標題: Titlebook: Cool Stars, Stellar Systems, and the Sun; Proceedings of the F Jeffrey L. Linsky,Robert E. Stencel Conference proceedings 1987 Springer-Ver [打印本頁] 作者: Hazardous 時間: 2025-3-21 18:20
書目名稱Cool Stars, Stellar Systems, and the Sun影響因子(影響力)
書目名稱Cool Stars, Stellar Systems, and the Sun影響因子(影響力)學(xué)科排名
書目名稱Cool Stars, Stellar Systems, and the Sun網(wǎng)絡(luò)公開度
書目名稱Cool Stars, Stellar Systems, and the Sun網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Cool Stars, Stellar Systems, and the Sun被引頻次
書目名稱Cool Stars, Stellar Systems, and the Sun被引頻次學(xué)科排名
書目名稱Cool Stars, Stellar Systems, and the Sun年度引用
書目名稱Cool Stars, Stellar Systems, and the Sun年度引用學(xué)科排名
書目名稱Cool Stars, Stellar Systems, and the Sun讀者反饋
書目名稱Cool Stars, Stellar Systems, and the Sun讀者反饋學(xué)科排名
作者: Excitotoxin 時間: 2025-3-21 21:35
Control Objectives and Strategies,ds of two close companions may also be important. For evolved binaries the energy probably is mainly gravitational, coming from the transfer of matter onto a compact star..Whatever the basic energy source, some energy appears in the form of fast electrons that are capable of generating intense radio作者: rectocele 時間: 2025-3-22 03:45 作者: admission 時間: 2025-3-22 05:57 作者: CHOIR 時間: 2025-3-22 11:08
The relation between the CA II K line-core flux density and the magnetic flux density on the sun,作者: VOK 時間: 2025-3-22 16:07
Shifts of the circular zeeman profile in small solar fluxtubes,作者: VOK 時間: 2025-3-22 19:34
Results of a southern radio survey of active chromosphere stars,作者: defray 時間: 2025-3-23 00:01 作者: 魯莽 時間: 2025-3-23 02:35
Control Objectives and Strategies,We derive and discuss relations between magnetic, X-ray, and Ca II H+K flux densities for a sample of G, K, and M dwarfs.作者: 骨 時間: 2025-3-23 05:38 作者: 不可接觸 時間: 2025-3-23 10:20 作者: FRAUD 時間: 2025-3-23 15:11
Magnetic fields on K and M dwarfs,Of seven late K and early M dwarfs, six were observed to have magnetic fields. No relationship was seen between effective temperature and either field strength or filling factor. Magnetic flux was observed not to be constant over this range of effective temperature.作者: 干旱 時間: 2025-3-23 21:47
Empirical relations between magnetic fluxes and atmospheric radiative losses for cool dwarf stars,We derive and discuss relations between magnetic, X-ray, and Ca II H+K flux densities for a sample of G, K, and M dwarfs.作者: 子女 時間: 2025-3-23 23:08
Broadband linear polarization and chromospheric CA II H and K emission in late-type main sequence sWe discuss correlations between broadband linear polarization, intrinsic stellar parameters, and Ca 11 H+K emission in G and K dwarfs.作者: 顯微鏡 時間: 2025-3-24 06:21
Measurements of stellar magnetic fields: Empirical constraints on stellar dynamo and rotational evoWe explore the implications of empirical stellar magnetic parameters for dynamo theories, stellar activity theories, and models of the evolution of stellar angular momentum.作者: 拋射物 時間: 2025-3-24 10:18
Design of Observer-based Controllers,ve been employed, producing a considerable body of data on the mean magnetic field strength in stellar active regions (B) and the fraction (filling factor = f) of the stellar surface covered by these fields (f) for G, K, and M dwarfs. I focus on some of the recent results of observational programs a作者: Gudgeon 時間: 2025-3-24 12:44 作者: 懶鬼才會衰弱 時間: 2025-3-24 16:07 作者: 諷刺滑稽戲劇 時間: 2025-3-24 21:46
Control Objectives and Strategies,gnetic fields in a wide class of stars has been greatly improved. Calculations of large scale (global) magnetic fields will be presented that utilize sequences of models of a rotating star (the Sun) that take into account differential rotation and meridional circulation. The influence of various mag作者: antedate 時間: 2025-3-25 00:04 作者: 完整 時間: 2025-3-25 07:14
Control Objectives and Strategies,ve energy generated in stellar convection zones may be largely carried away by flux tube waves, which then become important sources for the heating of the outer atmospheric layers. We report calculations for longitudinal tube waves generated in magnetic flux tubes embedded in an otherwise magnetic f作者: outer-ear 時間: 2025-3-25 07:37
Control Objectives and Strategies,the assumption that the embedded magnetic fields are uniform. In contradiction with previous results, we show that there is no significant increase in the efficiency of wave generation because of the presence of magnetic fields, at least within the theory‘s limits of applicability. Thus, we show tha作者: Measured 時間: 2025-3-25 13:06
Control Objectives and Strategies, radio emission is indicative of high energy, nonthermal processes: acceleration of electrons to some 10‘s of keV or, in some circumstances, several MeV or more. These electrons then emit radio waves by the incoherent processes of gyroresonance and gyrosynchrotron radiation, and the coherent process作者: bioavailability 時間: 2025-3-25 19:10 作者: Jocose 時間: 2025-3-25 21:43
Use Case Study of Grid Computing with CGSPof the Sun, and which have not yet been widely observed at radio wavelengths. At 20 cm, two bands centered at 1415 and 1515 MHz are observed and at 6 cm, two bands centered at 4535 and 4985 MHz are observed. Results so far, based on a total observing time of about one hour each during July 1986 have作者: Antimicrobial 時間: 2025-3-26 00:24 作者: Seminar 時間: 2025-3-26 05:25 作者: 創(chuàng)新 時間: 2025-3-26 08:34 作者: overshadow 時間: 2025-3-26 13:17
Cool Stars, Stellar Systems, and the Sun978-3-540-48041-9Series ISSN 0075-8450 Series E-ISSN 1616-6361 作者: 獨行者 時間: 2025-3-26 19:34 作者: 動脈 時間: 2025-3-26 22:29
Flux tube dynamics and solar/stellar redshift measurements,n. These downflows could be the result either of the cooling and downfall of material in coronal loops or of the steady end-to-end flow of plasma in smaller loops. Time-dependent numerical simulations suggest that the steady flow explanation is the most likely.作者: 即席 時間: 2025-3-27 04:22
The photospheric magnetic fields of cool stars: Recent results of survey and time-variability progrve been employed, producing a considerable body of data on the mean magnetic field strength in stellar active regions (B) and the fraction (filling factor = f) of the stellar surface covered by these fields (f) for G, K, and M dwarfs. I focus on some of the recent results of observational programs a作者: 作繭自縛 時間: 2025-3-27 07:47
Flux tube dynamics and solar/stellar redshift measurements,n. These downflows could be the result either of the cooling and downfall of material in coronal loops or of the steady end-to-end flow of plasma in smaller loops. Time-dependent numerical simulations suggest that the steady flow explanation is the most likely.作者: Malaise 時間: 2025-3-27 12:48
Calibration on the sun for stellar magnetic fields,roperty to detect the presence of global magnetic fields on sun - like stars. We have obtained a large number of K line profiles over a variety of plages on the sun and related the 1A emission flux centred at the K3 minimum for these profiles with the corresponding values of the longitudinal compone作者: obeisance 時間: 2025-3-27 17:26
Large scale solar and stellar magnetic fields,gnetic fields in a wide class of stars has been greatly improved. Calculations of large scale (global) magnetic fields will be presented that utilize sequences of models of a rotating star (the Sun) that take into account differential rotation and meridional circulation. The influence of various mag作者: 彎曲的人 時間: 2025-3-27 21:24
The dynamics of solar magnetic flux tubes subjected to resonant foot point shaking,isplacements of solar surface regions of much larger than granular size with a periodicity of the five minute oscillation. We investigate the time-dependent development of waves in thin magnetic flux tubes generated by this purely transverse foot point shaking. The resulting magnetic field and veloc作者: 有助于 時間: 2025-3-28 01:27 作者: NIB 時間: 2025-3-28 04:00
MHD wave energy fluxes for late-type dwarfs,the assumption that the embedded magnetic fields are uniform. In contradiction with previous results, we show that there is no significant increase in the efficiency of wave generation because of the presence of magnetic fields, at least within the theory‘s limits of applicability. Thus, we show tha作者: 招致 時間: 2025-3-28 07:04
Nonthermal phenomena in stellar coronae: Evidence from radio observations, radio emission is indicative of high energy, nonthermal processes: acceleration of electrons to some 10‘s of keV or, in some circumstances, several MeV or more. These electrons then emit radio waves by the incoherent processes of gyroresonance and gyrosynchrotron radiation, and the coherent process作者: Cholesterol 時間: 2025-3-28 11:50 作者: CRASS 時間: 2025-3-28 17:41
A VLA survey of dMe flare stars,of the Sun, and which have not yet been widely observed at radio wavelengths. At 20 cm, two bands centered at 1415 and 1515 MHz are observed and at 6 cm, two bands centered at 4535 and 4985 MHz are observed. Results so far, based on a total observing time of about one hour each during July 1986 have作者: Lumbar-Spine 時間: 2025-3-28 20:27 作者: 同時發(fā)生 時間: 2025-3-29 02:49 作者: Decongestant 時間: 2025-3-29 03:06 作者: octogenarian 時間: 2025-3-29 08:35
Control Objectives and Strategies,sequences of models of a rotating star (the Sun) that take into account differential rotation and meridional circulation. The influence of various magnetic field configurations and strengths will be considered as well as the possible effect of the Lorentz force on the equations of motion.作者: pulmonary 時間: 2025-3-29 12:30 作者: amenity 時間: 2025-3-29 19:33
Use Case Study of Grid Computing with CGSPcm, two bands centered at 4535 and 4985 MHz are observed. Results so far, based on a total observing time of about one hour each during July 1986 have yielded detections from 9 of the 27 stellar systems in the program.作者: maintenance 時間: 2025-3-29 21:41
The photospheric magnetic fields of cool stars: Recent results of survey and time-variability progrctor = f) of the stellar surface covered by these fields (f) for G, K, and M dwarfs. I focus on some of the recent results of observational programs aimed at surveying magnetic parameters on a broad range of stars and studying the time-variability of B and f.作者: LARK 時間: 2025-3-30 01:42 作者: 個人長篇演說 時間: 2025-3-30 05:05
Large scale solar and stellar magnetic fields,sequences of models of a rotating star (the Sun) that take into account differential rotation and meridional circulation. The influence of various magnetic field configurations and strengths will be considered as well as the possible effect of the Lorentz force on the equations of motion.作者: 飾帶 時間: 2025-3-30 10:41
The dynamics of solar magnetic flux tubes subjected to resonant foot point shaking,endent development of waves in thin magnetic flux tubes generated by this purely transverse foot point shaking. The resulting magnetic field and velocity variations, the pressure and temperature fluctuations generated by nonlinear coupling to the longitudinal wave mode, as well as the expected resonance effects are discussed.作者: 免費 時間: 2025-3-30 14:04
A VLA survey of dMe flare stars,cm, two bands centered at 4535 and 4985 MHz are observed. Results so far, based on a total observing time of about one hour each during July 1986 have yielded detections from 9 of the 27 stellar systems in the program.作者: intrude 時間: 2025-3-30 20:23 作者: Fulsome 時間: 2025-3-30 23:24
Dae-Hee Seo,Deok-Gyu Lee,Im-Yeong Leeo concerning the escape of the radiation through the strongly absorbing second harmonic layer. It is suggested that stellar bursts are likely to consist of narrowband drifting structures, and that observations to test this suggestion are desirable.作者: Entrancing 時間: 2025-3-31 04:39 作者: Introduction 時間: 2025-3-31 05:09 作者: 畸形 時間: 2025-3-31 10:17
Control Objectives and Strategies,function of the magnetic field strength. We also present wave flux calculations for magnetic flux tubes embedded in the solar convective zone; the main result is that the longitudinal tube wave fluxes are at least 2 orders of magnitude too low to play a significant role in the heating of the solar chromosphere.作者: Asymptomatic 時間: 2025-3-31 17:13 作者: 鞠躬 時間: 2025-3-31 20:02 作者: 百靈鳥 時間: 2025-4-1 01:29
MHD wave energy fluxes for late-type dwarfs,free atmosphere, and do not vary enough for a given spectral type in order to explain observed UV and X-ray fluxes. Thus, our results show that MHD energy fluxes obtained if stellar surface magnetic fields are uniform cannot explain the observed stellar coronal emissions.作者: Finasteride 時間: 2025-4-1 05:40 作者: 豎琴 時間: 2025-4-1 08:39
Lecture Notes in Computer Sciencehttp://image.papertrans.cn/b/image/185610.jpg作者: anchor 時間: 2025-4-1 11:30
Book 2015quality illustrations, with emphasis on those aspects of most relevance to differential diagnosis. In addition, prognostic features are fully covered. ? Urological Pathology: Rare Tumors and Tumor-Like Conditions will be ideal source of core information and practical guidance for residents, fellows, pathologists, urologists, and oncologists.作者: 有節(jié)制 時間: 2025-4-1 18:16
Stochastikunterricht in den Jahrgangsstufen 5 und 6,2 und 2.3). Dazu geh?ren die Herangehensweise an die Analyse stochastischer Situationen, das Planen und Durchführen statistischer Erhebungen und die Auswertung von Daten in Tabellen und Diagrammen sowie die Ausbildung inhaltlicher Vorstellungen zum Wahrscheinlichkeitsbegriff.
