標(biāo)題: Titlebook: Coronal Disturbances; Gordon Newkirk Book 1974 International Astronomical Union 1974 Corona.Planet.Solar flare.Variation.cosmic ray.observ [打印本頁] 作者: INEPT 時(shí)間: 2025-3-21 19:25
書目名稱Coronal Disturbances影響因子(影響力)
書目名稱Coronal Disturbances影響因子(影響力)學(xué)科排名
書目名稱Coronal Disturbances網(wǎng)絡(luò)公開度
書目名稱Coronal Disturbances網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Coronal Disturbances被引頻次
書目名稱Coronal Disturbances被引頻次學(xué)科排名
書目名稱Coronal Disturbances年度引用
書目名稱Coronal Disturbances年度引用學(xué)科排名
書目名稱Coronal Disturbances讀者反饋
書目名稱Coronal Disturbances讀者反饋學(xué)科排名
作者: 充滿人 時(shí)間: 2025-3-21 21:24 作者: PAN 時(shí)間: 2025-3-22 01:31 作者: 肉體 時(shí)間: 2025-3-22 07:49
Bulk growth of widegap II–VI single crystalson whether the electrons propagate along the axes of coronal streamers. Several important burst properties appear to be significantly affected by ray scattering on small-scale size density irregularities in the corona.作者: 發(fā)生 時(shí)間: 2025-3-22 11:36 作者: champaign 時(shí)間: 2025-3-22 16:44
II–VI electroluminescent devicesd the accelerated electrons provide the energy necessary for all the observed electromagnetic emissions produced during the flash phase of small solar flares. Models of the impulsive phase emissions in which energetic electrons play a prominant role are examined and crucial tests to check the accuracy of these models are indicated (Table IV).作者: champaign 時(shí)間: 2025-3-22 19:31
Bulk growth of widegap II–VI single crystalsions were joined by extended field lines with the acceleration mechanism somewhere in between. Although nothing was visible in Hα (such as surges or post flare ejections) that would indicate connecting field lines, higher coronal structures could explain the similarity in hard X-rays from two separate regions.作者: ESO 時(shí)間: 2025-3-22 21:29
Distribution of Circularly Polarized Emission across the Solar Disk at λ =4.3cmd a ‘neutral line’ divide the two polarized hemispheres, showing a contour that depends strongly on the presence of active centres and on their displacement with solar rotation. This suggest that the polarized features are strongly controlled, if not completely, by the presence of photospheric underlying magnetic areas.作者: 尖酸一點(diǎn) 時(shí)間: 2025-3-23 01:32 作者: Lineage 時(shí)間: 2025-3-23 08:29 作者: frenzy 時(shí)間: 2025-3-23 12:17
Coronal Disturbances Observed in the Optical Emmission Linesf the emission lines may occur after the disappearance of a filament. The events have a duration of up to several hours and consist of hot clouds of high density that are slowly rising from the upper chromosphere into the lower corona.作者: 停止償付 時(shí)間: 2025-3-23 15:22 作者: 注意 時(shí)間: 2025-3-23 19:35
II–VI electroluminescent devicesin the temperature range 9.3 × 10. K to 2.0 × 10. K. The photographic observations of the active region show clearly that the spatial distribution of material varies considerably with its temperature.作者: 露天歷史劇 時(shí)間: 2025-3-23 22:13
Analysis of EUV Observations of a Coronal Active Region Made during the 7 March 1970 Eclipsein the temperature range 9.3 × 10. K to 2.0 × 10. K. The photographic observations of the active region show clearly that the spatial distribution of material varies considerably with its temperature.作者: overture 時(shí)間: 2025-3-24 06:09
II–VI electroluminescent devicesedge of impulsive streams of solar electrons with energies extending from several hundred keV to several keV. Recent experiments measuring the direction of arrival of the radio emission allow the exciter particles to be tracked along the interplanetary magnetic field from regions near the Sun out to 1 AU.作者: 啞巴 時(shí)間: 2025-3-24 06:41
Bulk growth of widegap II–VI single crystalsy escape from the Sun. Direct spacecraft observations of the type III emission generated near 1 AU and the energetic electrons, provide quantitative information on the characteristics of the electrons exciting type III emission, the production of plasma waves, and the conversion from plasma waves to electromagnetic radiation.作者: 激勵(lì) 時(shí)間: 2025-3-24 12:16
Solar Radio Bursts at Low Frequenciesedge of impulsive streams of solar electrons with energies extending from several hundred keV to several keV. Recent experiments measuring the direction of arrival of the radio emission allow the exciter particles to be tracked along the interplanetary magnetic field from regions near the Sun out to 1 AU.作者: LATER 時(shí)間: 2025-3-24 18:21
The Flash Phase of Solar Flares: Satellite Observations of Electronsy escape from the Sun. Direct spacecraft observations of the type III emission generated near 1 AU and the energetic electrons, provide quantitative information on the characteristics of the electrons exciting type III emission, the production of plasma waves, and the conversion from plasma waves to electromagnetic radiation.作者: 鋼筆尖 時(shí)間: 2025-3-24 19:43 作者: 是突襲 時(shí)間: 2025-3-25 01:07
Large-Scale Magnetic Structures Responsible for Coronal Disturbancesr which the magnetic synoptic charts are available) the largest solar activity, usually connected with proton-flare occurrence, has been very closely related to a characteristic large-scale pattern in the magnetic field distribution with a life-time of the order of 8–10 solar rotations. These regula作者: mechanical 時(shí)間: 2025-3-25 05:23 作者: Kidnap 時(shí)間: 2025-3-25 09:42
Analysis of EUV Observations of a Coronal Active Region Made during the 7 March 1970 Eclipseon on the NE limb (Gabriel ., 1971). The condensation shows the existence of loop structure, which defines the local magnetic fields, and is apparent in forbidden lines including those of Si ., Si ., S ., Fe ., Fe . and Fe . which lie between 1200 ? and 2050 ? (Jordan, 1971). These lines are formed 作者: 白楊魚 時(shí)間: 2025-3-25 14:23 作者: defile 時(shí)間: 2025-3-25 19:13
Spectral Association of the 7 August 1972 Solar Radio Burst with Particle Accelerationory (Figure 1) provide a basis for correlation studies (especially timing information) of the associated white light flare, the high energy particle emission, type II bursts, and many other phenomena. This is perhaps the first time that sufficient radio coverage (i.e., data above 10000 MHz) was avai作者: defendant 時(shí)間: 2025-3-25 21:55
X-Ray Emission in Absence of Flares Related to Hα Activity and Type III Burst Productiontics of the particle acceleration process operating when a Hα-flare may or may not be detectable. The Hα observations were made by Meudon Observatory with a Hα telescope fitted with a 0.75 ? band pass Lyot filter. During a 10 s period, three pictures were obtained — one at the Hα line center, one at作者: right-atrium 時(shí)間: 2025-3-26 02:53 作者: 舔食 時(shí)間: 2025-3-26 04:21 作者: allude 時(shí)間: 2025-3-26 09:53 作者: Oversee 時(shí)間: 2025-3-26 15:21 作者: Gobble 時(shí)間: 2025-3-26 19:20
The Flash Phase of Solar Flares: Satellite Observations of Electronsrvations support a two stage acceleration process for electrons, one stage commonly occurring at the flare flash phase and accelerating electrons up to ~ 100 keV, and a second stage occurring only in large proton flares and accelerating electrons up to relativistic energies. The location of the acce作者: 喪失 時(shí)間: 2025-3-27 00:24 作者: 沒收 時(shí)間: 2025-3-27 03:17
Total Quality Management — worldwide effectt potential field) as well as disturbances which appear to be related to changes in these configurations. Thirdly, the role of the field in guiding coronal disturbances is considered. This is evident for bulk motions (sprays, surges, flare loops, green line events, etc.), wave motions (flare associa作者: Cosmopolitan 時(shí)間: 2025-3-27 05:29 作者: pus840 時(shí)間: 2025-3-27 12:13
Bulk growth of widegap II–VI single crystalsd for qualitative analysis of energetic particle and white light events. The ultimate good may possibly come from spectral analysis of the minute by minute variation of the burst microwave radiation spectral slope α (above .) in the area between 15 000 and 35 000 MHz. This may be used alone or in re作者: 和平主義 時(shí)間: 2025-3-27 15:09
II–VI electroluminescent devicesavelength range covered was 0.5–20 ?. The type III radio data was obtained from two sources: The 169 MHz radio-heliograph at Nancay which provided east-west position of the radio burst on the Sun with an accuracy of ~ 1′ and the radio spectra measured by various ground based observatories. The findi作者: EPT 時(shí)間: 2025-3-27 20:03 作者: 冒失 時(shí)間: 2025-3-27 23:43 作者: 啞巴 時(shí)間: 2025-3-28 05:19 作者: Guaff豪情痛飲 時(shí)間: 2025-3-28 06:34 作者: ESPY 時(shí)間: 2025-3-28 11:51
X-Ray Emission in Absence of Flares Related to Hα Activity and Type III Burst Productionavelength range covered was 0.5–20 ?. The type III radio data was obtained from two sources: The 169 MHz radio-heliograph at Nancay which provided east-west position of the radio burst on the Sun with an accuracy of ~ 1′ and the radio spectra measured by various ground based observatories. The findi作者: 結(jié)合 時(shí)間: 2025-3-28 14:58
Total Quality Management — worldwide effectpassively, in virtually all coronal disturbances. The purpose of this paper is to put into perspective the various roles magnetic fields can play in both exciting and guiding these observed transient phenomena. A discussion of our present theoretical concepts relevant to this subject can be convenie作者: 詢問 時(shí)間: 2025-3-28 19:09
TQM Structure and top-down requirementsr which the magnetic synoptic charts are available) the largest solar activity, usually connected with proton-flare occurrence, has been very closely related to a characteristic large-scale pattern in the magnetic field distribution with a life-time of the order of 8–10 solar rotations. These regula作者: Eosinophils 時(shí)間: 2025-3-29 00:47 作者: needle 時(shí)間: 2025-3-29 04:41
II–VI electroluminescent deviceson on the NE limb (Gabriel ., 1971). The condensation shows the existence of loop structure, which defines the local magnetic fields, and is apparent in forbidden lines including those of Si ., Si ., S ., Fe ., Fe . and Fe . which lie between 1200 ? and 2050 ? (Jordan, 1971). These lines are formed 作者: lethal 時(shí)間: 2025-3-29 11:18
II–VI electroluminescent devicesacteristics of the impulsive (flash) phase phenomenon in small solar flares particularly from the point of view of the acceleration of electrons and their role in producing the various impulsive phase emissions. Observed and deduced characteristics of the various electromagnetic emission sources are作者: chance 時(shí)間: 2025-3-29 12:31
Bulk growth of widegap II–VI single crystalsory (Figure 1) provide a basis for correlation studies (especially timing information) of the associated white light flare, the high energy particle emission, type II bursts, and many other phenomena. This is perhaps the first time that sufficient radio coverage (i.e., data above 10000 MHz) was avai作者: 征兵 時(shí)間: 2025-3-29 16:24 作者: 組裝 時(shí)間: 2025-3-29 23:04
Bulk growth of widegap II–VI single crystals5694 have been used. Most of the observed phenomena are flare-connected, but all of them are related to some kind of Hα-activity. Sudden brightening of the emission lines may occur after the disappearance of a filament. The events have a duration of up to several hours and consist of hot clouds of h作者: 直覺好 時(shí)間: 2025-3-30 03:39 作者: machination 時(shí)間: 2025-3-30 06:09 作者: insurrection 時(shí)間: 2025-3-30 09:05
II–VI electroluminescent devicesrsts are type III events (associated with particles) but several cases of type II emission (associated with shocks) have been reported. The analyses which lead to emission levels of type III solar bursts out to beyond 1 AU from the Sun also indicate that the low frequency radiation is observed at th作者: 鋼盔 時(shí)間: 2025-3-30 14:30 作者: conquer 時(shí)間: 2025-3-30 20:04
https://doi.org/10.1007/978-94-010-2257-6Corona; Planet; Solar flare; Variation; cosmic ray; observatory; solar; sun; telescope作者: 火車車輪 時(shí)間: 2025-3-30 23:38
978-90-277-0492-4International Astronomical Union 1974作者: 比喻好 時(shí)間: 2025-3-31 04:03 作者: 夜晚 時(shí)間: 2025-3-31 08:27
TQM Structure and top-down requirementsTwo results were obtained recently at Meudon concerning the metric type III production by flares which both emphasize the importance of the local magnetic configuration involved.作者: 無王時(shí)期, 時(shí)間: 2025-3-31 12:30 作者: Deduct 時(shí)間: 2025-3-31 13:36
TQM Structure and top-down requirementsAn exceptional variety of positions and polarizations was found for two type I storms and numerous sporadic bursts observed during 15 consecutive days with the Culgoora radio-heliograph at 80 and 160 MHz.作者: Rebate 時(shí)間: 2025-3-31 21:17
