High-resolution spectroscopy of the unique eclipsing binary system - Epsilon Aurigae

1986 ◽  
Vol 98 ◽  
pp. 637 ◽  
Author(s):  
M. Barsony ◽  
J. R. Mould ◽  
B. L. Lutz
Keyword(s):  
High Resolution ◽  
Binary System ◽  
High Resolution Spectroscopy ◽  
Eclipsing Binary ◽  
Epsilon Aurigae

scholarly journals ∊ Aur in eclipse: Post-AGB primary and disk-shaped secondary

2011 ◽  
Vol 7 (S283) ◽  
pp. 454-455
Author(s):  
Chinnathambi Muthumariappan ◽  
Mudumba Parthasarathy ◽  
Kanniah Jayakumar ◽  
Manickam Appakutty
Keyword(s):  
High Resolution ◽  
Binary System ◽  
Radiative Transfer ◽  
Transfer Problem ◽  
Line Profiles ◽  
Radiative Transfer Problem ◽  
Eclipsing Binary ◽  
Preliminary Results ◽  
Spectroscopic Monitoring

AbstractWe present physical and chemcal properties of the disk in the eclipsing binary system ∊ Aur by solving 2D radiative transfer problem. We also present preliminary results of our high resolution spectroscopic monitoring of K I, Na, and Hα line profiles variation during the totality phase of the recent eclipse of ∊ Aur.

scholarly journals CoRoT photometry and high-resolution spectroscopy of the interacting eclipsing binary AU Monocerotis

2010 ◽  
Vol 401 (1) ◽  
pp. 418-432 ◽  
Author(s):  
M. Desmet ◽  
Y. Frémat ◽  
F. Baudin ◽  
P. Harmanec ◽  
P. Lampens ◽  
...  
Keyword(s):  
High Resolution ◽  
High Resolution Spectroscopy ◽  
Eclipsing Binary

scholarly journals Long-term photospheric instabilities and envelopes dynamics in the post-AGB binary system 89 Herculis

2020 ◽  
Vol 500 (1) ◽  
pp. 926-941
Author(s):  
M Gangi ◽  
M Giarrusso ◽  
M Munari ◽  
C Ferrara ◽  
C Scalia ◽  
...  
Keyword(s):  
High Resolution ◽  
Binary System ◽  
Central Star ◽  
Asymptotic Giant Branch ◽  
High Resolution Spectroscopy ◽  
Time Interval ◽  
Radial Velocity Curve ◽  
Morphological Variations ◽  
Upper Level

ABSTRACT We present a long-term optical spectroscopic study of the post-asymptotic giant branch (AGB) binary system 89 Herculis, with the aim to characterize the relationship between photospheric instabilities and dynamics in the close circumstellar environment of the system. This study is based on spectra acquired with the high-resolution Catania Astrophysical Observatory Spectropolarimeter and archive data, covering a time interval between 1978 and 2018. We find long-term changes in the radial velocity curve of the system, occurring mostly in amplitude, which correlate with the variability observed in the blueshifted absorption component of the P Cygni-like H α profile. Two possible scenarios are discussed. We also find strong splitting in the s-process elements of Ba ii 6141.713- and 6496.898-Å  lines, with short-term morphological variations. A Gaussian decomposition of such profiles allows us to distinguish four shell components, two expanding and two infalling toward the central star, which are subject to the orbital motion of the system and are not affected by the long-term instabilities. Finally, we find that the numerous metal lines in emission could originate in regions of a structured circumbinary disc that have sizes proportional to the energy of the corresponding upper level transition Eup. This study demonstrates the potential of long-term high-resolution spectroscopy in linking together the instability processes occurring during the late evolutionary stages of post-AGBs and the subsequent phase of PNe.

scholarly journals The unusual binary HD 83058 in the region of the Scorpius-Centaurus OB association

2013 ◽  
Vol 9 (S302) ◽  
pp. 315-316 ◽  
Author(s):  
M. A. Pogodin ◽  
N. A. Drake ◽  
E. G. Jilinski ◽  
C. B. Pereira
Keyword(s):  
High Resolution ◽  
Binary System ◽  
Stellar Surface ◽  
High Resolution Spectroscopy ◽  
Line Profiles ◽  
Basic Parameters ◽  
Curve Solution

AbstractWe present the results of high-resolution spectroscopy of the binary system HD 83058 situated in the region of the Sco-Cen OB association. On the base of the radial-curve solution we have determined the elements of the orbit and determined the period P = 2.365102 days. We have disentangled the spectra of the two components of the system and derived the basic parameters of both components. We have shown that moving features in the Si iii line profiles seen in the spectra of the primary can be interpreted in the frame of the assumption of the rotation of local spot-like inhomogeneities on the stellar surface. We have also found that the lines in the spectrum of the secondary show another type of variability.

Microcalorimeters for X-Ray Spectroscopy

1988 ◽  
Vol 102 ◽  
pp. 41
Author(s):  
E. Silver ◽  
C. Hailey ◽  
S. Labov ◽  
N. Madden ◽  
D. Landis ◽  
...  
Keyword(s):  
High Resolution ◽  
High Efficiency ◽  
Thermal Response ◽  
Low Noise ◽  
High Resolution Spectroscopy ◽  
Superconducting Transition ◽  
Sapphire Substrates ◽  
Laboratory Plasmas ◽  
Adiabatic Demagnetization ◽  
Theoretical Predictions

The merits of microcalorimetry below 1°K for high resolution spectroscopy has become widely recognized on theoretical grounds. By combining the high efficiency, broadband spectral sensitivity of traditional photoelectric detectors with the high resolution capabilities characteristic of dispersive spectrometers, the microcalorimeter could potentially revolutionize spectroscopic measurements of astrophysical and laboratory plasmas. In actuality, however, the performance of prototype instruments has fallen short of theoretical predictions and practical detectors are still unavailable for use as laboratory and space-based instruments. These issues are currently being addressed by the new collaborative initiative between LLNL, LBL, U.C.I., U.C.B., and U.C.D.. Microcalorimeters of various types are being developed and tested at temperatures of 1.4, 0.3, and 0.1°K. These include monolithic devices made from NTD Germanium and composite configurations using sapphire substrates with temperature sensors fabricated from NTD Germanium, evaporative films of Germanium-Gold alloy, or material with superconducting transition edges. A new approache to low noise pulse counting electronics has been developed that allows the ultimate speed of the device to be determined solely by the detector thermal response and geometry. Our laboratory studies of the thermal and resistive properties of these and other candidate materials should enable us to characterize the pulse shape and subsequently predict the ultimate performance. We are building a compact adiabatic demagnetization refrigerator for conveniently reaching 0.1°K in the laboratory and for use in future satellite-borne missions. A description of this instrument together with results from our most recent experiments will be presented.

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