標題: Titlebook: Cataclysmic Variables. Recent Multi-Frequency Observations and Theoretical Developments; Proceedings of IAU C H. Drechsel,Y. Kondo,J. Rahe [打印本頁] 作者: TEMPO 時間: 2025-3-21 16:49
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書目名稱Cataclysmic Variables. Recent Multi-Frequency Observations and Theoretical Developments影響因子(影響力)學科排名
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書目名稱Cataclysmic Variables. Recent Multi-Frequency Observations and Theoretical Developments被引頻次
書目名稱Cataclysmic Variables. Recent Multi-Frequency Observations and Theoretical Developments被引頻次學科排名
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書目名稱Cataclysmic Variables. Recent Multi-Frequency Observations and Theoretical Developments年度引用學科排名
書目名稱Cataclysmic Variables. Recent Multi-Frequency Observations and Theoretical Developments讀者反饋
書目名稱Cataclysmic Variables. Recent Multi-Frequency Observations and Theoretical Developments讀者反饋學科排名
作者: 付出 時間: 2025-3-21 23:36 作者: insular 時間: 2025-3-22 01:22 作者: GROG 時間: 2025-3-22 07:11
Spectroscopy of the Primary and Secondary Components of the Dwarf Nova AH Herculisossible to calculate the relative contributions of the primary and secondary to the total light at the wavelength of Na D as a function of the exact spectral subtype of the secondary, using the measured equivalent width of the Na D lines. Taking the spectral gradient of primary and secondary from th作者: 顯而易見 時間: 2025-3-22 09:57
Conference proceedings 1987Colloguium No. 93, held in Bamberg from the 16th to 19th of June 1986. In all, 157 astronomers from 27 countries participated in this conference. Judging from the papers presented, both invited and contributed, and from the enthusiasm seen in discussions, the meeting was indeed a success.作者: 煤渣 時間: 2025-3-22 15:36 作者: 煤渣 時間: 2025-3-22 18:25 作者: 容易做 時間: 2025-3-23 01:05
Cataclysmic Variables. Recent Multi-Frequency Observations and Theoretical Developments978-94-009-3801-4作者: Epidural-Space 時間: 2025-3-23 02:04
there existed a strong, shared feeling among the workers in this field that an international colloquium sponsored by the International Astronomical Union would be timely. To be more specific, this was due primarily to the accumulation of the new data from satellite observatories, such as the Intern作者: 秘傳 時間: 2025-3-23 06:44 作者: Cryptic 時間: 2025-3-23 10:21 作者: Neuropeptides 時間: 2025-3-23 15:04
https://doi.org/10.1007/978-3-030-58872-4pass through the observed light centre of the bright spot eclipse. The light centre is defined as the point corresponding to the half flux points in the ingress and egress of the eclipse of the compact part of the bright spot. The theoretical stream width indicates that the centre of the stream must intersect the bright spot close to this point.作者: Contort 時間: 2025-3-23 21:29 作者: Derogate 時間: 2025-3-24 02:10
,The “Return” from the Transcendental,ge during quiescence. A delay in the progress of normal outbursts toward higher frequencies confirms the delay, seen with IUE, in the onset of a normal outburst toward higher frequencies. Just after outburst, the system is substantially bluer than later in quiescence.作者: Comprise 時間: 2025-3-24 04:51 作者: Flu表流動 時間: 2025-3-24 08:07 作者: 主講人 時間: 2025-3-24 10:59
Observations of Eclipsing Dwarf Novaepass through the observed light centre of the bright spot eclipse. The light centre is defined as the point corresponding to the half flux points in the ingress and egress of the eclipse of the compact part of the bright spot. The theoretical stream width indicates that the centre of the stream must intersect the bright spot close to this point.作者: AMOR 時間: 2025-3-24 16:15 作者: extinguish 時間: 2025-3-24 20:23
Long-Term Optical Photometry of the Dwarf Nova VW HYIge during quiescence. A delay in the progress of normal outbursts toward higher frequencies confirms the delay, seen with IUE, in the onset of a normal outburst toward higher frequencies. Just after outburst, the system is substantially bluer than later in quiescence.作者: Antagonism 時間: 2025-3-25 00:55 作者: 想象 時間: 2025-3-25 04:36
Alexei Gvishiani,Anatoly Solovievline profiles lie within the range of model spectra of optically thick and stationary accretion disks with stellar atmosphere characteristics. The different behavior of the far UV spectral indices can be explained by the excess radiation from an extended and optically thick boundary layer, which depends mainly on the orbital inclination.作者: 粘連 時間: 2025-3-25 10:10
Continuum Distributions and Line Profiles of Ux Uma-Type Novalike Systemsline profiles lie within the range of model spectra of optically thick and stationary accretion disks with stellar atmosphere characteristics. The different behavior of the far UV spectral indices can be explained by the excess radiation from an extended and optically thick boundary layer, which depends mainly on the orbital inclination.作者: Credence 時間: 2025-3-25 15:43
Wolfgang Bacsa,Revathi Bacsa,Tim Myers modulation, the double profile and recently discovered UBV light variations support an inclination angle i ~ 50°. The masses of the primary and secondary stars using this angle and the observed semiamplitudes are Mp = 0.60 M(c) and M. = 0.40 M., respectively. A detailed analysis of the absorption lines reveals a spectral type of K2V.作者: CALL 時間: 2025-3-25 17:43
https://doi.org/10.1007/978-3-030-59273-8minimum of SS Cyg..There are various investigations of SS Cyg, but up to now the cause of its variability, in particular, its rapid variability has not been determined. In addition, there are many other observations which have not been explained.作者: visual-cortex 時間: 2025-3-26 00:01 作者: Immobilize 時間: 2025-3-26 01:39
Some Notes On SS Cygniminimum of SS Cyg..There are various investigations of SS Cyg, but up to now the cause of its variability, in particular, its rapid variability has not been determined. In addition, there are many other observations which have not been explained.作者: 為現(xiàn)場 時間: 2025-3-26 08:14 作者: 山羊 時間: 2025-3-26 10:11
Radio Emission from Cataclysmic Variablesbserved radio emission are also discussed. These suggest that the red dwarf in AM Her and DQ Her is also magnetized and provides support for theories for the evolution of CVs which require a magnetized secondary star.作者: archaeology 時間: 2025-3-26 13:25
https://doi.org/10.1007/978-3-030-58144-2first detailed look at a freshly accreted white dwarf photosphere. The effective temperatures of CV white dwarfs plotted versus orbital period for each type of CV appears to reveal a tendency for the cooler white dwarf primaries to reside in the shorter period systems. Possible implications are briefly discussed.作者: Locale 時間: 2025-3-26 17:39
Anjia Wang,Xinyao Yi,Yonghong Yanbserved radio emission are also discussed. These suggest that the red dwarf in AM Her and DQ Her is also magnetized and provides support for theories for the evolution of CVs which require a magnetized secondary star.作者: amplitude 時間: 2025-3-26 21:20 作者: Fecal-Impaction 時間: 2025-3-27 02:19
978-94-010-8191-7Springer Science+Business Media Dordrecht 1987作者: 情節(jié)劇 時間: 2025-3-27 07:23
Anjia Wang,Xinyao Yi,Yonghong Yanomponent. Mass exchange leads to cataclysmic events in such systems. The rate of semidetached low- mass close binary formation is 5xl0. yr. if the accreting component is a He degenerate dwarf, 5xl0. yr. if it is a CO-dwarf and 3x10. yr. if it is a neutron star. Systems with compact accretors arise a作者: STEER 時間: 2025-3-27 12:20 作者: 厚顏 時間: 2025-3-27 16:35
https://doi.org/10.1007/978-3-030-58144-2nt implications and clues about the nature and long-term evolution of cataclysmic variables can emerge from an analysis of their physical properties. Detection of the underlying white dwarfs has led to a preliminary empirical CV white dwarf temperature distribution function and, in a few cases, the 作者: myalgia 時間: 2025-3-27 18:16 作者: Maximizer 時間: 2025-3-28 01:53
https://doi.org/10.1007/978-3-030-58144-20–130 min) with those directly above (P=190– 240 min). Significant differences are found in the mean U-B,V-J colors and in the Hβ equivalent widths on the 2 sides of the gap. A detailed comparison from UV-IR of 3 high inclination novalike systems with periods near 3.3 hr (PG1012-029,PG1030+590 and V作者: 無畏 時間: 2025-3-28 04:49
Tiago H. Moreira de Oliveira,Marco Painholysmic variables have been identified and new observations of one already known object have been accumulated. Observations in the visible and UV-region show variability and differences in spectral type.If compared to the numbers of cataclysmic variables/white dwarfs as computed by Ritter and Burkert作者: headlong 時間: 2025-3-28 06:32
https://doi.org/10.1007/978-3-030-58872-4he two stars in each system. The mass ratio, q, and inclination, i, are found by constraining theoretical stream trajectories (Lubow and Shu 1975) to pass through the observed light centre of the bright spot eclipse. The light centre is defined as the point corresponding to the half flux points in t作者: 嫻熟 時間: 2025-3-28 14:24
Alexei Gvishiani,Anatoly Solovievclysmic system PHL 227 were determined from multi-wavelength spectroscopic and photometric data to search for general characteristics of these systems. The observed variations of the UV to IR spectral indices are qualitatively very similar for all systems, whereas the absolute values show significan作者: maculated 時間: 2025-3-28 16:01 作者: byline 時間: 2025-3-28 22:18
Wolfgang Bacsa,Revathi Bacsa,Tim Myersith a complex profile. The intensity of the Hβ line appears to be modulated by the orbital period. Radial velocity measurements of the wings of Hβ and of the absorption line system of the late-type star yield semiamplitude values of K. = 101 ± 6 km s. and Kab = 151 ± 7 km s., respectively. Radial ve作者: 立即 時間: 2025-3-29 02:09 作者: 蛙鳴聲 時間: 2025-3-29 03:42
https://doi.org/10.1007/978-3-030-59273-8ge outburst of SS Cyg can probably be explained using a model of a double star which is surrounded by an absorbing gaseous shell. It is noted that the existing data are not numerous enough for the explanation of the SS Cyg variability, in particular, its short-term variations..SS Cyg is a spectrosco作者: FUME 時間: 2025-3-29 08:26 作者: 羽毛長成 時間: 2025-3-29 15:29 作者: 官僚統(tǒng)治 時間: 2025-3-29 18:52 作者: 委屈 時間: 2025-3-29 20:45 作者: BALK 時間: 2025-3-30 00:58 作者: Insubordinate 時間: 2025-3-30 06:47
Anjia Wang,Xinyao Yi,Yonghong YanFrom about 30 Dwarf Novae with the best determined distances the following relationships are found..This final correlation is interpreted in terms of the disc instability model of dwarf novae and successfully predicts the observed width of outburst versus P relationship.作者: bronchiole 時間: 2025-3-30 09:18
https://doi.org/10.1007/978-3-030-58144-2The present status of the period studies of cataclysmic variables is briefly reviewed, mainly from the observational point of view. A few comments on individual objects include EM Cyg, Z Cha, WZ Sge and AM CVn.作者: 錯 時間: 2025-3-30 14:25
https://doi.org/10.1007/978-3-030-58969-1We describe a method for imaging the accretion disc of a Cataclysmic Variable star. We use the two-dimensional information contained in the line profiles as they vary with phase to invert the line formation process. Asymmetries in the disc, as are caused by the bright-spot, for example, are accounted for naturally.作者: 起草 時間: 2025-3-30 19:41 作者: indubitable 時間: 2025-3-30 21:12 作者: neuron 時間: 2025-3-31 01:17
The Periods of Cataclysmic VariablesThe present status of the period studies of cataclysmic variables is briefly reviewed, mainly from the observational point of view. A few comments on individual objects include EM Cyg, Z Cha, WZ Sge and AM CVn.作者: 可行 時間: 2025-3-31 08:52
Mapping the Line Emission Distribution of Cataclismic Variable StarsWe describe a method for imaging the accretion disc of a Cataclysmic Variable star. We use the two-dimensional information contained in the line profiles as they vary with phase to invert the line formation process. Asymmetries in the disc, as are caused by the bright-spot, for example, are accounted for naturally.作者: chalice 時間: 2025-3-31 09:40 作者: 松緊帶 時間: 2025-3-31 15:40
Multi-Wavelength Observations of Dwarf Novae During Outburstst. Six objects were caught during the rise, and a short flare was detected in SU UMa. It lasted 20 hours and reached a maximum increase of 3.6 in flux at 5500 A. The flare was simultaneous at all observed wavelengths.作者: 他一致 時間: 2025-3-31 18:01 作者: 乳白光 時間: 2025-3-31 22:29
Tiago H. Moreira de Oliveira,Marco Painholysmic variables have been identified and new observations of one already known object have been accumulated. Observations in the visible and UV-region show variability and differences in spectral type.If compared to the numbers of cataclysmic variables/white dwarfs as computed by Ritter and Burkert (1985)there is a shortage of a factor of 5.作者: insipid 時間: 2025-4-1 05:13 作者: interior 時間: 2025-4-1 06:20
https://doi.org/10.1007/978-3-030-59273-8by (1) poor choices of lines for measuring its velocity and (2) large distortions in its velocity caused by heating from the white dwarf and its accretion disk. The correct . velocity of the center of mass of the K5 V star is 158 ± 3 ...作者: ingestion 時間: 2025-4-1 10:35 作者: Atmosphere 時間: 2025-4-1 18:15
