標題: Titlebook: Cataclysmic Variables and Related Objects; Proceedings of the 1 A. Evans,Janet H. Wood Conference proceedings 1996 Kluwer Academic Publishe [打印本頁] 作者: FORAY 時間: 2025-3-21 17:38
書目名稱Cataclysmic Variables and Related Objects影響因子(影響力)
書目名稱Cataclysmic Variables and Related Objects影響因子(影響力)學科排名
書目名稱Cataclysmic Variables and Related Objects網(wǎng)絡(luò)公開度
書目名稱Cataclysmic Variables and Related Objects網(wǎng)絡(luò)公開度學科排名
書目名稱Cataclysmic Variables and Related Objects被引頻次
書目名稱Cataclysmic Variables and Related Objects被引頻次學科排名
書目名稱Cataclysmic Variables and Related Objects年度引用
書目名稱Cataclysmic Variables and Related Objects年度引用學科排名
書目名稱Cataclysmic Variables and Related Objects讀者反饋
書目名稱Cataclysmic Variables and Related Objects讀者反饋學科排名
作者: Resistance 時間: 2025-3-21 23:24
The Nova-Likes Ac Cnc, Rw Tri, Ux Uma and the Nova Dq Her: Common and Different Propertiesysis is based on simultaneous high-speed UBVRI photometry, covering several dozens of orbital cycles evenly distributed over 14 years (1982...1995) for DQ Her, and over 11 years (1985...1995) for the other three stars. All data have been obtained with the 1.25 m telescope at the Crimean Astrophysica作者: LARK 時間: 2025-3-22 01:47 作者: 脆弱么 時間: 2025-3-22 08:00
Applications of Indirect Accretion Disc Imaging to Orbital Solutions for Primary Stars is a problem for which there is no universally applicable solution. Velocity measurements are handicapped because the accretion disc about the primary often dominates the optical spectrum. Therefore spectroscopists resort to measuring line profile symmetry in individual spectra of the accretion dis作者: cavity 時間: 2025-3-22 10:25 作者: 嚙齒動物 時間: 2025-3-22 15:45
Studies in Flickering bother studying this ‘noise’? Three reasons come to mind: (i) flickering is a fundamental signature of accretion, to the point of being a necessary characteristic (if it doesn’t flicker, it’s not a CV); (ii) energetically, flickering is not a small effect and can contribute up to a few tens of perc作者: 嚙齒動物 時間: 2025-3-22 17:55
Decomposing Interacting Binary Light Curves: The Eclipses of the Mean Light, Secular Variability andnes the orbital dependence (including eclipses) of the mean light, secular variability and RMS flickering. We identify the true line of centres of RW Tri and find that the accretion disc is a location of secular variability and a source of flickering.作者: 彎腰 時間: 2025-3-22 23:08
The Place of Origin of the Flickering in Z Cha(iv) scintillation (negligible) and (v) any residual noise. Calculating the rms-scatter of the count rates in a light curve as a function of orbital phase, ?, through accretion disk eclipse of high inclination CVs — after subtraction of a smoothed light curve to remove orbital and long-term variatio作者: 無節(jié)奏 時間: 2025-3-23 02:50
TT Ari-94: A Study of 1.6...60 Minute Variabilityy range 10...900 cycle d. are found. The highest peaks in the power spectrum cover the wide range of 28...139 cycle d.. Variations occur at a few preferred time-scales rather than at one cycle length, with a possible secular decrease. In the frequency range 90...900 cycle d. the power spectrum obeys作者: Gustatory 時間: 2025-3-23 09:06
Time Resolved Optical Spectroscopy of V795 Herurce is examined using two-dimensional image analysis and Doppler reconstruction techniques on the orbital profiles. A clear S-wave modulation of a weak emission feature in the H? and Hγ line wings (extending to ~1800kms.) is present, with complex asymmetric properties.作者: 考博 時間: 2025-3-23 10:03 作者: 漫不經(jīng)心 時間: 2025-3-23 16:23
Dwarf Nova Outbursts and Superoutburstsapproach, of putting some constraints on α. In particular, the strong dependence of the viscous time-scale on viscosity itself permits us to estimate aα almost directly from the observed time-scales. In the case of the hot branch of the Σ - .. relation, the most reliable estimates (α.) are based on 作者: boisterous 時間: 2025-3-23 20:40
New Observational Frontiers of Er Uma (= PG 0943+521) Type Dwarf Novaethe extremely short recurrence time of the superoutburst (～ 40 d in ER UMa and V1159 Ori, ～ 20 d in RZ LMi), (ii) short outbursts with short recurrence times (～ 4 d) between the bright states, and (iii) extremely long duty cycles (～ 0.5). Assuming that the mass transfer rate from the secondary is te作者: Notorious 時間: 2025-3-23 22:37
Superhumps in the SU UMa Star AK CNC (Chile), Ouda Station (Kyoto, Japan) and in England. Superhumps with amplitude 0.2 mag appeared at least 4d after maximum. They evolved from a single peak structure, developing a secondary peak during decline, until they reached a double-wave modulation with 0.05 mag amplitude, after 8 d. After rem作者: 按等級 時間: 2025-3-24 02:49
Applications of Indirect Accretion Disc Imaging to Orbital Solutions for Primary Starsc in order to provide information on the primary’s motion. However, discs are not axisymmetric structures and the standard approach generally fails because the asymmetry-free inner disc emission is usually dominated by statistical noise.作者: sed-rate 時間: 2025-3-24 08:57
Studies in Flickeringent of the total luminosity of the system (hence it is often more luminous than the entire secondary star); (iii) flickering is inherently a time—dependent phenomenon and it is hoped that it can provide clues to the nature of the disc viscosity, something that time—independent theory cannot provide.作者: ear-canal 時間: 2025-3-24 12:50
Waveforms and Instrumentation Overview, (1990) in order to establish whether these systems are truely at large distances, or are instead a population of intrinsically faint objects lying relatively nearby. The distances were determined using Bailey’s method (1982) and incorporated the recent .. calibrations by Ramseyer (1994).作者: transplantation 時間: 2025-3-24 16:37 作者: CROAK 時間: 2025-3-24 22:42 作者: jeopardize 時間: 2025-3-25 00:41
Online Resolution of E-commerce Disputes996) showed that the light curves of these stars can be reproduced by the disk instability model, which does not require mass transfer bursts. These indicate that ER UMa, VI159 Ori and RZ LMi are not on the natural extension of SU UMa-type dwarf novae.作者: 依法逮捕 時間: 2025-3-25 03:57
Distances and Absolute Magnitudes of a Sample of Faint Cataclysmic Variables (1990) in order to establish whether these systems are truely at large distances, or are instead a population of intrinsically faint objects lying relatively nearby. The distances were determined using Bailey’s method (1982) and incorporated the recent .. calibrations by Ramseyer (1994).作者: hereditary 時間: 2025-3-25 10:48
The Place of Origin of the Flickering in Z Chaif eclipses take place (assuming any residual source of noise to be constant in time). The rms-scatter curve is then defined as the function . where σ. is the variance due to flickering and . the variance due to residual noise.作者: 混亂生活 時間: 2025-3-25 14:09 作者: 集聚成團 時間: 2025-3-25 19:10 作者: 偶像 時間: 2025-3-25 23:28
0067-0057 ral meetings in the area of CVs recently (e. g. Eilat, Abano-Padova, Capetown). However as preparations for the Keele meeting progressed we realized that, while there had been a number of IAU meetings devoted to related and to peripheral topics (such as IAU Colloquium 122 on Classical Novae in 1989,作者: 信任 時間: 2025-3-26 04:01
Enforcement of the ODR Outcomes,erred time-scales rather than at one cycle length, with a possible secular decrease. In the frequency range 90...900 cycle d. the power spectrum obeys a power law with slope γ ranging from 0.8 to 2.6 for different runs.作者: 遭遇 時間: 2025-3-26 06:45
TT Ari-94: A Study of 1.6...60 Minute Variabilityerred time-scales rather than at one cycle length, with a possible secular decrease. In the frequency range 90...900 cycle d. the power spectrum obeys a power law with slope γ ranging from 0.8 to 2.6 for different runs.作者: Entrancing 時間: 2025-3-26 12:07 作者: Explicate 時間: 2025-3-26 14:28 作者: lambaste 時間: 2025-3-26 17:41 作者: Abbreviate 時間: 2025-3-26 22:34 作者: 不可侵犯 時間: 2025-3-27 03:02
0067-0057 umentation, had led to many advances in both CV and LMXB research. The conference provided a forum to review observations from ASCA, EUVE, ROSAT, Ginga and the 978-94-010-6632-7978-94-009-0325-8Series ISSN 0067-0057 Series E-ISSN 2214-7985 作者: PLAYS 時間: 2025-3-27 08:35
Conference proceedings 1996r-relations between them. The meeting was held at a time when powerful satellite observatories, and rapid improvements in ground based instrumentation, had led to many advances in both CV and LMXB research. The conference provided a forum to review observations from ASCA, EUVE, ROSAT, Ginga and the 作者: formula 時間: 2025-3-27 09:52
Superhumps in the SU UMa Star AK CNCod P. = 0.065(2) d, using the relationship given by Howell & Hurst (1994). The eruption duration was ? 10 d, and its amplitude > 6 mag. An abrupt and short luminosity decrease occured ≈ 12 d after maximum. Eleven outbursts have been observed since 1992 January, being the minimum reported lag between作者: 禍害隱伏 時間: 2025-3-27 16:40 作者: 舊式步槍 時間: 2025-3-27 21:01 作者: 狂怒 時間: 2025-3-28 01:34 作者: critique 時間: 2025-3-28 04:05
Oscilloscope as a Diagnostic Tool, is a problem for which there is no universally applicable solution. Velocity measurements are handicapped because the accretion disc about the primary often dominates the optical spectrum. Therefore spectroscopists resort to measuring line profile symmetry in individual spectra of the accretion dis作者: 舊石器 時間: 2025-3-28 07:01 作者: CLOUT 時間: 2025-3-28 14:29 作者: 兩棲動物 時間: 2025-3-28 16:54 作者: EVADE 時間: 2025-3-28 21:10
Online Resolution of E-commerce Disputes(iv) scintillation (negligible) and (v) any residual noise. Calculating the rms-scatter of the count rates in a light curve as a function of orbital phase, ?, through accretion disk eclipse of high inclination CVs — after subtraction of a smoothed light curve to remove orbital and long-term variatio作者: induct 時間: 2025-3-28 23:22 作者: 繁榮中國 時間: 2025-3-29 03:58
https://doi.org/10.1007/978-3-030-54120-0urce is examined using two-dimensional image analysis and Doppler reconstruction techniques on the orbital profiles. A clear S-wave modulation of a weak emission feature in the H? and Hγ line wings (extending to ~1800kms.) is present, with complex asymmetric properties.作者: anesthesia 時間: 2025-3-29 09:07 作者: Pastry 時間: 2025-3-29 12:34 作者: 樂章 時間: 2025-3-29 18:36 作者: GEN 時間: 2025-3-29 20:37
Causes of Clefts of the Secondary Palate, (Chile), Ouda Station (Kyoto, Japan) and in England. Superhumps with amplitude 0.2 mag appeared at least 4d after maximum. They evolved from a single peak structure, developing a secondary peak during decline, until they reached a double-wave modulation with 0.05 mag amplitude, after 8 d. After rem作者: 有害處 時間: 2025-3-30 00:09 作者: 經(jīng)典 時間: 2025-3-30 05:34 作者: 假裝是你 時間: 2025-3-30 11:37 作者: NOT 時間: 2025-3-30 14:34
Studies in Systems, Decision and Controlhat Roche tomography can be successfully employed to image the secondary stars in CVs, and that it also serves as an independent aid for determining binary system parameters. Our preliminary results suggest that the mass of the white-dwarf primary is 1.2 M⊙, significantly higher than previous estimates.作者: elastic 時間: 2025-3-30 17:56
Online Resolution of E-commerce Disputesnes the orbital dependence (including eclipses) of the mean light, secular variability and RMS flickering. We identify the true line of centres of RW Tri and find that the accretion disc is a location of secular variability and a source of flickering.作者: 冷淡周邊 時間: 2025-3-30 21:29
https://doi.org/10.1007/978-3-030-54120-0urce is examined using two-dimensional image analysis and Doppler reconstruction techniques on the orbital profiles. A clear S-wave modulation of a weak emission feature in the H? and Hγ line wings (extending to ~1800kms.) is present, with complex asymmetric properties.作者: abduction 時間: 2025-3-31 04:42 作者: ineluctable 時間: 2025-3-31 06:35
https://doi.org/10.1007/978-3-030-53579-7We present a progress report on the analysis of time-resolved spectrophotometric observations of the cataclysmic variable V1315 Aql. The spectral range of the data covers the entire Balmer series up to and including the Balmer jump. We aim to use these data to test the steady-state accretion disk model.作者: EVADE 時間: 2025-3-31 10:15
https://doi.org/10.1007/978-3-030-53832-3We report first results of the HST/FOS time-resolved, low-resolution spectroscopy of the eclipsing cataclysmic variable UX UMa, including multi-wavelength mapping of its accretion disk in the ultraviolet region.作者: Common-Migraine 時間: 2025-3-31 15:38
https://doi.org/10.1007/978-3-030-54120-0IUE and optical data were obtained throughout the supercycles of RZ LMi and ER UMa during 1993/94. While most of the spectral and photometric characteristics are consistent with disk changes in systems with a relatively high accretion rate and low inclination, the cause of the high accretion rate in this subset of SU UMa stars is not known.作者: 疲憊的老馬 時間: 2025-3-31 19:32
Causes of Clefts of the Secondary Palate,We have created a database with outburst activity for 269 selected cataclysmic variables. It includes nearly 1000 outburst measurements discovered through 1995 June. The database and a complete paper describing the observations and the sources of information that were consulted are accessible over the Internet.作者: menopause 時間: 2025-3-31 23:27
Temperature Structure of the Disk in V1315 AqlWe present a progress report on the analysis of time-resolved spectrophotometric observations of the cataclysmic variable V1315 Aql. The spectral range of the data covers the entire Balmer series up to and including the Balmer jump. We aim to use these data to test the steady-state accretion disk model.作者: 尊重 時間: 2025-4-1 02:35
Spectrally Resolved Maps of Optically Thick Accretion DisksWe report first results of the HST/FOS time-resolved, low-resolution spectroscopy of the eclipsing cataclysmic variable UX UMa, including multi-wavelength mapping of its accretion disk in the ultraviolet region.作者: APEX 時間: 2025-4-1 06:16 作者: Aviary 時間: 2025-4-1 12:46
