標(biāo)題: Titlebook: Angular Momentum Evolution of Young Stars; S. Catalano,J. R. Stauffer Book 1991 Springer Science+Business Media Dordrecht 1991 CCD.dynamic [打印本頁(yè)] 作者: lutein 時(shí)間: 2025-3-21 18:49
書(shū)目名稱(chēng)Angular Momentum Evolution of Young Stars影響因子(影響力)
書(shū)目名稱(chēng)Angular Momentum Evolution of Young Stars影響因子(影響力)學(xué)科排名
書(shū)目名稱(chēng)Angular Momentum Evolution of Young Stars網(wǎng)絡(luò)公開(kāi)度
書(shū)目名稱(chēng)Angular Momentum Evolution of Young Stars網(wǎng)絡(luò)公開(kāi)度學(xué)科排名
書(shū)目名稱(chēng)Angular Momentum Evolution of Young Stars被引頻次
書(shū)目名稱(chēng)Angular Momentum Evolution of Young Stars被引頻次學(xué)科排名
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書(shū)目名稱(chēng)Angular Momentum Evolution of Young Stars年度引用學(xué)科排名
書(shū)目名稱(chēng)Angular Momentum Evolution of Young Stars讀者反饋
書(shū)目名稱(chēng)Angular Momentum Evolution of Young Stars讀者反饋學(xué)科排名
作者: indices 時(shí)間: 2025-3-21 21:39 作者: 可互換 時(shí)間: 2025-3-22 00:36
Magnetic Activity and Rotationrefore, the various forms of magnetic activity manifestation are intimately connected with the internal structure and evolution of stars, hence with their age and rotation regime..The remarkable success achieved in understanding the general outline of magnetic activity requires, however, further obs作者: ARK 時(shí)間: 2025-3-22 04:39 作者: 一瞥 時(shí)間: 2025-3-22 11:41 作者: 使激動(dòng) 時(shí)間: 2025-3-22 16:57 作者: 圓木可阻礙 時(shí)間: 2025-3-22 17:41
Angular Momentum Effects in Star Formationis period, significant redistribution of angular momentum must occur in the star, as indicated by the substantial discrepancy between deduced angular momenta in star formation sites in the cores of molecular clouds and in the youngest optically visible stars. A major problem is the short time scale,作者: Thyroxine 時(shí)間: 2025-3-22 23:47
Small—Scale Structure and Angular Momentum Transfer in Protostellar Environments eddies of the turbulent cascade. We compute the probability distribution of the stochastic force and angular momentum fields induced by these eddies, assuming that the density and velocity correlation functions can be described as power laws. We also show that a point mass moving faster than the ve作者: 繁榮地區(qū) 時(shí)間: 2025-3-23 04:38 作者: 落葉劑 時(shí)間: 2025-3-23 06:28 作者: 持續(xù) 時(shí)間: 2025-3-23 12:06
Differential Rotation of Fully Convective Pre-Main Sequence Starsnsport coefficients. The models have a large scale circulation and differential rotation. Models with standard isotropic transport also have circulation and differential rotation; the circulation being driven by the latitudinal variation of convective and radiative heat flux in rotating stars in an 作者: Essential 時(shí)間: 2025-3-23 15:44 作者: hangdog 時(shí)間: 2025-3-23 18:51
Multifrequency Monitoring of RU Lupi: Observational Results and a Modelults and a first attempt of their interpretation. The various phenomena observed in RU Lupi can be explained in term of a disk accretion onto an young star with a moderately strong global magnetic field. The role of axial rotation is also discussed.作者: languid 時(shí)間: 2025-3-23 22:34 作者: Relinquish 時(shí)間: 2025-3-24 03:57 作者: 注意到 時(shí)間: 2025-3-24 07:17 作者: Alpha-Cells 時(shí)間: 2025-3-24 12:14
Rotational Velocities of Stars in Open Clusters: The Time Dependence Revisitedence of stellar rotation. The shape of the Vsini distribution is an extremely sensitive function of the α index of the braking law (dV/dt = -AV.). The comparison of Hyades + Praesepe and Pleiades observations favours the value . = 2. The Vsini distributions could not be reproduced with . = 3, the va作者: 抵制 時(shí)間: 2025-3-24 17:39 作者: Juvenile 時(shí)間: 2025-3-24 19:05 作者: gruelling 時(shí)間: 2025-3-25 03:10 作者: ASTER 時(shí)間: 2025-3-25 05:17
Rotation of Evolved Starsof evolved stars is slowed by moment-of-inertia increases and by magnetic braking. The observations are used to map out two magnetic and two acoustic domains related to the powering of chromospheres and magnetic braking. Within the magnetic domains, rotation and convection are presumed to interact r作者: 連鎖,連串 時(shí)間: 2025-3-25 08:20
Rotational Discontinuity of Evolved Stars: What Interpretation ? of about 1.0 km/s. As a result, the behaviour of the . distribution, as a function of colours and luminosity, is now well established..For the luminosity classes IV, III, II and Ib, the rotational discontinuity is now precisely defined and solid arguments inspire that the origin of this one is not 作者: Bronchial-Tubes 時(shí)間: 2025-3-25 12:06 作者: reserve 時(shí)間: 2025-3-25 18:10
Book 1991 1990 at Noto, Italy. The workshop had its immediate origin in a discussion about the availability of stel- lar rotation data, that took place in 1987 at Viana do Castelo Portugal during the NATO meeting, Formation and Evolution of Low Mass Stars. We recognized that nearly 20 years had passed since 作者: 衍生 時(shí)間: 2025-3-25 22:48 作者: ABIDE 時(shí)間: 2025-3-26 00:30
Economic Recovery After COVID-19ppropriate analytical techniques allows us to calculate the velocity field in the protostellar interior to the lowest order in a perturbative approach. The consequences for the evolution of an eventual protostellar magnetic field and of a magnetically coupled protostellar wind in the presence of this circulation are briefly discussed.作者: 責(zé)難 時(shí)間: 2025-3-26 06:57
Uncertainty and Austerity Policy,ures such as emission lines, association with dust clouds and reflection nebulosity, irregular variability, infrared excess and molecular line emission. These objects are recognized as representing a group of higher-mass analogs of the T Tauri stars.作者: Osteoporosis 時(shí)間: 2025-3-26 10:20 作者: 單獨(dú) 時(shí)間: 2025-3-26 14:19
Ekman Pumping in a Rotating Protostarppropriate analytical techniques allows us to calculate the velocity field in the protostellar interior to the lowest order in a perturbative approach. The consequences for the evolution of an eventual protostellar magnetic field and of a magnetically coupled protostellar wind in the presence of this circulation are briefly discussed.作者: 友好關(guān)系 時(shí)間: 2025-3-26 18:35
Polarimetry and CCD Imaging of Herbig Ae/Be Stars and Star Forming Regionsures such as emission lines, association with dust clouds and reflection nebulosity, irregular variability, infrared excess and molecular line emission. These objects are recognized as representing a group of higher-mass analogs of the T Tauri stars.作者: ungainly 時(shí)間: 2025-3-26 23:59
Rotation of Young Stars in the Orion Nebula Regione 10. years, and all are proper motion members. With 20 of the stars fully analyzed, there is no indication of extremely rapid rotation such as is seen among the K stars in the Pleiades. Typical . sin . values are 15–30 km s., and there is no apparent increase from younger to older stars as they approach the main sequence.作者: exclusice 時(shí)間: 2025-3-27 03:29
Small—Scale Structure and Angular Momentum Transfer in Protostellar Environmentslocity of the eddies’ system feels a net positive torque, and so its net angular momentum increases: the opposite happens to a particle moving with a velocity slower than the average. This mechanism of angular momentum transfer can be significant in the conditions observed in Molecular Clouds.作者: 精密 時(shí)間: 2025-3-27 07:33 作者: Anal-Canal 時(shí)間: 2025-3-27 10:33
Main Sequence Angular Momentum Loss in Low-Mass Starsfferential rotation and the relation of rotation to activity cycles. Finally, an observing program is outlined that could lead to significantly better understanding of angular momentum loss over the next few years.作者: BRACE 時(shí)間: 2025-3-27 14:41 作者: 婚姻生活 時(shí)間: 2025-3-27 19:36 作者: initiate 時(shí)間: 2025-3-27 22:10
Labor Markets and Economic Development,w rotators. This paper provides a brief review of the “classical” rotation studies of the 1960’s, an outline of the new discoveries of the 1980’s and their current interpretation, and a description of the outstanding problems that remain.作者: infatuation 時(shí)間: 2025-3-28 03:42
Rotational Velocities of Low Mass Stars in Young Clustersw rotators. This paper provides a brief review of the “classical” rotation studies of the 1960’s, an outline of the new discoveries of the 1980’s and their current interpretation, and a description of the outstanding problems that remain.作者: 不近人情 時(shí)間: 2025-3-28 10:02
https://doi.org/10.1007/978-94-011-1306-9locity of the eddies’ system feels a net positive torque, and so its net angular momentum increases: the opposite happens to a particle moving with a velocity slower than the average. This mechanism of angular momentum transfer can be significant in the conditions observed in Molecular Clouds.作者: 尖牙 時(shí)間: 2025-3-28 12:31
Migration Trend and Labor Market in Kosovoanalogous way to the driving of meridian circulation in radiative layers. Simple model calculations suggest that the differential rotation in pre-main sequence fully convective stars may be large and the stars may be heavily distorted.作者: 用不完 時(shí)間: 2025-3-28 14:39
Studies in Soviet History and Societyfferential rotation and the relation of rotation to activity cycles. Finally, an observing program is outlined that could lead to significantly better understanding of angular momentum loss over the next few years.作者: 運(yùn)動(dòng)吧 時(shí)間: 2025-3-28 21:17 作者: Hdl348 時(shí)間: 2025-3-29 01:27
https://doi.org/10.1007/978-1-349-09629-9the same for all classes. While for the subgiants the discontinuity seems to be the result of a magnetic braking, for the giants, that one results from a division between objects of significantly different ages. For the most luminous classes, the discontinuity results from the short duration of the first-crossing phase.作者: lymphedema 時(shí)間: 2025-3-29 03:17
International Political Economy Series appears as if intermediate mass stars are built via accretion of material from large (r ~ 300 AU), massive circumstellar disks (M ~ 1 M.) on timescales t < 1 Myr (for stars with M > 3 M.). The initial stellar angular momentum reflects a balance between the angular momentum added from accreting disk material, and that carried away by a wind.作者: 微枝末節(jié) 時(shí)間: 2025-3-29 08:41 作者: CROW 時(shí)間: 2025-3-29 13:19 作者: 管理員 時(shí)間: 2025-3-29 17:06
The X-Ray Emission from Pms Stars in Taurus-Auriga, and the Relationship with Other Diagnostics of Abetween the X-ray luminosity and the H-alpha emission, expressed as the ratio between the H-alpha and 25-micron far-infrared luminosity, indicator of disk emission. We argue that this indicates a real inhibition of the wind emission in the most X-ray active T Tauri stars and we suggest a picture in which this phenomenon is likely to take place.作者: CBC471 時(shí)間: 2025-3-29 20:06
Multifrequency Monitoring of RU Lupi: Observational Results and a Modelults and a first attempt of their interpretation. The various phenomena observed in RU Lupi can be explained in term of a disk accretion onto an young star with a moderately strong global magnetic field. The role of axial rotation is also discussed.作者: 出處 時(shí)間: 2025-3-30 00:31
Rotational Velocities of Stars in Open Clusters: The Time Dependence Revisitedence of stellar rotation. The shape of the Vsini distribution is an extremely sensitive function of the α index of the braking law (dV/dt = -AV.). The comparison of Hyades + Praesepe and Pleiades observations favours the value . = 2. The Vsini distributions could not be reproduced with . = 3, the value corresponding to the so-called t. law.作者: MORPH 時(shí)間: 2025-3-30 06:29 作者: 拉開(kāi)這車(chē)床 時(shí)間: 2025-3-30 11:59 作者: Neolithic 時(shí)間: 2025-3-30 15:11
Nato Science Series C:http://image.papertrans.cn/a/image/157522.jpg作者: Archipelago 時(shí)間: 2025-3-30 19:53
https://doi.org/10.1007/978-94-011-1306-9is period, significant redistribution of angular momentum must occur in the star, as indicated by the substantial discrepancy between deduced angular momenta in star formation sites in the cores of molecular clouds and in the youngest optically visible stars. A major problem is the short time scale,作者: exhilaration 時(shí)間: 2025-3-31 00:26 作者: Chauvinistic 時(shí)間: 2025-3-31 01:58
Economic Recovery After COVID-19 generates a meridional circulation (Ekman pumping) inside the protostar directed from the rotational poles to the equatorial plane. The adoption of appropriate analytical techniques allows us to calculate the velocity field in the protostellar interior to the lowest order in a perturbative approach作者: Recessive 時(shí)間: 2025-3-31 06:13
International Political Economy Seriesand masses of such circumstellar disks; 3) evidence for accretion through these disks and estimates of mass accretion rates; 4) the relation between mass accretion and mass outflows during early evolutionary phases; and 5) the timescales required for such disks to evolve from the massive, optically 作者: pus840 時(shí)間: 2025-3-31 09:32
Migration Trend and Labor Market in Kosovonsport coefficients. The models have a large scale circulation and differential rotation. Models with standard isotropic transport also have circulation and differential rotation; the circulation being driven by the latitudinal variation of convective and radiative heat flux in rotating stars in an 作者: 四目在模仿 時(shí)間: 2025-3-31 16:43 作者: Ophthalmologist 時(shí)間: 2025-3-31 21:00
Kristina Maric Gjorgjieva,Besnik Fetaiults and a first attempt of their interpretation. The various phenomena observed in RU Lupi can be explained in term of a disk accretion onto an young star with a moderately strong global magnetic field. The role of axial rotation is also discussed.作者: 疏遠(yuǎn)天際 時(shí)間: 2025-3-31 23:45 作者: Munificent 時(shí)間: 2025-4-1 05:20
Labor Markets and Economic Development,hat they were generally slow rotators. Due to the advent of new instrumental capabilities, a large body of data on the rotational velocities of low mass stars is now available. In particular, several nearby clusters have good rotational velocity data for low mass stars, allowing us to estimate the e作者: pericardium 時(shí)間: 2025-4-1 08:27
The Political Preconditions of Reform of rotation on the approach to the main sequence. Most of the stars are of 0.8 – 1.0 M., with apparent ages ranging from a few times 10. to a few time 10. years, and all are proper motion members. With 20 of the stars fully analyzed, there is no indication of extremely rapid rotation such as is see作者: 話 時(shí)間: 2025-4-1 11:31
Studies in Soviet History and Societyence of stellar rotation. The shape of the Vsini distribution is an extremely sensitive function of the α index of the braking law (dV/dt = -AV.). The comparison of Hyades + Praesepe and Pleiades observations favours the value . = 2. The Vsini distributions could not be reproduced with . = 3, the va作者: 不法行為 時(shí)間: 2025-4-1 16:09
Studies in Soviet History and Society that are responsible, yet rather few observations of good quality exist to delineate the rotation-age relation. The available data are here reviewed, including the existence of a rotation-age relation, its possible form, the statistics of rotation among solar-type stars, and other topics such as di作者: anatomical 時(shí)間: 2025-4-1 22:20
Studies in Soviet History and Society centrifugal wind excited by the high rotational velocity. The mechanism may be the same, in different physical conditions, independently of the age of the star. An important test in this respect is given by the components of late type close binaries rotating synchronously with the orbital motion. E作者: Evocative 時(shí)間: 2025-4-1 23:01
