標(biāo)題: Titlebook: Eruptive Solar Flares; Proceedings of Collo Zdeněk ?vestka,Bernard V. Jackson,Marcos E. Machad Conference proceedings 1992 Springer-Verlag [打印本頁(yè)] 作者: damped 時(shí)間: 2025-3-21 19:55
書目名稱Eruptive Solar Flares影響因子(影響力)
書目名稱Eruptive Solar Flares影響因子(影響力)學(xué)科排名
書目名稱Eruptive Solar Flares網(wǎng)絡(luò)公開(kāi)度
書目名稱Eruptive Solar Flares網(wǎng)絡(luò)公開(kāi)度學(xué)科排名
書目名稱Eruptive Solar Flares被引頻次
書目名稱Eruptive Solar Flares被引頻次學(xué)科排名
書目名稱Eruptive Solar Flares年度引用
書目名稱Eruptive Solar Flares年度引用學(xué)科排名
書目名稱Eruptive Solar Flares讀者反饋
書目名稱Eruptive Solar Flares讀者反饋學(xué)科排名
作者: 故意釣到白楊 時(shí)間: 2025-3-21 23:18 作者: 使混合 時(shí)間: 2025-3-22 03:37 作者: Aggregate 時(shí)間: 2025-3-22 07:29
Mechanismus der Kupplungsreaktion,this scenario involves the formation of a filament magnetic field in the corona above a photospheric polarity inversion where cancelling magnetic fields are observed. The formation of a filament magnetic field is accomplished in several recent models by first interpreting the cancelling fields as a 作者: overreach 時(shí)間: 2025-3-22 10:18 作者: 出血 時(shí)間: 2025-3-22 16:11
Hans Euler,Hans Euler,Karl Myrb?ckved the likely location of the separatrices, surfaces that separate cells of different field line connectivities, and of the separator which is the intersection of the separatrices. The connectivity of every magnetic field line, which is defined by the dipoles located at its ends, is computed by a c作者: 出血 時(shí)間: 2025-3-22 19:16 作者: TEM 時(shí)間: 2025-3-23 01:00 作者: morale 時(shí)間: 2025-3-23 03:27
Natürlich vorkommende Insektizideomes to lose its stability and erupt. From observed characteristics (1) of the preflare magnetic field configuration, (2) of the onset and development of the eruption of this configuration before and during the flare, and (3) of the onset and development of the flare energy release (i.e., the heatin作者: dithiolethione 時(shí)間: 2025-3-23 07:50
Definition und Systematik der Bindemittel,prior to the flare becomes opened. One of the requirements of flare models is to explain how the field can be opened while decreasing the overall magnetic energy of the system. After the field is opened, reconnection must occur in order to restore the field to its pre-flare configuration. The strong作者: HACK 時(shí)間: 2025-3-23 10:10
https://doi.org/10.1007/978-3-662-26553-6energy transport models: nonthermal thick-target electron precipitation; thermal conduction; and electricfield acceleration. Predictions made by each of these models for the Ca XIX blueshift and nonthermal broadening are compared with observations obtained during the flare impulsive phase. Agreement作者: cornucopia 時(shí)間: 2025-3-23 17:19 作者: expound 時(shí)間: 2025-3-23 21:20 作者: NAUT 時(shí)間: 2025-3-24 02:04 作者: synovium 時(shí)間: 2025-3-24 04:37 作者: Root494 時(shí)間: 2025-3-24 07:06 作者: 啟發(fā) 時(shí)間: 2025-3-24 12:57 作者: accrete 時(shí)間: 2025-3-24 17:29 作者: 禁止 時(shí)間: 2025-3-24 21:00
Conference proceedings 1992This is an exhaustive survey of present-day solar research including both theory and observations. It deals with eruptive flares, filament eruption in x-rays and radio waves, energy release and transport, and terrestrial response to solar flares. Details of the most recent SOLAR-A project (launched shortly after the conference) are also presented.作者: Ascribe 時(shí)間: 2025-3-25 02:21 作者: violate 時(shí)間: 2025-3-25 04:11
978-3-662-13874-8Springer-Verlag Berlin Heidelberg 1992作者: lipids 時(shí)間: 2025-3-25 10:36 作者: uncertain 時(shí)間: 2025-3-25 14:46
Lecture Notes in Physicshttp://image.papertrans.cn/e/image/315026.jpg作者: formula 時(shí)間: 2025-3-25 16:17 作者: 值得尊敬 時(shí)間: 2025-3-25 23:21 作者: 馬籠頭 時(shí)間: 2025-3-26 00:23 作者: 考古學(xué) 時(shí)間: 2025-3-26 07:40
Chemie der Beta-Dicarbonyl-Verbindungen established positive field at 0.2 km/s. Data from the JHU/APL vector magnetograph show that this motion led to the development of a sheared field. The flare started near the newly-sheared fields and spread to engulf most of the spot region. A magnetogram taken 45 min after flare onset shows possible relaxation of the sheared fields.作者: 聯(lián)想記憶 時(shí)間: 2025-3-26 10:50
https://doi.org/10.1007/978-3-642-66415-1ld-up within a day. High resolution H-alpha observations of these events indicate that large amount of ejected material was “siphoned out” from the chromosphere through, the top. of a low-lying compact emission loop within the active region.作者: 拖網(wǎng) 時(shí)間: 2025-3-26 16:25 作者: Paleontology 時(shí)間: 2025-3-26 19:54
0075-8450 ruption in x-rays and radio waves, energy release and transport, and terrestrial response to solar flares. Details of the most recent SOLAR-A project (launched shortly after the conference) are also presented.978-3-662-13874-8978-3-540-46794-6Series ISSN 0075-8450 Series E-ISSN 1616-6361 作者: GAVEL 時(shí)間: 2025-3-27 00:39 作者: dyspareunia 時(shí)間: 2025-3-27 02:43 作者: defendant 時(shí)間: 2025-3-27 09:17 作者: humectant 時(shí)間: 2025-3-27 09:28
Definition und Systematik der Bindemittel,vely that these apparent motions are not due to mass motions of the solar plasma. The motions can only be explained by the upward propagation of an energy source in the corona, and in the 1VIHD-reconnection model of flares, the propagating energy source is an x-line accompanied by slow-mode shocks.作者: 投射 時(shí)間: 2025-3-27 15:27
Field opening and reconnection,vely that these apparent motions are not due to mass motions of the solar plasma. The motions can only be explained by the upward propagation of an energy source in the corona, and in the 1VIHD-reconnection model of flares, the propagating energy source is an x-line accompanied by slow-mode shocks.作者: HOWL 時(shí)間: 2025-3-27 21:39
Variation of the vector magnetic field in an eruptive flare, established positive field at 0.2 km/s. Data from the JHU/APL vector magnetograph show that this motion led to the development of a sheared field. The flare started near the newly-sheared fields and spread to engulf most of the spot region. A magnetogram taken 45 min after flare onset shows possible relaxation of the sheared fields.作者: 表示向前 時(shí)間: 2025-3-28 01:55
Filament eruptions, flaring arches and eruptive flares,ld-up within a day. High resolution H-alpha observations of these events indicate that large amount of ejected material was “siphoned out” from the chromosphere through, the top. of a low-lying compact emission loop within the active region.作者: foppish 時(shí)間: 2025-3-28 02:57 作者: photopsia 時(shí)間: 2025-3-28 07:22 作者: 脊椎動(dòng)物 時(shí)間: 2025-3-28 12:30
https://doi.org/10.1007/978-3-642-81555-3e chromospheric emission and by the quiet photospheric emission. As a consequence, a temporary decrease of the continuum intensity ( negative flare ) is expected. After less than 20 seconds, the radiative heating of the upper photosphere and temperature minimum region produces a white-light flare.作者: uveitis 時(shí)間: 2025-3-28 17:51
The intrinsic relationship between flares and eruption of filament currents,ance of the X-ray flare is proportional to the rate of the increase of the total energy prior to the filament eruption. On the basis of these results, we concluded that there is an intimate relationship between the flare and eruptive filament quantitatively.作者: 同謀 時(shí)間: 2025-3-28 20:50 作者: MODE 時(shí)間: 2025-3-29 02:02
History and basic characteristics of eruptive flares, of a white-light flare by Carrington and Hodgson in 1859, we cover in succession the highlights: Hale‘s invention of the spectroheliograph in 1892 and the spectrohelioscope in 1926 started flare observations in Hα. The institution of a world-wide flare patrol brought significant advances in knowled作者: 孵卵器 時(shí)間: 2025-3-29 03:41
Basic magnetic configuration and energy supply processes for an interacting flux model of eruptive s and interactions of separate flux systems; the process of preflare energy storage in excess of potential due to photospheric motions; the conditions for flare occurrence, including shear in the corona and complexity and the roles of spot motions, flux cancellation and prominences; theories for eru作者: 溺愛(ài) 時(shí)間: 2025-3-29 10:14
The role of cancelling magnetic fields in the buildup to erupting filaments and flares,this scenario involves the formation of a filament magnetic field in the corona above a photospheric polarity inversion where cancelling magnetic fields are observed. The formation of a filament magnetic field is accomplished in several recent models by first interpreting the cancelling fields as a 作者: 情感 時(shí)間: 2025-3-29 14:21 作者: electrolyte 時(shí)間: 2025-3-29 19:29
Interaction of large-scale magnetic structures in solar flares,ved the likely location of the separatrices, surfaces that separate cells of different field line connectivities, and of the separator which is the intersection of the separatrices. The connectivity of every magnetic field line, which is defined by the dipoles located at its ends, is computed by a c作者: 假裝是你 時(shí)間: 2025-3-29 20:29 作者: 死亡 時(shí)間: 2025-3-30 02:10
Filament eruptions, flaring arches and eruptive flares,intaining filament stability is established; apart from the footpoint separation and height criteria. Further, a homologous series of more energetic events, namely, the flaring arches and eruptive flares of March 5–7, 1991, suggest a repetitive restoration of magnetic field conditions and energy bui作者: 注意到 時(shí)間: 2025-3-30 05:32 作者: LANCE 時(shí)間: 2025-3-30 11:50 作者: Outshine 時(shí)間: 2025-3-30 12:35 作者: synovium 時(shí)間: 2025-3-30 17:03 作者: accomplishment 時(shí)間: 2025-3-30 21:36 作者: 四指套 時(shí)間: 2025-3-31 02:22 作者: 絕緣 時(shí)間: 2025-3-31 07:25 作者: 失敗主義者 時(shí)間: 2025-3-31 10:08
Plasma parameters derived from MSDP observations of cool flare loops, been detected in the Hα line just after the flare maximum and they appeared in absorption against the disk. Using the first-order differential cloud model (DCM1) technique, we derive empirically some basic plasma parameters at 15 points along one loop leg. The flow velocities and true heights have 作者: 顯微鏡 時(shí)間: 2025-3-31 17:00 作者: Commentary 時(shí)間: 2025-3-31 21:07 作者: PATHY 時(shí)間: 2025-4-1 01:17 作者: Cougar 時(shí)間: 2025-4-1 05:03
History and basic characteristics of eruptive flares,was found that flares were often preceded by filament activations, and growing loop prominence systems were recognized as the limb counterpart of two-ribbon disk flares. The early 1970s brought Skylab observations of coronal mass ejections (CMEs) and arcades of coronal soft X-ray loops above two-rib作者: ARM 時(shí)間: 2025-4-1 08:14 作者: 生氣的邊緣 時(shí)間: 2025-4-1 11:52 作者: GEON 時(shí)間: 2025-4-1 15:16
Triggering of eruptive flares: Destabilization of the preflare magnetic field configuration, initial flare brightening typically stems from points where opposite-polarity flux is gradually merging and canceling at or near the main inversion line, it is argued (1) that eruptive flares are driven by the eruptive expansion of the strongly sheared core of the preflare magnetic field, (2) that
