:27 作者: 比賽用背帶 時(shí)間: 2025-3-22 14:15 作者: 比賽用背帶 時(shí)間: 2025-3-22 19:36 作者: septicemia 時(shí)間: 2025-3-23 00:17
Pseudospectral and Galerkin Methodsty to probe the plasma parameters of the solar atmosphere. Here, high-cadence observations of two “EIT wave” events taken using the . (AIA) instrument onboard the . (SDO) are combined with spectroscopic measurements from the . (EIS) onboard the . spacecraft and used to examine the variability of the作者: Trigger-Point 時(shí)間: 2025-3-23 03:18
Mathematics and Its Applications. onboard the .. Three minutes after the start of a C2.0 flare, wave trains were first observed along an open divergent loop system in 171?? observations at a distance of 150 Mm from the footpoint of the guiding loop system and with a speed of 689?km?s., then they appeared in 193?? observations afte作者: helper-T-cells 時(shí)間: 2025-3-23 06:00
International Regulatory Environment, cavities are elliptical regions of rarefied density lying above and around prominences. They can be long-lived (weeks to months) but are often observed to eventually erupt as part of a coronal mass ejection (CME). We determine morphological properties of the cavities both by qualitatively assessing作者: formula 時(shí)間: 2025-3-23 11:25
Hyperasymptotic Perturbation Theoryn lines contain information about the magnetic field, and to access this information either a forward or an inversion method must be used. We study three coronal magnetic configurations that are applicable to polar-crown filament cavities by doing forward calculations to produce synthetic polarizati作者: Chivalrous 時(shí)間: 2025-3-23 17:36
J. Litva,A. Sandhu,K. Cho,T. Lo, CoMP observations provide high-cadence image sequences of the coronal line intensity, Doppler shift, and line width simultaneously over a large field of view. By studying the Doppler shift and line width we may explore more of the physical processes of the initiation and propagation of coronal mas作者: NOTCH 時(shí)間: 2025-3-23 19:26 作者: CANT 時(shí)間: 2025-3-23 22:45 作者: 先鋒派 時(shí)間: 2025-3-24 06:21
Vincent E. Rubatzky,Mas Yamaguchiegion were taken into account. The north–south asymmetry of the magnetic fluxes was considered as well as the imbalance between positive and negative fluxes. The north–south asymmetry displays a regular alternation of the dominant hemisphere during the solar cycle: the northern hemisphere dominated 作者: packet 時(shí)間: 2025-3-24 08:07 作者: Allodynia 時(shí)間: 2025-3-24 12:42
Vincent E. Rubatzky,Mas Yamaguchibased on semi-empirical models locate this point at about 500?km above the photosphere. The consistency of these models has been tested by means of millimeter to infrared observations. We show that variations of the theoretical radial temperature profile near the temperature minimum impact the brigh作者: cleaver 時(shí)間: 2025-3-24 18:11
Vincent E. Rubatzky,Mas Yamaguchiressed magnetic activity spanning the second half of the 17th century. This spectral reconstruction is based on an extension of the Monte Carlo Solar Spectral Irradiance Model (MOCASSIM). The new version of the model, documented in this paper, extends its spectral range down to 150?nm, its temporal 作者: 休閑 時(shí)間: 2025-3-24 19:23 作者: 輕快來(lái)事 時(shí)間: 2025-3-24 23:58
Nitin R. Mangalvedhe,Jeffrey H. ReedEREO/COR1 data obtained during a deep minimum of solar activity in February 2008 (Carrington Rotation CR 2066) to retrieve and analyze the three-dimensional (3D) coronal electron density in the range of heights from 1.5 to 4 R. using a tomography method. With this, we qualitatively deduced structure作者: 陳腐思想 時(shí)間: 2025-3-25 07:04
Steven Tomczyk,Jie Zhang,Timothy BastianCaptures advances being made in the field of coronal magnetism, from theory to observations and instrumentation.Includes a collection of papers on coronal magnetism from the Workshop: Coronal Magnetis作者: Liberate 時(shí)間: 2025-3-25 10:03
http://image.papertrans.cn/c/image/238293.jpg作者: Myosin 時(shí)間: 2025-3-25 14:45 作者: Fibroid 時(shí)間: 2025-3-25 18:27
Magnetic Field Extrapolations into the Corona: Success and Future Improvements,r atmosphere has been an important task over the past decades. This task has been made complicated by the difficulties to measure the magnetic field in the corona, while it is currently known with a good accuracy in the photosphere and/or chromosphere. Thus, to determine the coronal magnetic field, 作者: 煩人 時(shí)間: 2025-3-25 20:29 作者: 冷峻 時(shí)間: 2025-3-26 03:10
Magnetic Field Diagnostics and Spatio-Temporal Variability of the Solar Transition Region,iolet (EUV) spectro-polarimetry. While for the coronal diagnostics techniques already exist in the form of infrared coronagraphy above the limb and radio observations on the disk, one has to investigate EUV observations for the transition region. However, so far the success of such observations has 作者: 發(fā)誓放棄 時(shí)間: 2025-3-26 07:19 作者: 淡紫色花 時(shí)間: 2025-3-26 08:55
,Measuring the Magnetic-Field Strength of the Quiet Solar Corona Using “EIT Waves”,ty to probe the plasma parameters of the solar atmosphere. Here, high-cadence observations of two “EIT wave” events taken using the . (AIA) instrument onboard the . (SDO) are combined with spectroscopic measurements from the . (EIS) onboard the . spacecraft and used to examine the variability of the作者: 走路左晃右晃 時(shí)間: 2025-3-26 16:08 作者: 砍伐 時(shí)間: 2025-3-26 19:24 作者: antiquated 時(shí)間: 2025-3-26 23:48 作者: maroon 時(shí)間: 2025-3-27 03:24
Observations of Coronal Mass Ejections with the Coronal Multichannel Polarimeter,, CoMP observations provide high-cadence image sequences of the coronal line intensity, Doppler shift, and line width simultaneously over a large field of view. By studying the Doppler shift and line width we may explore more of the physical processes of the initiation and propagation of coronal mas作者: 偶然 時(shí)間: 2025-3-27 07:56 作者: jet-lag 時(shí)間: 2025-3-27 13:24
3D Coronal Density Reconstruction and Retrieving the Magnetic Field Structure during Solar Minimum,EREO/COR1 data obtained during a deep minimum of solar activity in February 2008 (Carrington Rotation CR 2066) to retrieve and analyze the three-dimensional (3D) coronal electron density in the range of heights from 1.5 to 4 R. using a tomography method. With this, we qualitatively deduced structure作者: tenosynovitis 時(shí)間: 2025-3-27 17:28
,Photospheric Magnetic Field: Relationship Between North–South Asymmetry and Flux Imbalance,egion were taken into account. The north–south asymmetry of the magnetic fluxes was considered as well as the imbalance between positive and negative fluxes. The north–south asymmetry displays a regular alternation of the dominant hemisphere during the solar cycle: the northern hemisphere dominated 作者: Surgeon 時(shí)間: 2025-3-27 21:44 作者: 職業(yè) 時(shí)間: 2025-3-28 00:57 作者: 無(wú)脊椎 時(shí)間: 2025-3-28 02:26
A Reconstruction of Ultraviolet Spectral Irradiance During the Maunder Minimum,ressed magnetic activity spanning the second half of the 17th century. This spectral reconstruction is based on an extension of the Monte Carlo Solar Spectral Irradiance Model (MOCASSIM). The new version of the model, documented in this paper, extends its spectral range down to 150?nm, its temporal 作者: 新娘 時(shí)間: 2025-3-28 09:20 作者: 得罪 時(shí)間: 2025-3-28 12:10
3D Coronal Density Reconstruction and Retrieving the Magnetic Field Structure during Solar Minimum,EREO/COR1 data obtained during a deep minimum of solar activity in February 2008 (Carrington Rotation CR 2066) to retrieve and analyze the three-dimensional (3D) coronal electron density in the range of heights from 1.5 to 4 R. using a tomography method. With this, we qualitatively deduced structure作者: 者變 時(shí)間: 2025-3-28 17:35
ers on coronal magnetism from the Workshop: Coronal Magnetis.Captures advances being made in the field of coronal magnetism, from theory to observations and instrumentation..This volume is a collection of research articles on the subject of the solar corona, and particularly, coronal magnetism. The 作者: countenance 時(shí)間: 2025-3-28 18:47
Book 2014rch articles on the subject of the solar corona, and particularly, coronal magnetism. The book was motivated by the Workshop on Coronal Magnetism: Connecting Models to Data and the Corona to the Earth, which was held 21 - 23 May 2012 in Boulder, Colorado, USA. This workshop was attended by approxima作者: 審問,審訊 時(shí)間: 2025-3-29 00:15
Hyperasymptotic Perturbation Theoryith a special mask), and reducing the random and systematic errors are noted. An acceptable level of stray light in telescopes is estimated for the .-profile recording with a signal-to-noise ratio greater than three. Prospects for the limb chromosphere magnetic measurements are indicated.作者: charisma 時(shí)間: 2025-3-29 04:13 作者: Throttle 時(shí)間: 2025-3-29 07:43
,North–South Asymmetry in the Distribution of Solar Background Magnetic Field,ved in the vicinity of the equator. In addition to the main field, a weaker field of opposite polarity is always present in the polar regions. In the declining phase of the cycle, the main field dominates, but at the minimum and in the rising phase of the cycle, it is gradually replaced by the growing stronger secondary field.作者: Nomadic 時(shí)間: 2025-3-29 13:19
The Relation Between the Radial Temperature Profile in the Chromosphere and the Solar Spectrum at Ctness temperature at centimeter, submillimeter, and infrared wavelengths, but the millimeter wavelength emission remains unchanged. We found a region between 500?and 1000 km above the photosphere that remains hidden to observations at the frequencies that we studied here.作者: 真實(shí)的你 時(shí)間: 2025-3-29 19:26 作者: AVOID 時(shí)間: 2025-3-29 20:21 作者: Ganglion-Cyst 時(shí)間: 2025-3-30 03:55 作者: 變量 時(shí)間: 2025-3-30 07:25
International Regulatory Environment,tween cavity shape, aspect ratio, and propensity for eruption. We find that cavities with a teardrop-shaped morphology are more likely to erupt, and we discuss the implications of this morphology for magnetic topologies associated with CME models. We provide the full details of the survey for broad scientific use as supplemental material.作者: 親密 時(shí)間: 2025-3-30 09:08
Hyperasymptotic Perturbation Theorye consistent with observational measurements, it will mean positive identification of the magnetic morphology that surrounds certain quiescent filaments, which will lead to a better understanding of how they form and why they erupt.作者: 嘲弄 時(shí)間: 2025-3-30 14:48
J. Litva,A. Sandhu,K. Cho,T. Loormation to constrain CME models and probe various processes during the initial propagation of CMEs in the low corona, but also offer a possible cost-effective and low-risk means of space-weather monitoring.作者: parsimony 時(shí)間: 2025-3-30 18:17
Coronal Cavity Survey: Morphological Clues to Eruptive Magnetic Topologies,tween cavity shape, aspect ratio, and propensity for eruption. We find that cavities with a teardrop-shaped morphology are more likely to erupt, and we discuss the implications of this morphology for magnetic topologies associated with CME models. We provide the full details of the survey for broad scientific use as supplemental material.作者: 龍卷風(fēng) 時(shí)間: 2025-3-31 00:30
Polarimetric Properties of Flux Ropes and Sheared Arcades in Coronal Prominence Cavities,e consistent with observational measurements, it will mean positive identification of the magnetic morphology that surrounds certain quiescent filaments, which will lead to a better understanding of how they form and why they erupt.作者: Immobilize 時(shí)間: 2025-3-31 02:05 作者: 光滑 時(shí)間: 2025-3-31 08:21
he topical issue also contains contributions from researchers not present at the workshop..This volume is aimed at researchers and graduate students active in solar physics..Originally published in .Solar Physics., Vol. 288, Issue 2, 2013 and Vol. 289, Issue 8, 2014..978-1-4939-4983-0978-1-4939-2038-9作者: Vertebra 時(shí)間: 2025-3-31 10:22 作者: orthopedist 時(shí)間: 2025-3-31 14:30 作者: 召集 時(shí)間: 2025-3-31 20:15 作者: DEBT 時(shí)間: 2025-4-1 01:41
Transactional Aspects of Workflows,ven if one integrates for several minutes to reach the required signal-to-noise ratio, and despite the rapidly changing intensity in the model (just as in observations). This variability of the intensity is often used as an argument against transition region magnetic diagnostics, which requires expo作者: 浸軟 時(shí)間: 2025-4-1 05:06 作者: 補(bǔ)助 時(shí)間: 2025-4-1 09:22 作者: agenda 時(shí)間: 2025-4-1 11:24
Mathematics and Its Applicationsow frequencies are also identified in the QFP wave. We propose that the generation of the period of 80 seconds was caused by the periodic releasing of energy bursts through some nonlinear processes in magnetic reconnection, while the low frequencies were possibly the leakage of pressure-driven oscil作者: Euphonious 時(shí)間: 2025-4-1 17:51 作者: 刻苦讀書 時(shí)間: 2025-4-1 20:38
Vincent E. Rubatzky,Mas Yamaguchi the magnetic fluxes and the sign of the imbalance of the positive and the negative fluxes are related to the quarter of the 22-year magnetic cycle where the magnetic configuration of the Sun remains constant (from the minimum where the sunspot sign changes according to Hale’s law to the magnetic-fi作者: 生銹 時(shí)間: 2025-4-1 23:45
Vincent E. Rubatzky,Mas Yamaguchitransition region. We also reconstruct ultraviolet spectra for May 2008 and March 2009, spanning the extended phase of low activity separating Cycles 23 and 24. Our results suggest that despite the unusually long temporal extent of this activity minimum, the ultraviolet emission still remained sligh
