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Time-Resolved Spectroscopy of Q CYG

Published online by Cambridge University Press:  22 February 2018

S. Kafka ,
C. Tappert ,
R. K. Honeycutt  and
A. Bianchini
S. Kafka
Affiliation:
Astronomy Department, Indiana University, 319 Swain Hall West, Bloomington, IN 47405USA
C. Tappert
Affiliation:
Departamento de Física, Grupo de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile
R. K. Honeycutt
Affiliation:
Astronomy Department, Indiana University, 319 Swain Hall West, Bloomington, IN 47405USA
A. Bianchini
Affiliation:
Dipartimento di Astronomia, Università di Padova, Vicolo dell'Osservatorio 2, 1-35122 Padova, Italy

Extract

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A time-resolved optical spectroscopic study of the long-period (P=10.08h) old nova Q Cyg has revealed persistent yet erratic absorption features indicating the presence of a wind, while the system was rising to one of its stunded outbursts. Data taken with the WIYN 3.5m telescope show P Cygni profiles in the He I triplet lines at 5876Å and 7065Å, which are absent in the He I singlet emission line at 6678Å, despite the fact that the relevant energy levels of those three lines are at very similar excitation levels. The Hα line often has a red ward emission tail, characteristic of a receding outflow, and it possess a blueward absorption profile during only one wind event. Kafka et al. (2003) argued that this behavior is due to the strongly metastable 2 3S effective ground state of the He I triplets, which becomes over-populated in conditions of low density and a dilute radiation field, over-populating in turn the 23P common lower level of He I 5876Å and 7065Å, leading to absorption from a low density wind. Therefore, the triplet/singlet lines trace two different parts of the system: the wind and the disk respectively.

Type
The Contributed Papers
Information
International Astronomical Union Colloquium , Volume 194: Compact binaries in the galaxy and beyond , 2004 , pp. 237
Copyright
Copyright © Instituto de astronomia/revista mexicana de astronomίa y astrofίsica 2004

References

Kafka, S., Tappert, C., Honeycutt, R. K., & Bianchini, A. 2003, AJ, 126, 1472 Google Scholar
Cannizzo, J. K. & Cameron, A. G. W. 1988, ApJ, 330, 327 Google Scholar
Proga, D., Stone, J. M., & Drew, J. E. 1998, MNRAS, 295, 595 Google Scholar
Shlosman, I. & Vitello, P. 1993, ApJ, 409, 372 Google Scholar