標(biāo)題: Titlebook: Energy Storage and Release through the Solar Activity Cycle; Models Meet Radio Ob Christophe Marqué,Alexander Nindos Book 2012 Springer Sci [打印本頁] 作者: ODDS 時間: 2025-3-21 19:35
書目名稱Energy Storage and Release through the Solar Activity Cycle影響因子(影響力)
書目名稱Energy Storage and Release through the Solar Activity Cycle影響因子(影響力)學(xué)科排名
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書目名稱Energy Storage and Release through the Solar Activity Cycle網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Energy Storage and Release through the Solar Activity Cycle被引頻次
書目名稱Energy Storage and Release through the Solar Activity Cycle被引頻次學(xué)科排名
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書目名稱Energy Storage and Release through the Solar Activity Cycle讀者反饋
書目名稱Energy Storage and Release through the Solar Activity Cycle讀者反饋學(xué)科排名
作者: syncope 時間: 2025-3-22 00:08 作者: Lineage 時間: 2025-3-22 03:03
Coronal Shock Waves, EUV Waves, and Their Relation to CMEs. II. Modeling MHD Shock Wave Propagationof the modeling of the propagation of shock-associated extreme-ultraviolet (EUV) waves as well as Moreton waves along the solar surface in the simplest solar corona model. The calculations reveal deceleration and lengthening of the waves. In contrast, waves considered in the linear approximation keep their length unchanged and slightly accelerate.作者: 松軟 時間: 2025-3-22 07:28 作者: 代替 時間: 2025-3-22 09:51
mission and fundamental radio physicsFor nearly sixty years, radio observations have provided a unique insight into the physics of the active and quiescent solar atmosphere. Thanks to the variety of emission mechanisms and to the large altitude range available to observations, fundamental plasma par作者: 流動性 時間: 2025-3-22 13:17 作者: 流動性 時間: 2025-3-22 17:02
James K. Whitesell,Mark A. Mintonof the modeling of the propagation of shock-associated extreme-ultraviolet (EUV) waves as well as Moreton waves along the solar surface in the simplest solar corona model. The calculations reveal deceleration and lengthening of the waves. In contrast, waves considered in the linear approximation keep their length unchanged and slightly accelerate.作者: 異端邪說下 時間: 2025-3-23 01:12
https://doi.org/10.1007/978-3-662-10051-6nection between the parameters of the radio emission from three different layers of the solar atmosphere and the solar wind velocity near the Earth’s orbit was discovered. Such a connection is suggestive of a common mechanism of solar wind acceleration from chromospheric heights to the upper corona.作者: 稀釋前 時間: 2025-3-23 03:32 作者: Keratectomy 時間: 2025-3-23 08:53 作者: Gratuitous 時間: 2025-3-23 13:27 作者: MELD 時間: 2025-3-23 14:50
Location of Decimetric Pulsations in Solar Flares,er frequency. The average positions at different frequencies are on a line pointing approximately to the coronal hard X-ray source. Thus, the pulsations cannot be caused by electrons trapped in the flare loops, but are consistent with emission from a current sheet above the coronal source.作者: 逗留 時間: 2025-3-23 18:54
,Quasi-periodic Oscillations of Solar Active Regions in Connection with Their Flare Activity – NoRH ore the burst. This event is similar to the cases of the precursors investigated by Sych . (.., 791, .). We also found well-defined eight-minute oscillations of microwave emission from sunspot. We interpret our observations in terms of a relationship between MHD waves propagating from sunspots and flare processes.作者: 鑲嵌細(xì)工 時間: 2025-3-23 22:22 作者: 香料 時間: 2025-3-24 04:30 作者: 連系 時間: 2025-3-24 07:51
Energy Storage and Release through the Solar Activity CycleModels Meet Radio Ob作者: alabaster 時間: 2025-3-24 13:54
Energy Storage and Release through the Solar Activity Cycle978-1-4614-4403-9作者: BIDE 時間: 2025-3-24 17:26 作者: 不規(guī)則的跳動 時間: 2025-3-24 22:56 作者: Medley 時間: 2025-3-25 01:13 作者: 四溢 時間: 2025-3-25 04:10 作者: 注射器 時間: 2025-3-25 10:07
Relation Between the 3D-Geometry of the Coronal Wave and Associated CME During the 26 April 2008 Evrce region location. Applying the forward fitting model developed by Thernisien, Howard, and Vourlidas (Astrophys. J. ., 763, .), we derive the CME flux rope position on the solar surface to be close to the dimming regions. We conclude that the expanding flanks of the CME most likely drive and shape作者: 內(nèi)行 時間: 2025-3-25 11:52
Coronal Shock Waves, EUV Waves, and Their Relation to CMEs. III. Shock-Associated CME/EUV Wave in a solar radii. The second, quasi-stationary EUV component near the dimming was presumably associated with a stretched CME structure; no indications of opening magnetic fields have been detected far from the eruption region.作者: crumble 時間: 2025-3-25 16:11 作者: 極肥胖 時間: 2025-3-25 22:45 作者: Progesterone 時間: 2025-3-26 02:40 作者: expeditious 時間: 2025-3-26 08:16
Winfried Effelsberg,Hans Schadewaldtvents. Each spike shows positive or negative frequency drift. The mean negative and positive drifts of the investigated spikes are equal to ?776?MHz?s. and 1608?MHz?s., respectively. The emission sources of the dm-spikes are located mainly at disk center. We have noticed two kinds of chains, with an作者: Stagger 時間: 2025-3-26 12:33
https://doi.org/10.1007/978-3-531-18873-7f propagating magnetoacoustic wave trains, the results indicate the?presence of several wave trains in the fibers’ source. While the long-period wave trains trigger or modulate a?whole group of fibers, the short-period ones look like being connected with individual fiber bursts. This result supports作者: WAG 時間: 2025-3-26 14:38
Fundus Changes After Vitreoretinal Surgery,. From the time coincidence we infer that the mildly relativistic electrons are accelerated at the same time and at the same location as the accompanying type III emitting electrons and coronal EUV jets. The characteristics of the spikes reflect the injection and acceleration profiles in the corona 作者: 音樂等 時間: 2025-3-26 19:22
https://doi.org/10.1007/978-981-10-2089-6rce region location. Applying the forward fitting model developed by Thernisien, Howard, and Vourlidas (Astrophys. J. ., 763, .), we derive the CME flux rope position on the solar surface to be close to the dimming regions. We conclude that the expanding flanks of the CME most likely drive and shape作者: 連累 時間: 2025-3-26 21:20 作者: 讓你明白 時間: 2025-3-27 03:41 作者: sparse 時間: 2025-3-27 05:52
https://doi.org/10.1007/978-3-540-71708-9osonic speed, computed from a standard magnetic field model, was estimated as high as ～?600?km?s., implying that the CME speed was probably just sufficient to drive a weak fast-mode MHD shock ahead of the front. Simultaneously with the type?II radio emission, significant changes in the O?. doublet l作者: 茁壯成長 時間: 2025-3-27 13:26
Origin of the Submillimeter Radio Emission During the Time-Extended Phase of a Solar Flare,mpulsive phase and can last for a few tens of minutes to more than one hour. The few examples discussed in the literature indicate that such long-lasting submillimeter emission is most likely thermal bremsstrahlung. We present a detailed analysis of the time-extended phase of the 27?October?2003 (M6作者: 攝取 時間: 2025-3-27 17:39 作者: 主講人 時間: 2025-3-27 19:10
Millisecond Radio Spikes in the Decimetric Band,nts were obtained with a very high time resolution (80 microseconds) radio spectrograph in the 1352?–?1490?MHz range. These data were complemented with observations from the radio spectrograph at Ond?ejov in the 0.8?–?2.0?GHz band. We evaluated the basic characteristics of the individual spikes (dur作者: 施舍 時間: 2025-3-27 22:18
Magnetoacoustic Wave Trains in the 11 July 2005 Radio Event with Fiber Bursts,e found structures with different characteristic period?. and frequency drift FD: .)?fiber substructures (composed of dot emissions) with ..≈?0.5?s, FD.=??87?MHz?s. on average, .)?fiber structures with ..≈1.9?s, and .)?drifting structures with ..≈81.4?s, FD.=??8.7, +?98.5, and ??21.8?MHz?s.. In the 作者: 慢慢沖刷 時間: 2025-3-28 04:59
,Quasi-periodic Oscillations of Solar Active Regions in Connection with Their Flare Activity – NoRH level of the chromosphere-corona transition region. The observations of short period (from one to ten minutes) oscillations in sunspots reflect propagation of magnetohydrodynamic (MHD) waves in the magnetic flux tubes of the sunspots. We investigate the oscillation parameters in active regions in c作者: addition 時間: 2025-3-28 07:06 作者: artifice 時間: 2025-3-28 11:13 作者: 暴行 時間: 2025-3-28 16:55
,Coronal Shock Waves, EUV Waves, and Their Relation to CMEs. I. Reconciliation of “EIT Waves”, Type ned into shocks and freely propagated afterwards like decelerating blast waves that showed up as Moreton waves and EUV waves. We propose a simple quantitative description for such shock waves to reconcile their observed propagation with drift rates of metric type II bursts and kinematics of leading 作者: Foregery 時間: 2025-3-28 20:57
Coronal Shock Waves, EUV Waves, and Their Relation to CMEs. III. Shock-Associated CME/EUV Wave in ay connected off-limb and on-disk signatures. Veronig .. (.., L57, .) concluded that the dome was formed by a weak shock wave. We have revealed two EUV components, one of which corresponded to this transient. All of its properties found from EUV, white light, and a metric type II burst match expectat作者: Entirety 時間: 2025-3-29 00:38 作者: 遍及 時間: 2025-3-29 04:11
The 17 January 2005 Complex Solar Radio Event Associated with Interacting Fast Coronal Mass Ejectioanied by metre-to-kilometre type-III groups tracing energetic electrons that escape into the interplanetary space and by decametre-to-hectometre type-II bursts attributed to CME-driven shock waves. A?peculiar type-III burst group was observed below 600?kHz 1.5 hours after the second type-III group. 作者: 激勵 時間: 2025-3-29 09:00 作者: 砍伐 時間: 2025-3-29 11:29
The Connection of Solar Wind Parameters with Radio and UV Emission from Coronal Holes,MHz, from NoRH, SSRT and Nan?ay radioheliographs), and solar wind parameters, from ACE spacecraft data over the period 12?March?–?31?May?2007. The increase in the solar wind velocity up to ～?600?km?s. was found to correlate with a decrease in the UV flux in the central parts of the solar disk. A con作者: SHRIK 時間: 2025-3-29 19:17 作者: dithiolethione 時間: 2025-3-29 20:30
http://image.papertrans.cn/e/image/310424.jpg作者: Feedback 時間: 2025-3-30 01:40
978-1-4899-9309-0Springer Science+Business Media New York 2012作者: 疼死我了 時間: 2025-3-30 06:22
,Gehirnakrobatik? – Sich selbst überlisten?,mpulsive phase and can last for a few tens of minutes to more than one hour. The few examples discussed in the literature indicate that such long-lasting submillimeter emission is most likely thermal bremsstrahlung. We present a detailed analysis of the time-extended phase of the 27?October?2003 (M6作者: 變形詞 時間: 2025-3-30 08:51
Konkrete Ausdrucks- und Umgangsformen,ticle acceleration. Two limb events were selected during which the radio emission was well correlated in time with hard X-rays. The radio emissions were of the type of decimetric pulsations as determined from the spectrogram observed by Phoenix-2 of ETH Zurich. The radio positions were measured from作者: 千篇一律 時間: 2025-3-30 12:22
Winfried Effelsberg,Hans Schadewaldtnts were obtained with a very high time resolution (80 microseconds) radio spectrograph in the 1352?–?1490?MHz range. These data were complemented with observations from the radio spectrograph at Ond?ejov in the 0.8?–?2.0?GHz band. We evaluated the basic characteristics of the individual spikes (dur作者: Ballerina 時間: 2025-3-30 16:38 作者: negligence 時間: 2025-3-30 22:34
Trauern in der modernen Gesellschaft, level of the chromosphere-corona transition region. The observations of short period (from one to ten minutes) oscillations in sunspots reflect propagation of magnetohydrodynamic (MHD) waves in the magnetic flux tubes of the sunspots. We investigate the oscillation parameters in active regions in c作者: PIZZA 時間: 2025-3-31 00:57 作者: 東西 時間: 2025-3-31 06:53
https://doi.org/10.1007/978-981-10-2089-6vent. The wave was observed with the EUVI instruments aboard both STEREO spacecraft (STEREO-A and STEREO-B) with a mean speed of ～?240?km?s.. The wave is more pronounced in the eastern propagation direction, and is thus, better observable in STEREO-B images. From STEREO-B observations we derive two 作者: CESS 時間: 2025-3-31 11:27
Stereo Scene Flow for 3D Motion Analysisned into shocks and freely propagated afterwards like decelerating blast waves that showed up as Moreton waves and EUV waves. We propose a simple quantitative description for such shock waves to reconcile their observed propagation with drift rates of metric type II bursts and kinematics of leading 作者: 羽毛長成 時間: 2025-3-31 15:58
Die Homographie zwischen zwei Ansichten,y connected off-limb and on-disk signatures. Veronig .. (.., L57, .) concluded that the dome was formed by a weak shock wave. We have revealed two EUV components, one of which corresponded to this transient. All of its properties found from EUV, white light, and a metric type II burst match expectat
