標題: Titlebook: Astrotomography; Indirect Imaging Met Henri M.J. Boffin,Jan Cuypers,Danny Steeghs Book 2001 Springer-Verlag Berlin Heidelberg 2001 Accretio [打印本頁] 作者: 軍械 時間: 2025-3-21 16:16
書目名稱Astrotomography影響因子(影響力)
書目名稱Astrotomography影響因子(影響力)學科排名
書目名稱Astrotomography網(wǎng)絡公開度
書目名稱Astrotomography網(wǎng)絡公開度學科排名
書目名稱Astrotomography被引頻次
書目名稱Astrotomography被引頻次學科排名
書目名稱Astrotomography年度引用
書目名稱Astrotomography年度引用學科排名
書目名稱Astrotomography讀者反饋
書目名稱Astrotomography讀者反饋學科排名
作者: 大氣層 時間: 2025-3-21 20:37 作者: corn732 時間: 2025-3-22 01:18
Foundation iPhone App Developments and the irradiation of the secondary star in all systems. The latter indirectly reveals such effects as shadowing by the accretion disc or stream. I discuss all of these and finish with some musings on possible future directions for the method. At the end I include a tabulation of Doppler maps pub作者: thwart 時間: 2025-3-22 07:12
Jordan Hamson-Utley,Errin Heymanthe Doppler tomography technique that relaxes one of the basic assumptions of tomography, and is able to map modulated emission sources. This extension allows us to fit anisotropic emission from, for example, spirals shocks, the irradiated companion star and disc-stream interaction sites.作者: 確保 時間: 2025-3-22 08:50
Foundation iPhone App Developmenton over the binary. I begin with a discussion of the basic principles behind Doppler tomography, including a comparison of the relative merits of maximum entropy regularisation versus filtered back-projection for implementing the inversion. Following this I discuss the issue of noise in Doppler imag作者: Concerto 時間: 2025-3-22 16:31
David Gibson,Kathryn Coleman,Leah Irvingobserved in previous UV and optical data. We find that the central spike contributes to the flare spectra indicating that its origin is probably the compact object. We also detect that the central spike moves with orbital phase following an S-wave pattern. The radial velocity semiamplitude of the S-作者: esoteric 時間: 2025-3-22 20:46
Melinda J. Lewis,Jason M. Lodgeuring our observations. All of them have visible mass donor stars allowing us to establish precise orbital phases. None of them show what is often thought of as the classic pattern of symmetric disc plus bright-spot at the gas stream/disc impact. Instead they have regions of emission at low velociti作者: Heart-Rate 時間: 2025-3-22 22:31 作者: 山間窄路 時間: 2025-3-23 05:09
Jordan Hamson-Utley,Errin Heymano resolve and map such co-rotating patterns and allows a straightforward comparison with theory. The dwarf nova IP Pegasi presents the best studied case, carrying two spiral arms in a wide range of emission lines throughout its outbursts. Both arms appear at the locations where tidally driven spiral作者: Irrigate 時間: 2025-3-23 05:49 作者: 宮殿般 時間: 2025-3-23 11:45
Martin Dietzfelbinger,Martin Hühne We do not include artificial nor α-viscosity and supply gas from the inner L1 point. We construct Doppler maps and artificial trailed spectrograms. In the 2D calculation, the results agree very well with those observed in IP Peg. In the 3D calculations, the stream from the L1 point penetrates into 作者: 清澈 時間: 2025-3-23 15:08 作者: Adulate 時間: 2025-3-23 18:29
https://doi.org/10.1007/978-3-0348-4121-4systems. Many examples show that the lines are composed not only from (symmetrical) disc emission, but that additional contribution is provided by isolated, i.e. asymmetric emission sources, distorting the original line profile. In this paper, we study the distribution of these additional components作者: 錯誤 時間: 2025-3-24 01:16 作者: 動物 時間: 2025-3-24 02:49 作者: gerrymander 時間: 2025-3-24 08:30 作者: 殺菌劑 時間: 2025-3-24 12:19 作者: Infiltrate 時間: 2025-3-24 17:31 作者: 指派 時間: 2025-3-24 20:27 作者: 高談闊論 時間: 2025-3-25 01:41
Foundational Papers in Oculoplasticsneously reconstructing the surface distribution of magnetic fieldv ectors andone chemical element from a time sequence of line profles measuredin four Stokes parameters. The application of the code to a well studied magnetic Ap star α2CVn recovereda field distribution, resembling an oblique dipole w作者: 發(fā)現(xiàn) 時間: 2025-3-25 06:04
Blepharospasm and Facial Dystoniaof the accretion zones on the white dwarf. Stokes imaging of Potter et al. [.] is the first objective and analytical technique that robustly models the cyclotron emission and maps the accretion zones..Polarisation modelling is discussed, followed by a summary of the Stokes imaging technique. We demo作者: 無目標 時間: 2025-3-25 09:41 作者: 記憶法 時間: 2025-3-25 12:03 作者: Ige326 時間: 2025-3-25 18:29
https://doi.org/10.1007/3-540-45339-3Accretion; astronomy; astrophysics; imaging; simulation; spectrography; telescopes; tomography作者: GONG 時間: 2025-3-25 20:34 作者: Enzyme 時間: 2025-3-26 01:05 作者: 死亡 時間: 2025-3-26 06:31 作者: acolyte 時間: 2025-3-26 09:04 作者: 任意 時間: 2025-3-26 14:58
,Spiral Waves in Accretion Discs— Theory,me classes of close binary stars, and more particularly in cataclysmic variables. In this paper, we review the physics of spirals waves in accretion discs, present the results of numerical simulations and consider whether theory can be reconcilied with observations.作者: 退潮 時間: 2025-3-26 19:02 作者: 死亡率 時間: 2025-3-26 21:50
The Geometrical Configuration of Polars and Possible Reconstruction Artefacts of Eclipse Mapping Me streams is more complicated than that of accretion disks in non-magnetic systems, it is essential to gain knowledge about the geometrical con.guration of such a system. Here, I give a summary of the parameters with which the geometry can be described. I present some reconstruction artefacs that can be the results of wrong geometrical parameters.作者: 高度贊揚 時間: 2025-3-27 05:02
Spot Mapping in Cool Stars,eview I outline the signal enhancement and indirect imaging techniques available for mapping spots on stellar surfaces. I review recent developments in the use of starspots as tracers of surface differential rotation, and discuss the way in which starspot lifetimes appear to scale with stellar luminosity class.作者: 消毒 時間: 2025-3-27 06:38
Astrotomography978-3-540-45339-0Series ISSN 0075-8450 Series E-ISSN 1616-6361 作者: 核心 時間: 2025-3-27 09:34 作者: liposuction 時間: 2025-3-27 15:17 作者: lobster 時間: 2025-3-27 18:21
https://doi.org/10.1007/978-3-0348-4121-4systems. Many examples show that the lines are composed not only from (symmetrical) disc emission, but that additional contribution is provided by isolated, i.e. asymmetric emission sources, distorting the original line profile. In this paper, we study the distribution of these additional components with several system parameters.作者: 流行 時間: 2025-3-27 23:52 作者: periodontitis 時間: 2025-3-28 05:05
Compiling and Running Java Programs,eview I outline the signal enhancement and indirect imaging techniques available for mapping spots on stellar surfaces. I review recent developments in the use of starspots as tracers of surface differential rotation, and discuss the way in which starspot lifetimes appear to scale with stellar luminosity class.作者: Acumen 時間: 2025-3-28 06:31
Doppler Tomography,on over the binary. I begin with a discussion of the basic principles behind Doppler tomography, including a comparison of the relative merits of maximum entropy regularisation versus filtered back-projection for implementing the inversion. Following this I discuss the issue of noise in Doppler imag作者: Lineage 時間: 2025-3-28 12:08
Mapping the Peculiar Binary GP Com,observed in previous UV and optical data. We find that the central spike contributes to the flare spectra indicating that its origin is probably the compact object. We also detect that the central spike moves with orbital phase following an S-wave pattern. The radial velocity semiamplitude of the S-作者: 棲息地 時間: 2025-3-28 18:20
,Hα-Emission Doppler Tomography of Long-Period Cataclysmic Variable Stars,uring our observations. All of them have visible mass donor stars allowing us to establish precise orbital phases. None of them show what is often thought of as the classic pattern of symmetric disc plus bright-spot at the gas stream/disc impact. Instead they have regions of emission at low velociti作者: Indolent 時間: 2025-3-28 20:56 作者: MIR 時間: 2025-3-28 23:54
,Spiral Waves in Accretion Discs— Observations,o resolve and map such co-rotating patterns and allows a straightforward comparison with theory. The dwarf nova IP Pegasi presents the best studied case, carrying two spiral arms in a wide range of emission lines throughout its outbursts. Both arms appear at the locations where tidally driven spiral作者: 令人悲傷 時間: 2025-3-29 04:13
,Spiral Waves in Accretion Discs— Theory,me classes of close binary stars, and more particularly in cataclysmic variables. In this paper, we review the physics of spirals waves in accretion discs, present the results of numerical simulations and consider whether theory can be reconcilied with observations.作者: 獎牌 時間: 2025-3-29 10:09
Spiral Shocks in an Inviscid Simulation of Accretion Flow in a Close Binary System, We do not include artificial nor α-viscosity and supply gas from the inner L1 point. We construct Doppler maps and artificial trailed spectrograms. In the 2D calculation, the results agree very well with those observed in IP Peg. In the 3D calculations, the stream from the L1 point penetrates into 作者: 引起 時間: 2025-3-29 13:37 作者: 中子 時間: 2025-3-29 15:53
Statistics of Isolated Emission Sources in Cataclysmic Variables,systems. Many examples show that the lines are composed not only from (symmetrical) disc emission, but that additional contribution is provided by isolated, i.e. asymmetric emission sources, distorting the original line profile. In this paper, we study the distribution of these additional components作者: 誘拐 時間: 2025-3-29 23:47
Tomography of Polars,M Herculis type, the so-called .. The three main ingredients of such systems, the donor star, the accretor and the accretion stream between the two stars, are investigated by Doppler tomography, Roche tomography and eclipse mapping methods. Future applications currently in development will include Z作者: Project 時間: 2025-3-30 02:06 作者: 輕觸 時間: 2025-3-30 04:42 作者: 群居動物 時間: 2025-3-30 11:00
Spot Mapping in Cool Stars,eview I outline the signal enhancement and indirect imaging techniques available for mapping spots on stellar surfaces. I review recent developments in the use of starspots as tracers of surface differential rotation, and discuss the way in which starspot lifetimes appear to scale with stellar lumin作者: Gentry 時間: 2025-3-30 14:30 作者: 表臉 時間: 2025-3-30 19:24 作者: 中和 時間: 2025-3-30 23:43
Magnetic Doppler Imaging of Chemically Peculiar Stars,neously reconstructing the surface distribution of magnetic fieldv ectors andone chemical element from a time sequence of line profles measuredin four Stokes parameters. The application of the code to a well studied magnetic Ap star α2CVn recovereda field distribution, resembling an oblique dipole w作者: Basilar-Artery 時間: 2025-3-31 02:37
Stokes Imaging of the Accretion Region in Magnetic Cataclysmic Variables,of the accretion zones on the white dwarf. Stokes imaging of Potter et al. [.] is the first objective and analytical technique that robustly models the cyclotron emission and maps the accretion zones..Polarisation modelling is discussed, followed by a summary of the Stokes imaging technique. We demo作者: 閃光東本 時間: 2025-3-31 06:38
Doppler Images of the M Dwarf RE 1816 +541,a large number of photospheric absorption lines, we use a sophisticated cross-correlation technique to derive absorption profiles with S/N ratios of 350. The surface images of RE 1816 +541 reveal a moderately spotted surface, with starspots appearing at all latitudes. We attempt to measure the surfa作者: essential-fats 時間: 2025-3-31 10:52 作者: 阻塞 時間: 2025-3-31 13:54 作者: DEMN 時間: 2025-3-31 18:54 作者: decipher 時間: 2025-3-31 23:06 作者: hankering 時間: 2025-4-1 03:53
The Method of Spectra Disentangling and Its Links to Doppler Tomography,ial velocities for known component spectra - was best solved by the cross-correlation technique. The method of Fourier disentangling solves simultaneously both parts of this problem in a very effective way. It is shown here that its principle can also be used for Doppler tomography.作者: syncope 時間: 2025-4-1 08:23 作者: 有偏見 時間: 2025-4-1 14:11
David Gibson,Kathryn Coleman,Leah Irvingsting that it forms in a high electron density region. This again favours the idea that the central spike originates in the white dwarf. We present Doppler maps obtained for the emission lines which show three clear emission regions.作者: 柔美流暢 時間: 2025-4-1 17:37 作者: Ganglion-Cyst 時間: 2025-4-1 22:19
Midfacial Aging – Deflation or Descent?e recovered with good accuracy, even if the phase coverage per rotation cycle is poor, provided the total data set is long enough. From observations of the HR 1099 K1 subgiant secured in 1998, 1999 and 2000, we obtain that the equator rotates faster than the pole with a rotational shear about 3 times smaller than solar.
