hα observations on the be binary ζ tauri first some introduction words asking for patience by...
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![Page 1: Hα observations on the Be binary ζ Tauri First some introduction words asking for patience by Ernst Pollmann VdS Spectroscopy Group Germany](https://reader035.vdocuments.us/reader035/viewer/2022070403/56649f325503460f94c4d782/html5/thumbnails/1.jpg)
Hα observations on the Be binary ζ Tauri
First some introduction wordsasking for patience
by Ernst PollmannVdS Spectroscopy Group Germany
![Page 2: Hα observations on the Be binary ζ Tauri First some introduction words asking for patience by Ernst Pollmann VdS Spectroscopy Group Germany](https://reader035.vdocuments.us/reader035/viewer/2022070403/56649f325503460f94c4d782/html5/thumbnails/2.jpg)
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![Page 3: Hα observations on the Be binary ζ Tauri First some introduction words asking for patience by Ernst Pollmann VdS Spectroscopy Group Germany](https://reader035.vdocuments.us/reader035/viewer/2022070403/56649f325503460f94c4d782/html5/thumbnails/3.jpg)
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The binary system Tau
Development of a rotating one-armed density wave by disturbed orbits
Due to a radial disturbance the gas particles of the disk are moving on excentric Kepler-orbits
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Temporal development of the H-profile
(2003/09 to 2007/03)
Dispersion = 27Ǻ/mmR= λ/λ ≈ 14000
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Temporal development of the Hα-profile between 2000 and 2006
All Profiles from 2000-2006. The vertical offset is proportional to time and corresponds to 25 days per continuum unit. The lowermost spectra date from Nov./2000 (left), Sep./2002 (middle) and Aug./2004 (right).
The spectra are published electronically in the form of ASCII-tables IBVS-Nr. 5813
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![Page 6: Hα observations on the Be binary ζ Tauri First some introduction words asking for patience by Ernst Pollmann VdS Spectroscopy Group Germany](https://reader035.vdocuments.us/reader035/viewer/2022070403/56649f325503460f94c4d782/html5/thumbnails/6.jpg)
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Hα equivalent widths of ζ Tau since 1975
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Enlargement of the previous figure showing the data presented in this work in greater detail, also for comparison between values taken with
professional and amateur equipment.
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Development of a rotating one-armed density wave by disturbed orbits
Due to a radial disturbance the gas particles of the disk are moving on excentric Kepler-orbits
This leads to V/R-variations
V/R of Hα show the same period as the radial velocies
Period duration = 1500 d
V/R-Variation as function of phase
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![Page 9: Hα observations on the Be binary ζ Tauri First some introduction words asking for patience by Ernst Pollmann VdS Spectroscopy Group Germany](https://reader035.vdocuments.us/reader035/viewer/2022070403/56649f325503460f94c4d782/html5/thumbnails/9.jpg)
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![Page 10: Hα observations on the Be binary ζ Tauri First some introduction words asking for patience by Ernst Pollmann VdS Spectroscopy Group Germany](https://reader035.vdocuments.us/reader035/viewer/2022070403/56649f325503460f94c4d782/html5/thumbnails/10.jpg)
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The measured values vs. Julian date (open symbols) and the sine wave with P = 1471 d (plus signs).
Hα V/R-ratio
The residuals of the left panel, folded with P = 69.3 d and the respective sine fit. Shown are 1.4 cycles for clarification, i.e. 40% of the points are redundant.
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Causes of the V/R variations
V/R variations in binary stars may be locked to the orbital phase
follow quasi-cyles typical 5-10 years
or combines these two types of variations with long-term trends
length and amplitude of the quasi-cycle vary from cycle to cycle
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Conditions of the synchronisation of the V/R variations with the orbital periods ?
Several peculiarities of emission lines and their profiles can hardly be explained with one-armed oscillation model
Questions of the V/R variations
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Phase variations of the radial velocity of the HeI line 6678 and H-V/R (1)
(1) Stefl/Okazaki/Rivinius/Baade: V/R- Variations of binary Be stars (ASP-Conference Series, Vol. 361, 2007)
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Radial velocity of the HeI line 6678Ǻ
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…thanks for attention….
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